The AKARI (formerly Astro-F) mission is a Japanese second generation all-sky infrared
survey mission. SkyView currently includes surveys from the four bands of the FIS instrument:
N60, WIDE-S, WIDE-L and N160.
<p>
These surveys cover
99% of the sky in four photometric bands centred at 65μm, 90μm, 140μm, and 160μm,
with spatial resolutions ranging from 1-1.5'.
<p>
These data provide crucial information on the investigation and characterisation of the proper-
ties of dusty material in the interstellar medium (ISM), since a significant portion of its
energy is emitted between
∼50 and 200 μm. The large-scale distribution of interstellar
clouds, their thermal dust temperatures, and their column densities can be investigated
with the improved spatial resolution compared to earlier all-sky survey observations.
In addition to the point source distribution, the large-scale distribution of ISM cirrus emis-
sion, and its filamentary structure, are well traced.
<p>
Data are obtained using using the <a href="https://jvo.nao.ac.jp/index-e.html">JVO</a> AKARI Simple Image Access Service. Provenance: AKARI FIS map making team [Univ of Tokyo, ISAS/JAXA, Tohoku Univ, Tsukuba Univ,
The Rutherford Appleton Laboratory, The Open Univ]. This is a service of NASA HEASARC.
The ASCAMASTER table contains data on all ASCA observations that were ever in any of the following states: 'Accepted', 'Scheduled Long-Term', 'Scheduled Short-Term', 'Processed', and 'Archived'. The final status of an observation is given by the parameter Status. Specific dates that affect the status of an observation are listed as the parameters scheduled_date, observed_date, processed_date, archived_date, and cycle. Notice that, if one or more of the date parameters are empty for a given observation, this means that that those particular processes have not occurred: e.g., if observed_date is empty, this means that the planned observation was not observed. This is a service provided by NASA HEASARC .
This preliminary ASCA SIS Source Catalog contains a list of point sources detected by the Solid-state Imaging Spectrometers (SIS) on-board the ASCA Observatory. This catalog was generated by searching for point-like sources in all data available from the HEASARC's ASCA public archive (ASCAPUBLIC) as of 24 Oct 1996; and is populated by both target and serendipitous sources in the SIS field-of-view. For each catalogued source various information is available, which includes the celestial coordinates of the source, the count rate, the significance of detection, and the hardness ratio, total aperture counts, exposure time, and start time of the observation. In addition, a set of three GIF "thumbnail" images is available in the broad (0.5 - 12 keV), soft (2 < keV), and hard (> 2 keV) spectral bands centered on the apparent detection. These images are convenient for accessing the quality of the source detection. The current catalog is preliminary, the goal of the catalog authors being to make the SIS source list available as quickly as possible. To accomplish this, they took an incremental approach and placed their "work in progress" on-line, warts and all. They urge caution in using and citing these preliminary results, as they point out that the information is not, as yet, 100% reliable. This catalog was generated in January 1997 by Drs. Eric Gotthelf and Nicholas White and resulted from their search for point-like sources in all of the then-available SIS data files in the HEASARC's Public ASCA Data Archive as of 24 Oct 1996. The catalog is populated with both targeted and serendipitous sources that were present in the SIS field-of-view. This is a service provided by NASA HEASARC .
This survey was taken with the Bonn Stockert 25m telescope. It was
distributed on the NRAO <i>Images from the Radio Sky</i> CD-ROM. This image
was delivered as a four map mosaic but was combined into a single
map before being included in <i>SkyView</i>. Provenance: Max Planck Institute for Radio Astronomy, generated by P. Reich and W. Reich. This is a service of NASA HEASARC.
This survey is a maximum entropy solution to the data taken by the
CompTel instrument on the <i> Compton </i> Gamma Ray Observatory.
The data in this survey are intended only to give the general appearance
of the MeV gamma-ray sky. Fluxes, flux limits and spectra should be
derived using the Compass system for the analysis of CompTel
data. Compass is available at the
<a href="https://web.archive.org/web/20100622161007/http://wwwgro.unh.edu/comptel/compass/compass_users.html"> Compton Observatory
Science Support Center </a>.
<P>
The maps were originally generated
by the CompTel Instrument Team
as three separate maps in the bands:
<UL>
<LI>1-3 MeV
<LI>3-10 MeV
<LI>10-30 MeV
</ul>
<P>
All CompTel observations from phases 1, 2 and 3 were included in the
maps (May 1991 through October 1994).
These maps were combined into a single 3-D map at <i> SkyView </i>
<P> Provenance: CompTel Instrument Team. Maps generated
by Andrew Strong, Max-Planck
Institute for Extraterrestrial Physics (Garching).. This is a service of NASA HEASARC.
This database table contains all of the observations made by the Chandra X-Ray Observatory (CXO, formerly known as the Advanced X-ray Astrophysics Facility or AXAF) as part of the Performance Verification and Calibration (PVC) phase and also contains all of the subsequent Cycles' Guaranteed Time Observers (GTO) and General Observer (GO) targets, and any Director's Discretionary Time (DDT) targets that have been observed. It also includes scheduled and as-yet-not-scheduled targets. The HEASARC updates this database table on a twice-weekly basis by querying the database table at the Chandra X-Ray Center (CXC) website, as discussed in the Provenance section. For observations whose status is 'archived', data products can be retrieved from the HEASARC's mirror of the CXC's Chandra Data Archive (CDA). The CXC should be acknowledged as the source of Chandra data. The PVC phase was during the first few months of the CXO mission; some of the calibration observations that are for monitoring purposes will be performed in later mission cycles. All calibration data (entries with Type = CAL in this database) are placed immediately into the CXO public data archive at the Chandra X-Ray Observatory Center (CXC); please see the Web page at <a href="http://asc.harvard.edu/">http://asc.harvard.edu/</a> for more information on the CXC data archive). GTO observations during Cycle 1 or any subsequent Cycle will probably occupy 100% of months 3-4, 30% of months 5-22, and 15% of the available time for the remainder of the mission. Guaranteed Time Observers will have the same proprietary data rights as General Observers (i.e., their data will be placed in the public CXC archive 12 months after they have received the data in usable form). For detailed information on the Chandra Observatory and datasets see: <pre> <a href="http://cxc.harvard.edu/">http://cxc.harvard.edu/</a> for general Chandra information <a href="http://cxc.harvard.edu/cda/">http://cxc.harvard.edu/cda/</a> for the Chandra Data Archive <a href="http://cxc.harvard.edu/cal/">http://cxc.harvard.edu/cal/</a> for calibration information <a href="http://cxc.harvard.edu/caldb/">http://cxc.harvard.edu/caldb/</a> for the calibration database <a href="http://cxc.harvard.edu/ciao/">http://cxc.harvard.edu/ciao/</a> for data analysis <a href="http://cxc.harvard.edu/ciao/download/">http://cxc.harvard.edu/ciao/download/</a> for analysis software <a href="http://cxc.harvard.edu/ciao/threads/">http://cxc.harvard.edu/ciao/threads/</a> for analysis threads <a href="http://cda.harvard.edu/chaser/">http://cda.harvard.edu/chaser/</a> for WebChaSeR </pre> The HEASARC updates this database table on a twice-weekly basis based on information obtained from the Chandra Data Archive at the CXC website. This is a service provided by NASA HEASARC .
New large-scale CO surveys of the first and second Galactic quadrants and the
nearby molecular cloud complexes in Orion and Taurus, obtained with the
Harvard-Smithsonian Center for Astrophysics 1.2 m telescope, have been
combined with 31 other surveys obtained over the past two decades with that
instrument and a similar telescope on Cerro Tololo in Chile, to produce a
new composite CO survey of the entire Milky Way. The survey consists of
488,000 spectra that Nyquist or beamwidth (1/8 deg) sample the entire Galactic
plane over a strip 4 deg-10 deg wide in latitude, and beamwidth or 1/4 deg sample
nearly all large local clouds at higher latitudes. Compared with the previous
composite CO survey of Dame et al. (1987), the new survey has 16 times more
spectra, up to 3.4 times higher angular resolution, and up to 10 times higher
sensitivity per unit solid angle.
<P>
Users should be aware that both the angular resolution and the
sensitivity varies from region to region in the velocity-integrated map.
The component surveys were integrated individually using clipping or
moment masking in order to display nearly all statistically significant
emission but little noise above a level of ~1.5 K km/s. See the reference
below and the
<a href="https://lweb.cfa.harvard.edu/mmw/">
Millimeter-Wave Group site</a> for more details Provenance: Data taken by two nearly-identical 1.2 m
telescopes in Cambridge, MA and on Cerro Tololo, Chile combined into a
complete survey of the Milky Way with CO integrated over all velocities.. This is a service of NASA HEASARC.
Cosmic Background Explorer DIRBE Annual\ Average\ Map
Short Name:
COBE
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
The DIRBE Project Data Sets cover the whole sky and provide photometric data
in 10 bands ranging in wavelength from 1.25 to 240 microns. SkyView has supported
three maps: an early averaged map including including zodiacal and
Galactic components (COBE DIRBE (OLD)), a more recent cleaner version of
that data (COBE DIRBE/AAM) and a map with the zodaical light subtracted out
(COBE DIRBE/ZSMA). The early data is no longer supported. Please contact us if you
want access to these data.
<P>
Detailed descriptions of the DIRBE, the data processing, and the data products
are given in an Explanatory Supplement. A Small Source Spectral Energy Distribution
Browser can be used to assess the visibility of an unresolved or small extended source
in the DIRBE data and see its spectral energy distribution. As noted in section
5.6.6 of the Explanatory Supplement, the DIRBE Time-ordered Data are required to
derive definitive point source fluxes.
<p>
These maps provide an estimate of the infrared intensity at each pixel and
wavelength band based on an interpolation of the observations made at
various times at solar elongations close to 90&#176;;.
<P>
These COBE DIRBE maps are a combination original ten band passes with the following wavelengths:
<UL>
<LI>Band 1 - 1.25 &#181;;m
<LI>Band 2 - 2.2 &#181;;m
<LI>Band 3 - 3.5 &#181;;m
<LI>Band 4 - 4.9 &#181;;m
<LI>Band 5 - 12 &#181;;m
<LI>Band 6 - 25 &#181;;m
<li>Band 7 - 60 &#181;;m
<li>Band 8 - 100 &#181;;m
<li>Band 9 - 140 &#181;;m
<li>Band 10 - 240 &#181;;m
</ul>
<p>
The default two dimensional array uses Band 8 (100 &#181;;m).
<P>
The COBE DIRBE/Annual Average Maps (AAM) is the cumulative weighted
average of the photometry. This average is calculated using the
weighted number of observations from each Weekly Averaged Map
( WtNumObs from the Weekly Averaged Map) as the weight, such that
annual_average =sum( weekly_average * weekly_weight )/ sum( weekly_weight )
<p>
COBE DIRBE/Zodi-Subtracted Mission Average (ZSMA) Skymap represents
the extra-Solar system sky brightness. It is the average
residual map that results after the modelled interplanetary dust (IPD) signal
is subtracted from each of the DIRBE Weekly Skymaps from the cryogenic mission.
Individual weekly residual maps can be reconstructed from the data supplied in
the DIRBE Sky and Zodi Atlas (DSZA). Provenance: COBE Team. This is a service of NASA HEASARC.
This survey is derived from the 21cm maps presented by Dickey and Lockman
in the <i>ARAA</i> 28, p215. The nH is derived assuming optically thin
emission. The nH given should be considered a lower limit when the nH is
greater than several times 10<sup>20</sup>. Provenance: provided by S. Snowden from data by Dickey and Lockman. This is a service of NASA HEASARC.
Roger et al. (1999) presented a map of the 22 MHz radio emission between declinations -28° and +80°,
covering ~73% of the sky, derived from observations with the 22 MHz radiotelescope of the
Dominion Radio Astrophysical Observatory (DRAO).
The resolution of the telescope (EW x NS) is 1.2° x 1.7° secant(zenith angle).
Roger et al. emphasize that the main value of the data lies in the representation of structure
larger than the beam.
The strongest point sources (Cas A, Cyg A, Tau A and Vir A) have been removed from the map.
<p>
The Centre d'Analyse de Données Etendues group used the data to form an all-sky HEALPix format map
following the method described in Appendix A of Paradis et al. 2012, A&A, 543, 103, ADS.
Their HEALPix map is mirrored here.
The map is in units of K brightness temperature.
Map pixels are set to a sentinel value of -32768.0 for unobserved regions and
for regions affected by sidelobes around Cyg A, Tau A, and Vir A. Provenance: DRAO, MPI for Radio Astronomie. This is a service of NASA HEASARC.
The Effelsberg-Bonn HI Survey (EBHIS) is a 21-cm survey performed with the
100-m telescope at Effelsberg. It covers the whole northern sky out to a
redshift of z ~ 0.07 and comprises HI line emission from the Milky Way and the
Local Volume. This dataset is the atomic neutral hydrogen (HI) column density
map derived from the Milky-Way part of EBHIS (|Vlsr| < 600 km/s). Provenance: Argelander-Institut für Astronomie (AIfA) and Max-Planck-Institut
für Radioastronomie (MPIfR); data provided by B. Winkel. This is a service of NASA HEASARC.
