DARTS/Astro Query System - ADQL Search -

All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "ADQL Search".

Call example

【Basic Syntax】

 SELECT {*|column, column,...}
 [ TOP number ]
 FROM table name]
 [ WHERE conditions ]
 [ ORDER BY column, column,... ]
 ;

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This is an example query to obtain the first 10 rows of 
akari_fis_bsc_1 using radial search.

The akari_fis_bsc_1 is an catalogue, and each data has 
the coorinate position of the object. So, search the objects 
contained in the circle area you specify there.

Columns to display -> all
  Table name -> akari_fis_bsc_1
  Search condition -> radial search, 
   center position is (180.0, 60,0) and radius is 2 degree
  Displayed results -> from 1st to 10th

---------------------------------------------------------
Point:
  You can use functions of
  ADQL(http://www.ivoa.net/documents/latest/ADQL.html)
  on this system.

Data types:
    Point   ... POINT(coordinate, coordinate)
    Circle  ... CIRCLE(POINT(), radius)
    Polygon ... POLYGON(POINT(), POINT(), ...)

Operators:
    CONTAINS(a, b) = 1 ... a is contained by b
    CONTAINS(a, b) = 0 ... a is not contained by b
    INTERSECTS(a, b) = 1 ... overlaped each other
    INTERSECTS(a, b) = 0 ... do not overlaped each other

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This is an example query to obtain the first 10 rows of 
asca_observation_log using radial search.

The ASCA GIS has circular field of view with 22 arcmins 
as radius. Each data of asca_observation_log has the coordinate 
position of the center of the field of view. So, search the 
data overlaped with the two circles, the field of view and 
your specified one.

Columns to display -> all
  Table name -> asca_observation_log
  Search condition -> radial search, 
  center position is (122.0, -37,5) and radius is 2 degree
  Displayed results -> from 1st to 10th

---------------------------------------------------------
Point:
  You can use functions of
  ADQL(http://www.ivoa.net/documents/latest/ADQL.html)
  at this system.

Data types:
    Point   ... POINT(coordinate, coordinate)
    Circle  ... CIRCLE(POINT(), radius)
    Polygon ... POLYGON(POINT(), POINT(), ...)

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This is an example query to obtain the data near the 
galactic center of suzaku_xis_observation_log using radial search.
The SUZAKU XIS has rectanglar field of view with 18 arcmin 
x 18 arcmin. Each data of suzaku_xis_observation_log has the
coorinate of each corner position about field of view.
So, search the rectanglar area overlapd the circle area
you specified.

Columns to display -> all
  Table name -> suzaku_xis_observation_log
  Search condition -> radial search,
  center position is (0.0, 0.0) with Galactic coordinates
    and radius is 1 arcmin
  Displayed results -> from 1st to 200th

---------------------------------------------------------
Point:

1. Use the column of Galactic coordinates.

2. You can use functions of 
  ADQL(http://www.ivoa.net/documents/latest/ADQL.html)
  at this system.

Data types:
    Point   ... POINT(coordinate, coordinate)
    Circle  ... CIRCLE(POINT(), radius)
    Polygon ... POLYGON(POINT(), POINT(), ...)

---------------------------------------------------------

This is an example query to obtain the data near the
galactic center of suzaku_xis_observation_log using radial search.

The SUZAKU XIS has rectanglar field of view with 18 arcmin
x 18 arcmin. Each data of suzaku_xis_observation_log has the
coorinate of each corner position about field of view.
So, search the rectanglar area overlapd the rectanglar area
you specified.

Columns to display -> object_name, center_galactic_lon,
    center_galactic_lat, data_access_url
  Table name -> suzaku_xis_observation_log
  Search condition -> rectanglar search, 
    0.1(deg) <= Galactic Latitude <= .0.1(deg)
    and 0.1(deg) <= Galactic Latitude <= 0.1(deg)
  Displayed results -> from 1st to 100th

---------------------------------------------------------
Point:

1. Use the column of Galactic coordinates.

2. You can use functions of
   ADQL(http://www.ivoa.net/documents/latest/ADQL.html)
  at this system.

Data types:
	Point   ... POINT(coordinate, coordinate)
	Circle  ... CIRCLE(POINT(), radius)
	Polygon ... POLYGON(POINT(), POINT(), ...)

Operators:
	CONTAINS(a, b) = 1 ... a is contained by b
	CONTAINS(a, b) = 0 ... a is not contained by b
	INTERSECTS(a, b) = 1 ... overlaped each other
	INTERSECTS(a, b) = 0 ... do not overlaped each other

---------------------------------------------------------

This is an example query to obtain the first 10 rows of 
akari_fis_bsc_1 using radial search.

The akari_fis_bsc_1 is an catalogue, and each data has 
the coorinate position of the object. So, search the objects 
contained in the circle area you specify there.

Columns to display -> all
  Table name -> akari_fis_bsc_1
  Search condition -> radial search, 
   center position is (180.0, 60,0) and radius is 2 degree
  Displayed results -> from 1st to 10th

---------------------------------------------------------
Point:
  You can use functions of
  ADQL(http://www.ivoa.net/documents/latest/ADQL.html)
  on this system.

Data types:
    Point   ... POINT(coordinate, coordinate)
    Circle  ... CIRCLE(POINT(), radius)
    Polygon ... POLYGON(POINT(), POINT(), ...)

---------------------------------------------------------

This is an example query to obtain the first 10 rows of 
asca_observation_log using radial search.

Columns to display -> all
  Table name -> asca_observation_log
  Search condition -> radial search, 
  center position is (122.0, -37,5) and radius is 2 degree
  Displayed results -> from 1st to 10th

---------------------------------------------------------
Point:
  You can use functions of
  ADQL(http://www.ivoa.net/documents/latest/ADQL.html)
  at this system.

Data types:
    Point   ... POINT(coordinate, coordinate)
    Circle  ... CIRCLE(POINT(), radius)
    Polygon ... POLYGON(POINT(), POINT(), ...)

---------------------------------------------------------

---------------------------------------------------------
Point:

1. Use the column of Galactic coordinates.

2. You can use functions of 
  ADQL(http://www.ivoa.net/documents/latest/ADQL.html)
  at this system.

Data types:
    Point   ... POINT(coordinate, coordinate)
    Circle  ... CIRCLE(POINT(), radius)
    Polygon ... POLYGON(POINT(), POINT(), ...)

---------------------------------------------------------

This is an example query to obtain the data near the
galactic center of suzaku_xis_observation_log using radial search.

---------------------------------------------------------
Point:

1. Use the column of Galactic coordinates.

2. You can use functions of
   ADQL(http://www.ivoa.net/documents/latest/ADQL.html)
  at this system.

Data types:
	Point   ... POINT(coordinate, coordinate)
	Circle  ... CIRCLE(POINT(), radius)
	Polygon ... POLYGON(POINT(), POINT(), ...)

Operators:
	CONTAINS(a, b) = 1 ... a is contained by b
	CONTAINS(a, b) = 0 ... a is not contained by b
	INTERSECTS(a, b) = 1 ... overlaped each other
	INTERSECTS(a, b) = 0 ... do not overlaped each other

