The Frontier Fields is a Spitzer and HST Director's Discretionary program of six deep fields centered on strong lensing galaxy clusters in parallel with six deep "blank fields". These will be the second deepest observations of blank fields and deepest observations of clusters and their lensed galaxies ever obtained.
The first data release contains all archival data taken on these six clusters as well as data taken for the cycle-9 SURFS-UP (PID:90009) program as of April 1, 2013. Improved reductions with better artifact correction and deeper data will be released periodically over the three year period.
IRSA hosts the Spitzer portion of the Frontier Fields data set. For the HST Frontier Fields data, see MAST.
Sternberg Astronomical Institute Virtual Observatory Project
Description:
</pre><p>Gaia is an ambitious mission to chart a three-dimensional map of our Galaxy, the Milky Way, in the process revealing the composition, formation and evolution of the Galaxy. Gaia will provide unprecedented positional and radial velocity measurements with the accuracies needed to produce a stereoscopic and kinematic census of about one billion stars in our Galaxy and throughout the Local Group. This amounts to about 1 per cent of the Galactic stellar population.
<p>The data collected during the first 22 months of the nominal, five-year mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC), resulting into this second data release. A summary of the release properties is provided in Gaia Collaboration et al. (2018b). The overall scientific validation of the data is described in Arenou et al. (2018). Background information on the mission and the spacecraft can be found in Gaia Collaboration et al. (2016), with a more detailed presentation of the Radial Velocity Spectrometer (RVS) in Cropper et al. (2018). In addition, Gaia DR2 is accompanied by various, dedicated papers that describe the processing and validation of the various data products: Lindegren et al. (2018) for the Gaia DR2 astrometry, Riello et al. (2018) and Evans et al. (2018) for the Gaia DR2 photometry, Sartoretti et al. (2018), Soubiran et al. (2018), and Katz et al. (2018) for the Gaia DR2 spectroscopy (radial velocities), Holl et al. (2018) for the Gaia DR2 variability, Andrae et al. (2018) for the Gaia DR2 astrophysical parameters, Gaia Collaboration et al. (2018g) for the Solar-system objects, and Gaia Collaboration et al. (2018f) for the celestial reference frame. Four more papers present a glimpse of the scientific richness of the data in the areas of the Hertzsprung-Russell diagram (Gaia Collaboration et al. 2018a), the mapping of the kinematics and large-scale structure of the Milky Way (Gaia Collaboration et al. 2018e), parallaxes and proper motions of Milky Way satellite galaxies (Gaia Collaboration et al. 2018d), and variable stars in the colour-magnitude diagram (Gaia Collaboration et al. 2018c). In addition to the set of references mentioned above, this documentation provides a detailed, complete overview of the processing and validation of the Gaia DR2 data.
The Galactic Plane Infrared Polarization Survey (GPIPS) covers 76 sq. deg. of the first Galactic quadrant midplane, 18<l<56 deg and -1<b<1 deg, in H-band (1.6 micron) linear polarimetry to reveal the plane-of-the-sky orientation of the magnetic field in diffuse and denser atomic and molecular clouds. The Survey consists of 3234 overlapping 10x10 arcmin fields observed using the Mimir instrument on the 1.8 m Perkins telescope.
The Galaxy Evolution Explorer (GALEX), a NASA Small Explorer mission, is performing the first all-sky, deep imaging and spectroscopic ultraviolet surveys in space. The prime goal of GALEX is to study star formation in galaxies and its evolution with time.
This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m<sub>AB</sub> ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m<sub>AB</sub> ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m<sub>AB</sub> ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at <a href="http://galex.stsci.edu/">http://galex.stsci.edu/</a>. More information about GALEX can be found at <a href="http://www.galex.caltech.edu/">http://www.galex.caltech.edu/</a> and <a href="https://asd.gsfc.nasa.gov/archive/galex/">https://asd.gsfc.nasa.gov/archive/galex/</a>. This table was first created in July 2010 using the input file <a href="http://sherpa.caltech.edu/gips/ref/galex_obs_status.csv">http://sherpa.caltech.edu/gips/ref/galex_obs_status.csv</a> obtained from the Caltech GALEX site. This table is updated within a week of the update of the original file. This is a service provided by 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.
Galaxy Halos, Outer disks, Substructure, Thick disks and Star clusters (GHOSTS)
Short Name:
GHOSTS
Date:
22 Jul 2020 21:59:56
Publisher:
Space Telescope Science Institute Archive
Description:
The GHOSTS survey is the largest study to date of the resolved stellar populations in the outskirts of disk galaxies. The sample consists of 14 disk galaxies within 17 Mpc, whose outer disks and halos are imaged with the Hubble Space Telescope Advanced Camera for Surveys (ACS).