Energetic Gamma-Ray Event Telescope: 10 channel data
Short Name:
EGRET3D
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
These data are from the Compton GRO EGRET team. Data are from all pointings
of the EGRET instrument in the verification phase and phase 1-4 of the Compton
mission. The maps exist in energies 30-100 MeV, 100-10000 MeV, and
as a multi-dimensional, 10 channel survey. For the multi-dimensional
survey, channels 1-3 comprise energies less than 100 MeV, and channels
4-10 comprise energies greater than 100 MeV. Note that the energies
are not uniformly split among the channels.
<P>
The EGRET 3D map is comprised of ten channels with the following
energy ranges:
<UL>
<LI>Channel 1 30-50 MeV
<LI>Channel 2 50-70 MeV
<LI>Channel 3 70-100 MeV
<LI>Channel 4 100-150 MeV
<LI>Channel 5 150-300 MeV
<LI>Channel 6 300-500 MeV
<LI>Channel 7 500-1000 MeV
<LI>Channel 8 1000-2000 MeV
<LI>Channel 9 2000-4000 MeV
<LI>Channel 10 4000-10000 MeV
</ul>
<p>
The default two dimensional image for the EGRET 3D survey is an average
of Channels 4 - 10 (energies greater than 100 MeV). Provenance: EGRET Instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
These data are from the Compton GRO EGRET team. Data are from all pointings
of the EGRET instrument in the verification phase and phase 1-4 of the Compton
mission. The maps exist in energies 30-100 MeV, 100-100000 MeV, and
as a multi-dimensional, 10 channel survey. For the multi-dimensional
survey, channels 1-3 comprise energies less than 100 MeV, and channels
4-10 comprise energies greater than 100 MeV. Note that the energies
are not uniformly split among the channels.
<P>
The EGRET 3D map is comprised of ten channels with the following
energy ranges:
<UL>
<LI>Channel 1 30-50 MeV
<LI>Channel 2 50-70 MeV
<LI>Channel 3 70-100 MeV
<LI>Channel 4 100-150 MeV
<LI>Channel 5 150-300 MeV
<LI>Channel 6 300-500 MeV
<LI>Channel 7 500-1000 MeV
<LI>Channel 8 1000-2000 MeV
<LI>Channel 9 2000-4000 MeV
<LI>Channel 10 4000-10000 MeV
</ul>
<p>
The default two dimensional image for the EGRET 3D survey is an average
of Channels 4 - 10 (energies greater than 100 MeV). Provenance: EGRET Instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
VO-compliant publication of Schmidt survey ESO-R of the southern sky digitized with the MAMA microdensitometer at the Observatoire de Paris Image Analysis Centre (CAI).
The EUVE satellite surveyed the entire sky in the extreme ultraviolet
through a set of four filters. The filters include:
<UL>
<LI>Lexan/Boron filter: peak at 83A (full range 50-180)
<LI>Aluminium/Carbon/Titanium : 171A (160-240)
<LI>Aluminium/Titanium/Antimony: 405A (345-605)
<LI>Tin/SiO: 555A (500-740)
</UL>
<P>
The data currently in <i>SkyView</i> is direct from the Center for EUVE. Provenance: Center for Extreme UV Astronomy, UCB. This is a service of NASA HEASARC.
This survey sums all data observed by the Fermi mission up to week 396.
This version of the Fermi survey are intensity maps where the summed counts data
are divided by the exposure for each pixel (in cm^2 s) and the area of the pixel.
Data is broken into 5 energy bands
<ul>
<li> 30-100 MeV Band 1 </li>
<li> 100-300 MeV Band 2 </li>
<li> 300-1000 MeV Band 3 </li>
<li> 1-3 GeV Band 4 </li>
<li> 3-300 GeV Band 5 </li>
</ul>
The SkyView data are based upon a Cartesian projection of the counts divided by
the exposure maps. In the Cartesian projection pixels near the pole have
a much smaller area than pixels on the equator, so these pixels have smaller
integrated flux.
When creating large
scale images in other projections users may
wish to make sure to compensate for this effect
the flux conserving clip-resampling option. Provenance: Fermi LAT instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
The VLA FIRST (Faint Images of the Radio Sky at Twenty-centimeters)
is a project designed to produce the radio equivalent
of the Palomar Observatory Sky Survey over 10,000 square
degrees of the North Galactic Cap. The
<a href="https://sundog.stsci.edu/top.html"> FIRST home page </a>
has details of the instrumentation, status of the project,
and data available. Currently about 5000 images
of approximately .775x.58 degrees are available.
<P>
These FIRST data have been retrieved from the
<a href="ftp://archive.stsci.edu/pub/vla_first/data/"> FIRST FTP archive
</a> at the
<a href="https://www.stsci.edu/resources"> Space Telescope Science Institute</a>.
<p>
The FIRST survey is included on the <b>SkyView High Resolution Radio
Coverage </b><a href="/images/high_res_radio.jpg"> map</a>. This map shows
coverage on an Aitoff projection of the sky in equatorial coordinates. Provenance: The FIRST project team: R.J. Becker, D.H. Helfand, R.L. White
M.D. Gregg. S.A. Laurent-Muehleisen.. This is a service of NASA HEASARC.
This survey uses the POSS1 Blue plates. Provenance: Data taken by CalTech, Compression
and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
This survey is the POSS1 Red plates from the original POSS survey.
It covers the sky north of -30 degrees declination. Provenance: Data taken by CalTech Compression
and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
The GALEX, Galaxy Explorer, mission
was launched by a Pegasus-XL vehicle on April 28 2003 into
a 690km altitude, 29 degree inclination, circular orbit with a 98.6
minute period. The GALEX instrument allows imaging and spectroscopic
observations to be made in two ultraviolet bands,
Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A.
The instrument provides simultaneous co-aligned FUV and NUV
images with spatial resolution 4.3 and 5.3 arcseconds respectively.
Details of the performance of the instrument and detectors can be found in
Morrissey et al. (2007) ApJS, 173, 682.
<p>
The <i>SkyView</i> GALEX surveys mosaic the intensity images of
All-Sky Survey images. For a given pixel only the nearest image is used.
Since a given GALEX observation is circular, this maximizes the coverage
compared with default image finding algorithms which use the distance from
edge of the image.
<p>
As of February 10, 2011, SkyView uses the GALEX GR6 data release. Provenance: All data is downloaded from the <a href="https://galex.stsci.edu">
MAST GALEX archive</a>.. This is a service of NASA HEASARC.
GLEAM 72-103: GaLactic and Extragalactic Allsky MWA Survey
Short Name:
GLEAM1
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
GLEAM, the GaLactic and Extragalactic All-sky MWA survey, is a survey of
the entire radio sky south of declination 30 degrees at frequencies
between 72 and 231 MHz. It was made with the Murchison Widefield Array
(MWA) using a drift scan method that makes efficient use of the MWA's very
large field-of-view. The survey is described in Wayth et al. (2015) and
the <a href="https://www.mwatelescope.org/gleam">website</a> at https://www.mwatelescope.org/gleam.
<p>
The data presented here are from the first year of GLEAM observing, published in:
<ul>
<li> Hurley-Walker et al. (2017): 25,000 square degrees of extragalactic sky
<li> For et al. (2018): the Large and Small Magellanic Clouds
<li> Hurley-Walker et al. (2019c): 8,000 square degrees of the Galactic plane
</ul>
A region around Centaurus A, a few other small regions described by Hurley-Walker et al. (2017), and the Galactic plane between 180 < l < 345 degrees, are not available.
<p>
The most sensitive and highest-resolution image is the 170-231MHz image
which was used for all source-finding in generating the catalogue. It has
a resolution of approximately 2.2 x 2.2/cos (dec + 26.7) arcmin at this
frequency. However, due to ionospheric distortions, the final resolution
of the survey varies by ~10% over the sky, with a direction-dependent PSF.
<p>
The <i>SkyView</i> data for the GLEAM surveys was extracted using the team's
cutout server, into small (3 degree) raw cutouts over the region covered
by the GLEAM survey. These cutouts have somewhat variable size and resolution. The
default scale (i.e., pixel size) used for <i>SkyView</i> images is given in the table
below. Since the GLEAM cutout server will not create an appropriately sized tile for the Sourth Pole, a
larger tile offset from the pole is used.
<p>
<i>SkyView</i> resamples the cutouts retreived from the GLEAM website into the image
geometry requested by the user. Only four wide-band datasets are included.
The table below gives the frequency range, central frequency and a typical pixel
scale for each of these bands.
<table border>
<tr><th colspan=5> GLEAM Bands In <i>SkyView</i> </th></tr>
<tr><th>Band</th>
<th>f<sub>min</sub> (MHz)</th>
<th>f<sub>max</sub> (MHz)</th>
<th>f<sub>C</sub> (MHz)</tg>
<th>Pixel scale (") </th>
</tr>
<tr> <td> 1 </td><td> 72 </td><td>103 </td><td> 88 </td> <td> 56 </td></tr>
<tr> <td> 2 </td><td>103 </td><td>134 </td><td>118 </td> <td> 44 </td></tr>
<tr> <td> 3 </td><td>138 </td><td>170 </td><td>155 </td> <td> 34 </td></tr>
<tr> <td> 4 </td><td>170 </td><td>231 </td><td>200 </td> <td> 28 </td></tr>
</table>
These data and 20 narrower bands are available through the team website.
<p>
To minimize resampling artifacts, this survey defaults to the Lanczos third order resampler.
SkyView tracks the size and orientation of the beam as given in each of the tiles and includes
the averaged value (i.e., the average of the input images weighted by the output pixels sampled
from each input) in the BMAJ, BMIN, and BPA keywords of any result FITS file. Provenance: Source data extracted as cutouts from <a href="http://gleam-vo.icrar.org/gleam_postage/q/form">GLEAM cutout server</a> in March 2020 with updates in July 2020.. This is a service of NASA HEASARC.
GMRT 150 MHz All-sky Radio Survey: First Alternative Data Release
Short Name:
TGSS
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
The first full release of a survey of the 150 MHz radio sky observed with
the Giant Metrewave Radio Telescope between April 2010 and March 2012 as
part of the TGSS project.
Aimed at producing a reliable compact source survey, the automated data reduction
pipeline efficiently processed more than 2000 hours of observations with minimal
human interaction. Through application of innovative techniques such as image-based
flagging, direction-dependent calibration of ionospheric phase errors, correcting
for systematic offsets in antenna pointing, and improving the primary beam model,
good quality images were created for over 95 percent of the 5336 pointings.
This data release covers 36,900 square degrees (or 3.6 pi steradians) of the
sky between -53 deg and +90 deg DEC, which is 90 percent of the total sky.
The majority of pointing images have a background RMS noise below 5 mJy/beam
with an approximate resolution of 25" x 25" (or 25" x 25" / cos (DEC - 19 deg)
for pointings south of 19 deg DEC).
The associated catalog has 640 thousand radio sources derived from an initial,
high reliability source extraction at the 7 sigma level.
The measured overall astrometric accuracy is better than 2" in RA and DEC,
while the flux density accuracy is estimated at ~10 percent.
Data is stored as 5336 mosaic images (5 deg x 5 deg).
<p>
<i>SkyView</i> uses Lanczos resampling and Sqrt image scaling by default for this
survey. Provenance: TGS ADR Team. This is a service of NASA HEASARC.
This survey comprises the 2 Ms Chandra Deep Field North and 4 Ms Deep Field South ACIS observations.
All observations are co-added into two fields in the north and south. Data are provided in three bands,
the soft 0.5-2 keV band, the hard 2.0-8.0 keV and the full 0.5 to 8 keV band. Provenance: Taken from the Neil Brandt's PSU websites for the the
<a href="https://personal.psu.edu/wnb3/hdf/hdf-chandra.html">north</a>
and
<a href="https://personal.psu.edu/wnb3/cdfs/cdfs-chandra.html">south</a>.. This is a service of NASA HEASARC.
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
<p>
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is
available at 250, 350 and 500 microns (using SPIRE).
<p>
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the <a href="https://hedam.lam.fr/GOODS-Herschel/">Herschel Database in Marseille</a>. Release DR1.. This is a service of NASA HEASARC.
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
<p>
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is
available at 250, 350 and 500 microns (using SPIRE).
<p>
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the <a href="https://hedam.lam.fr/GOODS-Herschel/">Herschel Database in Marseille</a>. Release DR1.. This is a service of NASA HEASARC.
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
<p>
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is
available at 250, 350 and 500 microns (using SPIRE).
<p>
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the <a href="https://hedam.lam.fr/GOODS-Herschel/">Herschel Database in Marseille</a>. Release DR1.. This is a service of NASA HEASARC.
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
<p>
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is
available at 250, 350 and 500 microns (using SPIRE).
<p>
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the <a href="https://hedam.lam.fr/GOODS-Herschel/">Herschel Database in Marseille</a>. Release DR1.. This is a service of NASA HEASARC.
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
<p>
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is
available at 250, 350 and 500 microns (using SPIRE).
<p>
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the <a href="https://hedam.lam.fr/GOODS-Herschel/">Herschel Database in Marseille</a>. Release DR1.. This is a service of NASA HEASARC.
