DARTS/Astro Query System - SQL 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 "SQL Search".
total 1
No. |
object_name
|
center_ra
|
center_dec
|
center_ra_b1950
|
center_dec_b1950
|
center_ecliptic_lon
|
center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
|
observation_start_time_mjd
|
observation_start_time
|
observation_end_time_mjd
|
observation_end_time
|
observation_id
|
exposure
|
awarded_exposure
|
xis0_exposure
|
xis1_exposure
|
xis2_exposure
|
xis3_exposure
|
xis0_observation_mode
|
xis1_observation_mode
|
xis2_observation_mode
|
xis3_observation_mode
|
hxd_observation_mode
|
hxd_coarse_clock_rate_exposure
|
hxd_first_clock_rate_exposure
|
hxd_normal_clock_rate_exposure
|
hxd_all_clock_rate_exposure
|
hxd_wam_exposure
|
quantity_of_hxd_burst
|
processing_status
|
processing_date_mjd
|
processing_date
|
public_date_mjd
|
public_date
|
distribution_date_mjd
|
distribution_date
|
processing_version
|
processing_count
|
processing_software
|
proposal_id
|
proposal_abstract
|
proposal_category
|
proposal_category_code
|
proposal_priority
|
pi_name
|
co_pi_name
|
proposal_affiliated_country
|
proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
|
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1 | NGC5129 OFF-CENTER1 | 201.3141 | 14.0346 | 200.698603 | 14.294472 | 194.098163 | 21.268391 | 335.68408417 | 74.71314923 | 124.7585 | 55548.0427314815 | 2010-12-18 01:01:32 | 55548.7883101852 | 2010-12-18 18:55:10 | 805072010 | 30.2512 | 30 | 30.2512 | 30.2512 | 0 | 30.2512 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.4611 | 24.4611 | 64.4119 | 0 | PROCESSED | 57554.4566203704 | 2016-06-15 10:57:32 | 55960 | 2012-02-03 00:00:00 | 55592.9994444444 | 2011-01-31 23:59:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805072010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '805072010'
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