---------------------------------------------------------

ADQL query

Format

total 171

Translate to SQL Download WgetScript

No.	proposal_id	proposal_code	proposal_code_with_piname	pi_name	observation_category	observation_phase	proposal_title	proposal_abstruct	proposal_access_url
1	11	FISCA	FIS_CAL	FIS CAL
2	110	AGNUL	NAKAGAWA_AGNUL	Nakagawa, Takao (ISAS/JAXA)	MP	1&2	Evolution of ULIRGs and AGNs	We propose to study the evolution of ULIRGs (ultra luminous infrared galaxies) and AGN (active galactic nuclei) using the ASTRO-F observations. Our proposal consists of several observation programs, which can be categorized into two; one is detailed study of nearby ULIRGs and AGN as templates, and the other is an investigation of the evolution of these objects toward mid- to high-z on the basis of the knowledge obtained in the local universe.\nFor the detailed study near-by ULIRGs and AGNs, we propose to make systematic spectroscopic observations of PAH features in ULIRGs and AGNs in near-infrared to make the quantitative estimate of star-formation activity in these dusty systems. These observations are to make the best use of the imaging spectroscopy over wide spectral regions, which is a unique capability of ASTRO-F. We also study Spectral Energy Distribution of representative objects in several types using the all sky survey data.\nThe other category is the study of the evolution of ULIRGs and AGNs to mid- and high-z universe. We plan number-count studies in a hierarchical manner; the number count study based on the allsky survey is useful especially for the study of the evolution in mid-z universe, and medium deep survey with multiple observations in the survey mode and deep surveys in the slow scan mode are useful for the study of universe with higher z. We also propose slit-less spectroscopic observations as the rst un-biassed 3-D survey in the infrared.\nThe proposed infrared observations are essential for the study of ULIRGs and dusty AGNs because a large fraction of emitted energy in these galaxies are reemitted by dust in the thermal infrared. The unique capability of ASTRO-F will enable us to make the rst systematic study of the evolution of dusty universe.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
3	112	AGNUL	NAKAGAWA_AGNUL	Nakagawa, Takao (ISAS/JAXA)	MP	3	Revealing inner structure and energyr sources of ULIRG/AGN	We propose systematic AKARI/IRC 2-5 micron spectroscopic observations of ULIRG (Ul- tra Luminous Infrared Galaxies) and obscured AGNs (Activi Galactic Nucleis) to reveal(1) energy sources in ULIRGs and (2) inner structure around buried AGN. NIR 2-5 micron wavelength is a unique wavelength region which contains unique features enabling us to dis- tinguish between a buried AGN and a extreme starburst. This has been clearly demonstrated during the phase-2 observations by the combination of AKARI, Subaru, and SPITZER ob- servations. Phase-2 observations with IRC also showed us that some galaxies have wide CO molecule absorption. This indicated the existence very warm (~1000K) molecular clouds, which could be identified as evidence of putative molecular torus. AKARI/IRC is the only instrument which enables sensitive NIR spectroscopic observations covering 2-5 micron with- out the effect of the atmosphere of the earth. Our target list consists of several categories, and the combination will enable us to study the role of luminous buried AGNs as function of infrared luminosity. If previously more infrared luminous galaxies evolve into currently more massive galaxies, and if we find that luminous buried AGNs are more common in galaxies with higher infrared luminosities, then we may be able to provide the first observational support for the AGN-feedback scenario as the origin of the galaxy-downsizing. Our prelim- inary analysis of incomplete sample suggests that the importance of buried AGNs appears to increase with increasing infrared luminosity. It is extremely important to confirm this results, from a statistically significant number of sample, if we are to test the AGN-feedback scenario as the origin of the galaxy down-sizing phenomena.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
4	112	AGNUL	NAKAGAWA_AGNUL	Nakagawa, Takao (ISAS/JAXA)	MP	3-II	Systematic study of ULIRGs and AGN by AKARI/IRC spectroscopy	We propose a systematic spectral study of Ultraluminous infrared galaxies (ULIRGs) and luminous infrared galaxies (LIRGs) in the local universe.\nThe primary goals of this proposal are to (1) determine the star-formation rates and ages, (2) search for buried AGN and determine their contribution to the bolometric luminosity, and (3) prove physical conditions in the circum-nuclear region of AGN.\nSince most of the targets are heavily obscured, AKARFs unique near-infrared spectroscopic capability is indispensable for the current project.Together with our previous MP programs, the current study will provide an unprecedented spectroscopic database of a complete sample of luminous infrared galaxies in the local Universe.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
5		AGNMO	ENYA_AGNMO	Enya, Keigo (ISAS/JAXA)	MP	3	Infrared monitoring of Active Galactic Nuclei for dust reverbration search	We propose infrared monitorinf of z=0.4-1.6 Active Galactic Nuclei (AGN) by AKARI. The primary purpose of this observation is the search of dust reverberation to obtain unique information to understand structure and emitting mechanism of AGN. AKARI is needed, and the most suitable telescope for this work because infrared (2-4 micron at rest frame) monitoring of AGN close to the North Ecliptic Pole (NEP) is essential. For this study, extensive pre-observation with ground based telescope has been executed from 1995. 1) Near-IR variability of 200 AGN was investigated with 1.3m telescope at ISAS/JAXA. 2) Dust reverberation has been newly found and studied in nearby ADN by multicolor monitoring in optical and near-IR by the MAGNUM telescope. 3) Pre-monitoring at optical wavelength by the MAGNUM telescope has been executed for the targets of this MP observation, and promising variability was confirmed. This study needs about 1 pointings/month for 13 objects with IRC camera with AOTZ03. Long span of the observations is important, (2-3 years or more). The results of this work will be also useful for calibration of IRC, and the determination of distance to AGN and the cosmological parameter.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
6	134	QSONG	LEE_QSONG	Lee, HyungMok (Seoul National University)	MP	3-II	QSO Spectroscopic Observation with NIR Grism 2	We propose to continue our Phase-3 Mission Program, QSONG to obtain additional NIR Grism/Prism spectra of 43 low redshift bright PG QSOs, and 100 high redshift QSOs at z >3.4. The wavelength region between 2.5-5.0 //m contains a wealth of information on QSOs, but difficulties of accessing such a wavelength regime have hampered studies of spectra at the important spectral window. At low redshift, the 2.5-5.0 /zm window offers opportunities to study NIR Hydrogen lines which can give new insights into the AGN physics and also potentially provide useful AGN diagnostics for studying dust reddened systems. At high redshift, the H-alpha and H-beta lines - the popular estimators of the black hole mass 一 redshifts into 2.5-5.0 micron, making one to rely on much less robust mass estimators such as UV lines. By obtaining the 2.5-5.0 micron spectra of a carefully selected low redshift and high redshift QSOs, we will(i) assemble QSO spectra at the rarely studied wavelength regions of 2.5-5 micron; (ii) study the NIR Hydrogen lines such as Br, Br, and P as diagnostics to understand the nature of the Supermassive Black Holes (SMBHs); (iii) examine whether there is a trace of star formation activities in their host galaxies through PAH features, and (iv) study the mass evolution of the SMBHs at high redshift to today. The spectroscopic study of hundreds of high redshift QSOs will enable us to understand the evolution and the census of SMBHs in QSOs at high redshift.\nOur study will also provide a uniform, extensive set of the rest-frame 2.5-5.0 micron spectra of QSOs for the first time, which can serve as a strong basis for the future studies of the less-extinct rest-frame NIR Hydrogen lines to understand the nature of distant QSOs.\nThe combined number of QSOs will be 229 for high redshift sample, and 122, providing a dataset of Legacy value until the launch of JWST.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
7	114	AGNMO	ENYA_AGNMO	Enya, Keigo (ISAS/JAXA)	MP	3-II	AGN monitor with AKARI/IRC	We propose infrared monitoring of z=0.4-1.6 Active Galactic Nuclei (AGN) by AKARI. The primary purpose of this observation is the search of dust reverberation to obtain unique information to understand structure and emitting mechanism of AGN. AKARI is needed, and the most suitable telescope for this work because infrared (2-4 micron at rest frame) monitoring of AGN close to the North Ecliptic Pole (NEP) is essential. Our proposing observation is essentially same to the observation of the AGN monitor in the Phase 3-1 MP (AGNMO), i.e., this is a proposal to continue the monitoring. For this study, pre-observation with ground based telescope have been executed from 1995. 1)Near-IR variability of 200 AGN was inves- tigated with 1.3m telescope at ISAS/JAXA. 2) Dust reverberation has been newly found and studied in nearby AGN by multicolor monitoring in optical and near-IR by the MAGNUM telescope. 3) Pre-monitoring at optical wavelength by the MAGNUM telescope has been executed for the targets of this MP observation, and promising variability was confirmed. 4) the first detection of AGN variability by AKARI is going to be confirmed using the data of the Pahse 3-1 MP. This study needs 1 pointings/month for 6 objects with IRC camera with AOTZ03. Long span of the observations is important, (2-3 years or more). The results of this work will be also useful for calibration of IRC, and the determination of distance to AGN and the cosmological parameter.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
8	120	FBSEP	MATSUURA_FBSEP	Matsuura, Shuji (ISAS/JAXA)	MP	1&2	ASTRO-F Observations of Cosmic Far-Infrared Background Radiation and Distant Infrared Galaxies in Low-Cirrus Region near South Ecliptic Pole	We propose the ASTRO-F observations of the cosmic far-infrared background radiation (CFIRB) and its fluctuation, resolving the background into point sources as much as possible. Objectives of this program are to provide, 1) accurate source counts avoiding the cosmic variance and extended source counts toward fainter flux below the confusion limit of the ASTRO-F telescope (~10 mJy) by the background fluctuation analysis, in order to probe infrared galaxies at z>1, 2) angular power spectrum of the background fluctuation to study clustering and large-scale structure traced by infrared galaxies at z~1, 3) statistically significant number of source samples for the study of evolution and emission mechanism of infrared galaxies including ULIRG and AGN, and finally, 4) mean flux level of CFIRB minimizing the contribution of foreground galaxies. In order to accomplish these tasks, we plan deep and wide survey in the lowest column density region near the south ecliptic pole, in which the best sensitivity in the far-infrared can be achieved. The survey area of more than 15 square degrees will be mapped out by the FIS slow-scan observations in the four wave bands with the sensitivity better than the confusion limit. To identify the far-infrared background sources and discriminate the population of detected galaxies, the IRC slow-scan observations in mid-infrared bands will also be done in parallel to the FIS observations. The optical observations of R<25mag in the FIS survey area have been planned and partly finished. These efforts are still on-going, and another optical follow-up in multi-bands from the ground are being planned.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
9	121	FISS3	KAWADA_FISS3	Kawada, Mitsunobu (Nagoya University)	MP	1&2	FIS Serendipitous Spectroscopic Survey	We propose to operate the Fourier Transform Spectrometer (FTS) of the FIS at the pointing observations allocated for the IRC. It is expected that the FIS and the IRC works very well simultaneously, although the FOVs of both instruments are separated. The IRC is operated in the stealing mode of the attitude control system. In that case, the detection limit for each photometric band of the FIS achieves source confusion limit quickly, and there are no spatial information in sub-pixel scale. Then, the spectroscopic observation by using the FTS is effective with the IRC observations. In this proposal, we never request the additional pointing observations. We propose the operation of the FTS at the IRC observations proposed by other MPs. The observation is not systematic nor complete. If the FTS is operated at the large area surveys near the NEP, we expected to take rather systematic and complete datasets. According to the recent FTS performance, we can take spectra with full resolution by averaging with all pixels only for regions in \|b\| < 15deg. If we use the low resolution mode of the FTS, we can take spectral energy distributions with spectral resolution of 2.5cm-1 for a few Jy sources or for regions with surface brightness of about 10 MJy/sr by averaging all pixels. This sensitivity is improved by multiple observations or by reducing the spectral resolution. Using the dataset of this MP , we can discuss about the interstellar medium and, hopefully, Cosmic Infrared Background Radiation.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
10	122	FBSEP	MATSUURA_FBSEP	Matsuura, Shuji (ISAS/JAXA)	MP	3	IRC follow-up observations of the AKARI Deep Field South (ADF-S)	We propose IRC multi-band imaging follow-up observations of the AKARI Deep Field South (ADF-S), where we have carried out a far-infrared deep survey with the AKARI/FIS.\n\nDeep galaxy survey in the far-infrared provide us with a powerful tool to investigate the evolution of luminous infrared galaxies and the star-formation history in the Universe, since they measure thermal emission from dust heated by the UV light from massive stars. They also play an important role in tracing the large-scale structure and the cosmic infrared background measuring the clustering of luminous infrared galaxies.\n\nFor these purposes, we have carried out deep surveys at 65, 90,140 and 160 microns with the FIS instrument onboard the AKARI satellite. In order to minimize the contamination from the Galactic cirrus emission, we selected the region near the South Ecliptic Pole where the cirrus density is the lowest in the whole sky (AKARI Deep Field South; ADF-S).\n\nThe area of the survey is ~12 deg2. We have successfully detected almost 1700 galaxies in a wide flux range from a few Jy down to ~20 mJy at 90 um, and almost 300 galaxies down to ~180 mJy at 140 um. Galaxy number counts are useful to constrain the evolution scenario of galaxies. Our counts from the ADF-S show a significant evolution at the faint end, which is found to be a factor of 2-3 higher than no-evolution model predictions, and suggest that currently accepted galaxy evolution models should be modified.\n\nIn order to investigate the nature of the detected galaxies such as spectral energy distributions and redshifts, we propose a multi-band near-infrared imaging observation with the IRC instrument in the AKARI warm mission term. This multi-band imaging will enable us to estimate photometric redshifts and will be the only way to identify the detected far-infrared sources. Moreover, since ADF-S is continuous and large enough to contain large scale structures at z~1,we can examine the environmental dependence of various physical properties of galaxies. Especially, we can examine how the ratio between the star-formation rate (SFR) and the stellar mass of galaxies (specific SFR) varies with different environments, because the former is traced by FIR luminosity and the latter by NIR luminosity, respectively.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
11	122	FBSEP	MATSUURA_FBSEP	Matsuura, Shuji (ISAS/JAXA)	MP	3-II	IRC follow-up observations of the AKARI Deep Field South (ADF-S)	We propose follow-up observations with IRC multi-band imaging of the AKARI Deep Field South (ADF-S), where we have carried out a far-infrared deep survey with the AKARI/FIS. Far-infrared galaxy surveys provide us with a powerful tool to investigate the star-formation history in the Universe, because they measure thermal emission from dust heated by the UV light from massive stars. Far-infrared surveys also play an important role in tracing the large- scale structure, measuring the cosmic infrared background and analysis of the clustering of luminous infrared galaxies.\nFor these purposes, we have carried out a deep survey at 65, 90,140, and 160 microns with the FIS instrument onboard the AKARI satellite. In order to minimize the contamination from the Galactic cirrus emission, we selected the lowest cirrus density region near the South Ecliptic Pole as a survey field (AKARI Deep Survey South: ADF-S). The area of the survey is ~12 deg2. This survey is unique in having continuous wavelength coverage across four photometric bands including wavelengths not well explored by previous missions, and contiguous mapping in an unprecedentedly wide area.\nWe have successfully detected almost 2000 galaxies down to ~10 mjy at 90 um, and measured infrared colors for about 500 of them. Galaxy counts provide useful constraints for the evolution scenario of galaxies and/or SEDs of galaxies. The galaxy counts obtained in the ADFS require a significant modification of currently accepted models of infrared galaxy evolution, mainly because of the lower counts found at the 90 um band.\nIn order to investigate the nature of detected galaxies such as the spectral energy distributions and redshifts, we propose multi-band near-infrared imaging with the IRC instrument in AKARI warm mission term. This multi-band imaging will enable us the estimation of photometric redshifts and will be the only way to identify the detected far-infrared sources. Moreover, since ADF-S is enough continues and wide to include the large scale structure at z~1,we can discuss the environmental effect that the clustering gives the ratio of star-formation rate (SFR) and the mass assembly, which are traced by FIR luminosity and NIR luminosity, respectively.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
12	124	CNIRB	MATSUURA_CNIRB	Matsuura, Shuji (ISAS/JAXA)	MP	1&2	ASTRO-F Observations of Cosmic Near-Infrared Background Radiation	We propose observations of cosmic near-infrared background radiation (CNIRB) by the wide area survey at NEP of LS program. By previous background measurements in the near-infrared with IRTS and COBE satellites, strong background excess that is too bright to be accounted for by integrated light of faint galaxies was discovered. From a spectral signature of redshifted Ly-alpha in the background spectrum, the excess is attributed to integrated light from the first generation stars (Pop-III) populated at z~10. Motivation of this proposal is more accurate measurement and further study of the Pop-III background. Absolute sky brightness and its fluctuation at blank sky will be measured by imaging observations free from the contamination by foreground stars and galaxies, whose contribution was a major limiting factor for the accuracy of previous background measurements with large beam sizes. The angular power spectra of the background fluctuation will be measured in a wide range of angular scales from arcsec to degree. Based on the auto- and cross-correlation analysis for the multi-wavelength fluctuation data, the evolution and structure formation of Pop-III clusters will be investigated. In order to study further into the redshift distribution and surrounding nebula structure of Pop-III stars, spectroscopic measurements in near- and mid-infrared will also be performed by using the data taken for SPICY-MP and Solar-System-MP.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
13	124	CNIRB	MATSUURA_CNIRB	Matsuura, Shuji (ISAS/JAXA)	MP	3	AKARI observations of cosmic near-infrared background	The cosmic near-infrared background (CNIRB) is the integrated flux of unresolved extragalactic objects towards the line of sight. Therefore, measurement of the CNIRB is powerful method to research into very high redshift objects. Discovery of strong excess of the CNIRB by COBE and IRTS has given great impact to observational cosmology. Only a little fraction of the CNIRB energy could be attributed to known galaxies, and the remaining "excess" energy has to be due to unknown objects. Interestingly, the CNIRB spectrum peaking at ~1.2 um show good agreement with models of the first stars emitting strong Lyman-alpha at z>10, whose existence is suggested from the WMAP result of CMB anisotropy measurements. IRTS also found a characteristic angular scale of the CNIRB fluctuations at ~2 deg, which corresponds to the large-scale structure at z~10, an early phase of structure formation traced by Baryons.\n\nIn order to expand the CNIRB study, we have carried out AKARI observations as a subject of the LS-NEP program. Aim of this program is measurements of the CNIRB and its fluctuations in a wide rage of angular scale, which covers the predicted peak scale of the first-star background fluctuations. Imaging with IRC allowed us to minimize the point source contribution down to much fainter flux levels than previous observations. It should be noted that AKARI has great advantage against Spitzer of the capability of absolute measurement using the cold shutter, which is essential to detect the degree-scale fluctuations.\n\nAs preliminary results of the Phase-1/2 data, we have successfully detected the fluctuation signals, which exceed instrumental noise. The detected fluctuation levels are consistent with those of IRTS and COBE results. We think it has extragalactic origin and is possibly the first-star background. However, about a half of the data were unexpectedly affected by the stray light. The affected data cannot be used for the large-scale analysis, which requires absolute measurement. Then, the largest angular scale available with the current data set is limited to 1 degree. Hence, we propose to recover the lost half area in order to extend the angular range back to the original value of ~2 deg by the Phase-3 observations. In addition, we also propose confirmation of the Phase-1/2 results by using new AOT, which provides more accurate dark current estimate. The extended data set in Phase-3 should lead to much stronger conclusion on the origin of the CNIRB excess.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
14	130	CLEVL	LEE_CLEVL	Lee, HyungMok (Seoul National University)	MP	1&2	Evolution of Clusters of Galaxies	In order to understand the formation and evolution of galaxies in cluster environment, we propose to study clusters of galaxies over a wide range of redshifts using the wide-field capability of ASTRO-F. Since different observational strategies are required for clusters at different redshifts, we divide our program into three major components according to the redshifts of targets: low redshift, intermediate redshift, and high redshift clusters of galaxies. For low redshift clusters (z < 0.3) we focus on the effects of environment on star formation activity by choosing samples with different merging stages: major merging, minor merging and quiescent clusters. For intermediate redshift clusters (0.4 < z < 1.3), we will study star formation activity, stellar mass function, and environmental effect on them by conducting deep NIR-MIR imaging of selected sample clusters of galaxies and their surrounding groups along the large scale structures at 0.4 < z < 1.3. The high redshift cluster study can provide strong, direct constraints on the formation epoch of clusters galaxies. Since the sample of such high-z clusters is rather rare, we will focus on high-z objects with signs of overdensity based on other observational data, such as high-z radio galaxies, QSOs, and submm sources. Thus we propose to conduct NIR and MIR observations of overdense regions at 1.5 < z < 3.2, and NIR observations at z > 4. Specifically, we intend to perform deep observations centered on high-z radio galaxies around the NEP region. Overall, our program will explore the properties of galaxies in large areas extending out to a significant distances from cluster's center(about Mpc), enabling us, for the first time, to investigate the interaction of clusters and its surrounding environment over a large redshift range (0 < z < 5) in infrared. We will also sample the same MIR star formation indicator over 0 < z < 3 which will enable us to obtain a consistent IR SFR estimate.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
15	336	DPQSO	IM_DPQSO	Im Myungshin (Seoul National University)	OT-ISAS	3-I	Deep NIR Spectroscopy of QSOs at z > 4	We propose to perform a deep NIR spectroscopy of QSOs at z > 4 in the area near North Ecliptic Pole. Our previous (open time program, HZQSO) and the current mission program (QSONG) have been producing the rest-frame NIR spectra of QSOs at such high redshifts, only possible with AKARI. However, in order to study the rest-frame optical spectra of high redshift QSOs in detail, it is necessary to build up enough S/N (Fe complex, [OIII] line, and H-β). Building up sufficient S/N requires repeated observation, which is only possible in the ecliptic pole area. We have selected 4 QSOs at z > 4 near the NEP, and we will observe them to 25 pointing depth, to reveal the detailed picture of z > 4 QSO rest-frame optical spectra for the first time.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
16	131	GALEV	MATSUHARA_GALEV	Matsuhara, Hideo (ISAS, JAXA)	MP	1&2	Dusty Star-Formation History of the Universe	One of the key scientific goals to be performed with ASTRO-F deep surveys is to unveil the dusty star formation history of the Universe. The NEP survey, however, is not sufficient to perform this science goal. When the NEP survey will be performed, more than ten thousands of infrared galaxies will be detected. Since the spectroscopic follow-ups for such a large sample are still not realistic, we should rely on the so-called "photo-z" technique: estimation of the redshift by fitting the SED template to the obtained multi-wavelength data. Therefore, it is essentially important to establish the reliable SED templates of various star-forming galaxies with their physical understandings. Another weakness of the NEP survey is the lack of the far-infrared data with sufficient depth (i.e. confusion limit by the distant galaxies) to detect even z<=1 starburst galaxies, although the far-infrared flux is the direct measure of the star-formation rate of the dusty galaxies. Therefore, we propose the following strategy: 1. Mid-infrared SED studies of local star-forming galaxies in Virgo cluster, generating their SED templates (this MP). 2. The slitless spectroscopic survey in order to obtain the unbiased SED samples upto z=1 over the NEP survey field (separate MP : SPICY). 3. Far-infrared Deep Survey of the NEP deep survey field below the confusion limit by the galaxies with the FIS slow-scan survey (this MP). 4. The NEP survey (LSNEP). Determine the photometric redshifts of the detected sources by using the SED templates derived, and then we will address the evolution of the star-formation rate of the Universe with small uncertainties.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
17	132	FUHYU	PEARSON_FUHYU	Pearson, Chris (ISAS)	MP	1&2	FUHYU - SPITZER WELL STUDIED FIELD MISSION PROGRAM	We propose MIR imaging of several well studied Spitzer fields. This imaging fills in the bands lacking from the Spitzer surveys and gives an extremely high scientific return for minimal input for ASTRO-F. We select fields already rich in multi-wavelength data from radio to X-ray wavelengths to optimize the impact of the ASTRO-F observations. The deepest observations at 15microns with ISO unveiled a large population of luminous Infrared galaxies at redshifts around 0.8 that are responsible for the peak of the cosmic infrared background (CIRB) at 140microns. These galaxies are strongly evolving with co-moving densities of infrared light 40 times larger at z=1 compared to the local universe. Deep counts with Spitzer at 24microns have confirmed this strong evolution of the infrared luminosity function from redshift unity and have also detected a new population of luminous infrared galaxies at higher redshifts previously unpredicted by model fits to the ISO 15micron surveys. To link these populations and break the degeneracy in contemporary evolutionary scenarios, observations at multiple mid-infrared wavelengths that fully sample the PAH emission are demanded. In particular, observations deeper than 1mJy at 15microns will be of particular value in deciphering the dominant population responsible for the evolutionary upturn in the 15micron source counts. Spitzer has extremely restricted imaging capability between 8-24microns so ASTRO-F observations of the Spitzer fields will be vital to unravel the nature of the infrared populations in these fields thus linking the ISO-Spitzer populations.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
18	133	SPICY	WADA_SPICY	Wada, Takehiko (ISAS/JAXA)	MP	1&2	Unbiased Slit-less Spectroscopic Survey of Galaxies	Using the ABSOLUTELY UNIQUE capability of ASTRO-F's NIR/MIR slit-less spectroscopy, we propose an unbiased slit-less spectroscopic survey of galaxies.\nThe purpose of this survey is as follows. 1) Construction of the SED templates of the galaxies. With the redshift derived from PAH/silicate features and/or emission lines, 2) Investigations of PAH features along with the redshift, especially the MIR(PAH)/FIR(SFR) relationship. 3) Constraint on the galaxy evolution model by the luminosity function with type-classification, not by the galaxy counts. This survey will give a clear answer to the nature of excess in ISO 15um and SST 24um source counts around 1mJy. This survey also gives, 4) Discovery of spectroscopically peculiar galaxies such as ELGs, high-z QSOs, Lya/Ha emitters at the re-ionization era. 5) Strong constrains onto origin of the EBL.\nThe survey will use IRC prism and grisms (NP,SG1/2,LG1/2) in the slit-less spectroscopy mode and provide large number of unbiased galaxy samples with low resolution spectrum which covers wavelengths of 2-26 [um]. Together with FIS 4 band photometric data, the survey will provide SED template of galaxies which cover from NIR to FIR.\nTen pointed observations in AOT04 per FOV in the NEP survey (LSNEP) area (1 sq. deg.) will cover the sources brighter than 0.7[mJy@24um] and provide more than 600 SED template of galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
19		QSONG	LEE_QSONG	Lee, HyungMok (Seoul National University)	MP	3	Spectroscopic Observations of QSOs with NIR Grism	We propose to obtain NIR Grism spectra of 132 low redshift bright QSOs, and 225 high redshift QSOs at z > 3. The wavelength region between 2.5 - 5.0 micron contains a wealth of information on QSOs, but difficulties of accessing such a wavelength regime have hampered studies of spectra atthe important spectral window. At low redshift, the 2.5-5.0 micron window offers opportunities to study NIR Hydrogen lines which can give new insights into the AGN physics and also potentially provide useful AGN diagnostics for studying dust reddened systems. At high redshift, the H-alpha and H-beta lines - the popular estimators of the black hole mass - redshifts into 2.5-5.0 micron, making one to rely on much less robust mass estimators such as UV lines. By obtaining the 2.5 - 5.0 micron spectra of a carefully selected low redshift and high redshift QSOs, we will(i) assemble QSO spectra at the rarely studied wavelength regions of 2.5-5 micron; (ii) study the NIR Hydrogen lines such as Br-alpha, Br-beta, and Pa-alpha as diagnostics to understand the nature of the Supermassive Black Holes (SMBHs); (iii) examine whether there is a trace of star formation activities in their host galaxies through PAH features, and (iv) study the mass evolution of the SMBHs at high redshift to today. The spectroscopic study of hunderds of high redshift QSOs will enable us to understand the evolution and the census of SMBHs in QOSs at high redsfhit. Our study will also provide a uniform, extensive set of the rest-frame 2.5-5.0 micron spectra of QSOs for the first time, which can serve as a strong basis for the future studies of the less-extinct rest-frame NIR Hydrogen lines to understand the nature of distant QSOs.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
20	135	AMUSE	LEE_AMUSE	Lee ,HyungMok (Seoul National University)	MP	3-II	AKARI mJy Unbiased Survey of Extragalactic Sources in 5MUSES	We propose to take 2.5-5 /zm spectra of IR sources of the 5mJy Unbiased Spitzer Extra- galactic Survey (5MUSES). 5MUSES is one of the Spitzer Legacy surveys which performed a MIR spectroscopic observation of sources brighter than 5 mJy at 24 //m in the Spitzer First Look Survey field and SWIRE fields. The 5MUSES provides an unbiased library of IR spectra of sources bridging the gap between the bright nearby IR sources and faint, distant IR sources. Current 5MUSES spectral coverage is 5-40 /zm, missing the wavelength range of 2.5-5 //m where the 3.3 //m PAH feature and other interesting Hydrogen recombination lines fall. These lines are important for future investigation of dusty objects at high redshift and star formation activity in dusty systems. In this Mission Program, we will take AKARI IRC grism/prism spectra of 5MUSES sample whose 3.6 /im flux density exceeds 0.7-1 mJy. By combining the current Spitzer 5MUSES IR spectra and the AKARI IRC spectra, we will provide a complete coverage of the IR spectra of 5MUSES sample over 2.5-40 //m, which will be useful for understanding IR luminous objects for years to come.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
21	137	FUHYU	PEARSON_FUHYU	Pearson, Chris (RAL)	MP	3	FUHYU - WELL STUDIED FIELD MISSION PROGRAM	We propose to carry out point source aperture spectroscopy of a large sample of high red- shift, ultraluminous, sub-millimetre galaxies using the IRC near-infrared grism instrument on AKARI. Our targets are located in well studied fields with extensive photometry, spectroscopy and in many cases determined redshifts which will significantly aid in our analysis. Our target fields include thise already observed in AKARI IRC photometry for the same FUHYU Mission Program in Phase I & II.\n\nThe primary target of the spectroscopic observations are the Paschen alpha & Paschen beta recombination lines of Hydrogen, which will be used to estimate the extinction of the sources in our sample independent of any photometric data. The measured extinction combined with observed st ar-format ion rates will be used to constrain contemporary models of the spectra of these galaxies and investigate the evolutionary phase of dusty starbursts linking them with the formation of present day spheroidal systems. Secondary targets for our spectroscopy would include dust features such as the 1.6 micron bump, 2.3 micron feature and the 3.3 micron Polycyclic Aromatic Hydrocarbon (PAH) emission for lower redshift sources and their relationship to the st ar-formation rate. Finally, any additional, possibly anomalously powerful lines, and in a handful of high redshift sources, H alpha emission.\n\nThe objective of this Mission Program is to establish the evolutionary sequence of high-z massive starbursts, which once determined will further studies into the characteristics of starbursts as a function of mass in order to reveal the physical origin of the scaling relations of elliptical galaxies, thus linking the local and high redshift Universe, via the star-forming history and formation of the largest stellar systems we see today.\n\nSince Spitzer has no capability for spectroscopy in the near infrared region, AKARFs capability for slit spectroscopy exploits an instrumental and scientific niche of AKARI which is otherwise unachievable until JWST	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