This is a <i>SkyView</i> rendering of the HST ACS data as described in
the <a href="https://archive.stsci.edu/pub/hlsp/goods/v2/h_goods_v2.0_rdm.html">release
document</a>. This comprises four bands of observations of each both the north and south GOODS regions.
<p>
These data are stored in SkyView as a hierarchical image with 7 levels of pixels, each with a factor
of 2 change in scale. Thus the coarsest sampling using pixels 64 times larger than the finest. As we go to
coarser pixels, 4 adjacent pixels forming a square are averaged to create the pixel in the next level. The coarsest pixel
scale that is at least the resolution requested is used.
<p>
The exposure times are given as:
<table>
<tr><th colspan=3> GOODS ACS exposure (s)</th></td></tr>
<tr><th>Band</th><th>North></th><th>South</th>
<tr><td>z850</td><td>24760</td><td>18232</td></tr>
<tr><td>i775</td><td>8530</td><td>7028</td></tr>
<tr><td>V606</td><td>5650</td><td>5450</td></tr>
<tr><td>B435</td><tr>7200</td><td>7200</td></tr>
</table> Provenance: Created by the GOODS team and distributed by MAST. This is a service of NASA HEASARC.
The GOODS NICMOS Survey (GNS) is a 180 orbit Hubble Space Telescope survey
consisting of 60 pointings with the NICMOS-3 near-infrared camera.
Each pointing is centred on a massive galaxy (M<sub>*</sub> > 1011 M<sub>sun</sub>)
in the redshift range 1.7 < z < 3,
selected by their optical-to-infrared colours (Papovich+06,Yan+04,Daddi+07)
from the GOODS (Great Observatories Origins Deep Survey) fields.
<p>
The positions of the 60 GNS pointings were optimised to contain as
many massive galaxies as possible and are partly overlapping,
covering a total area of about 45 arcmin2.
The field of view of the NICMOS-3 camera is 51.2 × 51.2 arcsec with a
resolution of about 0.1 arcsec/pixel.
The PSF has a width of about 0.3 arcsec FWHM.
The limiting magnitude in H band reached at 5σ is HAB = 26.8,
about 2 magnitudes fainter than in available ground based data of the GOODS fields.
[Taken from reference website.] Provenance: University of Nottingham, GNS group.. This is a service of NASA HEASARC.
A combination of VLA measurements in all four configurations
combined to generate a very deep image of the GOODS North region. A total of about 150
hours of VLA time was used. Data are sensitive to about 5 microJanskies in
the central region. A total of 1230 discrete sources where found in the 40'x40' region. Provenance: VLA Observations taken by Morrison et al. as provided
through their <a href="https://www.ifa.hawaii.edu/~morrison/GOODSN/">website</a>.. This is a service of NASA HEASARC.
The Soviet orbital observatory GRANAT was launched in December 1989 and
was operational till November 1998. One of the main instruments
of the observatory was the French-Soviet hard X-ray coded mask telescope SIGMA
(Paul et al.1 1991, Adv.Space Res., 11, 279). It was the first
space telescope that used coded aperture technique for reconstruction of
sky images in hard X-rays (35-1300 keV). The angular
resolution of the telescope was approximately 12' and the accuracy of a source
localization is approximately 2-3'.<p>
SIGMA discovered numerous interesting hard X-ray sources including
GRS 1758-258, which is located
only 40' from bright soft X-ray source GX 5-1. It
detected hard X-ray flux from X-ray burster A1742-294, which is very
near to bright black hole binary 1E1740.7-2942. SIGMA set an upper
limit on the hard X-ray flux of from the central supermassive black hole in
our Galaxy.<p>
During the period 1990-1998 SIGMA observed more that one quarter of the sky
with sensitivity better than 100 mCrab. The Galactic Center region
had the deepest exposure ( approximately 9 million sec), with the
sensitivity to a source discovery (S/N > ~ 5) or approximately
10 mCrab.<p>
A list of all detected sources with references to publications
on them is presented in the paper of Revnivtsev et al. 2004, Astr. Lett. v.6.
In these survey images (40-100 keV) all performed observations are
averaged together. Transient sources that were discovered by
SIGMA may not visible in the averaged image.
<p>
This survey has some features that users should
keep in mind. The SIGMA telescope is a complicated instrument and
is strongly dominated by the accuracy of the background subtraction.
The presence of a very bright source in the field of view of the telescope
sometimes cannot be fully accounted for and as a result of it some 'ghost'
sources can appear. Such features can be seen in the regions near
very bright sources like Crab Nebula, Cyg X-1, Nova Per 1992,
Nova Mus 1991, Nova Oph 1993, and in the Galactic Center region.
In addition to its nominal field of view (~17x17 deg)
located around the optical axis of the telescope, SIGMA had another
window of relatively high transparency of its shield,
approximately 20-30&#176;; apart from the optical axis.
Becuase of this a very bright sources like Cyg X-1 can
cause non zero illumination of the SIGMA
detector if they are located approximately 20-30&#176;; from the optical axis.
The ring-like features caused by this effect, can be seen around Cyg X-1,
and Nova Per 1992.
<p>
The count rate of detected sources (or upper limits)
can be roughly translated into mCrab using the fact that
that Crab nebula gives the count rate approximately 2.8e<sup>-3</sup> cnts/s in the units, provided in 'flux' maps Provenance: High Energy Astrophysics Department,
Space Research Institute, Moscow, Russia; CEA, Centre d'Etudes de
Saclay Orme des Merisiers, France; Centre d'Etude Spatiale
des Rayonnements, Toulouse, France; F&eacute;d&eacute;ration de
Recherche Astroparticule et Cosmologie Universit&eacute; de Paris, France. This is a service of NASA HEASARC.
This survey is a mosaic of data taken at the low frequency T-array near Gauribidanur, India.
The data was distributed in the NRAO Images from the Radio Sky CD ROM.
<p>
The original 287x101 tiles had only 1 pixel overlap. To allow
higher order resampling, the data were retiled into two hemisphere
files of 1726x600 pixels with an overlap of 10 pixels.
<p>
The southernmost tiles were only 287x100 pixels. We assumed
that bottom row of these tiles (as compared with the others)
was truncated. Provenance: . This is a service of NASA HEASARC.
The full-sky H-alpha map (6' FWHM resolution) is a composite of the
Virginia Tech Spectral line Survey (VTSS) in the north and the
Southern H-Alpha Sky Survey Atlas (SHASSA) in the south. Stellar
artifacts and bleed trails have been carefully removed from these maps.
The Wisconsin H-Alpha Mapper (WHAM) survey provides a stable zero-point
over 3/4 of the sky on a one degree scale. This composite map can be used
to provide limits on thermal bremsstrahlung (free-free emission) from
ionized gas known to contaminate microwave-background data. The map
(in Rayleighs; 1R=10<sup>6</sup>/4pi photons/cm<sup>2</sup>/s/sr), an error map, and a
bitmask are provided in 8640x4320 Cartesian projections as well as
HEALPIX (Nside 256, 512, and 1024) projections on the
<a href="https://faun.rc.fas.harvard.edu/dfink/skymaps/halpha/"> H-Alpha Full-Sky Map website</a>. Provenance: . This is a service of NASA HEASARC.
These data were generated at the HEASARC in 1994. Certain
gaps and streaks in the image have been fixed by interpolating
over the the gap. Typically these gaps are no more than a pixel
or two wide. A brief description of the satellite and the
data analysis follows. The map used in <i> SkyView </i>
is the map designated <tt> 322_15_tot_ecl_samp.img</tt> in the
<a href=ftp://legacy.gsfc.nasa.gov/heao1/data/a2/maps/heasarc_med_hed>
HEASARC FTP area</a>. Many other maps are available. These differ
in epoch, resolution, energy band,
coordinate system and projection, and sampling methods.
Details are given in the README file in the archive.
<p>
See Allen, Jahoda, and Whitlock (1994) for full details about the
available maps, their processing, and methods for converting the
map intensities into familiar physical units. Provenance: NASA, HEASARC. This is a service of NASA HEASARC.
This survey is a mosaic of data taken at Jodrell Bank, Effelsberg and Parkes
telescopes. The data was distributed in the NRAO <i>Images from the
Radio Sky</i> CD ROM. Provenance: Max Planck Institute for Radio Astronomy, generated by Glyn Haslam. This is a service of NASA HEASARC.
The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at
prime focus of the 3.6m CFH telescope during the period 2003-2008. The Deep survey concerns 4 patchsof 1 square-degree. All will be observed in u,g,r,i and z, with very lon gexposure time<p>
This survey description was generated automatically from the <a href='https://alasky.u-strasbg.fr/CFHTLS-T0007b/Deep/UALLSKY/properties'>HiPS property file</a> Provenance: CFHT<br> HiPS generated by CDS. This is a service of NASA HEASARC.
The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at
prime focus of the 3.6m CFH telescope during the period 2003-2008. The WIDE survey concerns 4 patchs, 3 of about 7x7 square-degrees each and 1 of about 4x4 square-degrees. All will be observed in
u,g,r,i and z, with about 1 hr exposure time per filter<p> This survey description was generated automatically from the <a href='https://alasky.u-strasbg.fr/CFHTLS-T0007b/Wide/UALLSKY/properties'>HiPS property file</a> Provenance: CFHT<br> HiPS generated by CDS. This is a service of NASA HEASARC.
This is the TESS 2yr sky map. The Transiting Exoplanet Survey Satellite (TESS) is the next
step in the search for planets outside of our solar system, including those that could support life.
The mission will find exoplanets that periodically block part of the light from their host stars,
events called transits. TESS will survey 200,000 of the brightest stars near the sun to search for
transiting exoplanets. TESS aims for 50 ppm photometric precision on stars with TESS magnitude 9-15.
TESS launched on April 18, 2018, aboard a SpaceX Falcon 9 rocket. This dataset
is made of observations made during the first 2 years of the mission. See
<a href="https://ui.adsabs.harvard.edu/abs/2015JATIS...1a4003R/abstract">
https://ui.adsabs.harvard.edu/abs/2015JATIS...1a4003R/abstract</a>
for more information on the mission.
Funding for the TESS mission is provided by NASA's Science Mission directorate. Provenance: TESS Data were obtained by using the code provided by Ethan Kruse at https://github.com/ethankruse/tess_fullsky. HiPS generated by CDS. This is a service of NASA HEASARC.
HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band H
Short Name:
UltraVista-H
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
UltraVISTA is an Ultra Deep, near-infrared survey with the new VISTA surveys telescope of the European Southern Observatory (ESO). Over the course of 5 years, UltraVISTA will
repeatedly image the COSMOS field in 5 bands covering a 1.5deg^2 field.\n \nESO acknowledgment: Data products from observations made with ESO Telescopes at the La Silla Paranal Observatories under
ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.<p> This survey description was generated
automatically from the <a href='https://alasky.u-strasbg.fr/VISTA/UltraVista/H/properties'>HiPS property file</a> Provenance: Origin unknown. This is a service of NASA HEASARC.
The IRIS data is a reprocessing of the IRAS data set
and has the same geometry as the IRAS Sky Survey Atlas (ISSA,
labeled as IRAS nnn micron in <i>SkyView</i>) surveys.
This new generation of IRAS images, called IRIS,
benefits from a better zodiacal light subtraction,
from a calibration and zero level compatible with DIRBE,
and from a better destriping.
At 100 micron the IRIS product is also a significant improvement
from the Schlegel et al. (1998) maps.
IRIS keeps the full ISSA resolution,
it includes well calibrated point sources and the
diffuse emission calibration at scales smaller
than 1 degree was corrected for the variation of
the IRAS detector responsivity with scale and brightness.
The uncertainty on the IRIS calibration and zero level
are dominated by the uncertainty on the DIRBE calibration
and on the accuracy of the zodiacal light model.
<p>
More information about the IRIS dataset is available at
<a href="https://www.cita.utoronto.ca/~mamd/IRIS"> the IRIS website</a>
whence most of the preceding description came. Provenance: Original IRAS data: NASA/JPL IPAC, <br>
IRIS Reprocessing: Canadian Institute for Theoretical Astrophysics/Institut
d'Astrophysique Spatiale<br>
See the
<a href="https://www.cita.utoronto.ca/~mamd/IRIS"> IRIS website</a>.. This is a service of NASA HEASARC.
The INTEGRAL observatory (Winkler et al. 2003, A&A, 411, L1) was
launched in October 2002. The spectrograph SPI (Vedrenne et al. 2003,
A&A, 411, L63) consists of 19 Germanium detectors and is capable of
imaging in the 20 - 8000 keV band because of a coded mask. Part of the
core program of the INTEGRAL mission is a study of the Galactic Centre,
the Galactic Centre Deep Exposure (GCDE).<p>
The SPI significance map is based on the public GCDE data and
uses data in the 20 - 40 keV energy range. The analysis of the data was
done using the SPIROS software (Skinner & Connell 2003, A&A, 411, L123).
This software uses the 'Iterative Removal of Sources' technique in order
to find the most significant sources. In the output significance map the
sources found in this process are put on top of the residual map as
points with a FWHM of 1 degree.
<p>
Current data respresent the combination of all public observations as of
September 1, 2004. Provenance: INTEGRAL Science Data Center, Geneva, Switzerland. This is a service of NASA HEASARC.
