This table records high-level information for the observations obtained with Hitomi and provides access to the data archive. The Hitomi mission was launched on a JAXA H-IIA into low Earth orbit on February 17, 2016, at 5:45 pm JPS from Tanegashima Space Center. Hitomi was equipped with four different instruments that together cover a wide energy range 0.3-600 keV. The Soft X-ray Spectrometer (SXS), which combined a lightweight Soft X-ray Telescope paired with a X-ray Calorimeter Spectrometer, provided non-dispersive 7-eV resolution in the 0.3-10 keV bandpass with a field of view of about 3 arcminutes. The Soft X-ray Imager (SXI) expanded the field of view with a new generation CCD camera in the energy range of 0.5-12 keV at the focus of the second lightweights Soft X-ray Telescope; the Hard X-ray Imager (HXI, two units) performed sensitive imaging spectroscopy in the 5-80 keV band; the non-imaging Soft Gamma-ray Detector (SGD, two units) extended Hitomi's energy band to 600 keV. On March 27, 2016, JAXA lost contact with the satellite and, on April 28, announced the cessation of the efforts to restore mission operations. At that time Hitomi was in check-out phase and had started the calibration observations. Data were collected from six celestial objects (Perseus, N132D, IGR_J16318-4848, RXJ1856.5-3754, G21.5-0.9, and Crab) as well as black sky for a total of about one month of data. The data from these observations were divided into intervals of one day if the observation of a specific pointing was longer that one day. A sequence number was assigned to each observing day and within data from all instruments are included. The day division was mainly to limit the data size within a sequence number. There are in total 42 sequences, and each record in this database table is dedicated to a single sequence. The early observations do not contain data from all instruments and in cases the object was not always placed at the aim point. This database contains parameters to indicate which instrument was on and if the celestial source was in the field of view. The SXS was the first instrument to turn on and therefore all observations contain SXS data, although the thermal equilibrium was reached after March 4 2016. The second instrument was the SXI followed by the HXIs and, finally, the two SGDs. This database table was generated at the Hitomi Science Data Center processing site (Angelini, L., Terada, Y, et al., 2016, SPIE 9905E, 14) with additions to indicate which instrument was on and if the source was in the FOV. It was ingested into the HEASARC database in June 2017. This is a service provided by NASA HEASARC .
The Hopkins Ultraviolet Telescope (HUT) was one of three ultraviolet
instruments of the ASTRO-1 mission flown on the space shuttle Columbia
during 2-10 December 1990. 106 spectrophotometric observations of 77
targets were obtained in the far-UV (i.e., 912-1850 Ã…) at a resolution
of ~3 Ã…. A few sources were observed in the 415-912 Ã… region with a
1.5 Ã… resolution. The same three instruments were later flown on the
space shuttle Endeavour from 3-17 March 1995 as part of the ASTRO-2
mission. During the longer ASTRO-2 mission, 385 observations of 265
targets were obtained.
The Hopkins Ultraviolet Telescope (HUT) was a shuttle-borne instrument used to obtain ultraviolet spectra in the far ultraviolet region of the spectrum. It was part of the ASTRO payload complement of three co-mounted instruments that flew in December 1990 and March 1995 as Space Shuttle missions. More than 650 spectra were obtained of 340 targets. In April, 2013, the HUT data was reprocessed to improve calibration, expand metadata, add new data products, and update file formats. The current cone service uses the metadata from these reprocessed files.
HST ACS Coma cluster (Abell 1656) Treasury Survey (COMA)
Short Name:
HST.COMA
Date:
23 Jul 2020 19:33:05
Publisher:
Space Telescope Science Institute Archive
Description:
The HST ACS Coma cluster Treasury survey is a deep two-passband imaging survey of one of the nearest rich clusters of galaxies, the Coma cluster (Abell 1656).
In January 2005, the Hubble Heritage Team obtained a large 4-color mosaic image of the Whirlpool Galaxy NGC 5194 (M51), and its companion NGC 5195, with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST observing program 10452, PI: Steven V. W. Beckwith). A six-pointing ACS WFC mosaic of the galaxy pair M51 was obtained in four filters: B, V, I, and H-alpha.
The Archival Pure Parallel Project processed and combined about 2,000 WFPC2 images, primarily in the wide UBVI filters, obtained in parallel with other HST instruments. Combined, drizzled, cosmic-ray cleaned images were produced for each pointing. These data can be used to address a wide range of science topics: measuring the cosmic shear on scales from 20" to 2'; discovering ~ 50 starforming galaxies at z ~ 4; finding optical counterparts to AGNs in wide-area radio and X-ray catalogs; improving the determination of the scale length of the Galactic disk; and studying stellar populations down to 1 solar mass for about 25 separate lines of sight in the Magellanic Clouds.
COSMOS (P.I. Nicholas Scoville, California Institute of Technology, USA/CA) is an HST Treasury Program to survey a 2 square degree equatorial field, centered on RA=10:00:28.6 and DEC=+02:12:21.0 with the ACS in the I band of the VIMOS equatorial field. Parallel observations with WFPC2 and NICMOS were also obtained.
GEMs is a large-area (800 arcmin 2) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the Hubble Space Telescope. Centered on the Chandra Deep Field-South, it covers an area of ~ 28'x28', or about 120 HDF areas, to a depth of MAB(F606W)=28.5(5s) for compact sources. Focusing on the redshift range ~ 0.2<z<1.1, GEMS provides morphologies and structural parameters for nearly 10,000 galaxies where redshift estimates, luminosities, and SEDs exist from COMBO-17.
The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image a typical field at high galactic latitude in four wavelength passbands as deeply as reasonably possible. In order to optimize observing in the time available, a field in the northern continuous viewing zone (CVZ) was selected and images were taken for 10 consecutive days, or approximately 150 orbits. Shorter 1-orbit images were also obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground-based telescopes. The observations were carried out from 18-30 December 1995, and the data are available to the community for study.
A second Hubble Deep Field campaign was carried out between late September and October of 1998. The raw, pipeline calibrated and reprocessed data were released to the community on November 23, 1998. The rationale for undertaking a second deep field campaign followed from the wealth of information that has come out of HDF-N, and from the desire to provide a point of focus for similar studies of the distant universe from southern-hemisphere facilities. Simultaneous, parallel observations were made with the three HST instruments STIS, WFPC2 and NICMOS of separate, neighboring fields. As was the case for HDF-N, approximately 150 consecutive orbits were devoted to a single telescope pointing.
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