22	137	FUHYU	PEARSON_FUHYU	Pearson, Chris (RAL)	MP	3-II	FUHYU - WELL STUDIED FIELD MISSION PROGRAM	We propose to carry out point source aperture spectroscopy of a large sample of intermediate redshift, z~1luminous infrared galaxies using the IRC near-infrared grism spectrograph on board AKARI. The proposed targets are intended to bridge the gap between the local Universe and the high redshift Universe observed previously by the FUHYU Mission Pro- gramme.The proposed targets have all been detected in deep 70 microns surveys with the Spitzer Space Telescope. The primary target lines of our observations will be the Paschen alpha line where AKARFs IRC near-infrared grism spectrograph is the only instrument that combines sensitivity and wavelength coverage and is uniquely suited to study near-infrared Hydrogen recombination lines in medium redshift 0.5<z<1.0 galaxies. The observations will derive star formation rates which subsequently will be compared to SFRs derived from other indicators. The relationship with the IRAC 8 micron emission which correlates with the Paschen Alpha line luminosity will be investigated since the extended IR luminosity of our targets originate in deeply obscured star-forming regions making traditional star-formation rate (SFR) indicators, for example the UV continuum or the H-alpha line emission, unsuitable for use with LIRGs due to the heavy extinction caused by the dust associated with the star formation sites. We will also compare the near-infrared evidence for AGN activity with evidence from Spitzer mid-infrared colours via the hydrogen recombination lines.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
23	138	EGANS	MATSUHARA_EGANS	Matsuhara, Hideo (ISAS)	MP	3	Evolution of Galaxies with AKARI Near-IR Spectroscopy of the SDSS selected sample	We propose spectroscopic (NP(2-5micron) or NG( R=160 at 2.5-5micron)) study of Sloan Digital Sky Survey (SDSS) galaxies at z=0.1-0.5 which are not so local to be resolved out by AKARFs imaging capability. In total158 targets for the FY2008, with three pointing per each. Selected targets are well-known in terms of their redshift, age, st ar-formation rate, and their environment (cluster member or not).\n\nKey sciences are 1)identifying 1.6micron bump (& 2.3micron CO abs. bandhead) as a function of age, 2) correlating the optical star-formation rate and the 3.3micron PAH feature. These results will benefit to judge the nature of AKARI-unique sources discovered by the all-sky survey by their near-IR SEDs.\n\nBy using these unique spectroscopic capability of AKARI as shown above, we also aim to perform the following scientific outcome: star-formation in the brightest cluster galaxies, the nature of star-forming elliptical galaxies, the nature of passive spirals and star-forming activity is E+A galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
24	140	ISMGN	KANEDA_ISMGN	Kaneda, Hidehiro (ISAS/JAXA)	MP	1&2	Interstellar dust and gas in various environments of our Galaxy and nearby galaxies	The aim of this MP is to perform systematic studies on interstellar dust and gas in various environments of our Galaxy and nearby galaxies. Considering the ASTRO-F uniqueness, we place particular importance on (A) detailed MIR-FIR SED studies of interstellar dust for moderately large (5-10 arcmin) targets, and (B) FIR imaging and MIR slit-less spectroscopic studies of interstellar gas and dust for bright targets. The ISM can be found in various neutral and ionized phases: hot plasma, warm ionized medium, classical HII regions, warm neutral medium, and cold neutral medium. Owing to its wide and fine spectral coverage as well as good angular resolution, ASTRO-F is best suited to study the processing, evolution, and destruction of dust components spatially resolved in each ISM phase, and their connection with physical and chemical conditions of gas and star-forming activity. Our Galactic objects allow detailed studies of the ISM in various conditions of gas phases and density, while our sample of nearby galaxies provides us much more extensive ranges in ISM environments and star formation history; the LMC/SMC serves to bridge the gap between our Galaxy and the other external galaxies. A membership of this program includes several members of the UK and Korean teams; imaging analyses of the galactic plane will be carried out in collaboration with the UK team, while the SNR survey is one of the key observations for collaborative research with the Korean team.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
25	142	ISMGN	KANEDA_ISMGN	Kaneda, Hidehiro (ISAS/JAXA)	MP	3	ISM in our Galaxy and nearby galaxies	We have performed systematic studies on the ISM in various environments of our Galaxy and nearby galaxies in the AKARI Phases 1&2. In order to extend our studies based on the results obtained in the Phases 1&2, we will propose to observe the ISM in our Galaxy and nearby galaxies in a systematic manner in the Phase 3. Considering AKARI uniqueness, we lay stress on near-IR spectroscopy that Spitzer does not possess. In particular, we propose to obtain near-IR spectral maps of our Galaxy and nearby galaxies as AKARI legacy products.\n\nSpectroscopic observations in the 2-5um wavelength range covered by the AKARI/IRC pro- vide many pieces of information about the properties of the ISM; ultra-small grains exhibit several spectral features at 3.3-3.5um that are crucial probes into the physical/chemical states of the dust grains and their evolution. The chemical composition of molecular species can be studied through absorption features by interstellar ice/gas such as those of CO at 4.7um, CO2 at 4.3um, and H2O around 3um. For the SNRs interacting with molecular clouds, many ro-vibrational emission lines from interstellar H2 gas heated by shock are expected to emerge in the near-IR spectral range. The near-IR spectral continuum is sometimes dominated by photospheric emission from asymptotic giant branch (AGB) stars, and thus AGB stars in the aggregate can be studied for mature systems such as elliptical galaxies. Dust continuum emission is also expected to exist in the near-IR spectrum even after subtracting the stellar background.\n\nThe observation program proposed here consists of the following three sub-programs:(1) Galactic plane survey by near-IR spectroscopy, (2) supernova remnants, and (3) nearby galaxies. Our Galaxy contains ideal targets for probing the energy flow from stars into the ISM and the life cycle of the ISM; clouds illuminated by early-type stars enable us to examine various theoretical models, while SNRs are conspicuous cases of collisional heating of the ISM and dust destruction. The environs of evolved stars and SNRs are essential as dust formation sites. External galaxies provide a much wider range of physical conditions. Our sample of about 80 nearby galaxies includes various ranges in ISM environments and star formation rate. A membership of this program includes several members of the Korean team; the SNR survey is one of the key observations for collaborative research with the Korean team.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
26	142	ISMGN	KANEDA_ISMGN	Kaneda, Hidehiro (Nagoya University)	MP	3-II	ISM in our Galaxy and nearby galaxies	We performed systematic studies on the ISM in various environments of our Galaxy and nearby galaxies in the AKARI Phase 2. In Phase 3a, we have started near-IR spectral mapping of our Galaxy and nearby galaxies to obtain AKARI legacy products combined with the results in Phase 2. In order to extend our studies, we propose to continue our MP observations in Phase 3b. Considering AKARI uniqueness, we lay stress on near-IR spectroscopy that Spitzer does not possess. In particular, we propose to strengthen our near-IR spectral database on our Galaxy by newly selecting observational area on the basis of the AKARI mid-IR all-sky survey and the NANTEN/NANTEN2 galactic plane survey data. This database combined with the AKARI mid-IR all-sky survey data will play a key role for our AKARI-Planck collaboration. We also continue near-IR spectral studies on SNRs and nearby galaxies by focusing on targets, for which we have already obtained notable results with AKARI and/or Spitzer.\nSpectroscopic observations in the 2-5 um wavelength range covered by the AKARI/IRC provide many pieces of information about the properties of the ISM; ultra-small carbonaceous particles, such as polycyclic aromatic hydrocarbon (PAH) molecules, exhibit several spectral features at 3.3-3.5 um that are crucial probes into the physical/chemical states of the dust grains and their evolution. The chemical composition of molecular species can be studied through absorption features by interstellar ice/gas such as those of CO at 4.7 um, CO2 at 4.3 um, and H2O around 3 um. For SNRs interacting with molecular clouds, many ro-vibrational emission lines from molecular hydrogen gas heated by shock are expected to emerge in the near-IR spectral range. In contrast, for UV-dominated regions with active star formation, hydrogen recombination lines from Brackett and Pfund series become dominant in the near IR, and therefore near-IR line diagnoses are very important to discuss whether observed regions are dominated by shock heating or not. On the other hand, the near-IR spectral continuum is sometimes dominated by photospheric emission from asymptotic giant branch (AGB) stars, and thus AGB stars in the aggregate can be studied for mature systems such as elliptical galaxies. Dust continuum emission is also expected to exist in the near-IR spectrum even after subtracting the stellar background.\nThe observation program consists of the following three sub-programs:(1) Galactic plane survey by near-IR spectroscopy (lead: M. Tanaka, A. Kawamura, & D. Ishihara), (2) Supernova remnants (B.-C. Koo) and supernovae (I. Sakon), and (3) Nearby galaxies (T. Onaka & H. Kaneda).	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
27	150	SOSOS	UENO_SOSOS	Ueno, Munetaka (University of Tokyo)	MP	1&2	Origin and Evolution of Solar System Objects	There are large and small bodies in our solar system, and are also other objects such as comets and dust particles, but we do not fully understand the linkage among themselves yet. To establish a concrete idea on the inter-planetary dust (IPD) cloud complex under the planetary system must be one of the most important issue, since the mechanism of continuous supply of interplanetary dust particle is still in the haze of the solar system.\nBig problem on the zodiacal dust cloud is its origin, since the lifetime of the interplanetary dust under the Poynting-Robertson drag is much shorter than the age of the Solar System. ASTRO-F capabilities on good sensitivities for extended sources, better calibration accuracy, fine spatial resolutions and spectroscopy in middle infrared bands will open a new horizon for IPD studies. IRAS dramatically changed the smooth featureless picture of the zodiacal dust cloud by revealing numerous bands of asteroidal debris, several narrow trails of cometary dust, and a clumpy dust ring. However, problems of calibration drifting and half degree resolution hindered us from fully identifying dynamical origins of the IPD cloud complex in general and of the symmetry plane's tilt. COBE/DIRBE also mapped almost entire sky with a 0.7 arc-degree size beam and with better calibration, and confirmed the mean motion resonance (MMR) dust ring, and an isolation of the leading and trailing blobs in the MMR feature. The mission's coverage of the solar elongation angle is limited to very narrow span from 89 to 91 arc-degree but the mission has superbly high sensitivity and fine spatial resolution. Its pointing and calibration stability promises to make mission products trustworthy. The spectrum of the zodiacal emission also provides essential information on the composition and size distribution of the IPD, and it is a clue for understanding the origin and evolution of the IPD particles. We are also going to study IPD cloud complex using ASTRO-F scanning observations, because the morphology includes inportant hints for its origin, and also to analyze its attribute using her spectroscopic capabilities, and finally to comprehend the IPD cloud complex problem.\nOn the other hand small bodies in the solar system are also very important targets as well-known samples for the primordial conditions even after the evolution, since the minor bodies such as asteroids, comets, centaurs, and EKBOs are thought to be remnants of the planetesimals, and contain a primitive record of the initial conditions of the solar system nebula about 4.6Gy ago.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
28	152	SOSOS	UENO_SOSOS	Ueno, Munetaka (University of Tokyo)	MP	3	Origin and Evolution of Solar System Objects	Our knowledge of the origin and the evolution of the solar system comes from two sources. One is study of star formation and extra-solar planetary systems. The other is the study of the solar system itself. Different from the macroscopic view for the other planetary systems, we can obtain detailed information on the individual bodies in our solar system. The solar system we observe today is, however, a highly evolved, and it is very important to recognize which qualities reflect that often violent evolution and which truly record conditions at the time of solar system formation. Then, which solar system bodies leave a trace at early solar system? Minor bodies such as asteroids, comets, centaurs, and Trans-Neptunian objects must be remnants of planetesimals in the early solar-nebula. Meteorites which came from asteroids provide us the clock for timing and conditions in planetesimal formation by cosmochemistry and mineralogy. Minor bodies contain a relatively pristine record of the initial conditions that existed in our solar system nebula around 4.6Gy ago. To know the origin and the evolution of early solar system, it is essential to study the small solar system objects. As questions about origin and evolution of the solar system, three central questions were listed.\n\nI. What was compositional gradient from Mercury to beyond Neptune at the time of initial protoplanetary accretion?\nII. What fragments originated from the same primordial parent bodies, and what was the original distribution of those parent bodies?\nIII. What are early steps in planetesimals and planet formation and evolution?\n\nObservations of ices and silicate materials are important to solve these questions. These materials have spectral features in near-infrared wavelength regions. Spectroscopic observations of AKARI/IRC are very suited for the determinations of compositions and crystallinity of these materials. Thus, we propose "near-infrared spectroscopic survey of small solar system objects".	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
29	152	SOSOS	UENO_SOSOS	Ueno, Munetaka (University of Tokyo)	MP	3-II	Origin and Evolution of Solar System Objects	Our knowledge of the origin and the evolution of the solar system comes from two ways, one is study of star formation and extra-solar planetary systems, and the other is study of our own solar system. Different from the macroscopic view for the other planetary systems, we can obtain plenty of information in details on the individual bodies in the solar system. The current solar system is, however, a highly evolved, and it is very important for us to recognize which qualities reflect the violent evolution and which truly record conditions at the time of solar system formation. Then, which solar system bodies leave a trace at early solar system? Minor bodies such as asteroids, comets, centaurs, and Trans-Neptunian objects must be remnants of planetesimals in the early solar-nebula. Meteorites which came from asteroids provide us the clock for timing and conditions in planetesimal formation by cosmochemistry and mineralogy. Minor bodies contain a relatively pristine record of the initial conditions that existed in our solar system nebula 4.6Gy ago. To know the origin and the evolution of early solar system, it is essential to study the small solar system objects. As questions about origin and evolution of the solar system, we have following three questions.\n\nI. What was compositional gradient from Mercury to beyond Neptune at the time of initial protoplanetary accretion?\nII. What fragments originated from the same primordial parent bodies, and what was the original distribution of those parent bodies?\nIII. What are early steps in planetesimals and planet formation and evolution?\n\nObservations of ices and silicate materials are important to solve these questions. These materials have spectral features in near-infrared wavelength. Spectroscopic observations of AKARI/IRC are very unique and are suited for the determinations of compositions and crystallinity of these materials. Thus, we propose "near-infrared spectroscopic survey of small solar system objects".	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
30	160	AFSAS	UENO_AFSAS	Ueno, Munetaka (University of Tokyo)	MP	1&2	ASTRO-F/AKARI Studies on Star formation and Star forming regions	The mission program is based on the three pillars (projects). The first project, survey of Chamaeleon region, is really unique and an unrivaled project. ASTRO-F slow scanning mode gains her sensitivities reaching detection level of the photosphere of stars, and also remains wide coverage enough to find out the orphan stars. Actual time scale in the proto-planetary disk will be determined by the quantitative samples of this survey. A full use of ASTRO-F capabilities enables us to conduct an extended survey to cover from the diffuse interstellar matter up to main sequence stars. This project is the first survey that has enough sensitivities to detect any stages of YSOs and sufficient coverage, giving quantitative samples of stars with proto-planetary disks born in the same cloud complex. The second project must be the legacyof ASTRO-F, as her atlas of various star forming sites, including a deep survey for selected regions, collaboration with other heritages of Nobeyama Radio Observatory, NANTEN and ASTE. The formation of brown dwarfs and planetary-mass objects and their abundance, and also the cut-off in the initial mass function, are major topics in tis project. The third pillar is the astro-mineralogy. ASTRO-F's unique capabilities in 3 micron, 20 micron and FTS spectroscopies realize detailed analyzations of interstellar dust particle with icy mantle and silicate dust in the circumstellar disk. To know the composition of icy material is essentially important to understand the chemical processes in the proto-planetary disk.\nThe whole sky survey of ASTRO-F is also very important part of the mission program, since it realizes a significant unbiased census of starforming cores in a large number of molecular clouds. The sensitivity of the ASTRO-F survey of the whole Galactic Plane, coupled with the small beam will detect pre-stellar cores to lower luminosity than previously detected. The 160 micron channel will detect cooler sources than have been found in the IRAS data. The ASTRO-F survey will be the first all-Galaxy measurement of the SED's of sources in star formation regions, allowing estimation of density and temperature gradients of a very large sample of young cores. ASTRO-F will have sufficient resolution to resolve the prestellar and protostellar clumps within individual molecular clouds to measure the radial density profiles in the extended envelopes of the protostars. The data will allow the measurement of temperature and density gradients, and the grain properties of material in the clouds. Viewed from a Galaxy-wide perspective, it should help to tell us how molecular clouds fragment into cores, at what stage IMF of the star forming region frozen in, how the disks dissipate their gas and dust, and eventually how planetary systems form in the disks.\nWe are propose to use the all-sky survey data, and to conduct slow-scanning observations and spectroscopic observations of protoplanetary disks around low-and intermediate-mass pre-main-sequence stars with the ASTRO-F. Our main goal is to reveal the evolution of the disks in the possible planet building stage of ~10 Myr. The target list of this study consists of T Tauri and Herbig Ae/Be stars mainly located in the Chamaeleon and Taurus regions (d = 140 pc): the total number of the sources is ~1500. This study will be done in the following two steps: First, we will perform a photometric survey of the disks around the pre-main-sequence stars with the FIS and the IRC in the survey mode. Second, we will make spectroscopic observations over 2200 mm of the disks detected at the 1-st step toward the weak-line T Tauri and Herbig Ae/Be stars with ages of ~10 Myr: the number of the pointings is roughly estimated to be 1000. Since the Astro-F survey can detect the circumstellar disks with very high sensitivity in gas mass of MEarth, we will be able to unveil the evolution of disk dust mass with good statistics during the weak-line T Tauri stage of ~10 Myr. This survey is one of the most sensitive surveys of weak-line T Tauri stars over the whole sky. Furthermore, from the successive spectroscopic observations, we can obtain the detailed spectral energy distributions of the disks and can discuss the evolution of disk internal structures (i.e., the disk clearing in the innermost regions) relevant to planet building at ~10 Myr. Our large sample over several star-forming regions also makes it possible to understand how the disk evolution depends on stellar masses and formation sites.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
31	161	AFSAS	UENO_AFSAS	Ueno, Munetaka (University of Tokyo)	MP	1&2	ASTRO-F/AKARI Studies on Star formation and Star forming regions	The mission program is based on the three pillars (projects). The first project, survey of Chamaeleon region, is really unique and an unrivaled project. ASTRO-F slow scanning mode gains her sensitivities reaching detection level of the photosphere of stars, and also remains wide coverage enough to find out the orphan stars. Actual time scale in the proto-planetary disk will be determined by the quantitative samples of this survey. A full use of ASTRO-F capabilities enables us to conduct an extended survey to cover from the diffuse interstellar matter up to main sequence stars. This project is the first survey that has enough sensitivities to detect any stages of YSOs and sufficient coverage, giving quantitative samples of stars with proto-planetary disks born in the same cloud complex. The second project must be the legacyof ASTRO-F, as her atlas of various star forming sites, including a deep survey for selected regions, collaboration with other heritages of Nobeyama Radio Observatory, NANTEN and ASTE. The formation of brown dwarfs and planetary-mass objects and their abundance, and also the cut-off in the initial mass function, are major topics in tis project. The third pillar is the astro-mineralogy. ASTRO-F's unique capabilities in 3 micron, 20 micron and FTS spectroscopies realize detailed analyzations of interstellar dust particle with icy mantle and silicate dust in the circumstellar disk. To know the composition of icy material is essentially important to understand the chemical processes in the proto-planetary disk.\nThe whole sky survey of ASTRO-F is also very important part of the mission program, since it realizes a significant unbiased census of starforming cores in a large number of molecular clouds. The sensitivity of the ASTRO-F survey of the whole Galactic Plane, coupled with the small beam will detect pre-stellar cores to lower luminosity than previously detected. The 160 micron channel will detect cooler sources than have been found in the IRAS data. The ASTRO-F survey will be the first all-Galaxy measurement of the SED's of sources in star formation regions, allowing estimation of density and temperature gradients of a very large sample of young cores. ASTRO-F will have sufficient resolution to resolve the prestellar and protostellar clumps within individual molecular clouds to measure the radial density profiles in the extended envelopes of the protostars. The data will allow the measurement of temperature and density gradients, and the grain properties of material in the clouds. Viewed from a Galaxy-wide perspective, it should help to tell us how molecular clouds fragment into cores, at what stage IMF of the star forming region frozen in, how the disks dissipate their gas and dust, and eventually how planetary systems form in the disks.\nWe are propose to use the all-sky survey data, and to conduct slow-scanning observations and spectroscopic observations of protoplanetary disks around low-and intermediate-mass pre-main-sequence stars with the ASTRO-F. Our main goal is to reveal the evolution of the disks in the possible planet building stage of ~10 Myr. The target list of this study consists of T Tauri and Herbig Ae/Be stars mainly located in the Chamaeleon and Taurus regions (d = 140 pc): the total number of the sources is ~1500. This study will be done in the following two steps: First, we will perform a photometric survey of the disks around the pre-main-sequence stars with the FIS and the IRC in the survey mode. Second, we will make spectroscopic observations over 2200 mm of the disks detected at the 1-st step toward the weak-line T Tauri and Herbig Ae/Be stars with ages of ~10 Myr: the number of the pointings is roughly estimated to be 1000. Since the Astro-F survey can detect the circumstellar disks with very high sensitivity in gas mass of MEarth, we will be able to unveil the evolution of disk dust mass with good statistics during the weak-line T Tauri stage of ~10 Myr. This survey is one of the most sensitive surveys of weak-line T Tauri stars over the whole sky. Furthermore, from the successive spectroscopic observations, we can obtain the detailed spectral energy distributions of the disks and can discuss the evolution of disk internal structures (i.e., the disk clearing in the innermost regions) relevant to planet building at ~10 Myr. Our large sample over several star-forming regions also makes it possible to understand how the disk evolution depends on stellar masses and formation sites.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
32	164	AFSAS	UENO_AFSAS	Ueno, Munetaka (University of Tokyo)	MP	3	ASTRO-F/AKARI Studies on Star formation and Star forming regions	Our main goal is to reveal the evolution of the disks in the possible planet building stage of ~ 10 Myr. The target list of this study consists of T Tauri and Herbig Ae/Be stars mainly located in the Chamaeleon and Taurus regions (d =140 pc). This study will be done in the following two steps: First, we did perform a photometric survey of the disks around the pre-main-sequence stars with the FIS and the IRC. Second, we will make spectroscopic observations over 2-5 micron of the disks detected at the 1-st step toward the weak-line T Tauri and Herbig Ae/Be stars with ages of ~ 10 Myr.\n\nASTRO-F/AKARFs unique capabilities in 3 micron spectroscopies realize detailed analyzations of interstellar dust particle with icy mantle. To know the composition of icy material is essentially important to understand the chemical processes in interstellar matter, and the composition must be determined by the physical conditions such as temperature, density, and UV flux. The icy dust is also very important to control the speed of accumulations of planetesimal phase in proto-planetary disk. ASTRO-F/AKARI is the only mission which can examine a spectroscopic face of dust particle in various stage of star formation up to our solar system. The second project is a deep survey for selected regions under collaboration with tie-up observations. The formation of brown dwarfs and planetary-mass objects and their abundance, and the very low-mass end of the initial mass function, are two of the central topics for both of the low-mass star and star formation studies. The third project is a follow-up observations of Chamaeleon sky survey. Chamaeleon region is selected to be a test bench for our studies since it is situated in the excellent visibility area of ASTRO-F/AKARI. A full use of ASTRO-F/AKARI capabilities enables us to conduct an extended survey to cover from the diffuse interstellar matter up to rather evolved main sequence stars. This project is the first survey that has enough sensitivities to detect any stages of YSOs up to MS star and sufficient coverage in the sky, and which will provide us quantitative samples of stars with proto-planetary disks born in the cloud and will hopefully meet a brief phenomena with very short duration. The fourth one is a possible observation of atmosphere of an extra-solar planet	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
33	164	AFSAS	UENO_AFSAS	Ueno, Munetaka (University of Tokyo)	MP	3-II	ASTRO-F/AKARI Studies on Star formation and Star forming regions	AFSAS MP in phase3 mainly focuses on the following topics using ASTRO-F/AKARFs uniqueness.\nThe first topic is the astro-mineralogy. ASTRO-F/AKARFs unique capabilities in 3 micron spectroscopies realize detailed analyzations of interstellar dust particle with icy mantle. To know the composition of icy material is essentially important to understand the chemical processes in interstellar matter, and the composition must be determined by the physical conditions such as temperature, density, and UV flux. The icy dust is also very important to control the speed of accumulations of planetesimal phase in proto-planetary disk. ASTRO- F/AKARI is the only mission which can examine a spectroscopic face of dust particle in various stage of star formation up to our solar system.\nThe second project is a deep survey for selected regions under collaboration with tie-up observations. The formation of brown dwarfs and planetary-mass objects and their abundance, and the very low-mass end of the initial mass function, are two of the central topics for both of the low-mass star and star formation studies.\nThe third project is a follow-up observations of Chamaeleon sky survey. Chamaeleon region is selected to be a test bench for our studies since it is situated in the excellent visibility area of ASTRO-F/AKARI. A full use of ASTRO-F/AKARI capabilities enables us to conduct an extended survey to cover from the diffuse interstellar matter up to rather evolved main sequence stars. This project is the first survey that has enough sensitivities to detect any stages of YSOs up to MS star and sufficient coverage in the sky, and which will provide us quantitative samples of stars with proto-planetary disks born in the cloud and will hopefully meet a brief phenomena with very short duration.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
34	170	AGBGA	NAKADA_AGBGA	Nakada, Yoshikazu (University of Tokyo)	MP	1&2	Mass loss and stellar evolution in the AGB phase	We propose a systematic study of mass loss from AGB stars in the Milky Way globular clusters and the nearby dwarf galaxies. The targets are selected so that they span a wide range of age and metallicity.\nThe observations will be performed using the IRC and FIS pointing modes. The IRC images will be taken in six bands, N2, N4, S7, S11, L15, and L24. They are designed to provide information of mass-loss rate, silicate band strength, C-/M- star distinction, and stellar luminosity. The FIS observations are carried out only to globular clusters, in order to estimate total amount of mass lost from the stars in the system.\nWe plan to to make a point source catalog for each system. The evaluation of mass-loss rates for a number of AGB stars will be performed on this catalog. We will systematically investigate the effects of metallicity and stellar mass on the mass loss phenomena. The results will be of great importance on the understanding of the late evolution of low- to intermediate-mass stars as well as on the study of the galactic chemical evolution.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
35	305	NULIZ	HWANG_NULIZ	Hwang, HoSeong (Astronomy Program, School of Earth and Environmental Sciences, Seoul National University)	OT-ISAS	2	The Nature of New ULIRGs at intermediate redshift	We propose to obtain NIR spectra and NIR/MIR-S images of new ultraluminous infrared galaxies (ULIRGs) at intermediate redshift (mostly at 0.2 < z < 0.5) using ASTRO-F. Recently, we found about 230 new ULIRGs from a cross-correlation of the IRAS Faint Source Catalog with the spectroscopic galaxy catalogs of SDSS, 2dFGRS and 6dFGS. These new ULIRGs are mostly at 0.2 < z < 0.4, while previously known ULIRGs are mostly at z < 0.2. The observation of these new ULIRGs at z>0.2 using ASTRO-F extends our understanding about the nature of ULIRGs acquired from nearby universe. We are going to investigate the nature of these ULIRGs at intermediate redshift (z>0.2) using two modes of ASTRO-F observation: 1) NIR spectroscopy of 20 ULIRGs at 0.2 < z < 0.4 and 2) NIR/MIR-S imaging of 12 ULIRGs at 0.35 < z < 0.7. Primary goals of our study are 1) to obtain NIR spectra of new ULIRGs at 0.2 < z < 0.4 and to measure the equivalent width of 3.3 micron PAH emission and the slope of the continuum covering the PAH feature; 2) to search for dust absorption features at 3.1 and 3.4 microns; 3) to estimate the activity of starburst or active galactic nuclei (AGN) in the targets using above features; 4) to obtain spectral energy distribution (SED) of the new ULIRGs at 0.35 < z < 0.5 from NIR/MIR-S fluxes; and 5) to estimate the activity of starburst or active galactic nuclei (AGN) in the targets at 0.35 < z < 0.5 from the SED. We are also going to investigate any luminosity dependence of IR activity from the comparison of ULIRGs and hyperluminous infrared galaxies (HLIRGs). Our study is complementary to the ASTRO-F Mission Program (Evolution of ULIRGs and AGNs: AGNUL) which is composed of (a) NIR spectroscopy of known nearby ULIRGs at z < 0.2 and (b) deep imaging survey and slit-less spectroscopic survey of mid to high-z ULIRGs. Our targets will make a critical role bridging the Mission Program's nearby ULIRGs and mid to high z ULIRGs, and will allow us to understand the nature and the evolution of ULIRGs.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
36	171	MLHES	YAMAMURA_MLHES	Yamamura, Issei (ISAS/JAXA)	MP	1&2	Excavating Mass Loss History in Extended Dust Shells of Evolved Stars	Exploiting the superb sensitivity and mapping capabilities of ASTRO-F/FIS, we will perform a far-IR imaging survey of the circumstellar envelopes of evolved stars. Our primary goal is to fully understand the mass loss phenomena in the latest stages of stellar evolution by tracing the history of mass loss carved in the structure of very extended, cold dust shells around those evolved objects. We will obtain maps of 10x20 size of those extended dust shells with FIS by detecting thermal emission arising from cool dust grains and reconstruct the history of mass loss along the latest stages of stellar evolution. We will systematically examine the mass-loss history during the last 1E5 years with a time resolution of 1,000 years. From our set of coherent FIS data having variety of evolutionary state and chemistry, we will examine (1) if mass loss history can be affected by some stellar characteristics, and if so, how it happens, (2) if mass loss variation really occurs, and if so, how it occurs, (3) if mass loss is constant over the course of the mass loss history, and if not, if there is really a superwind, and (4) if the shell structure formation really begins early in the AGB phase. We will also perform a mid-IR imaging with IRC of some selected objects to examine physical conditions of dust in their shells, which would greatly improve our detailed modeling for the FIS far-IR imaging survey.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
37	172	NIRLT	YAMAMURA_NIRLT	Yamamura, Issei (ISAS/JAXA)	MP	1&2	Near-Infrared Spectroscopy of L and T Dwarfs	Ground based observations of ultracool dwarfs, including L and T dwarfs are almost limited to the NIR short-ward of 2.5 micron, with the exceptional case of Gl 229B. Although MIR (5.0~12.0 micron) is observed with Spitzer, there is no possibility of the NIR spectroscopy. The NIR region is especially important for ultracool dwarfs, because this region includes CO fundamental bands and CH4 nu3 fundamental bands. It was suggested from a very noisy spectra of Gl229B obtained with the ground-based observation that CO is over-produced by the non-equilibrium process as is known in Jupiter atmosphere. So far, the modelings of the atmospheres of brown dwarfs are mostly based on the equilibrium chemistry including the dust formation, and to clarify the nonequilibrium chemistry is an important next step to a more realistic modelings of the atmospheres of brown dwarfs. This can also be an important preparatory step for spectroscopy and modeling of extra-solar giant planets in the near future.\nWe propose to observe the NIR spectra of selected L and T dwarfs by ASTRO-F. ASTRO-F provides a unique and exclusive opportunity to take high-quality NIR spectra of ultracool dwarfs. Its data shall progress our understanding of the atmospheres of brown dwarfs significantly. Total number of targets listed here is 30, in which 9 are priority A and other 10 are B. Observations will be carried out in the AOT IRC04 with a selection of NG. Two to six pointings per object, depending on their brightness, are requested.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
