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 ERO program is an initiative of the Euclid Science Team / ESA to collect 1 day of observations to showcase the Euclid mission and its capabilities before the start of the nominal survey. The ERO data products available at IRSA for the convenience of the US astronomy community are the same data products that are available through ESAC. The FITS files were processed with an ERO-specific pipeline, which is different from the standard Euclid pipeline that will be used for future data releases.
The Eureka Lawrence Berkeley National Laboratory (LBNL) Far-IR Lockman Hole (ELFLock) maps are intended to measure the Far-IR background radiation with 160-micron observations from the Multiband Imaging Photometer for Spitzer (MIPS). The download gives the largest contiguous low-cirrus 160 micron far-infrared map made with Spitzer data, covering 8.5 square degrees. It also differs from standard Spitzer-processed mosaic maps in that the background information is preserved, where it is normally removed by median filtering (for point-source studies). The map is composed of BCD data from S16 processing of data sets with these Spitzer Astronomical Observation Requests (AORs). Its flux units are MJy/Sr and the pixel size is 15.9", though flux = 0.0 for pixels without data.
Science images from the HST and HLA collections hosted at ESAC/ESA. All public HST observations in calibrated and science-ready form are synchronised with the MAST services for HST reprocessed public data and corresponding metadata. The European HST archive interface can be accessed at https://hst.esac.esa.int/ehst
The goal of the "Evolution of interstellar dust" guaranteed time key project (PI: A. Abergel & A. Zavagno) is to explore with Herschel the far-infrared (FIR) to submillimeter (submm) emission properties of dust particles in a wide range of regions within our Galaxy, from very diffuse clouds to sites of star formation and proto-stars. Photometric data taken with SPIRE and PACS are complemented with spectroscopy using the FTS of SPIRE and PACS to derive the physical conditions of the gas from the lines of [CI], the high-level rotational lines of CO, and the major cooling lines of [CII] and [OI].
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.
Far-Infrared Deep Extragalactic Legacy Survey (FIDEL) contains sensitive and extensive far-infrared deep field observations with Spitzer to detect warm dust emission from hundreds of relatively ordinary starburst galaxies and active galactic nuclei at redshifts of 1 to 2 (7 to 10 billion years ago), and thousands more nearby. The survey also detected tens of thousands of high redshift objects at mid-infrared wavelengths. The program obtained data in three fields on the sky. The bulk of the data is in two fields, the Extended Chandra Deep Field South (ECDFS) and the Extended Groth Strip (EGS). A smaller amount of additional data was obtained in the GOODS-North area.
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.