The IRAS data include all data distributed as part of the IRAS Sky Survey Atlas. Data from the four IRAS bands are shown as individual surveys in SkyView. Users should be aware that IPAC does not
encourage the use of data near the ecliptic plane as they feel that contribution from local cirrus emission is significant.
<p>
The data are distributed in sets of 430 maps. Each map covers approximately 12.5x12.5 degrees, and the map centers are offset by 5 degrees so that there is a 2.5 degree overlap.
IPAC has processed to a uniform standard so that excellent mosaics of the maps can be made. Users should be cautious of data in saturated regions. Known problems in the analysis mean that data
values are unlikely to be correct. Note that IPAC has optimized the processing of these data for features of 5' or more although the resolution of the data is closer to the 1.5' pixel size.
<p>
There are occasional pixels in the IRAS maps which are given as NULL values. Unless these are explicitly trapped by user software, these data will appear as large negative values. SkyView ignores
these pixels when determining the color scale to display an image.
<p>
Essentially the entire sky is covered by the survey. However there are a few regions not surveyed and the data values in these regions are suspect. These are given to users as delivered from IPAC. Provenance: NASA IPAC/Jet Propulsion Laboratory. This is a service of NASA HEASARC.
LABOCA Extended Chandra Deep Field South Submillimetre Survey
Short Name:
CDFS LESS
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
The LABOCA Extended Chandra Deep Field South (ECDFS) Submillimetre Survey (LESS)
is a public legacy survey of the ECDFS at 870 μm using the LABOCA camera
(Siringo et al. 2009) on the APEX telescope.
<p>
The LABOCA data presented here were obtained between 2007 May and 2008 November
in excellent conditions using time from both ESO and Max Planck allocations.
The mapping pattern was designed to uniformly cover the 30'x30' extent of the ECDFS,
centered on 03:32:29.0, -27:48:47.0 (J2000).
The project used a total of 310 hrs of observations to achieve a beam-smoothed noise of
1.2 mJy/beam over 900 sq. arcmin (and <1.6mJy/beam over 1260 sq. arcmin).
The flux calibration of the map came from observations of Mars, Uranus and Neptune
(as well as secondary calibrators) and is accurate to within 8.5%. Provenance: Data downloaded from ESO archive. This is a service of NASA HEASARC.
This all sky mosaic was created by Axel Mellinger and is used
in <i>SkyView</i> with his permission. A fuller description
is available at the
<a href="https://www.milkywaysky.com/">survey website</a>.
<p>
Between October 2007 and August 2009 a digital all-sky mosaic
was assembled from more than 3000 individual CCD frames.
Using an SBIG STL-11000 camera, 70 fields (each covering 40x27 degrees)
were imaged from dark-sky locations in South Africa, Texas and Michigan.
In order to increase the dynamic range beyond the 16 bits of the camera's
analog-to-digital converter (of which approximately 12 bits provide data
above the noise leve) three different exposure times (240s, 15s and 0.5 s)
were used. Five frames were taken for each exposure time and
filter setting. The frames were photometrically calibrated using
standard catalog stars and sky background data
from the Pioneer 10 and 11 space probes. the panorama has an
image scale of 36"/pixel and a limiting magnitude of approximately 14. The
survey has an 18 bit dynamic range.
<p>
The processing of these data used a custom data pipeline built using
IRAF, Source Extractor and SWarp.
<p>
The data used here were converted to three independent RGB color planes
of 8 bits each and provided to SkyView as a single 36000x18000x3 Cartesian
projection cube.
To allow users to efficiently sample data in a region of the sky,
this cube was broken up into 2100x2100 pixel regions with a 50 pixel overlap
between adjacent images. Tiles at the poles were 2100x2050.
<p>
In <i>SkyView</i> each color plane comprises a survey. The individual planes may be
sampled as surveys independently as Mellinger-R, Mellinger-G and Mellinger-B.
The color mosaics can be regenerated by creating an RGB image of all three
surveys. Since <i>SkyView</i> may stretch the intensity values within
each color, linear scaling and a minimum of 0 and maximum of 255 should
be specified to keep the original intensity scalings.
<p>
The full spatial resolution data is used for images of less than
30 degrees on a side. If a user requests a larger region, data are sampled
from a lower resolution 3600x1800x3 data cube. Please contact the survey
author if you need to use the higher resolution data for larger regions.
The Mellinger survey is only available in
<i>SkyView</i> through the website. SkyView-in-a-Jar cannot access
the underlying data. Provenance: Axel Mellinger. This is a service of NASA HEASARC.
The 4850MHz data is a
combination of data from three different surveys: Parkes-MIT-NRAO (PMN)
Southern (-88&#176;; to -37&#176;; declination) and tropical surveys (-29&#176;;
to -9&#176;; declination, and (86+87) Green Bank survey (0&#176;; to +75&#176;;
declination). The data contains gaps between -27&#176;; to -39&#176;;,
-9&#176;; to 0&#176;;, and
+77&#176;; to +90&#176;; declination.
The 4850MHz survey data were obtained by tape from J.J. Condon and are comprised
of 576 images and are used by permission. Full information pertaining to
these surveys are found in the references.<P> Provenance: NRAO, generated by J.J. Condon, J.J. Broderick and G.A. Seielstad, Douglas, K., and Gregory, P.C.. This is a service of NASA HEASARC.
<P>
The native projection of these data is described as a high-order polynomial
distortion of a gnomonic projection using the same terms as the DSS. Provenance: Data taken by ROE, AAO, and CalTech, Compression
and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
The NEAT/SkyMorph survey provides access to the archives
of the Near Earth Asteroid Tracking (NEAT) project. NEAT is
designed to look for potentially hazardous asteroids, i.e., those
whose orbits cross the Earth's. Over 200,000 images are available
in the NEAT archive.
<a href=https://skyview.gsfc.nasa.gov/skymorph/skymorph.html>SkyMorph</a>
provides a Web interface to the NEAT
images and allows users to select all images in which a given fixed
or moving object is found.
<p>
Unlike most <i>SkyView</i> surveys, the NEAT data are extremely irregular in their
spatial distribution. <i>SkyView</i>'s algorithms for mosaicking images
together to form large images are not adequate for the NEAT data, so
mosaicking is surpressed. Only data within a single NEAT image will
be displayed. The system attempts to find the most recent image within
which has a offset in both RA and Dec of less than 0.8 degrees. If no
such image is found, then an image with the minimum offset is returned, or
the search may fail altogether if there are no nearby plates.
The NEAT telescope uses an array of 4 CCDs. The backgrounds of the
CCDs may differ significantly.
<p>
The NEAT survey covers approximately 30% of the sky. Extreme southern
and low-Galactic latitude regions are unsurveyed. Coverage is otherwise
particularly dense in the ecliptic plane.
<p>
NEAT data consists primarily of groups of three images taken with separations
of 20 minutes and almost identical positions. <i> SkyView </i> will normally
return the last of a 'triplet'. The SkyMorph site can be used to display
an overlay of triplets to look for targets which moved during the interval
between images.
<p>
A catalog of objects detected in the NEAT/SkyMorph pages is accessible
through the SkyMorph pages. 'Light-curves' from all images during which
an object was in the NEAT field of view can also be generated.
<P>
The NEAT data values are in arbitrary density units. To enhance the display
data are transformed such that all pixels below the median values
are scaled linearly to values 0-20, while all pixels above the median
are shifted (but not scaled) to values greater than 20.
Nine Year INTEGRAL IBIS 17\-35 keV Galactic Plane Survey: Exposure
Short Name:
INTGAL1735E
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
This survey combines 9 years of INTEGRAL IBIS observations from December 2002
through January 2011 into a single Galactic Plane image. A total of 135 megaseconds
of exposure is included in the observations used. Survey data is generated for
the Galactic plane in the region |b| <= 17.5. The original flux data has been convolved with
5' seeing kernel. To minimize loss of resolution in transformations, the Lanczos sampler is
suggested as the default, but may be overriden by the user.
Both the preconvolved and standard
convolved maps are available at the <a href="https://web.archive.org/web/20170620112312/https://hea.iki.rssi.ru/integral/nine-years-galactic-survey/index.php">Website</a>.
<p>
The exposure and sensitivity vary considerably over the coverage region, but 90% of the field
has a limiting sensitivity better than 2.2 x 10<sup>-11</sup>ergs s<sup>-1</sup>cm<sup>-2</sup>
or about 1.56 mCrab. Further details of the survey construction are given in the reference.
<p>
The flux and significance maps use the PSF convolved maps from the survey. The flux maps are in millicrab units.
Exposure maps (with exposures in seconds) were from the exposure extension in the MAPDLD files and
give the dead-time corrected exposure in seconds.
<p>
Links to the exposure and significance maps corresponding to the requested region will
be given in the Web output. These maps can be generated directly in the CLI interface.
For each waveband the flux, significance and exposure maps are available with just the
end of the survey names distinguishing them (e.g., INT Gal 17-35 [Flux|Sig|Exp] or
INTGal1735[F|S|E]) Provenance: <a href="https://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1205.3941">Krivonos et al., 2012</a><br>
Based on observations with INTEGRAL, an ESA project with instruments and
science data centre funded by ESA member states (especially the PI countries:
Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation
of Russia and the USA.. This is a service of NASA HEASARC.
<i> SkyView </i>
has copied the NVSS intensity data from the NRAO FTP site. The full
NVSS survey data includes information on other Stokes parameters.
<p>
Observations for the 1.4 GHz NRAO VLA Sky Survey (NVSS) began in 1993
September and should cover the sky north of -40 deg declination (82%
of the celestial sphere) before the end of 1996. The principal data
products are:
<ol>
<li> A set of 2326 continuum map "cubes," each covering 4 deg X 4 deg
with three planes containing Stokes I, Q, and U images. These maps
were made with a relatively large restoring beam (45 arcsec FWHM) to
yield the high surface-brightness sensitivity needed for completeness
and photometric accuracy. Their rms brightness fluctuations are
about 0.45 mJy/beam = 0.14 K (Stokes I) and 0.29 mJy/beam = 0.09 K
(Stokes Q and U). The rms uncertainties in right ascension and
declination vary from 0.3 arcsec for strong (S > 30 mJy) point
sources to 5 arcsec for the faintest (S = 2.5 mJy) detectable
sources.
<li> Lists of discrete sources.
</ol>
The NVSS is being made as a service to the astronomical community, and
the data products are being released as soon as they are produced and
verified.
<P>
The NVSS survey is included on the <b>SkyView High Resolution Radio
Coverage </b><a href="https://skyview.gsfc.nasa.gov/images/high_res_radio.jpg"> map</a>. This map shows
coverage on an Aitoff projection of the sky in equatorial coordinates.
<p> Provenance: National Radio Astronomy Observatory. The NVSS
project includes J. J. Condon, W. D. Cotton, E. W. Greisen, Q. F. Yin,
R. A. Perley (NRAO), and J. J. Broderick (VPI).. This is a service of NASA HEASARC.
The Nuclear Spectroscopic Telescope Array (NuSTAR) mission, launched on 2012 June 13, is the first focusing high-energy X-ray telescope in orbit. NuSTAR operates in the band from 3 to 79 keV, extending the sensitivity of focusing instruments far beyond the ~10 keV high-energy cutoff achieved by all previous X-ray satellites. The inherently low background associated with concentrating the X-ray light enables NuSTAR to probe the hard X-ray sky with a more than 100-fold improvement in sensitivity over the collimated or coded mask instruments that have operated in this bandpass. The observatory was placed into a 600-km altitude, 6 degree inclination circular orbit, and consists of two co-aligned grazing-incidence X-ray telescopes pointed at celestial targets by a three-axis stabilized spacecraft. NuSTAR has completed its two-year primary science mission, and, with an expected orbit lifetime of more than 10 years, the opportunity for proposing observations as part of the General Observer (GO) program is now available, with observations beginning in 2015. Using its unprecedented combination of sensitivity and spatial and spectral resolution, NuSTAR offers opportunities for a broad range of science investigations, ranging from probing cosmic ray origins to studying the extreme physics around compact objects to mapping micro-flares on the surface of the Sun. NuSTAR also responds to targets of opportunity including supernovae and gamma-ray bursts. This table contains a list of (a) unobserved targets that are planned or have been accepted for observation by NuSTAR in the future and (b) NuSTAR observations which have been processed and successfully validated by the NuSTAR Science Operation Center. The data from these observations may or may not be public and the user should check the value of the public_date parameter to determine the status of a specified data set. Only those ObsIDs which have a public_date in the past will have data publicly available. Observations with a public_date parameter value which is either blank or a date in the future have been ingested into the HEASARC archive but will remain encrypted until their public date. Entries with the status field set to 'accepted' are targets approved for scheduling, and the planned exposure time given in the exposure_a (and exposure_b) parameter will have a negative value for those targets. This database table is based on information supplied by the NuSTAR Project at Caltech. It is automatically updated on a regular basis. This is a service provided by NASA HEASARC .
This survey comprises the compressed digitization of the Southern Sky
Survey and the Palomar Sky Survey E plates as distributed on CD ROM
by the Space Telescope Science Institute. Coverage of the entire
sky is included.