38	174	AGBGA	NAKADA_AGBGA	Nakada, Yoshikazu (University of Tokyo)	MP	3	Mass loss and stellar evolution in the AGB phase	We propose imaging and spectroscopic observations of evolved stars (Asymptotic Giant Branch (AGB) stars, post-AGB stars and planetary nebulae) in nearby galaxies and Galactic globular clusters. The primary aims of these observations are (1)detecting mass-losing stars in these galaxies and clusters. (2) Understanding mass-loss process of these AGB stars. (3) Investigating the influence of metallicities of galaxies on compositions of dust and molecules.\n\nTargets of the imaging observations are 36 nearby galaxies within 1500 kpc and 54 galactic globular clusters. Furthermore, we request spectroscopic observations of stars in nearby galaxies and Galactic globular clusters in the NG and NP modes. AKARI near-infrared spectra will cover PAHs, C2H2, H2〇 and CO bands. Particular interests will be PAHs and C2H2, which are likely to have metallicity dependence in their abundance. These observations will help understanding stellar evolution and chemical evolution of galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
39	174	AGBGA	NAKADA_AGBGA	Nakada, Yoshikazu (University of Tokyo)	MP	3-II	Mass loss and stellar evolution in the AGB phase	We propose follow-up observations of our phase 3 I AGBGA, imaging and spectroscopic observations of evolved stars (Asymptotic Giant Branch (AGB) stars, post-AGB stars and planetary nebulae) in nearby galaxies and Galactic globular clusters. The primary aims of these observations are (1)establishing census of mass-losing stars in these galaxies and glob- ular clusters, (2) understanding mass-loss process of these AGB stars, and (3) Investigating the influence of metallicities of galaxies on compositions of dust and molecules.\nTargets of the imaging observations are six nearby dwarf galaxies. Furthermore, we request spectroscopic observations of stars in nearby galaxies and Galactic globular clusters in the NG and NP modes. AKARI near-infrared spectra will cover PAHs, C2H2, H2O and CO bands, and CO2 ice bands. Particular interests will be PAHs and C2H2, which are likely to have metallicity dependence in their abundance. These observations will help understanding stellar evolution and chemical evolution of galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
40	177	NIRLT	YAMAMURA_NIRLT	Yamamura, Issei (ISAS/JAXA)	MP	3	Near Infrared Spectroscopy of L and T Dwarfs	Ground based observations of brown dwarfs, including L and T dwarfs are almost limited to the NIR shortward of 2.5 micron, with the exceptional case of G1 229B. Although mid-infrared region (> 5.0 micron) can be observed with Spitzer, there is no possibility of the near-infrared spectroscopy. The NIR region is especially important for brown dwarfe, because this region includes CO fundamental bands and CH4 nu3 fundamental bands. It was suggested from a very noisy spectra of G1229B obtained with the ground-based observation that CO is over- produced by the non-equilibrium process as is known in Jupiter atmosphere. Recent analysis of the Spitzer mid-infrared data of the brown dwarfs indicates a remarkable contribution of the non-equilibrium effect such as vertical transport in the abundance of NH3. To clarify the non-equilibrium chemistry in other major molecules such as CO and CH4 is an important next step to a more realistic modeling of the atmospheres of brown dwarfe. This can also be an important preparatory step for spectroscopy and modeling of extra-solar giant planets in the near future. AKARI provides a unique and exclusive opportunity to take high-quality NIR spectra of brown dwarfs. Its data shall progress our understanding of the atmospheres of brown dwarfs significantly. We proposed a series of NIR spectroscopy of the brown dwarfs with AKARI/IRC/NIR for Phase 1 & 2 observations. Eleven stars have been observed and seven of them show spectra of good quality. The analysis is still ongoing but the first glance of the data already told us remarkable features in the spectra. Therefore, we will continue observations in Phase 3 to enlarge the sample of NIR spectra of the brown dwarfs. We also add nine M-type dwarfs to clarify the spectral sequence of ultracool dwarf stars. Ten stars from the Spitzer target are included in the current sample. In total we propose observations of 30 stars, 68 pointings all in the high-resolution spectroscopic mode of the IRC/NIR.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
41	172	NIRLT	YAMAMURA_NIRLT	Yamamura, Issei (ISAS/JAXA)	MP	3-II	Near-Infrared Spectroscopy of L and T Dwarfs	We propose extension of the currently running Mission Programme, NIRLT in the second year of the Phase 3. Ground based observations of brown dwarfs, including L and T dwarfe are almost limited to the NIR shortward of 2.5 micron, with the exceptional case of G1 229B and two other stars. Although mid-infrared region (> 5.0 micron) can be observed with Spitzer, there is no possibility of the near-infrared spectroscopy. The NIR region is especially important for brown dwarfs, because this region includes CO fundamental bands and CH4 nu3 fundamental bands. It was suggested from a very noisy spectra of G1229B obtained with the ground-based observation that CO is over-produced by the non-equilibrium process as is known in Jupiter atmosphere. Recent analysis of the Spitzer mid-infrared data of the brown dwarfe indicates a remarkable contribution of the non-equilibrium effect such as vertical transport in the abundance of NH3. To clarify the non-equilibrium chemistry in other major molecules such as CO and CH4 is an important next step to a more realistic modeling of the atmospheres of brown dwarfs. This can also be an important preparatory step for spectroscopy and modeling of extra-solar giant planets in the near future. AKARI provides a unique and exclusive opportunity to take high-quality NIR spectra of brown dwarfs. Its data shall progress our understanding of the atmospheres of brown dwarfs significantly. In the extension period in the Phase 3-II, we do not add any new targets as no more brown dwarfe that are bright enough to be observed with AKARI. Instead we intend to complete the observation previously observed, i.e., supplemental pointings for the targets not allocated yet, in addition, additional pointings to increase the redundancy against hot pixel problem. In total we request 45 pointed observations of 32 objects.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
42	180	VEGAD	MURAKAMI_VEGAD	Murakami, Hiroshi (ISAS/JAXA)	MP	1&2	Debris Disks around Main Sequence Stars and Extra-solar Zodiacal Emissions	The main purpose of this mission program is to trace the formation and dispersal processes of the debris disks around main sequence stars as well as to study whether the debris disks directly connected to the zodiacal dust or not. From the IRC and FIS all-sky survey data, new Vega-like star candidates with relatively large infrared excess can be discovered from the sample of stars that have not been observed with previous missions. IRC is capable of detecting stars having large excess such as betaPic out of more than 1000 stars. FIS is useful for the stars lack of warm dust such as Vega. The precise relative photometry is planned to detect very faint disks, showing less than a few percent excess from the photosphere emission. IRC (MIR-S and MIR-L) in pointing mode will mainly be used for this observation. Since this kind of ”faint disk” may be the analog of the zodiacal dust of out solar system, the investigation of the relationship to the planet formation is an important point of view. For this reason, more than 100 stars are selected from the TPF target list considering the instruments' specifications. In addition, some nearby stars from AFGKM spectral types, stars in Coma Berenices open clusters and known Vega-like stars will be observed to widen our knowledge of the properties of the debris disks. We are also planning to use FTS for the mineralogy of the bright debris disks around betaPic, alphaPsA and HR4796 if the performances of FTS will be improved on the orbits.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
43	182	EXOPT	MURAKAMI_EXOPT	Murakami, Hiroshi (ISAS/JAXA)	MP	3	Atmospheric Compositions and Temperature Structures of Extra Solar Planets	We propose to reveal atmospheric compositions and temperature structures of transiting exoplanets using spectroscopic mode of IRC. Transits and 2ry Eclipses of exoplanets give unprecedented opportunity for studying exoplanets otherwise impossible to distinguish them from their host stars. Spitzer has been providing most of the data on thermal emission from the exoplanets. However, it could not provide definite spectroscopic proofs for atmospheric features. Recent models on exoplanet atmosphere predict either absorption or emission features depending on the atmospheric temperature structure. There features are most prominent at 3-4 micron where Akari IRC spectroscopic mode covers but Spitzer IRS do not. The emission/absorption or the absence of these features will give important clues on the presence of inversion layers, stratospheres, or dusty clouds. Based on Spitzer (mainly) photometric data, there are some hint for a variety of the atmospheric structures; not all of them may show similar features. We can observe seven transiting exoplanets with Akari sensitivity and may be able to reveal a diversity of atmospheres among transiting exoplanets.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
44	190	P3LMC	ONAKA_P3LMC	Onaka, Takashi (University of Tokyo)	MP	3	Observations of the Magellanic Clouds	We propose to make about 600 pointing observations of the Large and Small Magellanic Clouds with NP (near-infrared prism slit-less spectroscopy in 2-5 micron). We propose to observe the same region of the LMC in the phase 1 and 2, which will give a redundant dataset to the LMC survey executed in the phase 1 and 2. It will significantly improve the quality and reliability of their NP data and drastically enhance its scientific output by enabling the extraction of fainter source spectra. The LMC bar region will not be observed because of its high source confusion, and instead we propose to make observations of the SMC that has similar ecliptic longitudes in a well-arranged plan. The proposed observation will make AKARI NP data of the LMC a legacy data product. It will provide crucial information for the study of a wide range of astronomy, including star-formation, interstellar processing, mass-loss in the late stellar evolution, and the energy and mass budget of interstellar medium. It will make a huge contribution to the study of the material circulation in a galaxy, the primary science goal of the LS LMC survey.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
45	191	LMCNG	ONAKA_LMCNG	Onaka, Takashi (Department of Astronomy, University of Tokyo)	MP	3-II	Near Infrared Spectroscopic Observations of Red Objects in the Large Magellanic Cloud	We propose to carry out about 750 pointing observations of red objects detected by AKARI or Spitzer Sage surveys of the Large Magellanic Cloud (LMC) with the grism mode (NG; 2.5-5 micron) of the IRC. The AKARI/IRC has a unique capability of the high-sensitivity near-infrared (NIR) spectroscopy, which can clearly distinguish young stellar objects (YSOs) from evolved stars enshrouded by dust shells. The present observation not only makes the correct classification of red objects, but also enables us to quantitatively study the physical properties of these objects, such as the ice chemistry in YSOs, photosphere chemistry of asymptotic-giant branch stars and interaction of supernova remnants with the interstellar medium. It will provide a unique dataset, which cannot be obtained by any other current facilities, for the study of a wide range of astronomy, from st ar-formation, mass-loss process in the late stellar evolution, and the energy to the mass budget of the interstellar medium. The proposed observation will make a significant contribution to the study of the material circulation in a galaxy, a primary goal of the AKARI LMC survey.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
46		MSAGN	OYABU_MSAGN	Oyabu, Shinki (ISAS/JAXA)	MP	3	MIR all-sky survey follow-up program: search for missing AGNs	This is a new proposal for a follow-up program of AKARI mid-infrared all-sky survey sources. Main purpose is to search for active galactic nuclei(AGNs) in the all sky using mid-infrared excess over 2MASS A^-band. Our survey can find not only normal AGNs but also very dusty AGNs which are excluded by selection criteria of other AGN surveys with optical as well as X-ray, radio and near-infrared. Spitzer can perform a deep, but small field of view survey in the infrared, while IRAS made all-sky survey with shallow sensitivities in the mid- and far-infrared. Instead our AKARI mid-infrared all-sky survey brought us deeper sensitivities and higher resolution. IRC NG spectroscopy can escape from dust extinction and provide their evidence of AGNs which have broad emission lines and/or steep continuum of hot dust. If it is very dusty, there might be molecule absorptions in the spectra. The contamination of sources are star-forming galaxies with strong PAH emissions. We can confirm 3.2//m PAH emission of such galaxies from IRC NG spectra. Using their spectra, we will make new AGN sample. We are going to discuss real AGN population in near-by universe. We also note that our survey have a possibility to find quasars at z~4 like the luminous and lensed quasar, APM 08279+5255.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
47	192	MSAGN	OYABU_MSAGN	Oyabu, Shinki (ISAS/JAXA)	MP	3-II	Mid-infrared all-sky survey follow-up program: search for missing Active Galactic Nuclei	This is the continuation proposal for a follow-up program of AKARI mid-infrared all-sky survey sources. Main purpose is to search for Active Galactic Nuclei (AGNs) in the all sky using mid-infrared excess over 2MASS Ks-band. Our survey can find not only normal AGNs but also very dusty AGNs which are excluded by selection criteria of other AGN surveys with optical as well as X-ray, radio and near-infrared. Spitzer can perform a deep, but small field of view survey in the infrared, while IRAS made all-sky survey with shallow sensitivities in the mid- and far-infrared. Instead, our AKARI mid-infrared all-sky survey brought us wider area than the Spitzer's survey and deeper sensitivities and higher resolution than the IRAS. IRC NG spectroscopy can escape from dust extinction and provide their evidence of AGNs which have broad emission lines and/or steep continuum of hot dust. If it is very dusty, there might be molecule absorptions in the spectra. The contamination of sources are star-forming galaxies with strong PAH emissions. We distinguish them using 3.2//m PAH emission and flat continuum of such galaxies on IRC NG spectra.\nUsing their spectra, we will make new AGN sample. We are going to discuss real AGN population in near-by universe. We also note that our survey have a possibility to find quasars at ~4 like the luminous and lensed quasar, APM 08279+5255.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
48	193	MSFGO	ISHIHARA_MSFGO	Ishihara, Daisuke (U-Tokyo)	MP	3-II	Mid-infrared all-sky survey follow-up program including Galactic objects	Main purpose of this proposal is a systematic follow-ups of newly detected sources in AKARI mid-infrared all-sky survey targeting identification of sub sample of these objects and finding new kind of objects or populations. AKARI mid-infrared all-sky point source catalog will provide over 700,000 sources including many unidentified sources (>70% of 9um detections are without IRAS detections and >60% of them are without SIMBAD IDs). Our targets are "red" objects thus expected to be surrounded by larger amount of gas and dust and show many kinds of spectral features. We will cover lower galactic latitude (\|b\| <30 deg) thus complementary with those of another follow-up program of AKARI mid-infrared all-sky survey : MSAGN (PI: S.Oyabu).	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
49		SPICY	WADA_SPICY	Wada, Takehiko (ISAS/JAXA)	MP	3	Unbiased Slit-Less Spectroscopic Survey of Galaxies for the Phase 3	Using the ABSOLUTELY UNIQUE capability of AKARFs NIR slit-less spectroscopy, we propose an unbiased slit-less spectroscopic survey of galaxies. The purpose of this survey ISAS follows.1)Construction of a library of accurate SED templates of galaxies. 2) Determination of the redshifts of galaxies by 3.3um PAH features and other emission lines. 3) Investigation of the PAH features along with the redshift, especially, the PAH/SFR relationship. 4) Constraints on galaxy evolution models by type dependent luminosity function classification, rather than galaxy counts. 5) Discovery of spectroscopically peculiar galaxies such as ELGs, high-z QSOs and Lya/Ha emitters at the re-ionization era. This survey will also give strong constraints on the origin of the EBL. This survey will mainly use IRC prism (NP) in the slit-less spectroscopy mode and provide us with a large number of unbiased samples of galaxies with low resolution spectrum covering wavelengths from 2.5 to 5 micron. Together with GALEX, CFHT, Uzbekistan lm telescope, KPNO 2.2m FLAMINGO, Spizter, and AKARI photometric data, this survey will provide us with a complete correction of SEDs of local(z=0.1-0.4) star-forming galaxies with a coverage from UV to FIR wavelengths, with a spectroscopic redshift determined by the 3.3 micron PAH feature. 895 pointed observations in AOTZ4 mainly in the NEP regions are requested for this unique survey.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3_Mission_Programmes_Abstracts.pdf
50	194	SPICY	WADA_SPICY	Wada, Takehiko (ISAS/JAXA)	MP	3-II	Unbiased Slit-Less Spectroscopic Survey of Galaxies for the Phase 3-II	Using the ABSOLUTELY UNIQUE capability of AKARFs NIR slit-less spectroscopy, we propose an unbiased slit-less spectroscopic survey of galaxies. The purpose of this survey ISAS follows.\n1) Construction of a library of accurate SED templates of galaxies.\n2) Determination of the redshifts of galaxies by 3.3um PAH features and other emission lines.\n3) Investigation of the PAH features, especially, the PAH/SFR relationship in a variety of clustering environment.\n4) Constraints on galaxy evolution models by type dependent luminosity function classifica- tion, rather than galaxy counts.\n5) Discovery of spectroscopically peculiar galaxies such as ELGs, high-z QSOs and Ly-a/H-a emitters at the re-ionization era.\n6) Detection of Ha emission from high redshift Lyman-a emitters.\n\nThis survey will also give strong constraints on the origin of the EBL. This survey will mainly use IRC prism (NP) in the slit-less spectroscopy mode and provide us with a large number of unbiased samples of galaxies with low resolution spectrum covering wavelengths from 2.5 to 5 um. Together with existing or on-going GALEX, CFHT, Uzbekistan lm telescope, KPNO 2m telescope, Spizter, and AKARI photometric data, this survey will provide us with a complete correction of SEDs of local (z=0.1-0.4) star forming galaxies with a coverage from UV to FIR wavelengths, with spectroscopic redshifts determined by the 3.3 micron PAH feature. This survey also search for Ha emission from high-redshift LABs and LAE. 521 pointed observations by AOTZ4 (partly AOTZO) mainly in the NEP regions are requested for this unique survey.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/AKARI_Phase_3II_MP_Abstracts.pdf
51		LSASS	SHIBAI_LSASS	Shibai, Hiroshi (Graduate School of Science, Nagoya University)		1&2	The ASTRO-F All-Sky Survey	The ASTRO-F All-Sky Survey is an unbiased infrared survey of the whole sky, following the IRAS All-Sky Survey made in 1983. Compared to the IRAS Survey, the wavelength coverage is extended to longer, and the spatial resolution and the point source sensitivity are improved by a factor of several to several tens. The survey wavebands are centered at 9, 20, 60, 90, 140, and 160 microns, respectively. ASTRO-F will allocate the survey scans primarily in Phase I, and supplemental scans in Phase II for completeness of the sky coverage and for reliability and sensitivity. The result of them, more than 90 % of the whole sky can be observed two or three times, more than 40 % of the sky by six times, and much deeper at near the both ecliptic poles. The products planned are a bright point source catalog at the earliest stage, two ore more faint source catalogues at later stage, as well as maps of extended sources. Those products are expected to be a fundamental database for the next generation of advanced observatories, for example Herschel, and JWST, and will complement the SIRTF mission by virtue of its wide sky coverage. The scientific fields covered by the All-Sky Survey spread over most part of modern astronomy /astrophysics, such as, solar-system objects, star-forming regions, young stars, Vega-like stars, late-type stars, SNRs, interstellar matter, near-by galaxies (including Magellanic Clouds), AGNs, star-forming galaxies, large-scale structure of the universe, and cosmology. Follow-up studies are crucial to achieve significant scientific results in many topics.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
52	210	LSNEP	MATSUHARA_LSNEP	Matsuhara, Hideo (ISAS/JAXA)	LS	1&2	The ASTRO-F NEP Survey	We will perform coordinated pointing surveys toward the North Ecliptic Pole (NEP) as a large-area survey program with ASTRO-F. The NEP survey is an ASTRO-F legacy especially for extragalactic astronomy and cosmology: unveiling the dusty star-formation history of the universe out to z=2.5, mass assembly and large scale structure evolution of the universe out to z=4, and the nature of the cosmic infrared background (CIRB). The NEP survey also provides us with unique information on AGN-ULIRG connection, evolution of dwarf galaxies, and Galactic stars. \nTwo kinds of surveys, "NEP-Deep" and "NEP-Wide" are so far planned. "NEP-Deep" will cover 0.5 square degree circular area with 28 pointing per FOV, while "NEP-Wide" covers 6.2 square degrees circular area with 2 pointing observations per FOV. We aim to perform both surveys with uniform depth for all 9 imaging bands of the infrared camera covering 2-24μm wavelengths. In total 954 pointing observations are requested (483 in phase-1). Ground-based optical, near infrared, and radio-wave pre-surveys of the area of the NEP survey have been obtained and analyzed, the images as well as the source catalogues will be soon open to the ASTRO-F team. Also submillimeter (with BLAST), UV (with GALEX), X-ray (with XMM) surveys are under consideration.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
53	211	LSNEP	MATSUHARA_LSNEP	Matsuhara, Hideo (ISAS/JAXA)	LS	1&2	The ASTRO-F NEP Survey	We will perform coordinated pointing surveys toward the North Ecliptic Pole (NEP) as a large-area survey program with ASTRO-F. The NEP survey is an ASTRO-F legacy especially for extragalactic astronomy and cosmology: unveiling the dusty star-formation history of the universe out to z=2.5, mass assembly and large scale structure evolution of the universe out to z=4, and the nature of the cosmic infrared background (CIRB). The NEP survey also provides us with unique information on AGN-ULIRG connection, evolution of dwarf galaxies, and Galactic stars. \nTwo kinds of surveys, "NEP-Deep" and "NEP-Wide" are so far planned. "NEP-Deep" will cover 0.5 square degree circular area with 28 pointing per FOV, while "NEP-Wide" covers 6.2 square degrees circular area with 2 pointing observations per FOV. We aim to perform both surveys with uniform depth for all 9 imaging bands of the infrared camera covering 2-24μm wavelengths. In total 954 pointing observations are requested (483 in phase-1). Ground-based optical, near infrared, and radio-wave pre-surveys of the area of the NEP survey have been obtained and analyzed, the images as well as the source catalogues will be soon open to the ASTRO-F team. Also submillimeter (with BLAST), UV (with GALEX), X-ray (with XMM) surveys are under consideration.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
54	220	LSLMC	ONAKA_LSLMC	Onaka, Takashi (Department of Astronomy, Graduate School of Science, University of Tokyo)	LS	1&2	The ASTRO-F LMC Survey	This Large Area Survey (LSLMC) plans to observe about a 15-square-degree area of the Large Magellanic cloud with the ASTRO-F/IRC using 866 pointing observations. The area will be observed with 5 filters (N3, S9, S11, L15, and L24) and the prism (NP) of the IRC in the observing mode of 2-filter observation per pointing (IRC02). These observations together with the FIS all-sky survey observations provide a new significant database for the various researches of the LMC. Particularly mid-infrared images of S11 and L15, the NIR spectroscopy, and the FIS 4-band data are unique to the ASTRO-F, which the SST will not be able to provide. The expected data can address a number of astrophysical problems, ranging from birth to death of stars, including protostars, late-type stars, super nova remnants, and interstellar medium, and give us a first insight into detailed material circulation in a galaxy. The 5-band + prism data can distinguish and identify the nature of detected objects, such as proto-stellar objects, young stellar objects, or asymptotic giant branch (AGB) stars. This survey is expected to detect most of Herbig Ae/Be stars and easily find out dusty AGB stars in the LMC. The spectra will elucidate the physical conditions and properties of the interstellar dust and gas in terms of the unidentified infrared bands and the mid-infrared continuum. We plan to provide a point source catalog within a year after the completion of the observations, followed by a faint source catalogue, mosaic images, and spectroscopic data.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
55	311	DEMDC	null	Kandori, Ryo (National Astronomical Observatory of Japan)	OT-ISAS	2	Deep Extinction Maps of Dense Cores	Taking an advantage of high sensitivity observations from space, we propose to perform both near-infrared (2-5.5 micron; K, L, M band) and mid-infrared (5.8-8.4 micron) imaging observations toward 47 dense cores using the Astro-F/IRC. The aim of our research is to reveal density structure of dense cores on the basis of the measurement of dust extinction (Av). Since the column density of dense cores increases as gravitational collapse proceeds, the cores with large extinction should be in the late phase of dynamical evolution to form stars. However, the dynamic range of ground-based infrared observations (Av < 50 mag) is not enough to investigate the structure of such kind of cores. The measurement of extinction at both near- and mid-infrared wavelengths can reveal internal structure of highly opaque cores (Av > 50 mag) with high angular resolution (typically 2" - 10"). This study will enable us to investigate detailed density structure inside very dense cores.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
56	221	LSLMC	ONAKA_LSLMC	Onaka, Takashi (Department of Astronomy, Graduate School of Science, University of Tokyo)	LS	1&2	The ASTRO-F LMC Survey	This Large Area Survey (LSLMC) plans to observe about a 15-square-degree area of the Large Magellanic cloud with the ASTRO-F/IRC using 866 pointing observations. The area will be observed with 5 filters (N3, S9, S11, L15, and L24) and the prism (NP) of the IRC in the observing mode of 2-filter observation per pointing (IRC02). These observations together with the FIS all-sky survey observations provide a new significant database for the various researches of the LMC. Particularly mid-infrared images of S11 and L15, the NIR spectroscopy, and the FIS 4-band data are unique to the ASTRO-F, which the SST will not be able to provide. The expected data can address a number of astrophysical problems, ranging from birth to death of stars, including protostars, late-type stars, super nova remnants, and interstellar medium, and give us a first insight into detailed material circulation in a galaxy. The 5-band + prism data can distinguish and identify the nature of detected objects, such as proto-stellar objects, young stellar objects, or asymptotic giant branch (AGB) stars. This survey is expected to detect most of Herbig Ae/Be stars and easily find out dusty AGB stars in the LMC. The spectra will elucidate the physical conditions and properties of the interstellar dust and gas in terms of the unidentified infrared bands and the mid-infrared continuum. We plan to provide a point source catalog within a year after the completion of the observations, followed by a faint source catalogue, mosaic images, and spectroscopic data.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/ASTRO-F_LSMP_Abstracts.pdf
57	501	PVFIS	PV_PVFIS	FIS Team	PV	1&2	PV for FIS
58	502	PVIRC	PV_PVIRC	IRC Team	PV	1&2	PV for IRC
59	503	PVIRC	PV_PVIRC	IRC Team	PV	1&2	PV for IRC
60	511	DTFIS	DT_DTFIS	FIS Team	DT	1&2	DT for FIS
61	512	DTIRC	DT_DTIRC	IRC Team	DT	1&2	DT for IRC
62	514	IDERR	ID_ERROR	ID_ERROR
63	520	DTIRC	DT_DTIRC_P3	IRC Team	DT	3	DT for IRC
64	301	ISICE	AIKAWA_ISICE	Aikawa, Yuri (Dept. of Earth and Planetary Sciences, Kobe University)	OT-ISAS	2	Formation and Evolution of Interstellar Ice	We observe the absorption of ice bands in star forming regions. Most of the background stars behind molecular clouds, low-mass protostars, and protoplanetary disks are too faint for the spectroscopic observation from the ground. The high sensitivity of Astro-F is required to investigate the chemical composition of ice towards these objects. Spitzer Space Telescope is currently undertaking similar ice observations, but it is restricted to lambda > 5 micron. Astro-F is currently the unique space telescope to observe the wavelength region of 3-5 micron, which contains various important ice bands.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
65	302	FISPL	DOI_FISPL	Doi, Yasuo (Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo)	OT-ISAS	2	Observation of FIR Polarimetry with FIS/FTS	Far-infrared (FIR) polarimetry of interstellar dust particles by ASTRO-F/FIS is proposed. Polarimetry in a FIR waveband is a powerful tool to investigate interstellar magnetic fields especially in the deep core regions of interstellar clouds. Thanks to its low absorption rate, FIR light can penetrate into the core regions of star-forming clouds, in which magnetic fields may play important roles in star-formation processes. FIR polarimetry, however, has been rarely done so far, because of the technical difficulties. The ASTRO-F/FIS has high sensitivity in 50-180um and its beam-splitting polarizer in a Fourier spectrometer can be applied to a measurement of an astronomical polarization. By observing both in spectroscopic mode and in photometric mode, we can measure FIR polarization of an astronomical object. In addition to the study of magnetic fields, FIR polarimetry can be a unique technique to investigate dust properties, such as shape, size and degree of alignment, because the FIR polarimetry is a direct measurement of thermal emission from interstellar dust particles. We propose to observe N159/N160 HII complexes to study dust properties as well as distributions of interstellar magnetic fields. These regions are adjacent active high-mass star formation regions in the LMC. Though the two regions show almost the same H2 molecular line intensity, CO emission is 4 times stronger in the N159 than in the N160. So the N160 region is more evolved and photo-dissociated. By observing with the ASTRO-F/FIS, we can expect that we will be able to study the time evolution of interstellar magnetic fields as well as dust properties in such active star-formation regions.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
66	303	EGAMI	EGAMI_EGAMI	Egami, Eiichi (University of Arizona)	OT-ISAS	2	Astro-F Ultra-Deep Imaging/Spectroscopy of the Spitzer/IRAC Dark Field	We propose to conduct an ultra-deep imaging/spectroscopic survey with Astro-F on the IRAC dark calibrationa field, a dark and clean field near the northern ecliptic pole which is being imaged repeatedly by IRAC for dark calibration. Although not yet widely known among the astronomical community, this field will eventually achieve a depth with IRAC similar to that of the GOODS ultra-deep survey (100 hrs per band). The abundance of high-quality data together with the high visibility to Astro-F makes this field an ideal target for Astro-F to conduct an ultra-deep imaging/spectroscopy survey which will push the Astro-F sensitivity to its limit. We will conduct the deepest Astro-F imaging and multi-object spectroscopy observations on a 10'x10' area, and will study the properties and evolution of infrared-lumninous galaxies at high redshift.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
67	304	BCDDE	HIRASHITA_BCDDE	Hirashita, Hiroyuki (Center for Computational Sciences, University of Tsukuba)	OT-ISAS	2	Blue Compact Dwarf Galaxies as Laboratories of High-z Dust Enrichment	Blue compact dwarf galaxies (BCDs) are characterized by their compactness, small metallicity, and high star formation activity. These characteristics are similar to those expected for high-z primeval galaxies, which are difficult to detect. Here we propose to use nearby BCDs as laboratories of high-z primeval galaxies to infer the dust-enrichment history of the high-z Universe. Dust mass derived from this observation enables us to constrain the dust formation and destruction in a metal-poor (1/10Z_odot) phase. We also derive the dust optical depth, which affects the escape fraction of ionizing photons. Thus, if we apply our results to high z, we can quantify effects of dust on the cosmic reionization.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
68	306	GROTH	IM_GROTH	Im, Myungshin (Seoul National University)	OT-ISAS	2	15 Micron Imaging of Extended Groth Strip	We propose to observe a 1200 sq.arcmin region of the Extended Groth Strip (EGS) at 15 micron with Astro-F IRC. EGS is a very unique galaxy redshift survey field where the high resolution Keck spectra enables us to construct the 3-D map of the universe comparable to the local universe surveys such as Las Campana Redshift Survey and Sloan Digital Sky Survey, while having a very extensive multi-wavelength coverages including the deep Spitzer IRAC (3-8 micron) and MIPS images (24 micron), HST ACS, radio, submm, and Chandra X-ray data. The highly complete redshift coverage of the entire region at the high spectral resolution enables us to identify different density environments (groups, clusters) and to measure the velocity dispersion of individual galaxy for dynamical mass estimate. The Spitzer and other multi-wavelength observations permit us to study the dusty nature of the universe in different environments out to z~2 and beyond. However, there is a large gap in the wavelength coverage between 8 and24 micron of the Spitzer data, which hampers the complete understanding of dusty star formation activities at z =1 - 1.5. Our observation at 15micron will fill the gap between Spitzer's 8 and 24 micron imaging data, and will allow us to (i) understand the influence of silicate absorption and AGN contribution on the star formation estimate for 0.5 < z < 1.5; (ii) sample 7 micron MIR light for z~1 galaxies to trace their dusty star formation history as a function environment; and (iii) understand the AGN/starburst connection at even higher redshifts. No other survey fields can be used for the proposed study, and with a moderate amount of investment (36 pointings), we will be able to gain a significant ground in the study of the environmental/mass dependence of star formation out to z~1 - 1.5.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
69	307	HZQSO	IM_HZQSO	Im, Myungshin (Seoul National University)	OT-ISAS	2	Astro-F Spectroscopic Observation of z = 6 QSOs	We propose to take the rest-frame optical spectra of 5 z = 6 QSOs discovered in the Sloan Digital Sky Survey. Although they are likely the most massive systems in the early universe, many properties of these objects remain unknown, in particular the black hole and chemical abundances. In order to better understand these intriguing yet mysterious QSOs, we propose to use the unique Astro-F capability of NIR/grsim observation to obtain the rest-frame optical spectra which will include important AGN lines such as H-alpha, H-beta, OIII, and Fe complex. This wavelength range is the missing-link of current spectral observationsof high-redshift quasars, while contains the most important diagnostic lines. The proposed observation will; (i) determine the mass of the supermassive blackhole by measuring H-alpha and H-beta velocity widths and the L(5100) continuum; (ii) test if the local correlation of L(5100) vs Balmer line fluxes holds; (iii) investigate the significance of the narrow line regions through the detection of OIII, (iv) investigate the chemical enrichment history through Fe complex; and (v) see any evidence if there is a significant amount of star forming activity by looking at OII. Our observation will shed a new light on the properties of z = 6 QSOs, and will serve as the scientific validation of the usage of NIR/grism mode on future high-z QSO studies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
