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.
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.