This database table contains the list of all Röntgen Satellite (ROSAT) X-Ray Telescope (XRT) pointing-mode observations for which data sets are available, i.e., it excludes the ROSAT All-Sky Survey observations. Users should consult the RASSMASTER database table for those XRT observations which were made in scanning mode during the ROSAT All-Sky Survey (RASS) phase (30 July 1990 to 25 January 1991, and 3 August 1991 to 13 August 1991). For each observation listed in this table, parameters such as the focal-plane instrument used, the data processing site, and the target name and coordinates are given, as well as the ROSAT Observation Request (ROR) number, the actual and requested exposure times, the date(s) on which the observation took place, etc. For details about the ROSAT instruments, consult the ROSAT Guest Observer Facility (GOF) website at <a href="https://heasarc.gsfc.nasa.gov/docs/rosat/">https://heasarc.gsfc.nasa.gov/docs/rosat/</a>. A list of the available online ROSAT documentation can be found at <a href="https://heasarc.gsfc.nasa.gov/docs/rosat/rosdocs.html">https://heasarc.gsfc.nasa.gov/docs/rosat/rosdocs.html</a>. This table was created by the HEASARC in July 2004 by combining the data from two long-standing HEASARC Browse tables into one master table. It was updated by the HEASARC in March 2022 to add start and end times for the 157 sequence IDs which did not already have start and end times. This is a service provided by NASA HEASARC .
The WFCPOINT database table contains the list of ROSAT-Wide Field Camera calibration (CAL), performance verification (PV), and AO phase observations. For each observation listed in WFCPOINT, the target name, celestial co-ordinates, sequence number, PI name, and proposal title are given. The date of the observation, date that the data were distributed, and the date that the data will be released to the public are also given. The public release date is nominally 1 year and 14 days after the distribution date; however, because of some processing problems with a few datasets, the actual release date will be delayed from the given date. One duplicate entry was removed from the HEASARC implementation of this catalog in June 2019. This is a service provided by NASA HEASARC .
ROSAT High Resolution Image Pointed Observations Mosaic: Intensity
Short Name:
HRI
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
This survey was generated from all available ROSAT HRI observations. Data
were mosaicked into 1.1 degree tiles by SkyView. Exposure maps were
generated for each HRI observation using the hriexpmap FTOOL. For each
tile, all observations that might contribute to that tile were located and
added to count and exposure map tiles. Exposures for each observation were
calculated using a nearest neighbor interpolation of the center of the tile
pixels to the exposure map pixels. Counts were computed by projecting the
RA and Decs of each eligible photon into the appropriate tile pixel.
Only photons with a PHA > 3 were included in the mosaic and within each
observation only counts within the region where the exposure was greater
than half the maximum exposure were included. Provenance: Data from GSFC and MPE. <i>SkyView</i> mosaic generated by SkyView.. This is a service of NASA HEASARC.
The ROSATLOG database table has been created for the purpose of providing a complete, accurate, and easily accessible record of ROSAT observations. ROSATLOG is made by cross-correlating ROSAT observation records with the short-term timeline and contains information about all pointings executed by the satellite during the performance verification (PV) and AO phases. For each observation, details are given concerning target name and coordinates, pointing start and stop times, PI name and country, ROSAT Observation Request sequence number, and more. ROSATLOG is based on the short-term timelines and observation records generated at the German ROSAT Science Data Center at the Max Planck Institute for Extraterrestrial Physics (MPE) and sent to the ROSAT Guest Observer Facility at Goddard Space Flight Center (GSFC). Many duplicate entries were removed from the HEASARC implementation of this catalog in June 2019. This is a service provided by NASA HEASARC .
The ROSPRSPEC table contains the proposal titles and abstracts for all the accepted ROSAT proposals. Please refer to the ROSAO database table for other proposal information. This is a service provided by NASA HEASARC .
This survey is a mosaic of images taken by the ROSAT Wide Field Camera and
comprises of 12,743 seperates fields in each of two filters. Each field
covers a region 2.6&#176;; x 2.6&#176;; with a
0.3&#176;; overlap. Currently, this data is not a complete coverage of
the sky; regions near the northern ecliptic pole are currently not
included. Provenance: University of Leicester. This is a service of NASA HEASARC.
Rossi X-ray Timing Explorer was launched at the end
of 1995 and up to now (2004) it has been successfully operating for more
than 7 years. The mission was primarily designed to study the variability of
X-ray sources on time scales from sub-milliseconds to years.
The maneuvering capability of the satellite combined with the high
photon throughput of its main
detector (PCA) and high quality of background prediction (thanks to
PCA intrumental group of LHEA, GSFC) has also made it possible to
construct maps of the sky in energy band 3-20 keV. During its life time
RXTE/PCA has collected a large amount of data from slew observations
covering almost the entire sky.