70	308	SMCPM	ITA_SMCPM	Ita, Yoshifusa (Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)	OT-ISAS	2	The role of pulsation in mass loss along the Asymptotic Giant Branch	We propose to observe variable AGB stars in the SMC with the IRC AOT02 and AOT04. We carefully selected fourteen 10'x10' areas in the SMC based on our near-IR (NIR) variable star monitoring survey in the Magellanic Clouds. They contain statistically significant number of AGB stars, that is, dozens of heavily mass-losing AGB stars, hundreds of moderately mass-losing AGB stars, and thousands of weakly mass-losing early-AGB or RGB stars. From our NIR monitoring survey, most of them are now known to be variable stars of wide variety of types pulsating in various pulsation modes. The ASTRO-F mid-IR photometric data will enable us to estimate their mass loss rates and also its mid-IR spectroscopic data will tell us the chemical composition of their circumstellar dust grains. Therefore, the combined data between ASTRO-F and our NIR survey allows us to investigate directly the relationship between the pulsation and the mass loss. Our primary goal is to study the role of pulsation in the mass loss process and their infrared characteristics. We also aim to study the dependence of metallicity on the mass loss and the AGB evolution by comparing the results from this proposed observation with the ASTRO-F LMC Large Area Survey. The total pointings requested for this proposal is 35.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
71	309	EXOSP	ITOH_EXOSP	Itoh, Yoichi (Graduate School of Sci. and Tech., Kobe University)	OT-ISAS	2	Spectroscopic Search for Atmospere of an Extra-Solar Planet	We propose spectroscopic observations of atmosphere of an extra-solar planet, using Astro-F/NIR and MIR-S. We attempt to detect the wide and deep absorption band of methane at 3 micron from a hot Jupiter, using transit events. When the planet is located behind the central star, we detect a spectrum of the central star, whereas we obtain a composite spectrum of the central star and the planet at the rest of the period. We can extract the spectrum of the atmosphere of the planet with high precision by subtracting the spectrum of the central star from the composite spectrum. By ground-based observations, even wide and deep features of water and methane cannot be detected due to the telluric absorption. This observation can be carried out only by an infrared satellite. This will show the first definitive evidence for the atmosphere of an extra-solar planet.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
72	310	DCFIB	JEONG_DCFIB	JEONG, WoongSeob (Institute of Space and Astronautical Science)	OT-ISAS	2	The Detection of Cosmic Far-Infrared Background	The ASTRO-F observation of Cosmic Far-Infrared Background Radiation near South Ecliptic Pole (SEP) is the one of the ASTRO-F mission programs. This observation in FIS slow scan mode will map out the survey area of more than 15 square degrees. However, this observation is only limited near the SEP regions. In order to detect Cosmic Far-Infrared Background (CFIRB) fluctuation effectively, we have to analyse carefully the spatial structure of cirrus emission at different Galactic latitudes. We propose to carry out deep far-Infrared imaging of regions of different Galactic latitudes. The image patches in low-to-medium cirrus regions can be obtained to segregate the CFIRB fluctuation from the cirrus fluctuation expressed as the power spectrum with a simple power-law. In order to detect CFIRB fluctuation expected from our models, we require at least the sky area of 490 arcmin^2 which can be easily covered by 1 pointing observation of FIS slow scan mode. The detected CFIRB fluctuation will help us to distinguish the evolutionary scenarios of galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
73	317	ETASP	null	Matsuo, Hiroshi (National Astronomical Observatory of Japan)	OT-ISAS	2	Far-Infrared Spectroscopic Observation of Eta Carinae	We are going to make far-infrared spectroscopic observation of one of the most massive star in our galaxy, Eta Carinae. The observation will be made by far-infrared spectrometer with high frequency resolution mode to make spectroscopic image of dust and gas distribution around the star. This is the first spectroscopic imaging observaiton of Eta Carinae and could be a good observing targe for FTS/FIS. From the observation we can estimate evolutional history of the the most massive stars in the universe, which could be a template for masive stars in the early history of the universe itself.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
74	312	NSPHQ	null	Kawara, Kimiaki (Institute of Astronomy, University of Tokyo)	OT-ISAS	2	IRC NIR Spectroscopy of High-Redshift Quasars	A delay of 1-2 Gyr in Fe enrichment relative to Mg represents a potential chronometer for measuring the age of quasars. With this idea in mind, several groups plot the FeII/MgII as a function of redshift. However, there are no trends of the expected break in a plot of FeII/MgII up to z = 6.4. Two causes which might obscure the break in FeII/MgII are possible. (1) The emissivity of FeII emission depends on not only the iron abundance but also non-abundance factors such as radiation field and gas density in broad line region. (2) Subtracting power-law and Balmer continua, which significantly contributes to the wavelength range where FeII and MgII emission exit, does not be performed accurately because of narrow wavelength coverage of observed spectrum. By mean of correlation analysis for our low-redshift sample and comparison between observed spectra and synthetic spectra predicted by the photoionization code, we found that observing the optical FeII emission is necessary to correct for the non-abundance effects. We also found that the error and deviation of measured FeII/MgII from the spectra with wavelength coverage from UV to optical in rest wavelength become half of those from spectra without optical part. Thus, we propose to do IRC NIR spectroscopy of 11 quasars at z = 3.9-6.4 to observe optical spectra in rest wavelength. Obtained IRC spectra will be combined with spectra observed with ground-based telescopes, and we will obtain the spectra with wide wavelength coverage from 1200 to 6600 Angstrom in rest wavelength. This wide wavelength coverage allows us for the first time to observe FeII(UV) and FeII(opt) emission simultaneously, and allows us to correct for the non-abundance effects for high-redshift quasars. This may enable us to find the expected break in FeII/MgII, and also to derive Fe/Mg abundance ratio, which allows us to test various models of galaxy formation and chemical evolution.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
75	313	WDISK	null	Kitamura, Yoshimi (Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)	OT-ISAS	2	Evolution of the disks around weak-line T Tauri stars in Chamaeleon	We would like to propose a sensitive survey of protoplanetary disks around weak-line T Tauri stars with the Astro-F. Our main goal is to reveal the evolution of the disks in the possible planet building stage of ~ 10 Myr, and therefore, the target list of this study consists of weak-line T Tauri stars (WTTSs) with ages of ~ 10 Myr in the Chamaeleon region (d = 140 pc). Although the target sources cannot be observed in the Star Formation MP owing to the limited number of pointing observations, they are of great significance in revealing the disk evolution at ~ 10 Myr. The total number of the sources is 49. In this study, to obtain the disk spectral energy distribution (SED) over 10 - 100 micron, we will perform pointing observations of the WTTS disks with both the FIS and the IRC: we adopt the AOTs of FIS01 and IRC11 (L and N). The number of the pointings, therefore, is estimated to be 147 (A: 49 with FIS, B: 49 with MIR-L, C: 49 with MIR-S). Since the Astro-F survey can detect the disks with very high sensitivity in dust mass of the lunar mass, comparable to that of debris disks around main-sequence stars, we will be able to unveil the evolution of disk dust mass with good statistics during the weak-line T Tauri stage of ~ 10 Myr: the transition stage from a protoplanetary to debris disk due to planet building. Together with the SF MP, this survey is one of the most sensitive unbiased surveys of weak-line T Tauri stars in Chamaeleon. Furthermore, the detailed analysis of the disk SEDs based on theoretical models provides us useful information about the evolution of disk internal structures (i.e., the disk clearing in the innermost regions) relevant to planet building at ~ 10 Myr. Combining our sample with that of the SF MP also makes it possible to understand how the star/disk system forms and evolves in the Chamaeleon cloud.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
76	314	FIREC	null	Kitayama, Tetsu (Department of Physics, Toho University)	OT-ISAS	2	Far-infrared Emission from the Coma Cluster of Galaxies	We propose FIS observations of the Coma cluster of galaxies (A1656), aiming at the first firm detection of intergalactic dust grains. Clusters of galaxies provide a unique environment of dust-gas interactions; the X-ray emitting plasma can heat the dust to 10-20 K via collisions, as well as destroy small grains via sputtering. Recent claim of detecting collisionally heated dust grains in Coma by ISOPHOT (Stickel et al. 2002), however, has been questioned owing to insufficient quality of the data. With FIS on ASTRO-F, we can test their result unambiguously for the first time. In addition, multi-wavelength detections enable us to determine both the amount and the mean temperature of the grains. Combined with X-ray and optical data, they further provide powerful clues to understanding the dust-gas interaction and the ejection history of dust from galaxies. In case of no detection, we are still able to place severe constraints on its amount, which is a meaningful step forward in the long-standing argument regarding the intergalactic dust. Our observation will therefore provide a unique opportunity of probing the nature of dust grains in relation to the ambient hot gas and host galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
77	315	CLNEP	null	Kodama, Tadayuki (National Astronomical Observatory)	OT-ISAS	2	Deep IR Imaging of the Unique NEP Cluster at z=0.813	We propose to take much deeper IR imaging on the unique X-ray selected NEP cluster (RXJ1716.4+6708) at z=0.813 with IRC on Astro-F than is planned as a part of the Mission Program (CLEVL). With its excellent visibility of Astro-F and lowest zodiacal light contribution offer us a unique opportunity for us to take unprecedentedly deep IR imaging on an intermediate redshift cluster down to 2 x 10^9 Msun for passively evolving galaxies at 3 micron and to 4 Msun/yr for star-forming galaxies at 15 micron. We have already completed a deep and wide multi-colour (VRi'z') optical imaging on this cluster with Suprime-Cam on Subaru, reaching down to M*+4 (well matching to 2 x 10^9 Msun) over a large field of view (30'). Also, we plan to conduct a panoramic narrow-band imaging survey with MOIRCS targeting Halpha emissions from cluster members at 1.19 micron in the near future. The unique aspects that this proposed IRC observation will provide are two-fold: (1) dust-free properties such as stellar masses of IR selected galaxies, and (2) dusty star forming activities traced by PAH features. Both are crucial to form a general view of galaxy evolution in dense environment at z=0.8 which may be largely hidden in the ground-based optical-NIR observations.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
78	316	VELLO	null	Lee, ChangWon (Korea Astronomy and Space Science Institute)	OT-ISAS	2	A Search for Very Low Luminosity Objects in Dense Molecular Cores	Recently discovered Very Low luminosity Objects toward dense molecular cores open a new pathway of the very early processes of the low star formation because the nature of the VeLLO is very different from that of the typical protostar. It is even less fainter (< ~ 0.09 lsun) than any other protostar, but showing the smallest outflow in its extent (~ 500pc) and mass ( < 10^-4 msun), and the smallest accretion rate ( 10^-9- 10^-8 msun yr^-1). These properties were found from only one VeLLO. Whether these are generally applied to other VeLLO is totally questionable at this moment. A systematic study of the large sample of the VeLLO is necessary. We propose to observe 20 starless cores showing 'expansion' asymmetry, a complex mixture of 'infall' and 'expansion' asymmetry in the molecular lines, and showing unusually broad line width, to search for a VeLLO. This survey will help to collect a whole ensemble of VeLLOs discovered in Infrared Space Telescopes, to clarify the physical properties of the VeLLOs, and eventually to understand the physical process in the very low mass protostar or proto-brown dwarf.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
79	318	COABS	null	Nakagawa, Takao (ISAS/JAXA)	OT-ISAS	2	Probing molecular tori n Obscured AGN through CO Absorption	In order to observe the molecular tori in Seyfert2 directly and to reveal their physical conditions, we propose to obtain spectra of fundamental vibration-rotation band line absorption of gaseous We propose to make CO around 4.7 micron towards the nuclei of bright Seyfert~2 galaxies and ULIRGs, using the central engine as a background continuum source. This is a new and unique technique which allows us to determine temperatures and column densities of molecular clouds very accurately. It is now generally accepted that much of the variety in Active Galactic Nuclei (AGN) types is just the result of varying orientation relative to the line of sight (unified model for AGN). The molecular torus is the key element for this model. However, physical conditions of the tori themselves have never been measured directly, and the exact nature of the molecular tori is still controversial, The proposed observation, with the detection of R- and P-branches of many lines at different excitation levels, will enable us to make the first "direct" observation of the physical conditions of molecular tori themselves. This will serve as the critical test for the "unified model".	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
80	319	COLVN	null	Onishi, Toshikazu (Nagoya University)	OT-ISAS	2	Extreme Colors: The smoking Gun of Dust Aggregation and Fragmentation	Dust is implicated in a wide variety of interstellar physics ranging from photoelectric heating to molecule formation. In order to understand these processes it is necessary to know the properties of dust in some detail, including size distribution and size-related changes in grain composition. Furthermore, dust properties evolve as dust cycles through different Galactic environments. It is by examination of such changes that more confidence can be gained regarding the underlying physical mechanisms. Most of the dust destruction takes place in the diffuse ISM, where IR color variations show a flattening of the dust size distribution due to shock-induced grain-grain and gas-grain collisions. Dust fragmentation must be compensated by efficient grain aggregation, mainly in denser molecular regions. The selection of regions in the diffuse ISM suitable for observations is rather challenging since the dynamical history and the physical parameters (shock velocity, energy) are generally unknown. In addition, aggregation and fragmentation are usually intermixed, complicating physical interpretation. Here, we propose an original approach, focusing on two clouds which exhibit large color variations and have been affected recently by the passage of a slow shock causing dust fragmentation but not powerful enough to have affected the gravitational integrity of the clouds. The AstroF data will allow us to fully characterize the dust size distribution and to pinpoint precisely the spatial locations and spectral signatures of its variations, providing a unique perspective on the processes regulating dust fragmentation and aggregation in space.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
81	320	IRSEP	null	Pearson, Chris (ISAS/JAXA)	OT-ISAS	2	Mid-Infrared Imaging of the ASTRO-F Deep SEP Field	The ASTRO-F Deep Field at the South Ecliptic Pole (SEP) has been secured as an ASTRO-F mission program. This field will be imaged in all 4 FIS bands and will be the deepest image ever taken of the Universe at far-infrared wavelengths far exceeding the All Sky Survey in depth. However, this field is at present devoid of any deep mid-infrared imaging and thus will suffer severe constraints in the interpretation of the detected far-infrared sources. We propose deep mid-infrared imaging with the IRC over some portion of this field to identify and characterize the emission from the sources detected by the FIS deep survey. This mid-infrared imaging will allow the estimation of photometric redshifts and will be the only way with which it will be possible to identify the sources responsible for the far-infrared background and to solve the degeneracy between the temperature of the dust emission spectra with redshift by classifying the infrared galaxy populations. Deep mid-infrared observations with the IRC in this field will be vital if the FIS SEP survey is to provide a valuable legacy from the ASTRO-F mission to the investigation of galaxy evolution in the infrared.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
82	321	DSTGC	null	Pyo, Jeonghyun (Seoul National University)	OT-ISAS	2	Dust in Globular Clusters	We propose to search and obtain far-infrared (FIR) emission of dust in the cores of globular clusters (GCs) and to understand the mechanism of dust formation and stripping in metal-rich and metal-poor GCs. The apparent absence of dust and gas in globular clusters had been a long standing problem in Galactic astronomy. Recent observations from ISO and Spitzer, however, revealed FIR emission by dust in the center of NGC 7078 with somewhat lower brightness than expectation. Therefore, it is opportune to survey the central regions of globular clusters and to differentiate the clusters having dust from the ones not having. This research aims at understanding the mechanisms of the removal of the cluster dust under the Galactic environment. The targets are selected within 30 kpc from the solar neighborhood with variety of metallicity and Galactic height. The observations will be performed with FIS slow-scan mode.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
83	322	SHARP	null	SAKON, ITSUKI (Department of Astronomy Graduate School of Science University of Tokyo)	OT-ISAS	2	ASTRO-F/IRC Slit-less Spectroscopy of Hickson Compact Groups	We propose near- to mid-infrared slit-less spectroscopy of Hickson Comapact groups (HCGs) to investigate the chemical processing of ubiquitous Poly-cyclic aromatic hydrocarbons (PAHs) in on-going evolutional site of galaxies. HCGs in our samples are all detected by IRAS and present the signs of Wolf-Rayet activities with several stages of interactions classified into three groups: merging, strongly interacting, and mildly interacting groups. These targets are quite unique in that they provide us environments with ranges of interactions among group members resulting in induced intense star forming activities and the formation of tidal dwarf galaxies. Especially HCG 31 as well as HCG 92 is one of the best studied compact groups and is made up of 8 galaxies including active central starburst ( in the merging region of Galaxy A+C) and the tidal dwarf galaxies (Galaxy E and F). The ISO spetra of the merging region of A+C has revealed the possible primitive species of PAHs. Since PAHs are supposed to be changed in nature and chemivally evolve in these highly dense environments, they are quite useful to constrain the dust environment in each of the group members with various evolutional stages. For this purpose, near- to mid- infrared spectra of whole members of a system is needed, which are brought from the ASTRO-F IRC slit-less spectroscopy (NIR/NP, MIR-S/SG1 and SG2) with, by far, much more efficiency and effectiveness than SPITZER IRS; every group has entirely a size of several arcmin made up of some relatively compact (~several arcsec) galaxies, which enable us to obtain the spectra from 2um to 13um of whole members at once with only one pointing. In these spectra, we can pick up the various UIR features at 3.3, 3.4, 6.2, 7.7, 8.6, 11.0, 11.2, 12.0, and 12.7um, whose relative band ratios as well as each intensity relative to the underlying continuum can be used effectively to determine the nature of PAHs and how they chemically evolve, which would potentially give us a scenario of transmigration of ubiquitous PAHs; where and how PAHs are created from the small carbonaceous materials in the inter stellar medium supplied by supernovae and/or Planetary Nebulae and, in reverse, how PAHs are collapsed back into them under the rule of galaxy evolutions. The Slit-less spectroscopy of HCGs with ASTRO-F IRC will surely lead us go further insight into the evolutional scenario of interstellar dust in the on-going evolution of galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
84	323	Z1LBG	null	Shim, Hyunjin (Astronomy Program, Seoul National University)	OT-ISAS	2	UV-selected Lyman Break Galaxies at 0.6<z<1.3 in the Spitzer FLS	We proposed to image Spitzer First Look survey area with ASTRO-F/IRC to obtain 11micron/15micron flux for 0.6<z<1.3 star forming galaxies. The sample galaxies are selected using rest frame UV colors, which is comparable to lyman break galaxies at higher redshift in the point of UV luminosity and morphology. The stellar mass and dust properties of lyman break galaxies at z>3 are still intriguing issue, because they are too faint to be detected at infrared regime. The alternative method is to study dust-related properties of lyman break galaxy counterparts at closer universe. We expect to detect enough(a few hundreds) number of sample objects with a depth of 40microJy at 11micron. Since 11micron and 15 micron imaging represent 6.7micron PAH emission of z=1 galaxies, the result can be directly imply the meaning of 24micron flux from z=3 LBGs. Our main scientific goals are: (1) to construct MIR luminosity function of lyman break galaxy counterparts at 0.6<z<1.3 (2) to see the evolution of MIR spectral energy distribution along the redshift. The observed datasets will be applicable to broad range of other topics including the correlation of SFR with morphological characteristics and the method to weed out AGNs from starburst samples. With the wide area coverage and the existence of multi wavelength data including UV/u band imaging, our observation will allow us profound understandings on star formation in early universe.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
85	324	FIRCL	null	Takagi, Toshinobu (University of Kent)	OT-ISAS	2	ULIRGs in clusters of galaxies at z~1	We propose confusion limited far-infrared surveys of eight clusters at z~1, in order to identify ultraluminous infrared galaxies (ULIRGs) in these distant clusters. While no nearby ULIRGs found by the IRAS all-sky survey reside in cluster regions, submillimetre observations with SCUBA revealed ULIRGs in (proto-)cluster regions at z>~1. Nevertheless, the sample of ULIRGs in clusters are very limited. Our targets are adopted from the Mission Program, CLEVL for which N3 and L15 observations are allocated. This program is complementary to this Mission Program. Far-infrared observations allow us to estimate the total infrared luminosity in clusters more reliably than using mid-infrared observations in the Mission Program, which observes the redshifted 7.7 micron PAH feature. On the other hand, we require sensitive mid-infrared observations with high angular resolution to identify optical counterparts of far-infrared sources. With this program, we intend to obtain a complete picture of star formation activity hidden by dust in clusters at z~1. With the help of panoramic deep optical images, we also study the environmental effects to trigger intense dusty starburst event.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
86	325	SGPWD	null	Tamura, Motohide (National Astronomical Observatory of Japan)	OT-ISAS	2	Search for Giant Planets around White Dwarfs	We propose to survey a sample of 25 white dwarfs (WDs) with ASTRO-F and IRC to search for mid-IR excesses using its prism spectroscopy mode (NP) at the wavelengths between 1.7 and 5.5 microns. The aim of our proposal is to detect planets around WDs. WDs are typically 1,000-10,000 times less luminous than their progenitors, thus in the IR wavelengths, the contrast between a self-luminous planet and a WD is much more favorable than between a planet and a main-sequence star. The gain in contrast and IR excess is strongest in the mid-IR, where the planet's thermal emission peaks well into the WD's Rayleigh-Jeans tail. Since all field WDs are descended from stars more massive than the Sun, our results will constrain the frequency of planets of down to a few Jupiter masses around intermediate-mass stars.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
87	326	SPECS	YAMAMURA_SPECS	YAMAMURA, Issei (ISAS/JAXA)	OT-ISAS	2	NIR--MIR Spectroscopic Survey of Selected Areas in the Galactic Plane	We propose a spectroscopic survey of selected areas in the Galactic plain. The observation is carried out in the AOT IRC04 (spectroscopic mode), with an option of a;Nc (prism + imaging field). Target positions are l = +-45, +-90, +- 135, and 180 deg. b = 5 deg. Five fields continuously connected along the scan direction are observed. Total number of requested pointing is A = 35, B = 35, C= 35, respectively. Main target of this programme is stars of M or later spectral types. These stars are in the last phase of their evolution, the Asymptotic Giant Branch (AGB) phase. These stars show various molecular bands in the near- to mid-infrared wavelengths. These features arise from the region just outside of their photosphere. This "extended atmosphere" is known to play an important role on the formation of dust grains and their subsequent acceleration as stellar wind (mass-loss wind). ASTRO-F/IRC is an only instrument currently available for observing spectra in the near-infrared region. In addition, MIR-S channel simultaneously takes the data in the mid-infrared range, which provide additional information of dust envelope. With these NIR--MIR spectra, we plan to carry out following three studies. (1) spectral classification of stars and their distribution in the Galaxy, (2) statistical study of relation between NIR molecular bands and dust emission, (3) search for peculiar stars, such like silicate carbon stars. At some of the target position we may be suffered by source confusion. Even such case we still can take hundreds of spectra of bright sources. The expected number of spectra obtained is something 10000--30000.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-jk.pdf
88	401	COSMS	AUSSEL_COSMS	Aussel, Herve (CNRS / AIM, France)	OT-ESA	2	Star Formation and Environment in the COSMOS Field	We propose to map a 90'x30' strip in the COSMOS field at 15 microns with the MIR-L camera of ASTRO-F to a depth of 185 micro Janskies (5 sigma). These observations will fill the gap in our Spitzer coverage of the field at 8 and 24 microns and enable us to observe the emission from Polycyclic Aromatic Hydrocarbures (PAH) of star forming galaxies and very hot dust of AGNs from z=0 to 2.5 as they are redshifted through our passbands. This dataset will alleviate the problem of measuring star formation from different indicators at different redshifts by observing the same rest-frame region of the mid-infrared spectrum of galaxies from z=0 to z=2.5. The combination of 15 and 24 microns data will allow us, together with our photometric redshifts, to correctly infer the total infrared emission of our galaxies from their mid-infrared emission, and derive more accurate star formation rates. Combining this sample of ~2500 galaxies with the COSMOS multiwavelength data, we will quantitatively study: i) The evolution of dust-enshrouded star formation with redshift. ii) The impact of environment in the triggering of the starburst and AGNs phases of galaxies. iii) The morphology of Mid Infra-red selected star forming galaxies out to z=2.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
89	402	DISKB	BARRADOYNAVASCUES_DISKB	Barrado y Navascues, David (LAEFF-INTA, Spain)	OT-ESA	2	Accretion and protoplanetary disks in brown dwarfs	We want to study a sample of brown dwarfs with disks and different ages (from 1 to 12 Myr) in order to establish the dependence with age of the grain growth and dust settling. This process is the initial and necessary step toward the formation planetesimals and planet formation. The proposed observations will allow us to: i) Built accurate Spectral Energy Distribution from the optical to 14 or 25 micron. ii) Search for evidence of truncated disks, in order to test the models of formation. iii) Study the composition and evolution of the disks, grain growth, dust settling/crystallization, and provide important inputs for the models of disks. In particular, we will focus on the silicates present at the S11 band. iv) The data at longer wavelengths (L15 & 25) will be very helpful in order to constrain the disk mass. v) By comparing samples with the same age (members of the same association), we will study the dependence with mass/spectra type and other parameters. vi) Study the timescales of disk decay (by comparing the SFRs with different ages). vii) Compare the disk properties (obtained with mid-IR observations) with the accretion properties (obtained with Halpha activity), in order to get crucial informations on the disk structure at small scale (where the Halpha emission takes place) and larger scale (where the mid-IR excess takes place).	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
90	403	OBSTR	BLOMME_OBSTR	Blomme, Ronny (Royal Observatory of Belgium)	OT-ESA	2	Structure in the stellar winds of OB stars	There is considerable evidence for structure (clumping) in the radiatively driven stellar winds of hot stars. The existence of clumping has important consequences for mass-loss rate determinations. Present mass-loss rates are usually not corrected for clumping, thereby providing incorrect input for stellar and galactic evolution models, and possibly influencing the extragalactic distances determined from Halpha observations of OB supergiants. Far-infrared observations are ideally suited to study the effect of clumping at a few stellar radii above the star's surface. We propose to measure the 60 mum and, possibly 160 mum, continuum fluxes of a few (2-4) representative OB stars. These observations, combined with existing Halpha and radio data, will allow us to quantify the amount of clumping. This, in turn, will put considerable constraints on the theoretical models for clumping, which is vital to our understanding of the hydrodynamics of these winds. It will allow the elimination of the systematic error in the mass-loss rate determinations.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
91	404	IRLBG	BURGARELLA_IRLBG	Burgarella, Denis (OAMP/LAM, France)	OT-ESA	2	Calibrating mid-IR dust attenuation tracers for LBGs with ASTRO-F	Lyman Break Galaxies (LBGs) are the main objects observed at high redshift in the rest-frame ultraviolet. They are, therefore, used to estimate the ultraviolet cosmic star formation density. However, to do so, we need to apply some correction for dust attenuation. The usual wy of correcting is by applying a correction determined from the ultraviolet slope beta of the spectrum. However, this method is now proven to provide dispersed and probably bad estimates. A good estimator is the Far-Infrared (FIR) to Ultraviolet (UV) FIR/UV ratio which gives much better results. But we need to estimate the FIR/UV ratio and the best way is to use the FIR. However, the FIR is not available for Lyman Break Galaxies and we propose to verify whether mid-IR (MIR) fluxes can provide good estimate for the total bolometric dust luminosity for LBG as was previously proposed. Several bands are available but one of the most promising is only observable from ASTRO-F. This task is not doable for z=3 LBGs which are too faint to be detected at wavelength of about 12 microns and above by SPITZER and ASTRO-F. However, we have built the first LBG sample at z=1 on which we will check the validity of the above methods and provide estimates for the uncertainties. The availability of the z=1 LBG sample and the mid-IR wavelength will provide the first opportunity to check whether UV and FIR cosmic star formation densities can be used simultaneously after corrections.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
92	405	HALOS	BURGDORF_HALOS	Burgdorf, Martin (Liverpool John Moores University, United Kingdom)	OT-ESA	2	Search for Emission Outside the Disks of Edge-on Galaxies	Flat galaxy rotation curves routinely observed out to large radii in HI and in optical emission lines are convincing evidence for the existence of dark matter. As yet, we know very little about the nature of this dark matter. An intriguing possibility is that a population of very cool objects - extreme brown dwarfs or "Jupiters" - accounts for a significant part of its mass. Their intrinsic faintness at visible wavelengths would explain why they have not yet been clearly detected. Guaranteed time (GT) observations with the InfraRed Array Camera (IRAC) on board Spitzer of two famous edge-on galaxies (NGC891 and NGC5907) have yielded good evidence for such a very thick, red disk component that could comprise some of this "missing mass", but the mid-infrared colours as yet offer no clear discriminant of these disks' makeup. We propose to use the IRC MIR channel for follow-up observations of the very thick disks seen in the edge-on IRAC GT program galaxies. By measuring fluxes at 7, 11, 15, and 24 microns we can obtain crucial information for example about the temperature of the objects in these disks and hence get a better idea of their nature. As the expected signal is much smaller than the foreground emission from the zodiacal light, we need the large FoV of the IRC to characterize any spatial variations in the zody emission. The radiation from the very thick disks will then appear as a surface brightness gradient measured as a function of distance on both sides of the galactic midplanes. We request one pointing per observation with AOT IRC02.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
93	411	DEAGB	ENGELS_DEAGB	Engels, Dieter (Hamburger Sternwarte, Germany)	OT-ESA	2	Stars departing from the Asymptotic Giant Branch	I propose to observe a sample of extremely red IRAS sources, which are considered to be in an advanced evolutionary state on the Asymptotic Giant Branch (AGB) or in different phases of their transition to become a Planetary Nebula (PN). The transition process itself is poorly understood. The departure from the AGB is characterized by short timescales, the loss of radial symmetry of the mass loss process, and increasing velocities of the outflows. The large diversity of properties of post-AGB stars is probably reflecting the complex processes involved, and make their identification with particular phases of the transition process difficult. It is proposed to observe with MIR-S the strength and shape of the 10 micron absorption feature which is due to absorption by dust composed of amorphous silicates, and with MIR-L the region 18-25 micron in which emission features of forsterite crystalline silicates are expected to be found. The 10 micron feature decreases in strength while features of crystalline silicates increase their strength during the transition. Optical depths, mass loss rates, and strengths of the dust features of the circumstellar shells will be derived from the observations. The goal is to map the stars on a evolutionary sequence, which characterizes the transition process.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
