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.
observation_id
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
exposure
awarded_exposure
resolve_exposure
xtend_exposure
resolve_data_mode
resolve_with_filter_be
resolve_with_filter_fe55
resolve_with_filter_nd
resolve_with_filter_poly
resolve_with_filter_open
resolve_with_filter_undef
is_resolve_gatevalve_closed
is_resolve_mxs1
is_resolve_mxs2
is_resolve_mxs3
is_resolve_mxs4
xtend_number_modes
xtend_dataclass_file1
xtend_dataclass_file2
xtend_window1_exposure
xtend_window2_exposure
xtend_window1_burst_exposure
xtend_window2_burst_exposure
xtend_code
resolve_code
gen_code
processing_status
processing_date
public_date
distribution_date
processing_version
caldb_version
processing_software
proposal_id
proposal_abstract
proposal_category
proposal_category_code
proposal_priority
pi_name
co_pi_name
proposal_affiliated_country
proposal_cycle
proposal_type
proposal_title
observation_status
data_access_url
xtend_data_mode1
xtend_data_mode2
processing_count
remarks
1 300005010 Kepler_SNR 262.66411 -21.48209 261.91487 -21.44474 263.17291 1.78351 4.52182 6.82944 90.00056 60357.23269 2024-02-17 05:35:04 60358.56532 2024-02-18 13:34:04 55.337 50.000 55.337 46.304 PX_NORMAL N Y N N Y Y Y OFF OFF OFF OFF 1 30000010 46.304 0.000 0.000 0.000 11110 313430 11310 PROCESSED 2024-09-22 23:11:27 2025-08-31 00:00:00 2024-03-01 03:03:27 03.00.013.009 gen20240315_xtd20240815_rsl20240815 Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001 000000016 We propose to observe Kepler's supernova remnant (SNR), which is a rare Type-Ia SNR associated with N-rich circumstellar medium (CSM). Our minimal goals are (1) to measure elemental abundances of the CSM and (2) to study electron-ion temperature nonequilibration. The CSM abundance will constrain the mass of the donor star in the progenitor system. If we are awarded 200 ks, then we will perform spatially-resolved spectroscopy, and we will reveal the CSM distribution. We will also clearly detect outermost ejecta materials, i.e., O and C (if present), from the southern rim, where the CSM contribution is much weaker than in the north. The amount of the outermost ejecta will allow us to infer explosion physics which also helps reveal the subclass of Kepler's SN. SUPERNOVA REMNANTS 3 C XRISM Collaboration JAP 0 NOR THE PROGENITOR SYSTEM AND EXPLOSION PHYSICS FOR KEPLER'S SNR archived https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/3/300005010/ WINDOW1 6 Observation Log: No remarks ; Pre-pipeline Log: No remarks

Used SQL

SELECT * FROM xrism_master_data WHERE observation_id = '300005010'

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