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
1 NGC5129 BACKGROUND 201.7433 13.5725 201.127421 13.831619 194.704871 21.009611 336.16988197 74.1046924 116.4041 55547.7947106482 2010-12-17 19:04:23 55548.0397106482 2010-12-18 00:57:11 805074010 12.2767 10 12.2767 12.2847 0 12.2927 2 2 0 2 1 0 0 10.7811 10.7811 21.16 0 PROCESSED 57554.4321180556 2016-06-15 10:22:15 55960 2012-02-03 00:00:00 55592.9616435185 2011-01-31 23:04:46 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/ver3.0/805074010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '805074010'

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