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 201120010 CYGNUS_A 299.86695 40.73369 299.43401 40.59597 317.70361 59.32564 76.1892 5.75605 275.39115 60589.92991 2024-10-06 22:19:04 60593.02852 2024-10-10 00:41:04 179.372 100.000 179.372 132.243 PX_NORMAL N Y N N Y Y Y OFF OFF OFF OFF 1 300000A0 132.243 0.000 0.000 0.000 11110 313430 11310 PROCESSED 2024-10-17 10:24:59 2025-10-19 00:00:00 2024-10-18 10:25:00 03.00.013.009 gen20240315_xtd20240815_rsl20240815 Hea_21Aug2024_V6.34_XRISM_21Aug2024_V001 000016001 The core region of Cygnus A hosts a remarkably powerful, high-Mach number cocoon shock with an energy up to 10^61 erg. This is clearly a very dynamical example of interaction between the central SMBH and the surrounding gas that should leave unique imprints on the velocity of the ICM. Owing to the high X-ray temperature and brightness of this source, a relatively short 45 ks XRISM observation is sufficient to provide a wealth of velocity diagnostics, including line shifts, widths, shapes, and line strengths which will constrain the resonant scattering effect. These complementary probes of the gas kinematics, sensitive to motions on different scales and their anisotropy, will allow us to study both the small-scale turbulence, and the large-scale motions due to the cocoon shock's expansion. GROUPS AND CLUSTERS OF GALAXIES 2 A ANWESH MAJUMDER TIMOTHY HECKMAN EUS 1 NOR EXPLORING THE NATURE OF AGN FEEDBACK NEAR THE COCOON OF CYGNUS A archived https://data.darts.isas.jaxa.jp/pub/xrism/data/obs/rev3/2/201120010/ WINDOW1 1 Observation Log: No remarks ; Pre-pipeline Log: No remarks

Used SQL

SELECT * FROM xrism_master_data WHERE observation_id = '201120010'

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