During the years 2004 to 2017, the Palomar 60 inch telescope (P60) operated as a fully robotic facility to obtain targeted optical observations of gamma-ray burst (GRB) afterglows and other transient events. An automated pipeline reduced the data in real time. The raw, calibration, and pipeline-processed data are available here.
The database of Gamma Ray Burst (GRB) photometrical observations
obtained on defferent telescopes at Fesenkov Astrophysical Institute,
Almaty, Kazakhstan. Observations were carried out in the optical
range.
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.
From 1986 through 1991, the Astronomical Institute of Münster
University performed a search for flare stars in several southern
associations and open stellar clusters using the GPO telescope (d=40
cm, WFPDB identifier ESO040); the fields suveyed include Coalsack,
M42, B228 Lup, the Chameleon T1 association, omicron Vel cluster, R
CrA association, the Pipe nebula (B59 Oph), and the Sco-Oph
association. This was done primarily through multiple exposures. The
files published here are plate scans done in 2017.
The obscore collection name for these files is Muenster Flare Survey.
In the context of Kapteyn's plan to obtain a photometric standard, in
Potsdam more than 400 photographic plates of several Selected Areas,
Special Areas, and Kapteyn-Pritchard areas were obtained between 1910 and
1933, both as direct images and with an object prism. This service
provides FITS images of the science area of the plates as well as images of
the entire plates, including previous markings.
Properties of the Dust and Gas in the Environs of V838 Monocerotis
Short Name:
V838MON
Date:
27 Oct 2022 19:00:00
Publisher:
NASA/IPAC Infrared Science Archive
Description:
Herschel far-infrared imaging and spectroscopy were taken at several epochs to probe the central point source and the extended environment of the stellar outburst object V838 Monocerotis.
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.