This survey consists of the digititized Southern Sky Survey conducted
at the UK Southern Schmidt Survey Group by the Royal Observatory, Edinburgh
(prior to 1988) and the Anglo-Australian Observatory (since 1988)
Additional plates covering regions with bright objects are also
included.
The plates were digitized at the Space Telescope Science Institute
and compressed using algorithms developed by R.White. These
data are distributed on a set of 101 CD-ROMs.
<P>
The following data are included:
<DL>
<DT>Southern hemisphere
<DD>
SERC Southern Sky Survey and the SERC J Equatorial extension.
These are typically deep, 3600s, IIIa-J exposures with a GG395 filter.
Also included are 94 short (1200s) V exposures typically at Galactic
latitudes below 15&#176;;. Special exposures are included in
the regions of the Magellenic clouds.
<DT>Northern hemisphere
<dd> The northern hemisphere is covered by 644 plates from the POSS E
survey. A special exposure of the M31 region that is distributed on
the CD ROMs is not used in <i> SkyView </i>.
</DL> Provenance: Data taken by ROE and AAO, CalTech, Compression
and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
Planck is ESA's third generation space based cosmic microwave background
experiment, operating at nine frequencies between 30 and 857 GHz and was
launched May 2009. Planck provides all-sky survey data at all nine
frequencies with higher resolution at the 6 higher frequencies.
It provides substantially higher resolution and sensitivity
than WMAP. Planck orbits in the L2 Lagrange point.
These data come from Release 1 of the Planck mission.
<p>
The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard
projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees.
The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the
pixels are treated properly. The special HealPixImage class is used so that SkyView can use
the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but
translates the pixels from that image to the nested HEALPix structure that is used
by the HEALPix data. Users of the SkyView Jar will be able to access this survey through the web
but performance may be poor since the FITS files are 150 to 600 MB in size and must be completely
read in. SkyView will not automatically
cache these files on the user machine as is done for non-HEALPix surveys.
</p>
Data from the frequencies of 100 GHz or higher are stored
in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with
half that resolution, approximately 3.4'.
Planck is ESA's third generation space based cosmic microwave background
experiment, operating at nine frequencies between 30 and 857 GHz and was
launched May 2009. Planck provides all-sky survey data at all nine
frequencies with higher resolution at the 6 higher frequencies.
It provides substantially higher resolution and sensitivity
than WMAP. Planck orbits in the L2 Lagrange point.
<p>
These data come from the legacy Release 3 of the Planck
mission.
<p>
These products include polarization information available to
visualize in several ways. The data contain Stokes parameters I, Q,
and U, and in addition to these, it is possible to visualize the
polarized intensity PI=sqrt(Q^2+U^2) and the polarization angle
PA=1/2atan(U/Q). Note that at their native resolution of a few
arcmin (depending on the frequency), these polarization data will
appear very noisy. In order to visualize the polarization
information, it is highly recommended that the data be resampled
with the "Clip (intensive)" sampler and the result smoothed. That
sampler will average all the data points within a given output pixel
rather than the more common nearest neighbor. It will do this averaging before
computing either PI or PA to reduce the effects of the noise. This
sampler is set as the default for this survey. If the output pixel
resolution is not significantly larger than the resolution, a smoothing of the
output pixels will also be necessary.
<p>
Note also that Q and U are defined relative to a given co-ordinate
system, in this case Galactic, and following the
CMB convention (not the IAU); see
https://lambda.gsfc.nasa.gov/product/about/pol_convention.cfm. This
means that they will appear to vary rapidly near the pole of that coordinate
system. The PI and PA will be computed correctly for any position
on the sky.
<p>
The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard
projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees.
The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the
pixels are treated properly. The special HealPixImage class is used so that SkyView can use
the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but
translates the pixels from that image to the nested HEALPix structure that is used
by the HEALPix data. Users of the SkyView Jar will be able to access this survey through the web
but performance may be poor since the FITS files are 150 to 600 MB in size and must be completely
read in. SkyView will not automatically
cache these files on the user machine as is done for non-HEALPix surveys.
</p>
Data from the frequencies of 100 GHz or higher are stored
in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with
half that resolution, approximately 3.4'. Provenance: Data split using skyview.survey.HealPixSplitter from the PR3 distriuted by the Planck Science team.. This is a service of NASA HEASARC.
The ROSAT PSPC surveys were generated by <i> SkyView </i> as
mosaics from publically available PSPC observations.
The surveys include
all data available through March 1, 1997. This includes the vast majority
of ROSAT PSPC observations. Filter observations and observations taken
during the verification phase in 1991 were not included in either
set. The details of the generation of the surveys are discussed
in a
<a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> companion document</a>.
Basically the counts and
exposure from all observations were added and then an intensity
map was generated as the ratio of the two.
<p>
The smaller
cut-offs allow users to distinguish point sources in fields where
a bright source may have been towards the edge of one observation
and near the center of another. In these cases the source appears
fuzzy due to the poor resolution of ROSAT near the edge of the field
of view. This comes at the cost of a substantial reduction in
the fraction of the sky covered. Counts and exposure maps are
included for users who may need this information (<i>e.g.</i>, to do
statistical analysis).
<p>
The global organization of the surveys is similar
to the IRAS survey. Each map covers an area of 2.5&#176;;x2.5&#176;; with a
minimum overlap of 0.25&#176;;. To cover the entire sky would require over
10,000 maps. However due to lack of coverage only approximately 4000-6000 maps
are actually populated. Users asking for reqions where there is no ROSAT
coverage may get a blank region returned.
<p>
Detailed information regarding the creation of the ROSAT suveys
can be found in the <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html">
ROSAT PSPC Generation Document</a>. Provenance: Observational data from NASA Goddard Space
Flight Center, mosaicking of images done by <i>SkyView</i>.. This is a service of NASA HEASARC.
The ROSAT PSPC surveys were generated by <i> SkyView </i> as
mosaics from publically available PSPC observations.
The surveys include
all data available through March 1, 1997. This includes the vast majority
of ROSAT PSPC observations. Filter observations and observations taken
during the verification phase in 1991 were not included in either
set. The details of the generation of the surveys are discussed
in a
<a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> companion document</a>.
Basically the counts and
exposure from all observations were added and then an intensity
map was generated as the ratio of the two.
<p>
The smaller
cut-offs allow users to distinguish point sources in fields where
a bright source may have been towards the edge of one observation
and near the center of another. In these cases the source appears
fuzzy due to the poor resolution of ROSAT near the edge of the field
of view. This comes at the cost of a substantial reduction in
the fraction of the sky covered. Counts and exposure maps are
included for users who may need this information (<i>e.g.</i>, to do
statistical analysis).
<p>
The global organization of the surveys is similar
to the IRAS survey. Each map covers an area of 2.5&#176;;x2.5&#176;; with a
minimum overlap of 0.25&#176;;. To cover the entire sky would require over
10,000 maps. However due to lack of coverage only approximately 4000-6000 maps
are actually populated. Users asking for reqions where there is no ROSAT
coverage may get a blank region returned.
<p>
Detailed information regarding the creation of the ROSAT suveys
can be found in the <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html">
ROSAT PSPC Generation Document</a>. Provenance: Observational data from NASA Goddard Space
Flight Center, mosaicking of images done by <i>SkyView</i>.. This is a service of NASA HEASARC.
The ROSAT PSPC surveys were generated by <i> SkyView </i> as
mosaics from publically available PSPC observations.
The surveys include
all data available through March 1, 1997. This includes the vast majority
of ROSAT PSPC observations. Filter observations and observations taken
during the verification phase in 1991 were not included in either
set. The details of the generation of the surveys are discussed
in a
<a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> companion document</a>.
Basically the counts and
exposure from all observations were added and then an intensity
map was generated as the ratio of the two.
<p>
The smaller
cut-offs allow users to distinguish point sources in fields where
a bright source may have been towards the edge of one observation
and near the center of another. In these cases the source appears
fuzzy due to the poor resolution of ROSAT near the edge of the field
of view. This comes at the cost of a substantial reduction in
the fraction of the sky covered. Counts and exposure maps are
included for users who may need this information (<i>e.g.</i>, to do
statistical analysis).
<p>
The global organization of the surveys is similar
to the IRAS survey. Each map covers an area of 2.5&#176;;x2.5&#176;; with a
minimum overlap of 0.25&#176;;. To cover the entire sky would require over
10,000 maps. However due to lack of coverage only approximately 4000-6000 maps
are actually populated. Users asking for reqions where there is no ROSAT
coverage may get a blank region returned.
<p>
Detailed information regarding the creation of the ROSAT suveys
can be found in the <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html">
ROSAT PSPC Generation Document</a>. Provenance: Observational data from NASA Goddard Space
Flight Center, mosaicking of images done by <i>SkyView</i>.. This is a service of NASA HEASARC.
This database table contains the list German ROSAT All-Sky Survey observations which were obtained during the ROSAT All-Sky Survey phase (1990 July 30 to 1991 Jan 25) and which have become available to the public. These data were obtained in scanning mode and therefore an individual dataset covers a much larger area of the sky than do pointed moded observations. In addition all these data were obtained with PSPC-C, while all pointed mode observations after the end of the All-Sky Survey were obtained with PSPC-B. For each observation listed in this database table, the instrument used, processing site, and coordinates of the field center are given, as well as the ROSAT observation request number (ROR), actual exposure time, date the observation took place, and more. For details about the ROSAT instruments, consult the ROSAT Mission Description (NASA Research Announcement for ROSAT, Appendix F and its addendum) and the ROSAT GSFC GOF website at <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rosgof.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rosgof.html</a> for more information. For more information about the ROSAT All Sky Survey, see the ROSAT All Sky Survey page at <a href="http://www.xray.mpe.mpg.de/cgi-bin/rosat/rosat-survey">http://www.xray.mpe.mpg.de/cgi-bin/rosat/rosat-survey</a>. This database table was created at the HEASARC in March 2002, based on information provided by Max-Planck-Institut fuer extraterrestrische Physik at <a href="http://wave.xray.mpe.mpg.de/">http://wave.xray.mpe.mpg.de/</a>. This is a service provided by NASA HEASARC .
These maps present maps of
ROSAT soft X-ray all-sky survey as presented in Snowden et al, ApJ 485, 125 (1997).
The maps cover approximately 98% of the sky. These maps have had all point sources
removed
These surveys supercede the RASS0.25, RASS0.75 and RASS1.5 Kev surveys
previously provided. Those surveys may still be invoked in SkyView using
batch and jar tools but are not accessible on the Web page.
<p>
The seven maps correspond to ranges in the pulse height analysis of the photons
detected. Since the energy resolution of the PSPC is poor, there is consider
overlap between adjacent bands.
<p>
The energy range for the bands corresponds to:
<table><tr><th>Band</th><th>Energy range (keV)</th></tr>
<tr><td>Band 1</td><td>0.11 - 0.284</td><tr>
<tr><td>Band 2</td><td>0.14 - 0.284</td><tr>
<tr><td>Band 3</td><td>0.2 - 0.83</td></tr>
<tr><td>Band 4</td><td>0.44 - 1.01</td><tr>
<tr><td>Band 5</td><td>0.56 - 1.21</td><tr>
<tr><td>Band 6</td><td>0.73 - 1.56</td><tr>
<tr><td>Band 7</td><td>1.05 - 2.04</td><tr>
</table>
Note the substantial overlap between bands. Each photon detected is assigned to
a band based on the pulse height analysis for that photon, but the energy resolution
of the detectors is relatively poor. Also note that Band 3 was not
included in the reference paper due to poor statistics and background modeling.
<p>
SkyView has several other sets of surveys derived from ROSAT data
with substantially higher resolution and which include point sources.
The RASS surveys are derived from the RASS all sky survey. These include count
and intensity maps. The PSPC maps are dervived from the PSPC pointed observations
which were combined by SkyView. The HRI survey is derived from a similar mosaicking
of all HRI observations. Provenance: Max Planck Institute for Exterrestrial Physics (Garching FRG). This is a service of NASA HEASARC.
The ROSAT All-Sky X-ray Survey was obtained during 1990/1991 using the
ROSAT Position Sensitive Proportional Counter (PSPC) in combination with
the ROSAT X-ray Telescope (XRT). More than 60,000 X-ray sources
were detected during this time.
<p>
SkyView has multiple surveys derived from the RASS data. The surveys whose
RASS are counts and exposure maps from the survey. Previously
The RASSBCK maps have had the point sources removed to show the diffuse X-ray background
and are presended at lower resolution.
<p>
The full-resolution RASS surveys
data are organized in 1378 fields each
6.4&#176;; x 6.4&#176;; covering the whole sky. Neighboring fields
overlap by at least 0.23&#176;;.<p>
Three bands are available through <i>SkyView</i>
<UL>
<LI> broad band (0.1-2.4 keV)
<LI> hard band (0.5-2.0 keV)
<LI> soft band (0.1-0.4 keV)
</ul>
Data was dowloaded from the
<a href="https://www.xray.mpe.mpg.de/rosat/survey/rass-3/main/help.html#ftp">MPE FTP site</a>.
<p>
The intensity maps are created from the exposure maps using the single exposure map available which
is appropriate for the broad
band images, so the intensities of the hard and soft bands are only approximate. Provenance: Max Planck Institute for Exterrestrial Physics (Garching FRG). This is a service of NASA HEASARC.