<p>
We have utilized the slew parts of all RXTE/PCA
observations performed from April 15, 1996-July 16, 2002 which
amounts in total to approximately 50,000 observations. The exposure
time at a given point in the map is typically between 200-500 seconds.
The observational period before April 15, 1996
(High Voltage Epochs 1 and 2) was
excluded from the analysis because during that time the PCA had
significantly different gain and dependence of the effective area on
energy. The data reduction was done using standard tools of the
LHEASOFT with a set of packages written by M. Revnivtsev
(HEAD/IKI, Moscow; MPA, Garching).<p>
<p>
The survey has several features. It has strongly different exposure times
at different points on the sky that lead to strong variability of the
statistical noise on images. Because of that the only meaningful
representation of images is the map in units of statistical significance.
After the detection of a source flux can be determined from the map
in the 'flux' units. Map resolution is determined mainly by
the slew rate of the RXTE (<0.05-0.1&#176;;/sec) and the time resolution of
used data (16 sec, Std2 mode of the PCA). Sources can be detected down
to the level of ~6e<sup>-12</sup> erg/s/cm<sup>2</sup>, but at this level the
confusion starts to play an important role. Details of the survey are
presented in the paper of Revnivtsev et al. (2004). Provenance: High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M
PA, Garching, Germany. This is a service of NASA HEASARC.
The SAS2RAW database is a log of the 28 SAS-2 observation intervals and contains target names, sky coordinates start times and other information for all 13056 photons detected by SAS-2. The original data came from 2 sources. The photon information was obtained from the Event Encyclopedia, and the exposures were derived from the original "Orbit Attitude Live Time" (OALT) tapes stored at NASA/GSFC. These data sets were combined into FITS format images at HEASARC. The images were formed by making the center pixel of a 512 x 512 pixel image correspond to the RA and DEC given in the event file. Each photon's RA and DEC was converted to a relative pixel in the image. This was done by using Aitoff projections. All the raw data from the original SAS-2 binary data files are now stored in 28 FITS files. These images can be accessed and plotted using XIMAGE and other columns of the FITS file extensions can be plotted with the FTOOL FPLOT. This is a service provided by NASA HEASARC .
This database is the Third Small Astronomy Satellite (SAS-3) Y-Axis Pointed Observation Log. It identifies possible pointed observations of celestial X-ray sources which were performed with the y-axis detectors of the SAS-3 X-Ray Observatory. This log was compiled (by R. Kelley, P. Goetz and L. Petro) from notes made at the time of the observations and it is expected that it is neither complete nor fully accurate. Possible errors in the log are (i) the misclassification of an observation as a pointed observation when it was either a spinning or dither observation and (ii) inaccuracy of the dates and times of the start and end of an observation. In addition, as described in the HEASARC_Updates section, the HEASARC added some additional information when creating this database. Further information about the SAS-3 detectors and their fields of view can be found at: <a href="http://heasarc.gsfc.nasa.gov/docs/sas3/sas3_about.html">http://heasarc.gsfc.nasa.gov/docs/sas3/sas3_about.html</a> Disclaimer: The HEASARC is aware of certain inconsistencies between the Start_date, End_date, and Duration fields for a number of rows in this database table. They appear to be errors present in the original table. Except for one entry where the HEASARC corrected an error where there was a near-certainty which parameter was incorrect (as noted in the 'HEASARC_Updates' section of this documentation), these inconsistencies have been left as they were in the original table. This database table was released by the HEASARC in June 2000, based on the SAS-3 Y-Axis pointed Observation Log (available from the NSSDC as dataset ID 75-037A-02B), together with some additional information provided by the HEASARC itself. This is a service provided by NASA HEASARC .
The full sky 100 micron map is a reprocessed composite of the COBE/DIRBE
and IRAS/ISSA maps, with the zodiacal foreground and confirmed point
sources removed. Artifacts from the IRAS scan pattern were removed.
The result of these manipulations is a map with DIRBE-quality calibration
and IR AS resolution. Provenance: David J. Schlegel, Douglas P. Finkbeiner
and Marc Davis, Princeton University and University of California, Berkeley. This is a service of NASA HEASARC.
![the Fornax VST Survey is licensed under the `Creative Commons Attribution 4.0 License <http://creativecommons.org/licenses/by/4.0/>`_ .. image:: /static/img/ccby.png :alt: [CC-BY]](/registry-search/?f%5BcontentLevel_facet%5D%5B%5D=Research&f%5Brights_facet%5D%5B%5D=the+Fornax+VST+Survey+is+licensed+under+the+%60Creative+Commons+Attribution+4.0+License+%3Chttp%3A%2F%2Fcreativecommons.org%2Flicenses%2Fby%2F4.0%2F%3E%60_%0A%0A..+image%3A%3A+%2Fstatic%2Fimg%2Fccby.png%0A+++%3Aalt%3A+%5BCC-BY%5D%0A%0A&f%5Btype_facet%5D%5B%5D=Archive){kind=link}