94	406	HALOS	BURGDORF_HALOS	Burgdorf, Martin (Liverpool John Moores University, United Kingdom)	OT-ESA	2	Search for Emission Outside the Disks of Edge-on Galaxies	Flat galaxy rotation curves routinely observed out to large radii in HI and in optical emission lines are convincing evidence for the existence of dark matter. As yet, we know very little about the nature of this dark matter. An intriguing possibility is that a population of very cool objects - extreme brown dwarfs or "Jupiters" - accounts for a significant part of its mass. Their intrinsic faintness at visible wavelengths would explain why they have not yet been clearly detected. Guaranteed time (GT) observations with the InfraRed Array Camera (IRAC) on board Spitzer of two famous edge-on galaxies (NGC891 and NGC5907) have yielded good evidence for such a very thick, red disk component that could comprise some of this "missing mass", but the mid-infrared colours as yet offer no clear discriminant of these disks' makeup. We propose to use the IRC MIR channel for follow-up observations of the very thick disks seen in the edge-on IRAC GT program galaxies. By measuring fluxes at 7, 11, 15, and 24 microns we can obtain crucial information for example about the temperature of the objects in these disks and hence get a better idea of their nature. As the expected signal is much smaller than the foreground emission from the zodiacal light, we need the large FoV of the IRC to characterize any spatial variations in the zody emission. The radiation from the very thick disks will then appear as a surface brightness gradient measured as a function of distance on both sides of the galactic midplanes. We request one pointing per observation with AOT IRC02.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
95	407	UNIRC	BURGDORF_UNIRC	Burgdorf, Martin (Liverpool John Moores University, United Kingdom)	OT-ESA	2	Near-Infrared Spectroscopy of the Atmospheres of Uranus and Neptune	We propose to study Uranus and Neptune in the near- and mid- infrared with the IRC. The observations will be performed at wavelengths that are not or only poorly accessible to the infrared spectrometer on board Spitzer. Therefore they will address questions that can only be answered by ASTRO-F: - What is the abundance of the disequilibrium species carbon monoxide and phosphine? - What is the spectral shape of the continuum flux of Uranus and Neptune in the near infrared? - Is there fluorescent emission from H3+ and methane? These investigations will yield important information about the diffusion processes in the atmospheres and the electromagnetic environments of both planets.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
96	408	CERN1	CERNICHARO_CERN1	Cernicharo, Jose (DAMIR. IEM-CSIC, Spain)	OT-ESA	2	Dust and gas properties in AGB and post-AGB objects	We propose to carry out a photometric and spectrometric study between 2-200 microns with ASTRO-F of the most prominent AGB and post-AGB objects in our galaxy in order to understand the chemical evolution of dust and the gas as a function of the distance to the central objects and the degree of evolution of the stars. We would like to use the FIS instrument in FTS mode (SED and FULL resolution), and in photometric mode, towards a representative sample of AGB and post-AGB objects rich in carbon and in oxygen. In addition IRC observations (9 filters) of most of them will allow to study, for the first time in most of the proposed AGB objects, the spatial distribution of dust emission in the mid and near-IR. This information is critical when analyzing the molecular emission at all wavelengths as the dust and molecules are strongly coupled radiatively in the far and mid-IR for dusty envelopes. Finally, we would like to use IRC in slit spectroscopy mode to obtain spectra between 2-40 microns from the molecular and dusty envelopes.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
97	409	CERN2	CERNICHARO_CERN2	Cernicharo, Jose (DAMIR. IEM-CSIC, Spain)	OT-ESA	2	Dust, PAHs and molecules in molecular clouds	We would like to study the dust and gas emission in star forming regions and molecular clouds in different physical conditions and evolutionary stages: from low mass stars, and the prominent molecular outflows associated to them, to molecular clouds illuminated from bright stars. The main goal is to study the composition of the dust and its evolution as the clouds evolve from quiescent gas to regions of high velocity shocks and extreme UV radiation. The gas properties at large scale will also be traced by ASTRO-F observations. Observations with the two instruments, in photometric and spectroscopic modes, are proposed to obtain the near, mid and far-IR spectrum in, and around, these objects.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
98	410	BLOBS	CHARMANDARIS_BLOBS	Charmandaris, Vassilis (University of Crete, Greece)	OT-ESA	2	15 Micron Imaging of the z=2.38 Filament	We propose 15 micron mid-infrared imaging of the central 400 arcmin^2 of the J2143-4423 filament structure (Palunas et al. 2004) at z=2.38. Extending more than 100 Mpc, it is the largest known structure above z=2. This field has been imaged with both the Spitzer MIPS 24um and IRAC 3.6-8um cameras, leading to the discovery multiple ultraviolet-bright ULIRGs, including its extended Lyman alpha "blobs". At z=2.38 the Astro-F 15um filter will provide the critical photometric data point between the stellar contribution measured by IRAC and the rest-wavelength 7um flux measured by MIPS, allowing discrimination between warm (AGN) and cool (star-forming) ULIRGs. The Spitzer Space Telescope can not image this area in a reasonable length of time, as its IRS 16um camera has a field-of-view roughly 100 times less than that of the Astro-F Infrared Camera (IRC).	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
99		ADEAS	DELBO_ADEAS	Delbo, Marco (INAF - Astronomical Observatory of Turin, Italy)	OT-ESA	2	ASTRO-F Deep Ecliptic Asteroid Survey	The present knowledge of the the size-frequency distribution (SFD) of main belt asteroids (MBAs) is increasingly uncertain as one goes to smaller sizes, and at a diameter of 1 km, this uncertainty is about a factor of 3. Information on the MBA SFD is crucial to improve our understanding of the mechanisms of formation and evolution of our planetary system and those processes (such as the Yarkovsky effect) invoked to explain the delivery of km-sized asteroids from the main belt to near Earth space. This project - the ASTRO-F Deep Ecliptic Survey (ADEAS) - aims at determining the SFD of main belt asteroids down to sub-kilometer sizes with ASTRO-F. Results expected from this project will thus also be important for understanding the Near Earth Object (NEO) numbers and size distribution. From observations of two (possibly four) 10'x50' sky areas at 0 (and -5 degree) ecliptic latitude will obtain with ASTRO-F the number of km- and sub km- sized asteroids through the entire main belt. Combining ASTRO-F observations with ground based follow up at visual wavelengths we will derive accurate diameters and albedos for all detected asteroids. From our sample of asteroids we will obtain a physically based SFD for small main belt asteroids. A second objective of this proposal, for which we require ASTRO-F to map our "priority B" region at ecliptic latitude -5 degree, addresses the investigation of the puzzling discrepancy in the ecliptic latitude distribution of MBAs discovered by the Spitzer First Look Survey-Ecliptic Plane Component (FLS-EPC). Determining the SFD of main belt asteroids from observations in the mid-infrared is a study that can only be performed from space telescopes. ASTRO-F is a superb instrument, due to the field of view and the sensitivity of the IRC. Furthermore, given its orbit around the Earth, ASTRO-F facilitates the critical ground-based follow-up observations in contrast to observations carried out e.g. from Spitzer.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
100	412	IMAPE	FRASER_IMAPE	Fraser, Helen (University of Strathclyde, United Kingdom)	OT-ESA	2	The spatial distribution of ices in Spitzer-selected molecular cores	In the densest star forming cores, over half the molecular species (excluding H2) are condensed onto dust grains. To effectively study the solid-state chemistry of star-forming cores, we require detailed observations of the abundances, and more importantly the spatial distribution, of as many condensed species as possible, in particular H2O, CO2 and CO. These species are directly observed via their strong stretching-mode bands at 2.5-5 micron seen toward the continua of background stars. We propose to obtain spatially well resolved maps of molecular ices towards a sample of isolated molecular cores located in front of regions with a high density of background stars. The cores have been selected from the sample of molecular cores imaged by Spitzer as part of the "cores to disks" Legacy Science program, and are therefore very well characterized. Astro-F presents a unique opportunity for mapping the spatial distribution of H2O, CO and CO2 ices toward background stars, due to its sensitive spectroscopic capability in the 2-5 micron region as well as its ability to obtain slitless spectroscopy over a large field of view. Ground-based facilities are far from sensitive enough to yield similar data and the Spitzer Space Telescope has no spectroscopic capability below 5.5 micron. While ices can be observed at longer wavelengths, the 2-5 micron region contains the strongest ice bands and background stars are bright, making it crucial for any spatial mapping of interstellar ices. The observing programme includes 28 targets. We will use both the prism (Np) and the grism (Ng) modes with the near-infrared camera (AOT IRC04) to obtain spectroscopy of background stars in the entire field of view. This will enable us to map the distribution of ices on scales of 10-20", or a few 1000 AU in the nearest dark clouds, thereby sampling the spatial scales of the chemistry and freeze-out processes of the most abundant ice species. The combination of the proposed observations with dynamical core models will enable a measurement of the time scales of the formation of water and CO2 ice.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
101	413	AGBPN	GARCIAHERNANDEZ_AGBPN	Garcia Hernandez, Domingo Anibal (European Space Astronomy Centre, ESA, Spain)	OT-ESA	2	The hidden evolution from AGB stars to PNe as seen by ASTRO-F/IRC	We propose to take 5-25 micron ASTRO-F/IRC spectra of a selected sample of heavily obscured objects in the transition phase between the Asymptotic Giant Branch (AGB) stars and the Planetary Nebulae (PNe) stage. They are all bright IRAS sources identified as optically invisible post-AGB stars during previous ground-based observations and they are suspected to represent a hidden population of PNe precursors not previously studied. Their strong obscuration is due to the thick circumstellar shell formed as a consequence of the strong mass loss rate (up to 10^-4 Msun/yr) experienced by these stars at the end of the AGB. Some of them are not even detectable in the near-infrared (<3 microns). In contrast, they are among the brightest sources of the sky at mid- to far-infrared wavelengths and, thus ideally suited to be observed from space with ASTRO-F by using a small number of pointings per target. The transition phase from AGB stars to PNe is thought to be very short (100-1000 years) but it is during this evolutionary phase where crucial processes (i.e. chemical composition changes) take place which completely determine the subsequent evolution of these stars as PNe. With the proposed observations we want to determine for the first time the dominant chemistry (C-rich vs. O-rich) of the dust in the circumstellar shell of these stars and establish connections between the characteristics of the solid state features (strength, relative intensities and shape) and the shape of the underlying continuum observed and the evolutionary stage and/or the mass loss history of each source in the sample. The results obtained will eventually be used to test the current evolutionary models which predict different chemical compositions depending on the initial mass of the progenitor star.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
102	414	FISPN	GARCIALARIO_FISPN	Garcia-Lario, Pedro (European Space Astronomy Centre, ESA, Spain)	OT-ESA	2	Far infrared imaging of young PN and PPNe with ASTRO-F/FIS	In this proposal we plan to take advantage of the sensitivity and spatial resolution of ASTRO-F/FIS and of its wide field of view to perform a systematic study of the infrared size and morphology of a carefully selected sample of very young PNe and proto-PNe in the four FIS filters N60, WIDE-S, N90 and WIDE-L, covering the range from 60 to 160 microns in order to trace the distribution of cool dust in their extended shells. Extended structures with a typical size of ~2 pc will be resolved by ASTRO-F up to distances of ~3 kpc. The main purpose of this research is to recover the mass loss history experienced by these stars in their recent past, an essential ingredient of the models which try to reproduce the AGB to PN transition phase. The results obtained will also be used to try to determine the overall optical properties of the dust (temperature, optical thickness, emissivity) and to impose constraints on the moment when the departure from spherical symmetry took place, if this is detected. The observations resulting from this proposal will undoubtfully constitute a unique database which will serve as a reference for future follow-up observations with the Herschel Space Observatory.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
103	415	EGALS	GOMEZ_EGALS	Gomez, Haley (Cardiff University, United Kingdom)	OT-ESA	2	Understanding the Dust Properties of Ellitpical Galaxies	Elliptical galaxies are thought to be the descendants of the spectacular star-forming galaxies discovered in deep sub-millimetre surveys. How they form into the gas and dust poor systems we see in the local Universe is largely unknown. The processes governing the evolution of the ISM in today's ellipticals is poorly understood and indeed there is no current consensus on the origin of dust seen in recent ISO observations. The two major competing theories are (1) dust formed via stellar mass loss in the galaxy and (2) dust accreted from merging/interacting systems. Elliptical galaxies are an ideal laboratory to study not only the origin of grains (now a controversial question even in our own galaxy), but also their evolution. Despite this, only a small fraction of ellipticals have been observed with ISO and IRAS. This project is designed to be a definitive study of elliptical galaxies, using a statistically significant, unbiased sample, allowing us to globally determine the relationship of the dust to galactic properties as well as the dust properties themselves. The high sensitivity of Astro-f combined with the large field-of-view and wide wavelength coverage from NIR to FIR will enable us to take on such an ambitious survey and begin to address the questions hinted at by previous IR observations.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
104	416	EGALS	GOMEZ_EGALS	Gomez, Haley (Cardiff University, United Kingdom)	OT-ESA	2	Understanding the Dust Properties of Ellitpical Galaxies	Elliptical galaxies are thought to be the descendants of the spectacular star-forming galaxies discovered in deep sub-millimetre surveys. How they form into the gas and dust poor systems we see in the local Universe is largely unknown. The processes governing the evolution of the ISM in today's ellipticals is poorly understood and indeed there is no current consensus on the origin of dust seen in recent ISO observations. The two major competing theories are (1) dust formed via stellar mass loss in the galaxy and (2) dust accreted from merging/interacting systems. Elliptical galaxies are an ideal laboratory to study not only the origin of grains (now a controversial question even in our own galaxy), but also their evolution. Despite this, only a small fraction of ellipticals have been observed with ISO and IRAS. This project is designed to be a definitive study of elliptical galaxies, using a statistically significant, unbiased sample, allowing us to globally determine the relationship of the dust to galactic properties as well as the dust properties themselves. The high sensitivity of Astro-f combined with the large field-of-view and wide wavelength coverage from NIR to FIR will enable us to take on such an ambitious survey and begin to address the questions hinted at by previous IR observations.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
105	417	DGPDR	HABART_DGPDR	Habart, Emilie (IAS, France)	OT-ESA	2	Evolution of dust and gas in Photodissociation Regions	The scientific motivation of this proposal is to study the nature and the evolution of the interstellar dust grains together with the physics and chemistry of the gas. The ASTRO-F mission, which offers a unique opportunity to observe continuously between 2 and 180 $mu$m including most of the dust components and gas lines emission from Photo-Dissociation Regions (PDRs), will provide a fundamental step in our understanding of the interstellar matter evolution. We propose to obtain images and spectra using the IRC camera and the FTS spectrometer for a selected sample of PDRs. Infrared spectro-imagery at high angular resolution, which allows to follow at small spatial scales the evolution of dust and gas through their IR emission, is a unique tool for tracing the dominant processes in grain/gas evolution which can take place at small scales. The selected sources has been observed with Spitzer and will be observed with Herschel (Guaranteed Time Observations), in imaging and spectroscopic modes. By combining ASTRO-F data with near- and mid-infrared data (mainly from Spitzer but also ISO) and observations at longer wavelengths (Herschel), the proposed observations will provide for the first time a complete view of the emission of interstellar gas and dust in PDRs from the infrared to the sub-millimetre and will allow us to identify and characterize (i) the processes that control the dust evolution (ii) the impact of dust grains on the heating and chemistry of the gas (ii) the structure of the interstellar clouds and the influence of the surrounding stars on their evolution and the star formation associated with the cloud.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
106	418	M20BL	LEFLOCH_M20BL	Lefloch, Bertrand (LAOG, France)	OT-ESA	2	Stellar Factories in Young HII Regions: the Trifid Nebula	HII regions play an important role in the formation of new generations of stars. In particular, about 15% of the high-mass stars could form under the influence of adjacent HII regions. Yet, the properties of the young stellar and protostellar populations which form at their periphery is not well characterized, nor the impact of the UV radiation on their evolution. The Trifid nebula is an ideal object for such study. We have undertaken a systematic multiwavelength program to understand the formation of young stars in such harsh conditions. Recent SPITZER/IRAC observations made by us have revealed a large population of about 150 young (proto)stellar objects. The sample appears to cover a broad range of evolutionary stages of objects, from Class 0 to Class II. All these objects form an homogeneous sample of sources which have all formed in the same cloud, under similar physical conditions. However, the characterization of the sources is based on SEDs built from fluxes measurements obtained between 1.5-24microns with IRAC and in the optical. Such determinations remain uncertain as they neglect the contribution of the cold material of the parental cocoon, which dominate the SED of protostars. ASTRO-F offers the unique opportunity to determine accurately the nature of the sources discovered with SPITZER and the physical conditions in their parental cores. By observing the emission of the cold material with FIS in its four colors, we will expand the SEDs up to 160 microns and will be able to characterize the whole young stellar population discovered, including the coldest, and youngest (proto)stellar objects. Using the IRC spectroscopic capabilities, we will precise the physical conditions of the parental cores in which young stellar objects are forming : the dust composition and its spatial variations across the core, the impact of the UV radiation on the gas and dust of the protostellar envelope.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
107	419	WRENV	MARSTON_WRENV	Marston, Anthony (European Space Astronomy Centre, ESA, Spain)	OT-ESA	2	Cool Dust in the Environments of Evolved Massive Stars	The evolution of massive stars have significant chemical and dynamical effects on the galaxies in which they reside. However, how and when material is lost during the evolution of the most massive stars is not well understood, due in large part to the lack of observational constraints on the genealogy of the intermediate phases of massive star evolution, namely in how Wolf-Rayet stars are connected to the Red Supergiant/OH-IR and Luminous Blue Variable star phases in different mass ranges. And yet the details of surface mass-loss in an evolutionary context are central to understanding the dynamical interactions with the interstellar medium that lead to galactic chemical enrichment and star formation. We propose to investigate the extended, cool, circumstellar environments of massive stars using ASTRO-F IRC and FIS imaging capabilities. These provide mass-loss history indicators via the distribution of material and the physical properties of the dust and gas, as well as indicating the extent to which star formation is being induced.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
108	420	ADAMB	MAZZOTTAEPIFANI_ADAMB	Mazzotta Epifani, Elena (INAF - Osservatorio Astronomico di Capodimonte,Italy)	OT-ESA	2	Activity of Small Solar System Bodies far from the Sun	Centaurs and Short Period Comets are two classes of the Minor Bodies orbiting in the Solar System. Centaurs are brief residents of the region between the gas giant planets, with calculated orbital lifetimes less than 10 million of years. They are often considered as objects originating from the Kuiper Belt, especially from the so called Scattered Disk. Centaurs that survive the dynamical environment of this region may evolve towards the class of Jupiter family comets. Comets are minor bodies populating the inner Solar System, believed to be remnant planetesimals of the early Solar System and to be composed of the less modified materials carrying information on the proto-solar nebula chemical and physical properties. Recent observations show that these two classes of Small Solar System Objects can exhibit coma activity at larger heliocentric distances than previously believed. The scientific aim of the proposal is to analyse in the IR range the far activity of a sample of Short Period Comets and Centaurs, at a heliocentric distance greater than 4 AU, in order to compare activity levels and obtain hints about evolutionary differences for objects with different dynamical histories. Beyond 4 AU, the water sublimation rate is low and so the sublimation of other surface volatiles, such for example CO, could drive the presence of a coma and give rise to a dust environment expected to be different from that due to water. The activity far from the Sun has important implication both for the cometary population (the total lifetimes of nuclei could be overestimated) and for the replenishment of the zodiacal dust cloud. This problem is strictly connected also to the presence of a trail, considered common to all Short Period Comets. To analyse the far activity of these Small Solar System Bodies, we propose to get images of the objects, in order to monitor the dust environment, and to get low resolution spectra of the coma, in order to analyse the far gaseous environment and the composition of the dust. Images in the continuum will be used as input for inverse coma and tail models, to get information on the dynamical evolution of grains in the coma and on dust physical parameters. Low resolution spectra will allow to evaluate the molecule production rate for non standard emission-driving compounds (CO, CO2) and to investigate the presence of amorphous or crystalline silicates grains in the coma.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
109	330	ABCGA	HWANG_ABCGA	Hwang HoSeong (Korea Institute for Advanced Study)	OT-ISAS	3-I	Activity of Brightest Cluster Galaxies probed by AKARI	We propose to observe 15 brightest cluster galaxies (BCGs) using the AKARI NIR spectrograph to understand the feedback process between BCGs and cooling flow (CF). Using the NIR spectra, we are going to measure the equivalent width of 3.3 micron PAH emission line and continuum slope, and to estimate the optical depth at 3.1 and 3.4 micron dust absorption lines, which are useful to study the connection between star formation and AGN. Primary goals of our study are 1) to identify the energy source (star formation or AGN) of BCGs clearly by detecting hidden AGN activity, and 2) to compare BCGs' activity with the characteristics of CF.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
110	421	ENVIR	NUTTER_ENVIR	Nutter, David (Cardiff University, United Kingdom)	OT-ESA	2	The Environments and Evolution of Pre-stellar Cores	The earliest stage of star formation, the evolution of pre-stellar cores, is the least understood aspect of star formation. One reason for this is that observational studies to date have used very different tracers to study pre-stellar cores and their natal molecular cloud. The thermal emission from cold (10-15 K) dust peaks in the far-IR. Data in this region of the spectrum is therefore crucial for determining the temperature of the emitting dust, and hence obtaining a reliable measure of the density. The FIS instrument on board Astro-F has the required sensitivity to image both the dense pre-stellar cores and the surrounding molecular cloud, and provides the first opportunity to observe both the cores and their environment using the same tracer. We therefore propose to map a number of pre-stellar cores and the surrounding molecular cloud using the FIS instrument. The density and temperature information will allow us to distinguish between competing theoretical models of pre-stellar collapse, which are controlled either by magnetic forces, or the dissipation of turbulence. We will measure the pressure both within and without the pre-stellar cores and hence ascertain whether the cores are gravitationally bound, or are confined by a higher pressure in the ambient cloud. The presence or absence of sharp edges between the pre-stellar cores and their surroundings will inform us as to whether or not the cores have detached from the molecular cloud, and are therefore evolving essentially independently of their surroundings.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
111	422	SUBMM	PEARSON_SUBMM	Pearson, Chris (European Space Astronomy Centre, ESA, Spain)	OT-ESA	2	Mapping the Spectral Energy Distributions of Sub-mm Bright QSOs	We propose to carry out photometry with the IRC and FIS instruments on a sample of SCUBA observed sub-mm QSOs selected so as to be well matched with optical luminosity (specifically brighter than -27.5 absolute B magnitude. Our sample is divided into 3 redshift ranges from local objects to the most distant objects in the Universe and are characterized by their sub--mm fluxes, or outstanding individual objects for which extensive follow up observations have already been made or targets for which it will be, or has already been possible to obtain good IR redshifts to facilitate CO follow up. All targets posses complementary SCUBA and a vast array of follow up data from X-ray to radio wavelengths with some including IR redshifts from CO measurements. The ASTRO-F data will fill the gap between the sub-mm and near infrared observations of these sources allowing us to investigate the AGN component as a function of redshift, optical/sub-mm ratio, the presence of molecular gas (indicative of starburst). By combining the data sets we will be able to provide a clear distinction between the AGN and Starburst components in QSOs leading to reliable radiative transfer models and determination of the Accretion/starburst energy budget of the Universe as a function of redshift.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
112	423	EROMU	SARACCO_EROMU	Saracco, Paolo (INAF - Osservatorio Astronomico di Brera, Italy)	OT-ESA	2	The stellar mass and the obscured star formation harboured by EROs	One of the difficulties of the galaxy formation models consists in explaining the large population of extremely red (R-K>5) galaxies (EROs) seen at z>1. In particular, models have to face with two uncertain properties of this population: (1) the "mass scale" of EROs, i.e. the abundance of massive red galaxies at 1<2 in the ERO population and (2) the "redness" of EROs, i.e. the balance among the number of early-type galaxies and that of obscured star-forming systems. The "mass scale" problem arises from the uncertainties affecting the estimate of the stellar mass of galaxies at z>1: the near-IR luminosity, best suited to trace the stellar mass, is extrapolated from the observed optical flux since no mid-IR observations are usually available. However, optical emission is affected by dust extinction and is dominated by young stars whose contribution to the near-IR emission is almost negligible. Thus, in the case of EROs, composed of old stellar systems and of dusty starbursts, these uncertainties are extremely high. The "redness" problem deals with the difficulty in identifying early-type galaxies and star-forming galaxies among the EROs and in quantifying the star formation and the dust extinction hidden by EROs. The photometric diagnostics proposed to distinguish the different classes of EROs are based on the observed colors of galaxies. In fact, these color-color plots deals with the rest-frame optical and UV continuum of EROs (being them at z>1) where the degeneracy between age and dust is extremely high. These facts, coupled with the faintness and the small size of the EROs samples collected so far, provide very poor constraints on the abundance of massive red galaxies at z>1 and no constraints at all on the star formation and on the dust content of EROs. We propose to survey an area of about 420 arcmin^2 with IRC (N3) and FIS (WIDE-L) in order to measure the rest-frame emission at 2 mu and at 50-90 mu for a complete sample of ~200 bright (K~19) EROs at 0.8<2. The IRC observations we propose will sample the rest-frame near-IR emission of the EROs allowing a reliable estimate of their near-IR luminosities. The FIS observations will sample the thermal emission from the hot dust characterizing the starburst galaxies. This will allow us (1) to distinguish starburst from passive early-type galaxies providing a statistic of about 80-100 objects per class; (2) to derive the SFR of the starburst galaxies through the mid-IR luminosity; (3) to constrain the mean dust content of starburst EROs by comparing the SFR derived from the un-obscured mid-IR light and from the L[2800] and L[O[II]] luminosities measured from the photometric and spectroscopic data; (4) to derive the stellar mass of early-types and starbursts from the rest-frame near-IR luminosity.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
113	424	A2218	SERJEANT_A2218	Serjeant, Stephen (University of Kent, United Kingdom)	OT-ESA	2	An ultra-deep survey through a well-constrained lensing cluster	We propose ultra-deep mapping of the exceptionally well-constrained gravitational lensing cluster Abell 2218 near the North Ecliptic Pole. Our 11+15 micron imaging to the confusion limits will complement the extremely deep Spitzer 3.6-8 micron and 24 micron imaging obtained by us, with the lens magnification taking our survey up to 10x deeper than even the deepest blank-field ASTRO-F survey. Uniquely for cluster lenses, the redshifts of multiply-imaged galaxies can be derived geometrically from the lens mass model (a technique pioneered by us); these directly test the photometric redshifts made possible only with our combined ASTRO-F + Spitzer wavelength coverage. Compared to blank-field surveys, our survey will probe a much more representative sample of galaxies which make up the remainder of the integrated near-mid-infrared extragalactic background light and the dust-shrouded cosmic star formation history. Subsequent studies will provide the gas masses and dynamical information necessary to place this population within its correct context in galaxy formation models.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
114	348	SSSGG	HWANG_SSSGG	Hwang HoSeong (Korea Institute for Advanced Study)	OT-ISAS	3-I	Slitless Spectroscopic Survey of Galaxy Groups	We propose to conduct NIR slitless spectroscopic survey for 30 galaxy groups to detect the enhanced star formation (SF) or AGN activities of group galaxies. Using the NIR spectra, we are going to measure the equivalent width of 3.3micron PAH emission line and continuum slope, and to estimate the optical depth at 3.1 and 3.4micron dust absorption lines, which are useful to study the connection between star formation and AGN. Primary goals of our study are 1) to detect the SF/AGN activity in group galaxies, 2) to characterize the energy source (SF or AGN) of group galaxies clearly by detecting hidden AGN activity, and 3) to compare the SF/AGN activities in group galaxies with global properties of galaxy groups.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
115	425	6AND7	SIMPSON_6AND7	Simpson, Chris (Durham University, United Kingdom)	OT-ESA	2	Making AGN come of age as cosmological probes	We propose four-band infrared imaging with the IRC of radio-loud active galactic nuclei (AGN) drawn from subsets of the 6C and 7C catalogues which have complete spectroscopic redshift information. These data will be combined with Spitzer data for the more luminous 3C objects to obtain SED information from 3-11 microns for a large number of AGN properly sampling the luminosity-redshift plane. This will enable us to break the degeneracy between redshift and luminosity inherent in flux-limited AGN samples. Our aims are (i) determine the true fraction of obscured AGN to allow a comparison between the AGN luminosity functions revealed by simulations and observations; (ii) determine the number of heavily-obscured (and likely Compton-thick) AGN to improve our understanding of the Cosmic X-ray Background; (iii) determine the distribution of extinctions as a function of luminosity and/or redshift to allow AGN number counts in the optical/infrared to be derived from simulations; (iv) investigate the relationship between black hole and host galaxy mass at high redshift to better understand the importance of AGN-driven feedback in controlling baryon cooling in galaxies. All these aims are essential if AGN are to be used to their full advantage to constrain simulations of the Universe and improve our understanding of their role in galaxy formation and evolution.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
116	426	SNRBS	SWINYARD_SNRBS	Swinyard, Bruce (Rutherford Appleton Laboratory, United Kingdom)	OT-ESA	2	FIR Spectroscopy of Super Nova Remnants	We propose to observe the SNR first observed using the ISOLWS in order better understand the physical characteristics of the shocked and unshocked neutral and ionised regions within the SNR. We plan to use the FIS03 AOT, which, with its higher spectral resolution than ISOLWS will enable us to better detect the FIR fine structure lines and better distinguish between the different velocity components present in the gas phase. Separating the cooler neutral phase from the hot ionised phase in a variety of objects will enable use to through some light on the debate about whether the cold dust "seen" in the sub-mm is pre-existing; originates for the Sn itself or is merely foreground material.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
117	427	YOUDD	WALKER_YOUDD	Walker, Helen (CCLRC Rutherford Appleton Laboratory, United Kingdom)	OT-ESA	2	Mapping young debris disks	Many young stars have massive dust disks and yet most main sequence stars have little or no dust around them. This proposal builds on work with ISOPHOT which has shown that it is possible to resolve some of the debris disks around stars younger than Vega and Beta Pictoris in the infrared. A sample of stars has been selected where we think ASTRO-F can resolve the debris disk at long infrared wavelengths, in order to produce a consistent set of data allowing scientific comparison of disk sizes, both amongst the sample itself and at two different infrared wavelengths.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