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 .
ROSAT Complete Results Archive Sources for the HRI
Short Name:
ROSAT/HRI
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
The ROSHRITOTAL data table contains a list of sources detected by the Standard Analysis Software System (SASS) in reprocessed, public HRI datasets. In addition to the parameters returned by SASS (like position, count rate, signal-to-noise, etc.) each source in the table has associated with it a set of source and sequence "flags." These flags are provided by the ROSAT data centers in the US, Germany and the UK to help the user of the ROSHRITOTAL database table quickly judge the reliability of a given source. The ROSHRITOTAL database table is a superset of the ROSHRI database table. The ROSHRI table excludes sources that meet the following parameter criteria: false_det = 'T' or deferred = 'T' or not_checked = 'T' or un_unique ='T'. See the documentation below for descriptions of these parameters. These data have been screened by ROSAT data centers in the US, Germany, and the UK as a step in the production of the ROSAT Results Archive. The RRA contains extracted source and associated products with an indication of reliability for the primary parameters. This database table was last updated in August 2001. More information about the ROSAT Results Archive for HRI sources can be obtained at the following web pages: <pre> <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html</a> <a href="http://hea-www.harvard.edu/rosat/rra.html">http://hea-www.harvard.edu/rosat/rra.html</a> <a href="http://www.aip.de/groups/xray/rosat/rra.html">http://www.aip.de/groups/xray/rosat/rra.html</a> <a href="http://ledas-www.star.le.ac.uk/rra">http://ledas-www.star.le.ac.uk/rra</a> </pre> This is a service provided by NASA HEASARC .
ROSAT High Resolution Image Pointed Observations Mosaic: Intensity
Short Name:
HRI
Date:
10 May 2024
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 ROSHRI data table contains a list of sources detected by the Standard Analysis Software System (SASS) in reprocessed, public HRI datasets. In addition to the parameters returned by SASS (like position, count rate, signal-to-noise, etc.) each source in the table has associated with it a set of source and sequence "flags." These flags are provided by the ROSAT data centers in the US, Germany and the UK to help the user of the ROSHRI database table quickly judge the reliability of a given source. The ROSHRI table excludes sources that meet the following parameter criteria: false_det = 'T' or deferred = 'T' or not_checked = 'T' or un_unique ='T'. See the documentation below for descriptions of these parameters. These data have been screened by ROSAT data centers in the US, Germany, and the UK as a step in the production of the ROSAT Results Archive. The RRA contains extracted source and associated products with an indication of reliability for the primary parameters. This database table was last updated in August 2001. More information about the ROSAT Results Archive for HRI sources can be obtained at the following web pages: <pre> <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html</a> <a href="http://hea-www.harvard.edu/rosat/rra.html">http://hea-www.harvard.edu/rosat/rra.html</a> <a href="http://www.aip.de/groups/xray/rosat/rra.html">http://www.aip.de/groups/xray/rosat/rra.html</a> <a href="http://ledas-www.star.le.ac.uk/rra">http://ledas-www.star.le.ac.uk/rra</a> </pre> This is a service provided by NASA HEASARC .
The ROSPSPC database table contains a list of sources detected by the Standard Analysis Software System (SASS) in public, unfiltered, pointed PSPC datasets. In addition to the parameters returned by SASS (like position, count rate, likelihood, etc.) each source in the table has associated with it a set of source and sequence "flags." These flags are provided by the ROSAT data centers in the US, Germany and the UK to help the user of the ROSPSPC database table quickly judge the reliability of a given source. The ROSPSPC table excludes sources that meet the following parameter criteria: false_det = 'T' or deferred = 'T' or not_checked = 'T'. See the documentation below for descriptions of these parameters. The catalog consists of all primary source parameters from the automated detection algorithm employed by the SASS. In addition each observation has been quality checked, both by automatic algorithms and by detailed visual inspection. The results of this quality checking are contained as a set of logical-value flags for a set of principal source parameters. If a source parameter is suspect, the associated flag is set to "TRUE"; parameters with no obvious problems maintain the default, "FALSE", value. This database table was last updated in August 2001. More information about the ROSAT Results Archive for PSPC sources can be obtained at the following web pages: <pre> <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html</a> <a href="http://hea-www.harvard.edu/rosat/rra.html">http://hea-www.harvard.edu/rosat/rra.html</a> <a href="http://www.aip.de/groups/xray/rosat/rra.html">http://www.aip.de/groups/xray/rosat/rra.html</a> <a href="http://ledas-www.star.le.ac.uk/rra">http://ledas-www.star.le.ac.uk/rra</a> </pre> 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 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 Sloan Digital Sky Survey is the deepest large scale survey of the
sky currently available. SkyView dynamically queries the SDSS archive
(currently release DR9) to retrieve information and resample it into the user
requested frame. Further information on the SDSS and many additional services
are available at the <a href="https://www.sdss.org">SDSS website</a>. Provenance: Sloan Digital Sky Survey Team. This is a service of NASA HEASARC.
The Sloan Digital Sky Survey is the deepest large scale survey of the
sky currently available. SkyView dynamically queries the SDSS archive
to retrieve information and resample it into the user
requested frame. Further information on the SDSS and many additional services
are available at the <a href="https://www.sdss.org/">SDSS website</a>. Provenance: Sloan Digital Sky Survey Team. This is a service of NASA HEASARC.
Southern GOODS Field: VLT ISAAC Observations, H band
Short Name:
GOODS ISAAC H
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
As part of the Great Observatories Origins Deep Survey (GOODS),
near-infrared imaging observations of the Chandra Deep Field South (CDF-S)
were carried out in J, H, Ks bands, using the ISAAC instrument mounted at
the Antu Unit Telescope of the VLT at ESO's Cerro Paranal Observatory, Chile.
<p>
These data were obtained as part of the ESO Large Programme 168.A-0485 (PI: C. Cesarsky).
Data covering four ISAAC fields in J and Ks bands were also drawn from the ESO programmes 64.O-0643, 66.A-0572 and 68.A-0544 (PI: E.Giallongo),
which were part of the previous data releases.
<p>
This data release covers 172.4, 159.6, and 173.1 arcmin2 of the GOODS/CDF-S
region in J, H and Ks respectively. More than 50% of the images reach a 5-sigma depth
for point sources of at least 25.2 mag (J), 24.7 mag (H and Ks) in the AB system ("median depth").
<p>
This final GOODS/ISAAC data release accumulates observational data which have
been acquired in 12814 science integrations between October 1999 and January 2007
totaling 1.3 Msec integration time.
[Above adapted from reference website.]
<p>
<i> SkyView</i> uses the mosaic files provided in this delivery. The Version 1.5 mosaic
is used for the KS band. Provenance: Data downloaded from VLT archive. This is a service of NASA HEASARC.
Southern GOODS Field: VLT VIMOS Observations, R band
Short Name:
GOODS VIMOS R
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
As part of the Great Observatories Origins Deep Survey (GOODS),
deep imaging in the Chandra Deep Field South (CDF-S) has been carried out,
using the VIMOS instrument mounted at the Melipal Unit Telescope of
the VLT at ESO's Cerro Paranal Observatory, Chile.
<p>
This data release contains the coadded images in U band from the ESO large programme
168.A-0485 (P.I. C. Cesarsky) which have been obtained in
service mode observations between August 2004 and fall 2006.
The 1-sigma depth for VIMOS U band in the area covered by the GOODS-ACS observations
is ~30 AB (within an aperture of 1" radius, ranging from 29.5 and 30.2 AB).
The PSF of the VIMOS U band mosaic is ~0.8" FWHM, but varies over the field.
<p>
Also included in this data release is a coadded image in R band obtained from
data retrieved from the ESO archive. Due to the different observing strategies
adopted in the programmes the resulting coverage of the GOODS-ACS
area is more complex than for the U band.
The depth of the VIMOS R band mosaic over the ACS area ranges from ~28 AB to 29 AB
(1-sigma, 1" aperture radius).
The PSF of the VIMOS R band mosaic is ~0".7 FWHM and varies over the field.
[Adapted from reference website.] Provenance: Data downloaded from VLT archive. This is a service of NASA HEASARC.
Spitzer IRAC medium infrared observations taken in all four IRAC channels in both the north
and south GOODS fields. Provenance: IRAC Goods Team, IRSA data center. This is a service of NASA HEASARC.
Spitzer MIPS observations of the GOODS North and South fields in the
24 micron channel. Provenance: IRSA, GOODS team. This is a service of NASA HEASARC.
VO-compliant publication of Schmidt survey SRC-J of the southern sky digitized with the MAMA microdensitometer at the Observatoire de Paris Image Analysis Centre (CAI).
This database table records high-level information for each Suzaku observation and provides access to the data archive. Each record is associated with a single observation. An observation contains data from all instruments on board Suzaku. This database table is generated at the Suzaku processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
The BAT can operate several configuration modes simultaneously. Each of the simultaneous modes is listed in separate records within this table. For a given time interval, there are several records (partially overlapping in time), each describing a single configuration/mode. The BAT modes collect data for the entire FOV but also have the capability to record rates (tag mask rate) for up to a few specific sky positions (typically 3) that correspond to a pre-assigned target ID. It is possible that at least two or more of these positions do not coincide with the BAT or NFI pointing position and therefore the target ID does necessarily coincide with Target_ID of the BAT or NFI pointing position. This table records for the position (RA and Dec) and Target_ID parameters the correct values associated to each of the mask tag data. This database table is generated at the Swift processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
Swift BAT 70 Month All-Sky Survey: 14\-20 keV: flux
Short Name:
BAT-flux-1
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
This BAT Hard X-ray Survey data is the 70-month survey product of the BAT instrument on
the Swift observatory. Swift/BAT is a wide field-of-view (70x100
degrees) hard X-ray imager consisting of a coded mask and a large array
of CdZnTe detectors (with an effective area of ~ 5000 cm<sup>2</sup>).
<p>
BAT is sensitive in the energy range 14-195 keV. The data are divided
into 8 energy bands
<table border>
<tr><th>Band<th>Energy (keV)<th>Frequency (EHz) </tr>
<tr><td>1<td> 14-20 <td> 3.38-4.84</tr>
<tr><td>2<td> 20-24 <td> 4.84-5.80</tr>
<tr><td>3<td> 24-35 <td> 5.80-8.46</tr>
<tr><td>4<td> 35-50 <td> 8.46-12.1</tr>
<tr><td>5<td> 50-75 <td> 12.1-18.1</tr>
<tr><td>6<td> 75-100 <td> 18.1-24.2</tr>
<tr><td>7<td> 100-150<td> 24.2-36.3</tr>
<tr><td>8<td> 150-195<td> 36.3-47.2</tr>
<tr><td>Sum (SNR only)<td>14-195<td> 3.38-47.2</tr>
</table>
Each band is represented as as two separate surveys, a signal-to-noise (SNR) map and a flux map.
(e.g., BAT-snr-1 or BAT SNR 1 or BAT SNR 14-20, or BAT-Flux-1, ...).
An additional summed survey, BAT-SNR-SUM or BAT SNR SUM or BAT SNR 14-195, is also available, but there
is no summed flux survey. In our Web interface only the SNR surveys are
shown in the Web form. Users can get flux maps corresponding to a given SNR image
from the results pages. The batch interfaces may directly query any of the surveys since
the user chooses the names explicitly rather than from a selection box.
<p>
The values displayed in the significance
maps are the local signal to noise ratio in each pixel. The noise in
these coded-mask images follows a Gaussian distribution with center at
zero and a characteristic width (sigma) of 1.0. The noise is
calculated locally for each pixel by measuring the RMS value of all
pixel values in an annulus around each pixel and hence includs both
statistical and systematic components. Known sources are excluded from
the annuli.
<p>
The signal in each pixel is taken from the flux maps.
<p>
The flux values are in the native BAT survey units of
counts/sec/detector. The detector is an individual piece of CZT in
the BAT array with an area of 1.6 x 10<sup>-7</sup>m<sup>2</sub>.
<p>
While the Swift mission is primarily designed to follow gamma-ray bursts,
the random distribution of bursts in the sky means that these survey's sky coverage
is relatively uniform with the exposure at any point varying between about 6 to 16 megaseconds.
The survey limits for source detection are about 10<sup>-11</sup> ergs/s/cm<sup>2</sup>
over about half the sky and 1.3x10<sup>-11</sup> ergs/s/cm<sup>2</sup> over 90%.
<p>
These data replace the 9-month BAT datasets which we have retired. If you wish access to the older data please let us know.
Note that for the 9-month data we provided access through the web page to the flux data
and gave links to the signal-to-noise maps. Since the existence of sources is most
easily seen in the SNR maps, we decided to invert that for this release.
<p>
For the 8 band data, the source data were provided by the BAT team as 6 FITS files. Each of these contained the 8 bands in separate image
extensions for a region centered at l=0,b=+/-90 or l=0,90,180,270,b=0, the centers of 6 cubic facets. However these data are not the classical
cube-faced projections, e.g., as used in COBE data. The data on the facets overlap, so that this is just a convenient way to tile the sky.
<i>SkyView</i> separated each of the FITS image extensions into a separate file, but no other modifications were made to the data. The summed image was
provided as six separate files. Provenance: NASA BAT Team. This is a service of NASA HEASARC.
