The Orbiting Solar Observatory-I (OSO-8) was launched on 21 June 1975 into a 550 km circular orbit at 33 degrees inclination. Data were obtained from the mission until late September 1978. The spacecraft structure consisted of a rotating cylindrical base section called the "wheel" and a non-spinning upper section called the "sail". While the primary objectives of the mission were solar in nature, there were 3 detectors, the GSFC Cosmic X-ray Spectroscopy experiments (GCXSE detectors A, B and C), mounted in the rotating wheel which had exclusively non-solar objectives. Their fields-of-view were either aligned to the spin axis or at small angles to it, hence they always view the portion of the sky at right angles to the earth-sun line. This database accesses the raw rates FITS datafile for the A, B and C GCXSE detectors, accumulated every 160 ms in the 2-60 keV energy band. This is a service provided by NASA HEASARC .
The PACS Evolutionary Probe (PEP, Lutz et al. 2011) is a Herschel guaranteed time deep extragalactic survey (KPGT_dlutz_1) targeting six among the most popular "blank fields", ten lensing clusters of galaxies, and two z ~1 clusters at wavelengths of 100 and 160 microns. PEP includes SPIRE observations of the two z ~1 clusters at wavelengths of 250, 350, and 500 microns. SPIRE coverage of all other fields is available from the HerMES survey (Oliver et al. 2010). In addition, deep SPIRE GOODS-N data are provided by the GOODS-Herschel program (Elbaz et al. 2011).
All Herschel observations are processed through an automatic pipeline, which corrects a number of instrumental artifacts. The Highly Processed Data Products (HPDP) have gone through additional interactive processing, and represent an improvement over the standard products. HPDP from Herschel's Photoconductor Array Camera and Spectrometer (PACS) are available for JScanam maps, Unimap maps, and Red Leak Spectra.
The Panchromatic Hubble Andromeda Treasury is a Hubble Space Telescope Multi-cycle program to map roughly a third of M31's star forming disk,
using 6 filters covering from the ultraviolet through the near infrared. With HST's resolution and sensitivity, the disk of M31 will be resolved
into more than 100 million stars, enabling a wide range of scientific endeavors.
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.
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.
PPAKM31 – Optical Integral Field Spectroscopy of Star-Forming Regions
in M31
Date:
12 Jun 2024 13:04:11
Publisher:
The GAVO DC team
Description:
These observations cover five star-forming regions in the Andromeda
galaxy (M31) with optical integral field spectroscopy. Each has a
field of view of roughly 1 kpc across, at 10pc physical resolution. In
addition to the calibrated data cubes, we provide flux maps of the Hβ,
[OIII]5007, Hα, [NII]6583, [SII]6716 and [SII]6730 line emission. Line
fluxes have not been corrected for dust extinction. All data products
have associated error maps.
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.