118	428	AZTSF	ZAVAGNO_AZTSF	Zavagno, Annie (Observatoire Astronomique de Marseille Provence, France)	OT-ESA	2	Triggered massive-star formation in the Galaxy	Massive stars ionize their environment, forming HII regions. These regions expands into the surrounding medium, ionizing the molecular material. A shock front travels ahead of the ionization front; the region between the two is a hot photo-dissociation region. Several processes linked to the expansion of an HII region may trigger star formation at their borders. Among those, the collect and collapse process is particularly attractive because it leads to the formation of massive fragments, and thus of massive objects (stars or clusters). In this process, the expansion of an HII region leads to the accumulation of a dense layer between the ionization and the shock fronts. This layer then eventually collapses in dense fragments, observed on the borders of the ionized zones. Those fragments represent potential sites of triggered massive-star forming regions. We are engaged in a multi-wavelength analysis of bright Galactic HII regions surrounded by annular hot photo-dissociation regions. We have shown the first evidences for the collect and collapse being at work, as the main triggering agent of massive-star formation in two Galactic HII regions. With ASTRO-F, we want to further study this way of forming massive star. Imaging the sites of massive star formation observed on the borders of ionized regions at longer wavelengths will allow us to derive the spectral energy distribution of those sources and to better characterize their nature and evolutionary stage. We also want to derive physical conditions in the hot photo-dissociation regions that host massive-star formation sites, using the Fourier Transform Spectrometer. Apart than characterizing this star forming process, the ASTRO-F observations will represent a precious and unique input to carefully prepare the Guaranteed Time observations we have on Herschel, especially on the SPIRE-Fourier Transform Spectrometer for which we develop the simulator and pipeline for data analysis.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
119	429	DUDES	ZIBETTI_DUDES	Zibetti, Stefano (MPI fuer Extraterrestrische Physisk, Germany)	OT-ESA	2	The Nature of the Dusty Medium in Dwarf Elliptical Galaxies	Dwarf early-type galaxies are the most common galaxies in the local Universe, nevertheless almost nothing is known about their dusty medium, owing to the intrinsic faintness of these systems also at mid- and far-IR wavelengths. The advent of the last generation IR satellites, such as ASTRO-F, allows to detect the emission from the native populations of dust grains present in these low-mass, small systems thanks to their excellent sensitivity both in the mid- and the far-IR. Furthermore, the IRC camera on ASTRO-F allows to map at a suitable spatial resolution the distribution of the mixture of dust grains emitting at wavelengths between 3 and 24 micron. Therefore, we propose to obtain IRC and FIS imaging at all bands for a pair of well-studied, dwarf elliptical galaxies (dEs) in the Virgo cluster, one evolving passively and the other being in a post-starburst phase. With these observations, we will determine the total amount of dust and the distribution of the different dust grains emitting at different IR wavelengths with respect to the local sources of the stellar radiation field. Hence, we will be able to investigate the nature of the sources of dust and the existence of a dusty interstellar medium (ISM) in addition to the circumstellar one in these two dE galaxies with extremely different star-formation histories within the last 2 Gyr. These results are needed to interpret the origin of the dusty ISM in giant elliptical galaxies and to establish the sources of metals (and dust) in the intracluster medium.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp2-apprv-esa.pdf
120	338	H2IRC	EGAMI_H2IRC	Egami Eiichi (Steward Observatory, University of Arizona)	OT-ISAS	3-I	Akari IRC Grism Spectroscopy of Extragalactic Strong H2 Emitters	Over the last few years, our team has discovered a number of extragalactic strong H2 emitters using IRS on the Spitzer Space Telescope. Some of them are associated with strong star formation while others are not. The amount of a warm H2 gas we find in some of these systems is spectacularly large, reaching up to 1010 Msun. As we discover more and more such sources, the scientific focus is now shifting to the identification of the excitation mechanism. However, the pure-rotational lines we detect with Spitzer/IRS provide little information in this regard. Here, we propose to conduct a spectroscopic follow-up observations of these strong H2 emitters using Akari/IRC, taking advantage of its capability to obtain spectra in the 2.5-5um range, a crucial range to detect H2 ro-vibrational lines, which should enable us to decipher the excitation mechanism(s) in these extraordinary objects.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
121	340	HQSO2	IM_HQSO2	Im Myungshin (Seoul National University)	OT-ISAS	3-I	Supermassive Black Holes at z > 5.4	We propose NIR spectroscopic observation of 16 high redshift QSOs at z > 5.4. During the AKARI phase 1+2 observations, we have performed a NIR grism/prism study of 14 QSOs at z > 4.5, detecting Hα lines in the spectra of 8 QSOs at z > 4.5 for the first time and determining the mass of the central black holes in them. The surprising result from the HZQSO is the lack of very massive SMBHs (~1010 Msun) at z > 5. Building up on the success of the open time program, we are currently performing a phase-3 mission program, QSONG, which observes 130 QSOs at 3.3 < z < 5.4 with the AKARI IRC NIR grism. The QSONG will pin down the mass distribution of QSOs at 3.3 < z < 5.4, but the QSONG sample does not extend above z > 5.4 where the deficiency of very massive SMBHs becomes significant. Here, we propose to observe 16 QSOs at z > 5.4 in order to study the important epoch where the growth of the SMBHs seems to be occurring. This observation will most likely triple the number of the high-z QSOs with the mass measurement based on Hα, and will provide us with a clearer picture of the history of the growth of the SMBHs in the universe than ever before.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
122	337	GOALS	INAMI_GOALS	Inami Hanae (The Graduate University for Advanced Studies (ISAS/JAXA))	OT-ISAS	3-I	Galaxy Evolution induced by galaxy interaction based on GOALS sample	GOALS project (Great Observatory All-Sky LIRG Survey; Armus P.I.) is a Spitzer Legacy program, a comprehensive multiwavelength imaging and spectroscopic survey of 180 LIRGs and 23 ULIRGs in the local universe but which lacks any significant spectroscopic coverage at Akari IRC wavelengths. The GOALS sample is based on IRAS Revised Bright Galaxy Sample (RBGS), which is a complete sample of extragalactic objects with IRAS 60 micron flux densities above 5.24 Jy and covering the full sky Galactic latitudes above five degrees. An important sub-sample of GOALS are those 88 LIRGs with L > 1011.4 Lsun - the luminosity at which the space density of LIRGs exceeds that of optically selected galaxies. These 88 bright LIRGs have been observed with the IRAC, MIPS and IRS instruments on the Spitzer Space Telescope, the ACS and NICMOS on-board the HST, the ACIS on the Chandra X-ray Observatory and with GALEX. These multi-wavelength datasets provide excellent coverage from the X-ray through the infrared, allowing us to build complete SEDs. Our objectives of the proposal are (1) to estimate continuum (hot-to-cold thermal dust) emission and emission/absorption lines in LIRGs through near- to mid-infrared SEDs, (2) to built more accurate starburst/AGN diagnostics with combination of Akari and GOALS data, and (3) to investigate these diagnostics as a function of LIRG morphology and luminosity. Akari is the only platform sensitive enough to obtain near-mid infrared spectra of a large number of LIRGs and thus provide a solid, global estimate of the importance of AGN emission (via hot dust) and star formation (via cold dust, 3.3 micron PAH, and Br-α emission). We propose two IRCZ4 spectroscopic and one IRCZ3 imaging pointings for each of 45 LIRGs selected from the sample of 88 which have not been previously targeted with Akari. Then the priority A and B total request pointing is 120: 20 targets for each priority and 3 pointings for each target (the rest five is priority C). We will complete all of LIRGs with L>1011.4 Lsun except Akari mission program observed or reserved sources. Our 45 LIRG targets sample are in many merging/interaction phases and this is one of the most important selection criteria of us. Hence, we need to complete sample of 88 without any selection bias since our purposes are to compose precise starburst/AGN diagnostics, to study the diagnostics probably related on morphology and luminosity, and to understand galaxy evolution caused by galaxy-galaxy interaction.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
123	332	ATLAS	ITA_ATLAS	Ita Yoshifusa (National Astronomical Observatory of Japan)	OT-ISAS	3-I	Making a 3 to 5 um spectroscopic atlas of galactic evolved stars	We propose to make a spectroscopic atlas of galactic S-type stars, post-AGB stars, luminous blue variables, and Wolf-Rayet stars by observing them with AKARI/IRC using AOTZ4/NG spectroscopic mode. They are all in the late stage of their evolution, but differ in their initial mass. We carefully selected 286 well studied and flux limited sample stars that have 2MASS K-band magnitudes of 2.3 < K [mag] < 8.5, so that they are not saturated in the NG grating spectroscopic mode, and also that we can take spectra with high signal-to-noise ratio (S/N > 20) over the whole wavelength range that IRC's NG grating covers (3 to 5 um). The 3 to 5 um spectroscopic data will enable us to study their photospheric and also circumstellar chemistries, to check the existence of PAH molecules, and also to know ionization conditions close to the star. Especially, it is known that the spectra of S-type stars are significantly different one by one, because small changes in their surface C/O ratio (C/O about 0.95 -- 1.05) will make large changes in their photospheric and circumstellar chemistries. By observing a large number of well-studied S-type stars, we study how spectrum change with the increase of C/O ratio. Some of our sample stars have been observed by SWS on ISO satellite that is capable of taking spectra in that wavelength range. Because almost all of our sample stars show chromospheric and/or atmospheric activities (e.g., stellar pulsation), then it is more preferable if there are previous observations, since we also want to study how the spectral features vary with these "activities". Combining the AKARI spectrum with the existing data, we study the correlations between the equivalent widths of some spectral features and the mid-infrared colors (using IRAS, MSX, and also AKARI all-sky survey data), which are also correlated with circumstellar dust properties and hence the mass-loss from stars. We explore dust condensation processes in these evolved stars, if any. These types of stars are considered to be dust sources in the interstellar medium of our Galaxy. The only missing type of dust producers is supernovae, but they have been observed with AKARI by other investigators. Repeated spectroscopic observations are also made on some targets to see the time variations of spectral features. The total pointings requested for this proposal is 316.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
124	345	P3SMC	ITA_P3SMC	Ita Yoshifusa (National Astronomical Observatory of Japan)	OT-ISAS	3-I	The role of pulsation in mass loss along the AGB, take 2	We propose to make a complementary observation toward two 10' x 10' areas, which have been observed as part of the AKARI Open Time Program, "The role of pulsation in mass loss along the Asymptotic Giant Branch (PI. Y.Ita)". Although we are approved to observe the two regions with imaging mode in NIR&MIRS and MIRL, and also spectroscopic mode in NP&SG1&SG2, AKARI ran out of its on-board supply of cryogen, liquid Helium before the allocated observing date. Then we have only spectroscopic data for an area, and only imaging data for the other. Therefore, we want to take imaging data for an area, and also NP spectroscopic data for the other. The preliminary analysis of data taken in the Phase1&2 showed that there are very red and bright sources in the two areas. They may be heavily mass-losing AGB stars, which are very rare but should hold keys to understand stellar mass-loss. The combined data of AKARI, Spitzer (mid-IR), IRSF/SIRIUS (NIR), Zaritsky (Optical) will enable us to estimate their mass loss rates and also the NP spectroscopic data will tell us their chemistries. Our primary goal is to study the role of pulsation in the mass loss process and their infrared characteristics. We also aim to study the dependence of metallicity on the mass loss and the AGB evolution by comparing the results from this proposed observation with the AKARI LMC survey. The total pointings requested for this proposal is 3.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
125	351	YPUMA	ITOH_YPUMA	Itoh Yoichi (Graduate School of Science, Kobe University)	OT-ISAS	3-I	Search for Young Planets in the Ursa Major Cluster	Two models are currently proposed for planet formation; the disk instability model and the core accretion model. The previous search for proto-planets by the Subaru Telescope concluded that it is very rare chance for planet formation by disk instability, at least, with a large separation. We propose imaging search for young planets around 18 young dwarfs of the Ursa Major cluster. If a planet forms by core accretion process, it should be detected in vicinity of a young dwarf by thermal infrared imaging with high sensitivity. Due to its proximity (<25 pc) and youth (500 Myr), this cluster is the best target for searching of young planets formed by core accretion process.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
126	335	CLNSL	LEE_CLNSL	Lee JongChul (Seoul National University)	OT-ISAS	3-I	NIR Spectroscopy of Composite and LINER LIRGs	We propose near infrared spectroscopy (NIR) of composite galaxies and low-ionization narrow emission-line regions (LINERs). Target are selected base on the infrared galaxies of Hwang et al. (2007) with a wide range of infrared (IR) luminosity. We will measure the equivalent width of 3.3 micron PAH emission line and the NIR continuum slope, and estimate the optical depth at 3.1 and 3.4 micron from the spectra. Using these parameters, we will search for the hidden active galactic nuclei (AGNs), and constrain the characteristics of power source in the composite galaxies and LINERs. We will also investigate the dependence of star-formation and/or AGN activity on IR luminosity. Our targets are the Sloan Digital Sky Survey selected sample, so we can obtain their various optical properties. Then we will study any correlations between these optical features and NIR features.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
127	342	ISBEG	LEE_ISBEG	Lee JoonHyeop (Korea Astronomy and Space Science Institute)	OT-ISAS	3-I	Infrared Spectroscopy of Blue Early-type Galaxies	We propose an infrared (IR) spectroscopic survey of Blue Early-type Galaxies (BEGs) in the Sloan Digital Sky Survey. BEGs are early-type galaxies with unusually blue colors, which are expected to be in the final phase of early-type galaxy formation. To understand the evolutionary mechanism of BEGs, it is necessary to distinguish the energy sources of BEGs between star formation (SF) and AGN. The main scientific goals in this survey are: 1) estimation of 3.3 micron PAH emission and continuum features in BEGs as SF/AGN indicators; 2) comparison between the optical features and the IR features of BEGs; and 3) investigation of the luminosity and redshift dependence of the IR features. We select 59 target BEGs with Ks < 12.5 Vega mag, at 0.02 < z < 0.1. Each target is proposed to observe with 2 pointings, using the IRCZ4 AOT with the grism (b) and the point source aperture (Np). This survey is expected to reveal the nature of BEGs including their SF/AGN composition, so that we can comprehend what is going on in BEGs and how BEGs are connected to typical red early-type galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
128	347	SFICE	LEE_SFICE	Lee JeongEun (Sejong University)	OT-ISAS	3-I	Ices in Star Forming Cores	We propose to use AKARI/IRC spectroscopy to observe 32 YSOs, VeLLOs, and background stars, in order to study the chemical and thermal conditions in the star forming cores. A wide variety of observations (including SST IRAC, MIPS, and IRS observations) have been acquired toward those sources, and these complimentary data set will be combined with the NIR spectra, which trace the composition of icy grain mantles. We have a self-consistent model for the process of star formation, which couples the chemical evolution with the dynamics of surrounding material and the evolution of the central luminosity. The ice features of H2O, CO, and CO2 covered by the AKARI/IRC spectra are vital to constrain the dust and chemical properties in our self-consistent model. In addition, comparisons of ice features of VeLLOs with those toward normal YSOs and background stars will provide a crucial opportunity to understand the dynamical process of VeLLOs. Therefore, the obtained NIR spectral data cubes acquired by the proposed observations will enable three scientific goals: (1) to compare ice features in various evolutionary stages of star formation from molecular clouds to Class 0, I, and II protostellar cores, (2) to understand the dynamical process in VeLLOs, and (3) constrain self-consistently our chemical and dynamical evolutionary model.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
129	349	WDISK	LEE_WDISK	Lee JeongEun (Sejong University)	OT-ISAS	3-I	A Focused Search for Circumstellar Dust Orbiting White Dwarfs	We propose to use Akari to observe 10 single, metal-polluted white dwarfs to search for an infrared excess. Such an excess, already known for about 10 other white dwarfs, likely is the consequence of the tidal-disruption of a minor planet, resulting in a dust distribution analogous to Saturn's rings. Our proposed Akari observations target 5 hydrogen-rich white dwarfs with accretion rates greater than 3 x 108g s-1 and will test the prediction that these stars display an infrared excess. We also propose to observe 5 helium-rich white dwarfs with [Ca]/[He] > -8.0 to determine whether these metal-enhanced stars also have an infrared excess. With an improved understanding of the tidal-disruption scenario, we will further our ability to use white dwarf photospheric abundances to constrain the origin and evolution of minor planets --- the building blocks of terrestrial planets. Current data on contaminated white dwarfs show that their pollutants are deficient in carbon relative to other metals by at least a factor of 10. This result parallels the observed composition of the inner planets in our solar system and provides a strong, but as-yet poorly understood, constraint on models for planet formation.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
130	333	BRSFR	MATSUHARA_BRSFR	Matsuhara Hideo (ISAS/JAXA)	OT-ISAS	3-I	Extinction-Independent Determination of SFR in Star-forming Galaxies	One of the most fundamental properties of galaxies,their star formation rates (SFRs), are currently determined from applying recombination theory to H emission lines to infer the ionizing photon luminosities produced by O/B stars. Unfortunately, the "gold standard" line, Hα, is known to be very susceptible to extinction by interstellar dust. The limited measurements of H lines in the infrared in fact suggest that Hα often misses MOST (>90percent) of the ionizing luminosity from newly formed stars, embedded in dust. Using the definitive Brα line (which suffers an extinction of only 0.035 Av), Akari/IRC has shown that this is the case in many ULIRGs. By measuring reliable Brα/Hα ratios, we will determine whether the Hα method for estimating SFRs in more normal, less luminous star-forming galaxies can be salvaged, or needs a radical overhaul. The key to defining our targets has been examining direct narrow-band filter imaging of Hα in a large sample of galaxies at cz~7000km/sec. This allowed us to identify those with bright enough lines (Hα-estimated SFRs of 1Sun/year) in a compact spatial distribution suitable for measurement in the IRC 1-arcminute aperture. Even under the conservative assumption of only 1 magnitude of absorption at Hα, the Brα lines in all 30 of the target galaxies will be well detected in 3 to 6-pointings. This new exploration of Brα (and secondarily the PAH feature) as reddening-free SFR indicators requires this sample size to probe a wide range of galaxy properties.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
131	339	HOTCO	MINH_HOTCO	Minh YoungChol (Korea Astronomy and Space Science Institute)	OT-ISAS	3-I	Dense Molecular Gas interacting with Outflows of the Starbursts	We plan to observe the CO 4.7 micron fundamental ro-vibrational band toward two starburst galaxies, M82 and NGC253. These sources are nearby (~3.5 Mpc) archetypical starbursts having large star formation rates (~2-4 Mo/yr), estimated from the strong infrared emission in the nuclear region. Both have prominent galactic-scale nuclear outflows associated with starbursts. The dense molecular gas in the nuclear region makes up 10% of the circumnuclear dynamical mass and fuels large star formations. The strong nuclear outflows will generate shocks in the surrounding dense gas. The major cooling agents of the shocked gas are thought to be CO, H2O,and OH, and the CO fundamental emission bands is an ideal tracer of the dense post-shock gas. Although the prominent nuclear outflows are thought to be originated from the mechanical power of the supernovae, it is still not known how they are related with starbursting regions. In addition, the outflows also trigger the next generation starburst in the surrounding molecular clouds (e.g., Minh et al. 2007), but the actual connection between the outflows and the embedded starburst is not clear. Using the excitation-radiation model of CO, we plan to investigate the morphology and kinematics of warm (~500 K) and dense (n(H2) > 107 cm-3) post-shock gas in the galactic center to study the origin and nature of the associated nuclear outflows.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
132	343	MAGNE	MORII_MAGNE	Morii Mikio (Rikkyo University)	OT-ISAS	3-I	Infrared/Optical Emission Mechanism of Magnetars	We propose to observe three magnetars with Akari to understand the infrared/optical emission mechanism. Several models have been proposed for the emission mechanism, which are based on the magnetospheric emission, disk emission, and hybrid of them. By the SED fitting for the spectrum obtained by Akari, Spitzer, and near-infrared/optical observations, the disk models can be tested. Emission features are expected in the mechanism of the magnetospheric origin (cyclotron line and maser frequency peak). By twice observations with a half year interval, variability of the SED also can be checked and hence the correlation with the X-ray flux is also tested. Disk model would produce strong and wide impact on astrophysics, not only on pulsar astronomy, but also on mechanism of supernova explosion and planet formation.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
133	334	CASSP	ONAKA_CASSP	Onaka Takashi (Department of Astronomy, University of Tokyo)	OT-ISAS	3-I	Dust and Molecules Formed in the Cas A Supernova Remnant	We propose to observe the young supernova remnant Cas A with AKARI IRC to detect the CO fundamental band, dust features, and ionic lines. Spitzer observations of Cas A with IRAC and IRS indicate that some 0.05 solar masses of dust were freshly formed in the ejecta. The near-infrared emission (<3 microns) is from synchrotron emission, and the mid-infrared wide-band spectra are a mix of lines and dust. At present, there is no explanation for the brightness of IRAC band 2 (4-5 microns) based on existing dust models and known gas lines. We suggest the presence of a CO fundamental band due to ejecta that failed to condense into dust. A ground-based (Palomar) narrow-band image in the CO overtone band (2.3 microns) appears to detect faint CO emission, confirming its presence but at the level required to explain all of the IRAC channel 2 emission. Near-infrared spectroscopy with AKARI will directly detect the CO fundamental band as well as other possible lines (like Brα). Presence of significant quantities of warm CO in Cas A indicate ongoing processes of astrochemistry in a 300-yr old SNR. Since CO is the most important molecule in astrochemistry (in particular in the H-poor ejecta), the proposed observations will be diagnostic of physical conditions such as the temperature and density, and degree of mixing in the SN ejecta. Understanding incomplete dust formation in supernovae will advance our understanding of dust formation efficiency in SNe and dust production in SNe in early Universe.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
134	346	PNSPC	ONAKA_PNSPC	Onaka Takashi (Department of Astronomy, University of Tokyo)	OT-ISAS	3-I	Near-Infrared Spectroscopy of Planetary Nebulae	We propose to make a systematic near-infrared spectroscopic observation of planetary nebulae (PNe) and investigate the destruction process of the unidentified band (UIR) carriers under strong ultraviolet radiation fields. The 3.3 micron UIR band carriers are thought be most sensitive to harsh conditions and the correlation of its presence/absence with the age of PNe will indicate the destruction efficiency of the band carriers. 87 planetary nebulae with known kinematic distance are selected, whose ages range 600 to 30000 yr. Near-infrared spectroscopy of IRC provides information not only on the 3.3 micron UIR band, but also on hydrogen recombination and forbidden ionic lines, latter of which the physical conditions and ultraviolet radiation intensity in the nebula can be derived from. The present observation will enable a systematic investigation of the UIR band carrier processing in the radiation field. It will also provide a near-infrared spectrum atlas of PNe for the first time owing to the unique capability of IRC.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
135	344	NEWSY	SAKON_NEWSY	Sakon Itsuki (University of Tokyo)	OT-ISAS	3-I	Near-IR Spectroscopy of Galaxies; Waiting for Supernovae Momentarily	In this program, we plan to obtain the near-infrared slit-less spectroscopic datasets of nearby galaxies in preparation for a future supernova there. Our samples in the target list have relatively higher supernovae frequency (10-20 years per a supernova) and 2-3 supernovae per year, in total, are expected in our samples. The data obtained in this program is definitely important to obtain the accurate near-infrared spectra of supernovae expected to explode in a future during the lifetime of AKARI. the near-infrared spectra from 2 to 5.5um of the core-collapse supernova within less than 1 year after the explosion have ever been obtained for only two cases including the SN1987A and the SN2006jc and, therefore, those datasets for other future supernovae are highly desired. AKARI/IRC is, so far, the only instrument that are capable of obtain the near-infrared (from 2 to 5.5um) spectra of supernovae within 6 months after explosion. The obtained datasets in this program are quite useful to derive these spectra of supernovae with higher accuracy, which will surely help us understand the role of massive stars in the formation of interstellar dust and reveal what the fundamental difference between the supernovae with and without the signs of dust formation should be. At the same time, we can obtain the near-infrared spectral catalogue of infrared sources for each galaxy in our samples via the robust data reduction techniques which we have developed to obtain the spectra of point-like sources embedded in complicated diffuse background structures.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
136	341	IEYSO	SHIMONISHI_IEYSO	Shimonishi Takashi (Department of Astronomy, Graduate School of Science, The University of Tokyo)	OT-ISAS	3-I	Ices Around Extragalactic Young Stellar Objects	Properties of extragalactic Young Stellar Objects (YSOs) provide us important information on the understanding of the diversity of YSOs in different galactic environments. The Large Magellanic Cloud (LMC), the nearest irregular galaxy to our galaxy, offers an ideal environment for this study. An infrared spectrum of YSOs shows absorption features of various ices which are thought to be an important reservoir of heavy elements and complex molecules in a cold environment. We detected absorption features of the H2O ice 3.05um and the CO2 ice 4.27um stretching mode toward 7 massive young stellar objects (YSO) by the IRC LMC near infrared spectroscopic survey. We calculated the column densities of the ices, and derived the average CO2/H2O ice ratio to be 0.64. This ratio is clearly higher than that seen in galactic massive YSOs of 0.17±0.03. We suggest that the strong ultraviolet radiation field and/or the high dust temperature in the LMC may be responsible for the observed high CO2 ice abundance. It is inferred from our results that the YSOs in the LMC hold different chemical balance from the Galactic ones. We selected 31 YSO candidates which show a hint of ice absorption features based on recent YSO catalog and near infrared spectrum taken by the IRC LMC survey. We here propose IRC NG spectroscopic observations toward these 31 objects. The proposed observations should detect important species of ices such as H2O, CO2, CO, CH3OH, XCN simultaneously. We try to clarify the reason of a high CO2 ice abundance in the LMC using the detection of XCN feature which is thought to be a tracer of strong UV radiation field and a detail profile analysis of 3.05um H2O ice feature which is thought to be a probe of an ice temperature. In addition, we try to investigate the correlation between ice abundances and physical environments of YSOs such as stellar parameters of central star or distribution of interstellar matter. The proposed observations should clarify the reason of the high CO2 ice abundance in the LMC, and determine the chemical abundances of ices as functions of physical environments of YSOs. Near infrared spectra obtained in this observations should be a valuable dataset for the study of extragalactic YSOs and ices.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
137	350	YDRWF	SONG_YDRWF	Song Inseok (University of Georgia)	OT-ISAS	3-I	Hunting the Coolest Substellar Dwarfs	The very few lowest mass substellar companions discovered in previous imaging surveys at nearby stars and brown dwarfs are found to have large semi-major axes, typically hundreds of AU. We show that, at such large separations and toward old stars, one has the best chance to detect the coolest dwarfs, with effective temperatures of <~500K (the so-called "Y dwarfs"). Effective temperatures of 500K represent a region of temperature space that has yet to be probed. Therefore, the discovery of such cool objects will illuminate their physics and chemistry and will provide observational data to test planetary models. To discover one or more Y dwarfs, we are proposing to survey white dwarfs with ages >2Gyr that lie within 25pc of Earth with (post-helium) AKARI.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
138	331	ASCSG	WOO_ASCSG	Woo JongHak (University of California Santa Barbara)	OT-ISAS	3-I	The AGN-starburst connection of Seyfert galaxies at z~0.36	To investigate the AGN-starburst connection, we propose to measure starburst activity based on the 3.3 micron PAH emissions, using a sample of 29 Seyfert-luminosity AGNs at z~0.36. This epoch, z~0.36, is cosmologically interesting for studies of the coeval growth of black holes and their host galaxies, as suggested in our previous studies. With unprecedented multiwavelength data, covering from the hard X-ray to the mid-IR from our parallel programs (Chandra, Spitzer, HST, GALEX and Keck), we are in a unique position to accurately measure the AGN activity, i.e., bolometric luminosity, black holes mass, and the Eddington accretion rate, thus unveiling how black hole accretion is related with global starburst activity. Measuring "global" star formation rate of these host galaxies is only possible with the powerful slitless spectroscopy capability of the AKARI IRC. We ask 4 pointings for each object, 116 pointings in total, to obtain S/N~10 in the continuum for securely measuring the 3.3 micron PAH emission luminosity.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-jk.pdf
139	430	DABUN	WATERS_DABUN	Waters, Rens (Astronomical Institute, University of Amsterdam, The Netherlands)	OT-ESA	3-I	The interstellar deuterium abundance	The interstellar deuterium abundance provides a direct measure of the cosmic history of nucleosynthesis. Recent FUV studies imply that a large fraction of the deuterium is missing from the gas phase and likely locked up either in carbonaceous grains or Polycyclic Aromatic Hydrocarbon molecules. Here, we propose to measure the CD stretching mode associated with deuterated carbon-grains in the absorption spectrum of interstellar dust and the CD stretching mode associated with deuterated Polycyclic Aromatic Hydrocarbon molecules in the interstellar emission spectrum. Here we request a pilot study to establish the importance of carbon grains and/or PAHs as a main reservoir of deuterium. If successful, we plan to follow up with a large survey, in the next call, to probe the galactic variation of the deuterium abundance in order to determine the effects of astration and star formation on the elemental deuterium abundance.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
140	434	DISKD	DENT_DISKD	Dent, William (UK ATC, Royal Observatory, Edinburgh, United Kingdom)	OT-ESA	3-I	A survey of hot dust at the inner radius of protoplanetary disks	We propose a sensitive, systematic survey of the hot dust in a broad sample of young protoplanetary disks, using near-ir low-resolution spectroscopy with AKARI IRC. The targets have ages in the critical range 1-30Myr, which defines the transition from massive, gas-rich primordial disks to dust-rich debris disks. Sensitive measurements of the near-ir excesses are necessary for understanding the innermost (R<1AU) structure of these protoplanetary disks, addressing questions such as: 1) what affects the radius and vertical extent of the hot inner region facing the star? How is it affected by disk mass, spectral type, accretion, age, etc? 2) is a separate "puffed up" inner wall component required to fit the Spectral Energy Distributions? 3) how extensive is the depletion in the inner "holes" of transition objects? Such information is necessary to understand the interaction between the inner disk and the pre-main-sequence star, as well as the global disk evolution. Up to now, measurements of near-IR excesses have generally relied on broadband photometry. Using IRC in slitless spectroscopy with NP, we will make a significant advance on this by obtaining low-resolution 2-5um spectra from a broad sample of such disks, covering a multivariate parameter space, with a wide range of stellar luminosity, disk mass, accretion rate and SED Class. Low-resolution spectroscopy will be significantly more reliable at detecting and measuring the excess compared with broad-band photometry, and so the results will provide sensitive new observations of the hottest, closest dust to the stars. Additionally, all of the proposed targets will be observed as part of our Herschel Key Project (GASPS) allowing us to combine near-infrared and far-infrared observations of the same disks and build a coherent model of the disks and their interactions with their host stars.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
141	361	NISIG	LEE_NISIG	Lee JongChul (Seoul National University)	OT-ISAS	3-II	Near infrared spectroscopy of star-forming infrared galaxies	We propose near infrared (NIR) spectroscopy of star-forming (SF) infrared galaxies (IRGs). Targets are selected from the catalog of Hwang et al. (2007) based on Sloan Digital Sky Survey. We will measure the flux and equivalent width of 3.3 micron PAH emission line and the NIR continuum slope, and estimate the optical depth from 3.1 micron water ice absorption and 3.4 micron hydrocarbon absorption. Using these parameters, we will search for any hidden active galactic nuclei (AGNs), and determine the intrinsic power source in the SF IRGs. We will also investigate the dependence of SF/AGN contribution on IR luminosity and correlations between optical and NIR SF indicators. From this observation, we can understand the role of AGN in SF IRGs.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
