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 G11.2-0.3 272.8676 19.433 272.324919 19.420376 273.677117 42.836704 46.34586116 17.29738119 77.6432 53834.4626041667 2006-04-09 11:06:09 53835.6634143518 2006-04-10 15:55:19 401010010 43.9846 50 43.9926 43.9846 43.9926 43.9926 2 2 2 2 1 0 0 37.3879 37.3879 83.6799 1 PROCESSED 57533.4279166667 2016-05-25 10:16:12 54397 2007-10-24 00:00:00 53905.4671875 2006-06-19 11:12:45 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 010049 The PSR 1811-1925 in a historical supernova remnant G11.2-0.3 has its characteristic age as 10 times longer than the age of the remnant. The pulsar has its period 64 ms and the hard spectrum. We suggest that the pulsar shows the signs of having the small magnetic field. The SUZAKU observation must give the answer for this hypothesis. First, HXD allows us to observe the spectrum in the high energy range, and if the cut-off would be observed, the magnetic fields of pulsar will be estimate. Seconds, XIS has the great energy resolution to determine the abundance of the shell. This would let us estimate the mass of the progenitor. Third, HXD provides the new spin down rate observation. Then, we can make sure the constancy of the spin down rate. The pulsar age mystery must be solved by SUZAKU. GALACTIC POINT SOURCES 4 C ASAMI HAYATO JAP 1 AO1 CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3 XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401010010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '401010010'

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