The GALEX Atlas of Nearby Galaxies contains images of 1034 nearby galaxies recently observed by the GALEX satellite in its far-ultraviolet (FUV; 1516A) and near-ultraviolet (NUV; 2267A) bands. The Atlas was prepared by A. Gil de Paz,S. Boissier, B.F. Madore, M. Seibert and associated members of the GALEX Team. The full paper is posted on astroph/0606440 and will be published in ApJS in 2007.
The Interplanetary Network (IPN) is a group of spacecraft equipped with gamma-ray burst detectors used to localize gamma-ray bursts (GRB) and soft gamma repeaters (SGRs, or magnetars). The astronomical locations of GRBs are determined by the comparison of the arrival times of the event at the locations of the detectors used on different space missions. The precision is proportional to the distance of spacecraft separations, so that the localizational accuracy of a network with baselines of thousands of light-seconds can be equal or superior to that of any other technique. The primary disadvantage of the IPN method, however, is the 1-day to 1.5-day delay in the acquisition of data from all the spacecraft in the network. Interplanetary GRB networks have been in existence since 1977, contributing to the studies of various astrophysical gamma-ray transients, most notably GRBs and SGRs (soft gamma repeaters). The IPN3 began operations in 1990, with the launch of the Ulysses spacecraft. It was joined by the Compton Gamma Ray Observatory in 1991. Pioneer Venus Orbiter, Mars Observer, and the Italian X-ray astronomy satellite BeppoSAX were part of the network while they were operating. Twenty-six experiments or missions have joined the network so far. Today, the main spacecrafts contributing their data are Konus-WIND, Mars Odyssey, INTEGRAL, RHESSI, Swift, Agile, BepiColombo, and Fermi. XMM-Newton and MAXI are kept to record the cosmic ray and SGR but not used for triangulation because of the different energy range. The IPNGRB database table is derived from a list provided by Kevin Hurley <khurley@ssl.berkeley.edu>, based on the IPN3. The initial list also includes particles and solar events as well as unconfirmed SGRs and GRBs. The IPNGRB database includes only the observations of confirmed cosmic gamma-ray bursts and SGR since the launch of the Ulysses spacecraft. It is updated every time a new list is provided to the HEASARC. This HEASARC catalog is derived from the master list of IPN3 events provided by Kevin Hurley. He also provided a FORTRAN program that generates the list of selected events. The output of this program is run at GSFC and ingested into the HEASARC database system. Information on the IPN3 system is available at <a href="http://ipn3.ssl.berkeley.edu/">http://ipn3.ssl.berkeley.edu/</a>. <p> Information on the IPN can be found at <a href="http://heasarc.gsfc.nasa.gov/docs/heasarc/missions/ipn.html">http://heasarc.gsfc.nasa.gov/docs/heasarc/missions/ipn.html</a>. <p> In December 2021 Kevin Hurley passed away. He was one of the initiator of the IPN and its evolution. The last table provided is dated August 2021. This is a service provided by NASA HEASARC .
This database table contains the slightly revised contents of the detailed Tables 2A - 2G from the General Gamma-Ray Source Catalog of Macomb & Gehrels (1999). It lists details of all known gamma-ray observations within the energy range from 50 keV to ~1 TeV for 314 discrete gamma-ray sources that were listed in Tables 2A - 2G of the published version of this catalog, including all 310 sources listed in the published Summary Table 1, together with 4 sources (2CG 054+01, A0620-00, GX 340+0, and H1822-000) that were listed only in Table 2 of the published catalog but were (presumably accidentally) omitted from Table 1. The positions for the sources in the present database were taken from Table 1 of the General Gamma-Ray Source Catalog. Thus, this table is essentially a compilation of gamma-ray observations of discrete sources as known to the authors as of early 1999. There is another HEASARC database table called the Gamma-Ray Source Summary Catalog (Macomb & Gehrels 1999) or MGGAMMACAT that contains the summary information on these sources that was given in Table 1 of the General Gamma-Ray Source Catalog. As noted above, this is a slightly revised version compared to the published Tables 2A - 2G. The known differences between the HEASARC and published versions are discussed in the HEASARC_Version section of the help documentation. This database table was created by the HEASARC in March 2002 based upon machine-readable versions of Tables 2A-2G of the Macomb & Gehrels (1999) General Gamma-Ray Source Catalog that were supplied by the authors. One duplicate entry was removed from this table in June 2019. This is a service provided by NASA HEASARC .