The Swift UVOT instrument is a 30 cm modified Ritchey-Chretien reflecting telescope launched on
board the Swift satellite on November 20, 2004.
The range of optical and UV filters can accomodate wavebands between 1700 and 6500 Angstroms.
A full field image covers 17x17 arcminutes and at maximum spatial sampling is imaged onto 2048x2048 0.5"
pixels. A 1000 second observation can detect point sources to m=22.3 when no filter is used.
The Swift Serendipitous Source Catalog (Page et al., 2015) detects sources down to m=23-26 for
the six filters in very deep observations, but the typical limits are substantially brighter (~20-23 magnitude).
<p>
These surveys are mosaics of all Swift UVOT observations released between the start of the mission and July 2017.
Data were extracted from the HEASARC archive from the UVOT products directory. Mosaics are provided
in six filters and also with no filter, i.e., WHITE. The table below gives the number of
observations and bandpasses for each of the filters. For each UVOT observation standard processing generates a
counts and exposure file as a single multi-extension FITS file with a separate extension for each filter. To aid
processing, these extensions were copied into separate files in directory trees for each filter.
Four observations in which the exposure and counts maps did not agree on the filters
used were omitted from the processing.
<p>
Some observations were recorded with 0.5" pixels while others were binned to 1". All 0.5" observations
(typically fewer than 10%) were rebinned to the larger pixels for the counts maps since the counts
data scales with the pixel size.
Since the exposure values are intensive and do not vary significantly based upon the resolution, these data were
not generally rebinned unless it was needed to ensure that Order 9 Hips data were produced.
<p>
The CDS Hipsgen software was used to generate Order 9 HiPS data (~0.8" pixels) for both the Counts and
Exposure images. The HiPS (Hierarchical Progressive Survey VO standard) supports multi-resolution mosaics.
Any quantitative use of these images should note that the rebinning increases the
total counts by a factor of ~(1.0/0.8)^2 ~ 1.56. This software uses a bilinear interpolation to generate HEALPix tiles of an appropriate
order (18 in this case). <i>SkyView</i> developed software was used to divide the level 9 counts maps
tiles by the corresponding exposure maps to create intensity tiles.
Pixels where the exposure was less than 5 seconds were left as NaNs.
The lower order (8 to 3) order intensity tiles were then generated by averaging
2x2 sets of the higher order maps treating any missing maps or pixels as NaNs.
A HiPS all-sky image was generated by averaged the Order 3 tiles.
<p>
Only the Intensity HIPS files are presented in the SkyView web page directly, but intensity, counts and
exposure maps are available for all seven filters. Note that unlike the XRT HiPS data, the exposure
and counts maps have not been clipped. I.e., the source FITS files have been aligned with the
coordinate system and thus contain large numbers of unexposed pixels with 0 values.
These 0's are simply propogated to HiPS tiles.
NaNs are returned in regions which lie outside any of the original source images. For the Intensity map,
any pixel for which the exposure was less than 5s is returned as a NaN.
<table border>
<tr><th align=center>Filter</th><th>Count</th><th>Central Wavelength (&#8491;;)</th><th>Bandpass (&#8491;;)</th><th>Central Frequency(THz)</th><th>Bandpass (THz)</th><th>Coverage</th></tr>
<tr><th align=center>WHITE</th><td align='center'>3,000</td><td align='center'>3600</td><td align='center'>1600-6000</td><td align='center'>832</td><td align='center'>500-1874</td> <td>0.0017</td></tr>
<tr><th align=center>V</th><td align='center'>30,557</td><td align='center'>5468</td><td align='center'>5083-5852</td>< <td align='center'>548</td><td align='center'>512-590</td> <td>0.0171</td></tr>
<tr><th align=center>B</th><td align='center'>28,347</td><td align='center'>4392</td><td align='center'>3904-4880</td> <td align='center'>683</td><td align='center'>614-768</td> <td>0.0112<td></tr>
<tr><th align=center>U</th><td align='center'>49,954</td><td align='center'>3465</td><td align='center'>3072-3875</td> <td align='center'>865</td><td align='center'>774-975</td> <td>0.0287</td></tr>
<tr><th align=center>UVW1</th><td align='center'>60,690</td><td align='center'>2600</td><td align='center'>2253-2946</td> <td align='center'>1154</td><td align='center'>1017-1330</td><td>0.0277</td></tr>
<tr><th align=center>UVM2</th><td align='center'>56,977</td><td align='center'>2246</td><td align='center'>1997-2495</td> <td align='center'>1334</td><td align='center'>1201-1501</td>>td>0.0314</td></tr>
<tr><th align=center>UVW2</th><td align='center'>54,590</td><td align='center'>1928</td><td align='center'>1600-2256</td> <td align='center'>1554</td><td align='center'>1328-1874</td><td>0.0260</td></tr>
</table>
<strong>Observation counts and bandpasses for UVOT Filters</strong>
<p> Provenance: Data generated from public images at HEASARC archive. This is a service of NASA HEASARC.
The UVOT runs only one type of configuration filter/mode/window in a given time interval. This database table, therefore, contains for a given time interval a single record that describes one configuration. This database table is generated by the Swift Data Center. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
The Swift XRT (<a href="https://ads.harvard.edu/abs/2005SSRv..120..165B">Burrows et al 2005, SSRv, 120, 165</a>)
is a sensitive, broad-band (0.2 - 10 keV) X-ray imager
with an effective area of about 125 cm**2 at 1.5 keV.
The 600 x 600 pixel CCD at the focus provides
a 23.6' x 23.6' field of view with a pixel scale
of 2.36". The point spread function
is 18" (HPD) at 1.5 keV.
<p>
These XRT surveys represent the data from the first 12.5 years of Swift X-ray observations.
They include all data taken in photon counting mode. A total of just over 8% of the sky
has some non-zero exposure. The fraction of sky exposed as a function of the exposure is given
in the following table:
<table border>
<tr><th>Exposure</th><td>>0</td> <td>10</td> <td>30</td> <td>100</td> <td>300</td> <td>1000</td> <td>3000</td>
<td>1000</td> <td>30000</td> <td>100000</td><td>300000</td></tr>
<tr><th>Coverage</th>
<td> 8.42 </td><td> 8.37 </td><td> 8.29 </td><td> 7.67 </td><td> 7.29 </td><td> 5.68 </td>
<td> 3.40 </td><td> 1.26 </td><td> 0.35 </td><td> 0.044 </td><td> 0.00118</td></th>
</table>
The individual exposure and counts maps have been combined
into a Hierarchical Progressive Survey (HiPS) where the data are stored in tiles
in the HEALPix projection at a number of different resulutions. The highest resolution
pixels (HEALPix order 17) have a size of roughly 1.6". Data are also stored at lower
resolutions at factors of 1/2, 1/4, 1/8, 1/16, and 1/32, and in an all sky image with a resolution
1/256 of the higest resolution. An intensity map has been created as the ratio
of the counts and exposure maps.
<p>
These surveys combine the basic count and exposure maps provided as standard products
in the Swift XRT archive in obsid/xrt/products/*xpc_(sk|ex).img.gz. The surveys were created as follows:
<ul>
<li>All of the exposure maps available in the archive in mid-May 2017 were combined
using the CDS-developed Hipsgen tool. This includes 129,063 observations for which
both count and exposure files were found in PC mode. Three exposures where there was
a counts map but no exposure map were ignored. A few exposure files had more than
one exposure extension. 1,082 files had two extensions and 1 file had 3 extensions.
The 1084 HDUs in extensions were extracted as separate files and included in the total exposure.
The value of 0 was given to the Hipsgen software as the null value for the FITS files.
This caused the CDS software to treat such pixels as missing rather than 0 exposure.
<li>
The counts data was extracted from the counts maps for each observation using <i>SkyView</i>
developed software. For any pixel in which a count was recorded, the corresponding
exposure file was checked and if there was any exposure (in any of the associated
extensions), then the count was retained. If there was no exposure in any of the extensions
of the corresponding exposure file, the counts in the pixel were omitted. Once a count
was accepted, the overlap between the counts map pixel and the pixels of the corresponding
HiPS tile (or tiles) was computed. Each count was then assigned entirely to a single
pixel in the HiPS tile randomly but with the destination pixel probabilities weighted by area of
the overlap. Thus if several pixels were found in a given counts map pixel they
might be assigned to different pixels in the output image. The HiPS pixels (~1.6") used were
of substantially higher resolution than the XRT resolution of 18" and somewhat higher than
the counts map resolution of 2.36".
<p>
A total of 183,750,428 photons were extracted from the counts maps while 15,226 were rejected
as being from pixels with 0 exposure. There were 501 pixels which required special
treatment as straddling the boundaries of the HEALPix projection.
<li>
The resulting counts tiles were then clipped using the exposure tiles that had been
previously generated. Basically this transferred the coverage of the exposure tiles
to the counts tiles. Any counts pixel where the corresponding exposure pixel was a NaN
was changed to a NaN to indicate that there was no coverage in this region.
<p>
During the clipping process 137,730 HiPS level 8 were clipped (of 786,432 over the entire sky). There were
12,236 tiles for which there was some exposure but no counts found. During the clipping process
2 photons were found on pixels where there was no corresponding exposure in the exposure tiles.
This can happen when the pixel assignment process noted above shifts a photon just outside the
exposed region but should be -- as it was -- rare. These photons were deleted.
<li>
After creating the clipped level 8 counts maps, level 7 to 3 tiles and an all sky map
where generated by averaging pixels 2x2 to decrease each level.
When adding the four pixels in the level N map together
only pixels whose value was not NaN were considered.
<li>
Finally an intensity map was created by dividing the counts tiles by the exposure tiles.
To eliminate gross fluctuations due to rare counts in regions with very low exposure, only
regions with exposure > 1 second were retained. A total of 30 photons were deleted due to
this criterion.
</ul>
<p>
Note that while any sampler may in principle be used with these data, the Spline sampler may
give unexpected results. The spline computation propogates NaNs thought the image and
means that even occasional NaNs can corrupt the
output image completely. NaNs are very common in this dataset.
Also, if the region straddles a boundary in the HEALPix projection,
the size of the requested input region is likely to exceed memory limits since the HiPS
data are considered a single very large image. Provenance: Data generated from public images at HEASARC archive. This is a service of NASA HEASARC.
The XRT runs only one type of configuration mode/window in a given time interval. The table therefore contains for a given time interval a single record that describes one configuration. A new record is generated when the following is changing within an observation: new operating mode , new pointing mode, or new window configuration. This database table is generated by the Swift Data Center. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
The Sydney University Molonglo Sky Survey (SUMSS) is a deep radio
survey at 843 MHz of the entire sky south of declination -30&#176;;, made using
the Molonglo Observatory Synthesis Telescope (<a href="https://www.physics.usyd.edu.au/astrop/most/"> MOST </a>), located near Canberra, Australia.
The images from the SUMSS are produced as 4 x 4 degree mosaics of up to
seventeen individual observations, to ensure even sensitivity across
the sky. The mosaics slightly overlap each other. Data were last updated on January 28, 2015.
<p>
Images can also be obtained from the <a href="https://www.astrop.physics.usyd.edu.au/cgi-bin/postage.pl">SUMSS Postage Stamp Server</a>.
<p>
The SUMSS is intended to complement the NRAO-VLA Sky Survey (NVSS) which
covered the sky between +90 and -40 deg declination, at a
frequency of 1400MHz.
<p> Provenance: The SUMSS project team, University of Sydney. This is a service of NASA HEASARC.
The Tartarus database contains the results of a detailed but systematic analysis of ASCA observations of active galactic nuclei (AGN). It contains source and background events files, spectra, ancillary response files and response matrices, images, and assorted light curves for a large number of ASCA AGN observations. Spectral fit results are done by automatic XSPEC fitting. This database table allows easy access to reduced AGN data for the whole community, allowing the maximum scientific return from the data. Availability of publishable light curves, images, and spectra (which can also be readily re-fitted) should be particularly valuable to astronomers with little direct experience in the reduction of X-ray data. Version 3.1 has been created by analyzing all ASCA observing sequences with targets designated as AGN, as indicated by a leading "7" in the ASCA observing sequence number. Version 3.1 contains products for all 611 observing sequences designated as AGN observations. This is a significant improvement over Versions 1 and 2. Moreover, the 611 sequences for which products are available are complete in the sense that either the target object was not detected (in which case an upper limit on GIS2 source counts is given) or the intended AGN target was detected and the data were fully analyzed. In order to obtain the most accurate background subtraction and minimize contamination from any nearby sources, version 3.1 makes more use of custom extraction regions than previous versions. It is expected that version 3.1 will be replaced when the final ASCA calibration is completed. This database table has been created by the Tartarus Team, and they, rather than Imperial College London or the HEASARC, are responsible for the contents. It was ingested by the HEASARC in August, 2005. This is a service provided by NASA HEASARC .
The Hawaii-HDF-N is an intensive multi-color imaging survey of 0.2 sq.
degrees centered on the HDF-N. Data were collected on the NOAO 4m Mayall telescope,
the National Astronomical Observatory of Japan 8.2m Subaru telescope and the
University of Hawaii 2.2m telescope.
