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 A399/401 FILAMENT 44.7475 13.2485 44.061375 13.049612 46.15841 -3.573964 164.45015039 -39.12843885 74.1756 53966.1736921296 2006-08-19 04:10:07 53969.4641666667 2006-08-22 11:08:24 801020010 151.0601 150 151.0601 151.0681 151.0681 151.0681 2 2 2 2 1 0 0 142.2036 142.2036 284.2738 5 PROCESSED 57535.3984837963 2016-05-27 09:33:49 54526 2008-03-01 00:00:00 54021.1056944444 2006-10-13 02:32:12 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 010063 Although warm-hot intergalactic medium (WHIM) is supposed to account for most of the baryon in the Universe, its detection is extremely difficult. Here, we propose to observe the cosmological filament between clusters A399 and A401 with Suzaku. We try to detect the OVII emission line and confirm the existence of WHIM in the filament. We expect that the density of the WHIM in the filament is high, and that the detection will be easier than that in other regions in the Universe. Moreover, since the redshift of the filament is relatively high, we can discriminate between the OVII mission from the WHIM and that from our Galaxy by studying the redshift of the line. EXTRAGALACTIC DIFFUSE SOURCES 8 A YUTAKA FUJITA JAP 1 AO1 THE DETECTION OF WHIM IN THE A399/401 FILAMENT XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801020010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '801020010'

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