142	433	DISCO	BURGDORF_DISCO	Burgdorf, Martin (Liverpool John Moores University, United Kingdom)	OT-ESA	3-I	Spectroscopy at the Disk-Halo Interface of Spiral Galaxies	We propose IRC NIR-NP spectroscopy of 16 edge-on galaxies (including back-up) at different positions in the Hubble Tuning-Fork in order to characterize the physical/chemical state of diffuse dust and the stellar populations that reside at the disk-halo interfaces. This would be the first comprehensive study of spectral features between 2 and 5.5 microns in outer disks and inner halos. It would reveal the distributions of evolved stars, PAH scale sizes, and the composition of the extra-planar interstellar matter, and show how they depend on galaxy type. Variations for example of the PAH band at 3.3 microns as a function of height above the mid-plane can provide us with a much better understanding of how interstellar dust is ejected from the disks by galactic winds. For each object we propose to observe five different positions bracketing the mid-planes in order to characterize the emission from both disk and halo in the presence of strong foreground emission. All our targets have already been observed with Spitzer/IRAC to ensure that extra-planar emission is present in the near infrared. In combination with the existing observations, which trace the "reddest" stellar populations in the halo, thin disk, thick disk, and bulge, the proposed AKARI program will address open questions about thick disks as tracers of merger history. Such highly sensitive near-infrared spectra, which only AKARI can provide, are indispensable to a full understanding the cycle of matter in the outskirts of spiral galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
143	438	NESID	BOULANGER_NESID	Boulanger, Francois (Institut d'Astrophysique Spatiale, Paris, France)	OT-ESA	3-I	Nature and Evolution of Small Interstellar Dust	Small dust particles (PAHs and VSGs) are major constituents of interstellar dust that play key roles in the physics and chemistry of the interstellar medium. Their mid-IR emission features have been observed to be an ubiquitous spectroscopic signature of dust in galaxies but the origin, nature and link between PAHs and VSGs are still debated issues. While this research field was initiated by near-IR observations, results from the IRAS, IRTS, ISO and Spitzer that followed were almost exclusively from mid-IR emission at wavelengths larger than 5 micron. The AKARI warm mission provides the opportunity to obtain the missing dust spectroscopy data at shorter wavelengths. We propose AKARI observations that will provide combined spectral and spatial information on the 3.3 micron feature, the 3.2 to 3.6 micron plateau and the near-IR dust continuum for a set of archetype PDRs with mild UV excitation conditions. The observations will also allow us to search for a spectroscopic signature of deuterated PAHs and VSGs with unprecedented sensitivity. The data will address the three following questions. (1) Is there an evolutionary link from aliphatic to aromatic carbon dust? (2) Are PAH cations the carriers of the near-IR dust continuum? (3) Do small dust particles hold a major fraction of the interstellar deuterium ?	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
144	432	DEPPN	ENGELS_DEPPN	Engels, Dieter (Hamburger Sternwarte, Hamburg, Germany)	OT-ESA	3-I	The chemistry of warm dust in early post-AGB stars	We propose to use the AKARI warm phase for a study of the circumstellar envelope (CSE) emission of 33 young post-AGB stars in the 1.8 -- 5.5 micron wavelength range. We have used the AKARI and Spitzer satellite in the past to study stars, which are completely obscured in the optical and sometimes even in the near-infrared (lambda < 2 micron.) and which are thought to be in the process of terminating the AGB evolution or beginning the post-AGB phase. These stars are very bright at 10-40 micron and their emission comes from the CSE formed by the ongoing or recently terminated AGB mass loss. With the help of recent Spitzer photometry (GLIMPSE survey), we verified for quite a number of stars a near infrared excess in the spectral energy distribution. This excess is due to warm gas and dust illuminated by the remnant AGB core and which becomes visible now that the heavy AGB mass loss apparently has stopped. We propose to take near-infrared spectra to determine the chemistry of the material which is currently lost by the AGB core.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
145	435	EMSCA	EMSCA	Juvela, Mika (Helsinki University Observatory, Helsinki, Finland)	OT-ESA	3-I	The ratio of NIR dust emission and scattering in interstellar clouds	Near-infrared scattered light provides a way to map interstellar clouds at close to an arc-second resolution. However, the role of NIR dust emission is poorly known and could affect the reliability of these results. In wavelength, the transition between scattering dominated NIR and emission dominated MIR takes place somewhere close to the Akari IRC N2 filter. We propose to map a cometary globule in the N2 and N4 filters. Our ground-based NIR observations trace the scattered radiation while the Akari N4 filter will reveal the distribution of pure dust emission. By correlating the surface brightness data with each other and with our extinction map, we will determine the ratio and spatial distribution of the two intensity components, dust emission and dust scattering. The results could have serious implications for the use of K-band data in the mapping of interstellar clouds. Furthermore, they will provide strong constraints to dust models concerning the abundance and spatial distribution of the smallest dust grains.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
146	439	REDHA	JUVELA_REDHA	Zackrisson, Erik (Tuorla Observatory, Finland)	OT-ESA	3-I	The red halos of blue compact galaxies: the case of Haro 11	Deep ground-based optical/near-IR images of blue compact galaxies have revealed faint and extremely red envelopes outside their bright star-forming centres. The colours of these structures are difficult to reconcile with normal stellar populations, and instead indicative of stellar populations with bottom-heavy initial mass functions. These red halos do, however, remain controversial due to the immense problems of accuately measuring the near-IR flux at the very faint surface brightness levels where the red excess turns up. Here, we propose deep imaging of Haro 11, the blue compact galaxy with the most extreme halo colours reported so far, to trace the near-IR surface brightness profile to unprecedented depth and to investigate the nature of its red halo.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
147	436	IMAP2	FRASER_IMAP2	Fraser, HelenJane (University of Strathclyde, Glasgow, United Kingdom)	OT-ESA	3-I	The spatial distribution of ices in Spitzer-selected molecular cores	In the densest star forming cores, over half the molecular species (excluding H2) are condensed onto dust grains. To effectively study the solid-state chemistry of star-forming cores, we require detailed observations of the abundances, and more importantly the spatial distribution, of as many condensed species as possible, in particular H2O, CO2 and CO. These species are directly observed via their strong stretching-mode bands at 2.5-5 microns, seen toward the continua of background stars. Ground-based facilities are far from sensitive enough to yield similar data and the Spitzer Space Telescope has no spectroscopic capability below 5.5 microns. While ices can be observed at longer wavelengths, the 2-5 micron region contains the strongest ice bands and background stars are bright, making it crucial for any spatial mapping of interstellar ices. We propose to obtain spatially well-resolved maps of molecular ices towards a sample of isolated molecular cores located in front of regions with a high density of background stars. The cores have been selected from the well-characterized sample of molecular cores imaged by Spitzer as part of the "cores to disks" Legacy Science program. Akari presents a unique opportunity for mapping the spatial distribution of water, CO and CO2 ices toward background stars, due to its sensitive spectroscopic capability in the NIR, as well as its ability to obtain slitless spectroscopy over a large field of view. This proposal is an extension of a successful and pioneering ice-mapping endeavour, commenced during Phase II Akari Open-Time observations. The observing program includes 25 targets, each observed on at least 2 pointings, as well a crucial calibration observations (18 pointings) to enhance the quality of the ice-mapping results. Based on our experience in Phase II, we have significantly improved the observing strategy. We will use both the prism (Np) and the grism (Ng) modes with the near-infrared camera (AOT IRCZ4) to obtain spectroscopy of background stars in the entire field of view. The data be used to map the H2O, CO and CO2 ice abundances across each core. Our Phase II experience shows that we are typically able to map the distribution of ices on scales of 20-60", or 2000-6000 AU in the nearest dark clouds, thereby sampling the chemical and freeze-out scales. The proposed sample of ice maps will constitute a highly unique survey that will not be possible to match for many years into the future.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
148	431	DEBIR	DUC_DEBIR	Duc, PierreAlain (CEA-Saclay, France)	OT-ESA	3-I	Stellar populations and hot dust in debris of galaxy collisions	Debris of galaxy-galaxy collisions have recently proven to be particularly useful laboratories to address a variety of challenging questions, from the triggering of star formation to the distribution of dark matter in and around galaxies. Collisional debris expelled in the intergalactic space by tidal forces provide a peculiar environment where stars may be formed in a different way than in disks, while sharing with them a similar interstellar medium. Comparing both modes of star formation (SF), one may learn about the role of large scale environmental effects on the SF process. In that aim, we have compiled the Spectral Energy Distributions (SED) of gas-rich collisional debris. One key wavelength domain is the near-infrared one where stellar emission (from UV to near-IR) and dust emission (from near-IR to mm) meet and mix. Uncertainties in the near-IR fluxes translate into large errors in the star formation history, and stellar masses, as reconstructed using evolutionary synthesis codes, while making any dust model elusive. Our Akari observations in the N2 band will provide photometric data points with the precision required to constrain our models. These data will allow us to estimate the fraction of old stars (expelled during the collision) vs young stars born in situ in gaseous tidal tails. From our numerical models, we expect some of our structures to be totally devoid of old stars. For such objects that experience their first starburst, we will be able to constrain their Initial Mass Function, in an environment where it had never been probed. Exploiting the IR side of our SED, we will confirm the existence of a possible near-IR excess in the star-forming debris which might be due to very hot dust. Finally, we will be able to obtain a precise measure of the total stellar mass, used in particular in the determination of the specific star formation. For some debris that proved to be gravitationally bound and for which we could determine a dynamical mass, we will compare it with the luminous mass (the sum of the gaseous and total stellar masses). Previous similar results revealed the existence of an unexpected missing mass in tidal debris and thus in the disk of their parent galaxies.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
149	437	MASYS	ANGELONI_MASYS	Angeloni, Rodolfo (Dept. of Astronomy, University of Padova, Italy)	OT-ESA	3-I	A Near-IR spectroscopic survey of Magellanic Symbiotic Stars	We would like to observe the whole sample (14 objects) of Symbiotic Stars (SSs) in the Magellanic Clouds (MCs), in both the moderate (NP) and high resolution (NG) spectroscopic mode (AOT IRCZ4). These observations would provide the first ever near-IR spectra of SSs in the MCs, giving a fundamental and unique contribution to the understanding of the symbiotic phenomenon in its diverse appearance and, in general, of gas and dust properties in complex environments at different metallicity. The ecliptic latitude of MCs ensures high visibility for all the objects of the sample. No MSS in the sample is duplicated with the blocked target list.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
150	440	WITCH	BARRADOYNAVASCUES_WITCH	BarradoyNavascues, David (LAEFF-INTA, Madrid, Spain)	OT-ESA	3-I	IC2118: star formation at high galactic latitude	Several aggregates in the high galactic latitude molecular cloud (HLC) in the region of IC 2118, the Witch Head Nebula, appear to be forming stars (Kun et al. 2004). Star formation in HLCs, while rare, may be the origin of some of the apparently isolated T Tauri stars revealed by ROSAT. IC 2118 is a very interesting HLC located at l=208, b=-28, with an age of about 2 Myr and a distance of 210 pc. We have recently applied with success to the X-ray observatory XMM-Newton, and to ESO NTT SOFI near-infrared camera to obtain data in three regions of the Witch Head Nebula. With the present proposal we request deep mid-IR imaging. The combination of the three sets of data will allow us to derive for the first time the Initial Mass Function in a Star Forming Region (SFR) at high galactic latitudes, and compare it with other SFRs with different environment and star formation history.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3-apprv-esa.pdf
151	301	ISICE	AIKAWA_ISICE	Aikawa Yuri (Dept of Earth and Planetary Sciences, Kobe University)	OT-ISAS	3-II	Formation and Evolution of Interstellar Ice	We observe the absorption of ice bands in star forming regions. Most of the background stars behind molecular clouds, low-mass protostars, and protoplanetary disks are too faint for the spectroscopic observation from the ground. The high sensitivity of AKARI is required to investigate the chemical composition of ice towards these objects. Spitzer Space Telescope is currently undertaking similar ice observations, but it is restricted to > 5 micron. AKARI is currently the unique space telescope to observe the wavelength region of 3-5 micron, which contains various important ice bands. So far, we have reduced phase II data and clearly detected water, CO2 and CO bands towards background stars and edge-on YSOs. Although we continued the observation in phase III-1, we assigned only 1 pointing (with grism mode) per coordinate, and thus cannot correct for the hot pixels. We request additional pointings for our phase III objects, so that we can analyze the phase III data.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
152	353	H2BCG	EGAMI_H2BCG	Egami Eiichi (Steward Observatory, University of Arizona)	OT-ISAS	3-II	2.5-5um Spectroscopy of Infrared-Luminous Brightest Cluster Galaxies	Over the last few years, our team has discovered a number of extragalactic strong H2 emitters using IRS on the Spitzer Space Telescope. The amount of a warm H2 gas we find in some of these systems is spectacularly large, reaching up to 1010 Msun. As we discover more and more such sources, the scientific focus is now shifting toward the identification of the excitation mechanism. However, the pure-rotational lines we detect with Spitzer/IRS provide little information in this regard. Here, we propose to continue our Phase 3a AKARI/IRC spectroscopic follow-up observations of strong extragalactic H2 emitters, focusing this time on the population of infrared-luminous brightest cluster galaxies with exceptionally strong H2 emission. Through our Spitzer Cycle-5 program, which just completed, we have found such BCGs at lower redshift (0.1 and below), which would increase the observed line fluxes and enhance the chance of H2 line detections. The 2.5-5 μm range covered by AKARI/IRC is crucial to detect H2 rovibrational lines, which should enable us to decipher the excitation mechanism in these extraordinary objects.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
153	355	HASEO	HASEGAWA_HASEO	Hasegawa Takashi (Gunma astronomical observatory)	OT-ISAS	3-II	AKARI-Untouched AGB-rich old open cluster Berkeley 54	Since no instruments that cover longer than 5 micron is available, we would focus on accumulating observational basis with respect to mass-loss (that can be covered from N3 and N4 band) on star clusters, with a few comparison clusters that show marked contrast in cluster properties. The main observable that we are going to obtain in this study is the time series mass-loss rate on the AGB stars on the various parts along AGB sequence. This is highly taking advantage of studying open clusters which are single population in age and metallicity by nature. By doing this, for example, we could have discriminate whether mass-loss events takes place constantly or periodically at various stages along AGB. We are going to continue photometry in the optical bandpass for two years at least, and therefore it is possible to establish the possible time-lag between optical and infrared.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
154	337	GOALS	INAMI_GOALS	Inami Hanae (The Graduate University for Advanced Studies, ISAS/JAXA)	OT-ISAS	3-II	The Complete NIR Spectroscopic Survey of LIRGs in the Local Universe	We request AKARI IRC spectroscopic observations to complete an unbiased near-infrared spectroscopic survey of Luminous InfraRed Galaxies (LIRGs, which have more than 1011 solar luminosities) in the local universe. Our objectives are (1) to estimate the 3.3 microns PAH emission line flux and constrain the small grain properties such as the ionization state, (2) to measure the Br-alpha recombination line and study the ionized gas, (3) to evaluate the presence of hot thermal dust emission and search for buried AGN, and (4) to investigate starburst/AGN diagnostics as a function of morphology and luminosity. AKARI is the only platform sensitive enough to obtain spectra in the range 2.5-5.0 microns, of a large number of LIRGs and thus provide a solid, global estimate of the importance of AGN emission (via hot dust) and star formation (via cold dust, 3.3 microns PAH, and Br-alpha emission). These near-infrared LIRG observations will be combined with a comprehensive multi-wavelength imaging and spectroscopic survey (GOALS; The Great Observatories All-sky LIRG Survey) of 202 LIRGs in the nearby universe taken with Spitzer, Hubble, Chandra and GALEX. However GOALS lacks the near-infrared spectroscopic coverage needed to detect many important features (e.g. 3.3 microns PAH emission, Br-alpha recombination line) of LIRGs. Hence AKARI coverage is required, to build complete spectral energy distributions. This is the second OT proposal to request observations of the GOALS sample. In the previous proposal, we observed 39 sources to obtain an important sub-sample of LIRGs with luminosities greater than 1011.4 solar luminosities. In this proposal, we request to observe 19 lower luminosity galaxies and re-observe 31 sources in the previous proposal. Then we will combine them with the blocked targets from the archive to complete all of the GOALS sources. We propose IRCZ4 observations of each of 50 LIRGs selected from the GOALS sample, to bring the total number of pointings per source, up to a number between four and 10, in order to achieve our signal-to-noise ratio goals. The total number of priority A and B requested pointings is 265. This will complete observations of all of the LIRGs in the local universe observed by GOALS, except the AKARI blocked sources of the MP observations. This will allow us, without any selection bias, to build accurate starburst/AGN diagnostics, to investigate a correlation between these diagnostics and both the merger stage and the luminosity, and to understand galaxy evolution caused by galaxy-galaxy interactions.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
155	357	YPNMG	ITOH_YPNMG	Itoh Yoichi (Graduate School of Science, Kobe University)	OT-ISAS	3-II	Search for Young Planets in Nearby Moving Groups	Two models are currently proposed for planet formation; the disk instability model and the core accretion model. The previous search for extra-solar planets by the Subaru Telescope concluded that it is very rare chance for planet formation by disk instability, at least, with a large separation. We propose imaging search for young planets around 16 young dwarfs of the AB Dor group and the beta Pic group. If a planet forms by core accretion process, it should be detected in vicinity of a young dwarf by thermal infrared imaging with high sensitivity. Due to its proximity (< 30 pc) and youth (30 Myr), these groups are the best target for searching of young planets formed by core accretion process.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
156	359	UBSMG	KOHNO_UBSMG	Kohno Kotaro (Institute of Astronomy, Univ. of Tokyo)	OT-ISAS	3-II	AKARI/IRC Observations of Ultra-bright Submillimeter Galaxies	We propose to use AKARI in its warm phase to pinpoint the locations of 8 newly discovered extremely bright submillimeter galaxies (SMGs) during a course of our unprecedentedly wide (~ a few deg2) and deep (1 σ ~ 0.5--1 mJy) λ 1.1 mm sky survey using the bolometer camera AzTEC mounted on the submillimeter telescope ASTE in northern Chile. Due to our enormous survey coverage up to a few deg2, we could successfully uncover a very rare population of extreme starbursts; the flux densities of the targeted sources proposed here are >=10 mJy at 1.1 mm, so they are one of the brightest populations of SMGs so far. These provide us with important samples of the extreme starburst populations (SFR ~ a few 1000 Msun yr-1), which was difficult to address with the previous limited area deep survey. The proposed AKARI/IRC observations will find a promising infrared counterpart of AzTEC-ASTE SMGs, because recent multi-wavelengths follow up observations demonstrate that the SMGs are often intimately associated with "red" sources in Spitzer/IRAC bands. The objectives of this proposal could be listed as follows. (1) we can pinpoint the possible location of the SMGs if we find a red IRC source within error circles of the SMGs. (2) we will then estimate their redshifts through a SED modeling from infrared to radio wavelengths. (3) eventually, the heating sources of such a ultra-bright galaxies will be investigated based on multi-wavelengths follow up observations. Recent results suggest that more luminous IR galaxies tend to host active galactic nuclei as well as dusty extremely starburst. Our ultra-bright SMGs will provide us with a unique opportunity to explore such an extreme populations.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
157	347	SFICE	LEE_SFICE	Lee JeongEun (Sejong University)	OT-ISAS	3-II	Ices in Star Forming Cores	We propose to use AKARI/IRC spectroscopy to observe 15 YSOs, VeLLOs, and background stars, in order to study the chemical and thermal conditions in the star forming cores. A wide variety of observations (including SST IRAC, MIPS, and IRS observations) have been acquired toward those sources, and these complimentary data set will be combined with the NIR spectra, which trace the composition of icy grain mantles. We have a self-consistent model for the process of star formation, which couples the chemical evolution with the dynamics of surrounding material and the evolution of the central luminosity. The ice features of H2O, CO, and CO2 covered by the AKARI/IRC spectra are vital to constrain the dust and chemical properties in our self-consistent model. In addition, comparisons of ice features of VeLLOs with those toward normal YSOs and background stars will provide a crucial opportunity to understand the dynamical process of VeLLOs. Therefore, the obtained NIR spectral data cubes acquired by the proposed observations will enable three scientific goals: (1) to compare ice features in various evolutionary stages of star formation from molecular clouds to Class 0, I, and II protostellar cores, (2) to understand the dynamical process in VeLLOs, and (3) constrain self-consistently our chemical and dynamical evolutionary model.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
158	333	BRSFR	MATSUHARA_BRSFR	Matsuhara Hideo (JAXA)	OT-ISAS	3-II	Extinction-Independent Measurement of Star Formation Rates in Galaxies	We propose to complete our survey of Star Formation Rates (SFRs) in galaxies in the local Universe. We can do this by comparing our existing Hα imaging with new IRC grism spectra of the Brα emission line and the 3.3μm PAH emission. The goal of this project is to produce the definitive calibration of SFRs as a function of cosmic time. We do this by correcting the Hα luminosities for reddening by measuring Brα luminosities in the same compact star-forming regions. SFR is one of the most fundamental properties of galaxies, and is currently determined from applying recombination theory to H emission lines to infer the ionizing photon luminosities produced by O/B stars. Unfortunately, the 'gold standard' line, Hα, is known to be very susceptible to extinction by interstellar dust. The limited measurements of H lines in the infrared suggest that Hα often misses MOST (> 80%) of the ionizing luminosity from newly formed stars, embedded in dust. Using the definitive Brα line (which suffers extinction of only 0.035Av), IRC has shown that this is indeed the case in some ULIRGs, as well as some more normal, less luminous star-forming galaxies. Our preliminary results indicate that the 'canonical' assumption of one magnitude extinction correction to Hα flux is often too low by an additional 1--1.5mags! Our reduced 3--4.5μm IRC/grism spectra also show that a sufficient sample of Brα detections can be obtained by further observations of high-surface brightness gas emission-line regions in a wide sample of star-forming galaxies, with the accumulation of 6 pointings-where possible-to provide high enough SNRs.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
159	343	MAGNE	MORII_MAGNE	Morii Mikio (Tokyo Institute of Technology)	OT-ISAS	3-II	Emissson Mechanism of Magnetars: Disk or Magnetosphere?	We propose to observe four magnetars with AKARI to understand the infrared/optical emission mechanism. Several models have been proposed for the emission mechanism, which are based on the magnetospheric emission and disk emission. By the SED fitting for the spectrum obtained by AKARI, Spitzer, and near-infrared/optical observations, the disk models can be tested. Emission features are expected in the mechanism of the magnetospheric origin (cyclotron line and maser frequency peak). By multiple observations with a half year interval, variability of the SED also can be checked and hence the correlation with the X-ray flux is also tested. Disk model would produce strong and wide impact on astrophysics, not only on pulsar astronomy, but also on mechanism of supernova explosion and planet formation.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
160	363	SENNA	SAKON_SENNA	Sakon Itsuki (University of Tokyo)	OT-ISAS	3-II	Spectral Evolution of Novae in the Near-IR Based on AKARI Observations	Attempts to understand the dust formation scenario as well as the process of chemical enrichment by low to intermediate-mass stars are important to explore the origin of dust contained in the Milky Way and to understand the chemical evolution of the current universe. For this purpose, Classical Novae are one of the most interesting targets and, in this program, we plan to carry out the near-infrared spectroscopic observations of recent novae with AKARI/IRC at multiple epochs within a few years after the outburst. The goal of this program is to systematically understand the material evolution including the formation of precursor molecules and the process of dust condensation in the nova ejecta. The homogeneous datasets of successive near-infrared spectra from 2.5 to 5 micron with AKARI/IRC collected in this program are extremely unique and crucial to infer the physical conditions of the shell formed by the ejected materials and to examine the elemental abundance in nova ejecta. The obtained information will surely enable us to illustrate the dust formation scenario by novae and to understand their contribution towards the chemical evolution of the ISM in the current universe and to inspect the chemical linkage with the solar system meteorites.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
161	365	BVIOG	SASADA_BVIOG	Sasada Mahito (Hiroshima University)	OT-ISAS	3-II	Blazar Variability in near-Infrared, Optical and Gamma-ray regions	Blazars emit the broad band spectrum from radio to gamma-ray. The infrared data has been few because of the difficulty of observation in this range. We propose the infrared observations of blazars with AKARI IRCZ4. We will determine the synchrotron peak frequency and flux from simultaneous observations in the infrared range with AKARI, optical with KANATA, and gamma-rays with Fermi. The observation enables us to determine the physical parameters of the blazar, for example the strength of the magnetic field, unambiguously for the first time.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
162	367	PAHSR	SEOK_PAHSR	Seok JiYeon (Seoul National University)	OT-ISAS	3-II	Searching for 3.3 um PAH Emission in SNRs with AKARI/IRC Spectroscopy	Recently we have detected 3.3 μm polycyclic aromatic hydrocarbon (PAH) features in a supernova remnant (SNR) for the first time using AKARI. This SNR, N49 in the LMC, is interacting with a molecular cloud and the PAH emission is limited to the interacting region, which indicates that the origin of the 3.3 μm PAH emission is closely related to the interaction with molecular clouds. We propose to carry out AKARI/IRC spectroscopic observations of 3.3 μm PAH emission in three Galactic SNRs interacting with molecular clouds; 3C391, W44, and W28. These SNRs are the ones that showed PAH features in Spitzer IRS spectra. We want to compare the relative strengths of different PAH features in these SNRs, which can probe how various-sized PAH molecules, especially small neutral PAHs emitting 3.3 μm features, can be formed and/or survive in fast SNR shocks. Also, the heating mechanism of PAH molecules will be verified.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
163	369	IPYSO	SHIMONISHI_IPYSO	Shimonishi Takashi (Department of Astronomy, Graduate School of Science, University of Tokyo)	OT-ISAS	3-II	Ices and PAHs around Massive Young Stellar Objects	We propose to make near-infrared spectroscopic observations of 109 massive embedded young stellar objects(YSOs) in our Galaxy with AKARI/IRC. The proposed observations are to study Galactic massive YSOs complementarily to the Mission Program "Near Infrared Spectroscopic Observations of Red Objects in the Large Magellanic Cloud with AKARI in Phase III" (LMCNG; P.I. T. Onaka), which will observe a large number of extragalactic massive YSOs in the LMC and SMC. Near-infrared spectra of embedded YSOs show characteristic features due to ices and PAHs. These materials are important reservoir of heavy elements, and their features have potential to be a powerful diagnostics of circumstellar environments of YSOs. However, formation, evolution and diversity of ices and PAHs around embedded YSOs are not understood well due to the lack of systematic investigations of these features. The goal of the present observations is three-fold. First the CO2 ice formation process is investigated based on the data of a largest Galactic YSO sample ever studied. The second aim is to study spatial variations in the 3.3μm UIR band complex and investigate the properties and processing of the band carriers. The third aim is to search for new dust features in 2.5-5μm, including the deuterated PAH features. The proposed observation is crucial to investigate the formation, evolution and diversity of ices and PAHs around massive embedded YSOs. Also, near-infrared spectra obtained in the proposed observations should be a valuable dataset which for the first time enables us to compare the chemical properties of Galactic and extragalactic YSOs based on a large number of samples.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
164	371	SCKH2	SHINN_SCKH2	Shinn JongHo (Seoul National University)	OT-ISAS	3-II	Shocked H2 Gas around SNRs and Jets of YSOs	We propose spectral observations with AKARI's slit spectroscopy to observe shocked H2 gas toward supernova remnants and jets around young stellar objects. AKARI's near-infrared wavelength coverage (~ 2.5-5.0 μm) is useful to study the population of H2 (v=0, J>7) states, together with those of some (v>0, low-J) states. The relative population between these states is a useful probe to identify the excitation mechanism of H2 gas, since shock and radiations make distinctive populations, respectively. In addition, from these observations, we could check the validity of the thermal admixture model of H2 gas, which was known to describe the population of shocked H2 gas well. We found many jet features around young stellar objects from Spitzer IRAC band images, which are thought to be shocked H2 emissions and where the H2 thermal admixture model was successfully applied. When we obtain the near-infrared spectrum toward these diffuse features, we could test the validity of the model, and obtain the true ortho-to-para ratio of H2 gas, which cannot be obtained from the band images.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
165	373	YTTNK	TANAKA_YTTNK	Yasuyuki Tanaka (ISAS/JAXA)	OT-ISAS	3-II	Jets or Circumbinary disk? An AKARI Investigation	From some of neutron star and black hole X-ray binaries, Spitzer have recently detected excess infrared emission with respect to the Rayleigh-Jeans tail of a companion star or a accretion disk. To account for this enigmatic excess, two possible scenarios are now proposed: a circumbinary dust disk illuminated by the donor star or a synchrotron radiation from a jet. Since the infrared data points are scarce, it is difficult to determine either of the two models are really responsible from spectral fitting alone. The jet emission is expected to be highly variable, while the circumbinary disk emission is thought to be steady. Therefore, a variability study is a promising method to determine which of the two possible mechanisms actually works. From this viewpoint, we propose AKARI/IRC imaging observation to investigate temporal variation of infrared fluxes. This observation definitely reveals the origin of the excess infrared emission.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
166	375	SYDUS	WOO_SYDUS	Woo Jonghak (University of California Los Angeles)	OT-ISAS	3-II	Investigating the Nature of Dust in Active Galaxies	In the standard unification model of active galactic nuclei, dust plays a key role in explaining the difference in the observed properties between Seyfert 1 and 2 galaxies. Investigating the properties of dust grains that are either part of the central torus or mixed in the ionization cones in Seyfert galaxies can shed light on the understanding of the unification model of AGN. Using a 12 micron sample of 116 nearby Seyfert 1 and 2 galaxies, for the first time, we will investigate how the carbonaceous dust feature at 3.4 micron is distributed among the various types of Seyfert galaxies, and systematically compare the strength of carbonaceous feature with that of silicate feature at 9.7 micron. We will also Investigate distribution of the micron-size dust particles in Seyfert galaxies by measuring reddening using near-IR hydrogen recombination line ratios. We request 108 pointing observation for 55 Seyfert galaxies without previous AKARI grism spectroscopy. Combining our new data with Phase I and II data for the other 61 Seyfert galaxies, we will study dust properties and test the unification model.	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-jk.pdf
167	442	PLNTX	CARSON_PLNTX	Carson, Joseph (Max-Planck-Institut fur Astronomie, Germany)	OT-ESA	3-II	Search for Planetary Mass Companions of Nearby Young Stars	null	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-esa.pdf
168		DBIR2	DUC_DBIR2	Duc, Pierre Alain (AIM, CEA-Saclay, France)	OT-ESA	3-II	Stellar populations and hot dust in debris of galaxy collisions.	null	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-esa.pdf
169	444	DISEL	HOPWOOD_DISEL	Hopwood, Rosalind (The Open University, U.K.)	OT-ESA	3-II	Deep NIR spectroscopy and imaging of Abell 2218	null	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-esa.pdf
170		DEPPO	ENGELS_DEPPO	Engels, Dieter (Hamburger Sternwarte, Germany)	OT-ESA	3-II	The chemistry of warm dust in early post-AGB stars	null	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-esa.pdf
171	446	UTIRC	BURGDORF_UTIRC	Burgdorf, Martin (Deutsches SOFIA Institut, Germany)	OT-ESA	3-II	Spectroscopy of Ice Giants and Icy Moons	null	https://darts.isas.jaxa.jp/astro/akari/observations/proposals/otp3ii-apprv-esa.pdf

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