Deep U, B, V, R, I, and z' data were obtained over the whole field and deep HK' data over
the Chandra Deep Field North. Details are available in the references.
[Adapted from reference website.]
<P>
Two different images are given in the V band (V0201 and V0401) from observations
separated by about a month that had substantial differences in seeing. Provenance: Data downloaded from the reference website. A formatting
error in the FITS files was corrected.. This is a service of NASA HEASARC.
The HI 4-PI Survey (HI4PI) is a 21-cm all-sky survey of neutral atomic
hydrogen. It is constructed from the Effelsberg-Bonn HI Survey (EBHIS), made
with the 100-m radio telescope at Effelsberg/Germany, and the Galactic All-Sky
Survey (GASS), observed with the Parkes 64-m dish in Australia. HI4PI
comprises HI line emission from the Milky Way. This dataset is the atomic
neutral hydrogen (HI) column density map derived from HI4PI
(|Vlsr| < 600 km/s). Provenance: Argelander-Institut für Astronomie (AIfA), Max-Planck-Institut für
Radioastronomie (MPIfR), and CSIRO/Australia; data provided by B. Winkel. This is a service of NASA HEASARC.
The Southern H-Alpha Sky Survey Atlas is the product of a wide-angle
digital imaging survey of the H-alpha emission from the warm ionized
interstellar gas of our Galaxy. This atlas covers the southern hemisphere
sky (declinations less than +15 degrees). The observations were taken with
a robotic camera operating at Cerro Tololo Inter-American Observatory (CTIO)
in Chile. The atlas consists of 2168 images covering 542 fields. There are four
images available for each field: <b>H-alpha</b>, <b>Continuum</b>, <b>Continuum-Corrected</b>
(the difference of the H-alpha and Continuum images), and <b>Smoothed</b> (median filtered to 5 pixel, or 4.0 arcminute, resolution to remove star residuals better). The <a href="https://amundsen.swarthmore.edu/SHASSA">SHASSA website</a> has more details of the data and the status of this and related projects. Images can also be
obtained from the <a href="https://amundsen.astro.swarthmore.edu/SHASSA/#Images">Download Images</a> section at the SHASSA site. Provenance: John E. Gaustad (Swarthmore College), Peter R. McCullough (University of Illinois), Wayne Rosing (Las Cumbres Observatory), and Dave Van Buren (Extrasolar Research Corporation). This is a service of NASA HEASARC.
2MASS data were collected by uniformly scanning the entire sky in three
near-infrared bands to detect and characterize point sources brighter than
about 1 mJy in each band, with signal-to-noise ratio (SNR) greater than 10,
using a pixel size of 2.0". This achieves an 80,000-fold improvement in
sensitivity relative to earlier surveys.
2MASS used two new, highly-automated 1.3-m telescopes, one at Mt. Hopkins,
AZ, and one at CTIO, Chile. Each telescope is equipped with a three-channel
camera, each channel consisting of a 256 by 256 array of HgCdTe detectors,
capable of observing the sky simultaneously at J (1.25 microns),
H (1.65 microns), and K<sub>s</sub> (2.17 microns).
<p>2MASS images and other data products can be obtained at the <a href="https://irsa.ipac.caltech.edu/applications/2MASS/QL/">NASA/IPAC Infrared Science Archive</a> Provenance: The Two Micron All Sky Survey is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center, funded by
the National Aeronautics and Space Administration and the National
Science Foundation.. This is a service of NASA HEASARC.
The UKIDSS survey is the next generation infrared survey, a successor
to 2MASS. It will ultimately cover 7000 square degrees in the
northern sky at both high and low Galactic latitudes and goes about
three magnitudes deeper than 2MASS in the coverage area. Most data is
taken in the J, H and K bands. A Y band is available in some regions.
<p>
UKIDSS is comprised of several distinct surveys in different regions of the
sky. Of primary interest to <i>SkyView</i> users (since they have the largest
sky coverage) are the Large Area Survey, the Galactic Plane Survey, and the
Galactic Clusters Survey. There are deep and ultadeep surveys which cover
much smaller fractions of the sky. The planned coverage for the UKIDSS
surveys may be seen at the <a href="http://wsa.roe.ac.uk/theSurveys.html">
UKIDSS survey page</a>. All UKIDSS data products are published by the Wide-Field
Astronomy Unit (WFAU) at the University of Edinburgh through the
<a href="http://wsa.roe.ac.uk/">WFCAM Science Archive (WSA)</a> which includes
more detailed coverage information for each data release.
<p>
<i>SkyView</i> currently uses the DR11 data release. Many thanks to
the WSA team at WFAU for providing an interface to make all the latest
data easily accessed. Note that coverage is not uniform across the different bands so
that at a given point there might be H and K band data, but nothing in the J band. Provenance: UKIDSS Project. This is a service of NASA HEASARC.
The VLA Low-Frequency Sky Survey (VLSS) is a 74 MHz continuum survey
covering the entire sky north of -30 degrees declination. Using the
VLA in BnA and B-configurations, it will map the entire survey region
at a resolution of 80" and with an average rms noise of 0.1 Jy/beam.
<p>
This version include the data from the VLSS redux which increased the coverage
region slightly and substantially improved the data reduction. Details are in the
Lane et al. (2012) reference. Provenance: <b>VLSS Team: </b>R.A. Perley, J.J. Condon, W.D. Cotton (NRAO);
A.S. Cohen, W.M. Lane (NRC/NRL),
N.E. Kassim, T.J.W. Lazio (NRL),
W.C. Erickson (UMd). This is a service of NASA HEASARC.
This survey is a deep, high resolution radio survey of a relatively small region that has particularly deep coverage
in the Sloan Digital Sky Survey. As described in the reference abstract:
This is a high-resolution radio survey of the Sloan Digital Sky Survey (SDSS) Southern Equatorial
Stripe, a.k.a., Stripe 82. This 1.4 GHz survey was conducted from 2007 to 2009 with the Very Large Array primarily in the A-configuration,
with supplemental B-configuration data to increase sensitivity to extended structure.
The survey has an angular resolution of 1.8" and achieves a median rms noise of 53 microJy/beam over 92 square degrees.
This is the deepest 1.4 GHz survey to achieve this large of an area filling in the
phase space between small&deep and large&shallow surveys.
<p>
The astrometric accuracy of the data is excellent with errors in observed sources of 0.10" in both RA and declination.
A comparison with the SDSS DR7 Quasar Catalog confirms that the astrometry is well tied to the optical reference
frame with mean offsets of 0.02+/-0.01" in RA and 0.01+/-0.02 in declination. Provenance: TBD. This is a service of NASA HEASARC.
VLT ISAAC Ks Observations of the Southern Hubble Ultradeep Field
Short Name:
HUDFISAAC
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
A very deep Ks observation of the Hubble Ultradeep Field. This observation is
approximately 0.6 magnitudes deeper than the GOODS ISAAC Ks image but covers
only small fraction of the area. Provenance: Data downloaded from VLT archive. This is a service of NASA HEASARC.
VOPSAT is a set of southern sky digital surveys based on ESO-R, SRC-J and POSS1-E atlases. The plates have been digitized with the MAMA microdensitometer with a resolution of 0.7 arc-sec. Pixel resampling will allow mosaicing neighbouring Schmidt fields up to hundreds of square degrees.
The Westerbork Northern Sky Survey (<i>WENSS</i>) is a low-frequency
radio survey that covers the whole sky north of delta=30 degree at a
wavelength of 92 cm to a limiting flux density of approximately 18 mJy
(5 sigma). This survey has a resolution of 54" x 54" cosec (delta)
and a positional accuracy for strong sources of 1.5''.
<p>
Further information on the survey including links to catalogs
derived from the survey is available at the
<a href="https://web.archive.org/web/20041204180313/http://www.strw.leidenuniv.nl/wenss/"><i>WENSS</i> website</a>.
<p>
The <i>WENSS</i> survey is included on the <b>SkyView High Resolution Radio
Coverage </b><a href="https://skyview.gsfc.nasa.gov/images/high_res_radio.jpg"> map</a>. This map shows
coverage on an Aitoff projection of the sky in equatorial coordinates.
<p> Provenance: <i>WENSS</i> Team. Data downloaded
from
<a href=ftp://vliet.strw.leidenuniv.nl/pub/wenss/HIGHRES/>
<i>WENSS</i> FTP site</a> 1999-03-18.
The <i>WENSS</i> project is a collaboration between the
<a href="https://www.astron.nl/astronomy/">Netherlands Foundation for Research in
Astronomy</a> (NFRA/ASTRON) and the
<a href="https://local.strw.leidenuniv.nl/">Leiden Observatory</a>.. This is a service of NASA HEASARC.
WISE 3\.4 Micron All-Sky Survey>: All-WISE data release
Short Name:
WISE
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
From the <a href="https://wise2.ipac.caltech.edu/docs/release/allsky">WISE mission site:</a>.
<hr>
NASA's Wide-field Infrared Survey Explorer (WISE) mapped the
sky at 3.4, 4.6, 12 and 22 micrometers in 2010 with an
angular resolution of 6.1", 6.4", 6.5" and 12.0" in the four bands.
WISE achieved a 5 sigma point source sensitivities better and 0.08, 0.11
1 and 6 mJy in unconfused regions on the ecliptic in the four
bands. Sensitivity improves toward the ecliptic poles due to denser
coverage and lower zodaical background.
<p>
The WISE All-WISE
includes all data taking during the WISE full cryogenic phase, from January 7, 2010 to August 6, 2010, that were processed
with improved calibrations and reduction algorithms and combines this with the NEOWISE postcryogenic
survey to form the most comprehensive view of the full mid-infrared sky.
bibcode=1995ApJ...451..564V,2010ApJ...713..912W <hr>
<p>
SkyView includes the four WISE bands as separate surveys. Many non-image
data products are available at the WISE site. Note that WISE data is
distributed in relatively large (>50 MB) image files. When SkyView generates
an image for a part of the sky where it has not yet cached the
data from the IPAC server there may be a delay as full tiles are downloaded
even when only a small fraction of a tile is needed. Images
in cached regions, are generated much faster. Access to
the WISE data uses the VO SIA interface maintained at IPAC. Even when
data is cached, the SIA service must still be available for successful
queries. Provenance: WISE Archive (IRSA/IPAC). This is a service of NASA HEASARC.
These survey represents a combination of the 9-year data combined
in a way that is intended
to minimize the contribution from the galaxy. The data measure the temperature deviation
from a uniform black body.
<p>
The original data are available at the <https://lambda.gsfc.nasa.gov>LAMBDA archive</a>.
<p>
The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard
projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees.
The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the
pixels are treated properly. The special HealPixImage class is used so that SkyView can use
the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but
translates the pixels from that image to the nested HEALPix structure that is used
by the WMAP data.
</p> Provenance: WMAP Mission/LAMBDA archive. This is a service of NASA HEASARC.
This is the XMM-Newton Master Catalog and Public Archive table which has been created from information supplied to the HEASARC by the XMM-Newton Project. It is periodically updated as necessary. This database table contains the list of observations which have already been made by the XMM-Newton observatory, as well as those which are scheduled to be made in the near future (usually a a few weeks to a month ahead of the present). It does not contain observations which are scheduled to be performed further in the future, nor does it contain accepted observations which have not yet been scheduled. The list of all accepted XMM-Newton observations, including a number of ones which are unlikely to ever be carried out, such as accepted priority C targets, is available in the XMMAO Browse table. This table includes entries for both pointed data and for data obtained during spacecraft slews. The slew observations all have obsid values beginning with the digit 9 and, because they were not made at a fixed position, lack any positional information such as RA and Declination. Some XMM-Newton observations for which the archived data has become publicly available as indicated by the public_date parameter value, i.e., the proprietary period has expired, are not currently available at the HEASARC: such cases will have values of 'N' for the data_in_heasarc parameter. These datasets in most cases are available at the ESA XMM-Newton Science Archive (XSA) at <a href="http://nxsa.esac.esa.int/nxsa-web/">http://nxsa.esac.esa.int/nxsa-web/</a>. For much more detailed information on the XMM-Newton instruments and their operation, please refer to the XMM-Newton Users Handbook at <a href="http://heasarc.gsfc.nasa.gov/docs/xmm/uhb/">http://heasarc.gsfc.nasa.gov/docs/xmm/uhb/</a>. This database table was created by the HEASARC based on information supplied by the XMM-Newton Project at the following URLs: <pre> <a href="http://nxsa.esac.esa.int/ftp_public/heasarc_obslog/xsaobslog.txt">http://nxsa.esac.esa.int/ftp_public/heasarc_obslog/xsaobslog.txt</a> <a href="http://nxsa.esac.esa.int/ftp_public/heasarc_obslog/xsaslewlog.txt">http://nxsa.esac.esa.int/ftp_public/heasarc_obslog/xsaslewlog.txt</a> <a href="https://xmm-tools.cosmos.esa.int/external/xmm_mission_plan/odf_pps/catstrip.shtml">https://xmm-tools.cosmos.esa.int/external/xmm_mission_plan/odf_pps/catstrip.shtml</a> </pre> It is periodically updated within a few days of whenever these XMM-Newton Project's URLs are modified. This is a service provided by NASA HEASARC .