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 | RCW86 SW | 220.2761 | -62.6782 | 219.292066 | -62.464185 | 240.754321 | -44.190898 | 315.14426109 | -2.43598628 | 109.6929 | 53778.0961689815 | 2006-02-12 02:18:29 | 53780.2814699074 | 2006-02-14 06:45:19 | 500004010 | 100.7659 | 100 | 100.7819 | 100.7659 | 100.7819 | 100.7819 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 90.6819 | 90.6819 | 188.7918 | 2 | PROCESSED | 57533.035787037 | 2016-05-25 00:51:32 | 54247 | 2007-05-27 00:00:00 | 54041.2835648148 | 2006-11-02 06:48:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001019 | The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 0 | SWG | THE FIRST DIRECT MAPPING OF ACCELERATED PROTONS IN THE SW SHELL OF RCW 86 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500004010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '500004010'
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