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.
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.
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:
07 Mar 2025
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:
07 Mar 2025
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.
