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 PKS 1510-089 228.2108 -9.1043 227.537329 -8.917552 228.287746 8.492539 351.2856545 40.1353659 286.8003 53949.3968634259 2006-08-02 09:31:29 53952.2544444445 2006-08-05 06:06:24 701094010 119.1577 120 119.1577 119.1577 119.1657 119.1657 2 2 2 2 1 0 0 106.2588 106.2588 246.8638 5 PROCESSED 57535.1605208333 2016-05-27 03:51:09 54394 2007-10-21 00:00:00 54018.7363194444 2006-10-10 17:40:18 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 013016 It has been a long mystery (i) how the relativistic jets are formed, and (ii) what is the composition of a jet. In the theoretical view, strong magnetic field (u_B >> u_e) is necessary to produce such outflows with baryonic matters, but observations favor opposite scenario, namely particle dominated (u_e >> u_B), leptonic jet. Such discrepancies can be resolved if moderate numbers of protons (n_e/n_p > 50) are mixed in the non-tnermal pair populations. This can be easily tested if we can observe characteristic "soft X-ray bump" produced by the bulk-Comptonization of UV photons emitted from an accretion disk. We propose a deep observation (40ksec x3) of an EGRET quasar PKS 1510-089, which shows a clear sign of soft X-ray bump in BeppoSAX, ROSAT and ASCA observations. EXTRAGALACTIC COMPACT SOURCES 7 B JUN KATAOKA GRZEGORZ MADEJSKI JUS 1 AO1 DIRECT TESTING THE JET COMPOSITION IN A POWERFUL EGRET QUASAR PKS 1510-089 XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701094010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '701094010'

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