DARTS/Astro Query System - SQL Search -

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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 202063010 SIGMA_GEM 115.82683 28.88398 115.04722 29.00354 112.62545 7.45076 191.18856 23.27364 100.00138 60985.92991 2025-11-06 22:19:04 60988.36949 2025-11-09 08:52:04 109.076 100.000 109.076 112.880 PX_NORMAL N Y N N Y Y Y OFF OFF OFF OFF 1 300000A0 112.880 0.000 0.000 0.000 11110 313430 11310 PROCESSED 2025-11-14 08:15:51 2026-11-15 00:00:00 2025-11-15 08:15:52 03.03.015.012 gen20241115_xtd20250915_rsl20250915 Hea_26Sep2025_V6.36_XRISM_12Sep2025_V003 000021386 Nano/micro flare heating is a promising explanation for the solar/stellar coronal heating problem. The low-ionized Fe Ka line at 6.4 keV can be a tracer of stellar nano/micro flares. High-energy-resolution spectroscopy is necessary to determine the intensity and photoionization state of the Fe Ka line accurately. The ionization parameter of the Fe Ka line depends on the flare energy scale. We propose a 100 ks Resolve observation of the RS CVn-type star Sigma Gem to reproduce the flare frequency distribution of stellar nano/micro flares and investigate whether the temperature of the Sigma Gem corona can be explained by the sum of the energies of them. We also use Xtend to determine the temperature of the quiescent corona of Sigma Gem during the Resolve observation. STELLAR CORONAE, WINDS, AND YOUNG STARS 2 B SHUN INOUE JAP 2 NOR STELLAR CORONAL HEATING PROBLEM STUDIED BY OBSERVATIONS OF THE FE KA LINE OF THE RS CVN-TYPE STAR SIGMA GEM processed https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/202063010/ WINDOW1 1 Observation Log: No remarks ; Pre-pipeline Log: No remarks

Used SQL

SELECT * FROM xrism_master_data WHERE observation_id = '202063010'

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