All MAST catalog holdings are available via a ConeSearch endpoint.
This service provides access to all, with an optional non-standard parameter for an individual catalog to query.
The available missions are listed at http://archive.stsci.edu/vo/mast_services.html,
and include Hubble (HST) data, Kepler, K2, IUE, HUT, EUVE, FUSE, UIT, WUPPE, BEFS, TUES, IMAPS, High Level Science Products (HLSP), Copernicus, HPOL, VLA First, XMM-OM, and SWIFT.
All MAST catalog holdings are available via a ConeSearch endpoint.
This service provides access to all MAST holdings with positional information that have been ingested into the Common Archive Observation Model (CAOM) and its summarized ObsCore format. It provides access to the same data as the CAOMTAP TAP service, linked as an auxiliary resource.
Available missions are listed at http://archive.stsci.edu/vo/mast_services.html.
MAST SkyMapper Southern Survey Data Release 4 (SMSS DR4)
Short Name:
MAST SkyMapper
Date:
16 Apr 2024 20:18:39
Publisher:
Space Telescope Science Institute Archive
Description:
MAST hosts a copy of the SkyMapper DR4 catalog.
SMSS DR4 contains optical photometry in the 6 SkyMapper filters (u,v,g,r,i,z) for ~700 million astrophysical sources over 26,000 sq.deg, ranging from the South Celestial Pole to Dec=+16 degrees for objects with data in all bands, and some sources as far North as +29 degrees. The photometry is drawn from over 15 billion measurements made from more than 400,000 images acquired by the 1.3m SkyMapper telescope between March 2014 and September 2021. The typical 10-sigma depths for each field range between 18.5 and 20.5 ABmag, depending on the filter, but certain sky regions include longer exposures that reach as deep as 22 ABmag.
Compared to previous SkyMapper data releases, DR4 includes significant enhancements in data processing, most notably a new photometric calibration anchored to synthetic photometry from Gaia low-resolution spectroscopy, which resolves reddening- and spatial-trends identified in previous releases, especially in the bluest filters, u and v.
A large number of other photometric and spectroscopic surveys have been cross-matched to the dr4.master table of objects, to facilitate various scientific investigations.
Near Infrared Camera and Multi Object Spectrograph
Short Name:
HST.NICMOS
Date:
23 Jul 2020 19:50:23
Publisher:
Space Telescope Science Institute Archive
Description:
The HST Near Infrared Camera and Multi-Object Spectrometer (NICMOS) provides imaging capabilities in broad, medium, and narrow band filters, broad-band imaging polarimetry, coronographic imaging, and slitless grism spectroscopy, in the wavelength range 0.8-2.5 microns. NICMOS has three adjacent but not contiguous cameras, designed to operate independently, each with a dedicated array at a different magnification scale.
ASCA (Advanced Satellite for Cosmology and Astrophysics) is the fourth Japanese X-ray astronomy satellite launched on February 20, 1993 (see Tanaka et al., 1994PASJ...46L..37T) The collaboration between Japanese and US scientists has been carried out in the developments of the X-ray telescopes, the X-ray CCD cameras, and software. ASCA observed more than 3000 targets before stopping scientific observations as a consequence of a huge solar flare occured in mid July, 2000. ISAS continued monitoring operation until the ASCA reentered the atmosphere on March 2, 2001. Scientific instrumentation of ASCA consists of four X-ray telescopes and corresponding focal plane detectors. Focal plane detectors are two X-ray CCD cameras (SIS: Solid-state Imaging Spectrometers) and two Gas Imaging Spectrometers (GIS). With these detectors, ASCA covers the energy range of 0.5-10 keV. This catalogue is a copy of the ASCA Observation log from the Data ARchive and Transmission System (DARTS), provided by the PLAIN center at ISAS/JAXA, Japan. All the ASCA data have been public. The data is archived in a target-oriented (strictly speaking, observation-oriented) structure, i.e., all the data produced from an observation is put into a directory --- although some exceptions exist for observations in very early epoch. Each dataset includes telemetry data, data products (event files, images, energy spectra, light curves, etc.), and calibration data. ISAS provides the telemetry and calibration data, and ASCA data processing center in ADF (Astrophysics Data Facility) at NASA/GSFC reproduces the data products.
Our aims are to determine flux densities and their photometric accuracy for a set of seventeen stars that range in flux from intermediately bright (<~2.5Jy) to faint (>~5mJy) in the far-infrared (FIR). We also aim to derive signal-to-noise dependence with flux and time, and compare the results with predictions from the Herschel exposure-time calculation tool. We obtain aperture photometry from Herschel-PACS high-pass-filtered scan maps and chop/nod observations of the faint stars. The issues of detection limits and sky confusion noise are addressed by comparison of the field-of-view at different wavelengths, by multi-aperture photometry, by special processing of the maps to preserve extended emission, and with the help of large-scale absolute sky brightness maps from AKARI. This photometry is compared with flux-density predictions based on photospheric models for these stars. We obtain a robust noise estimate by fitting the flux distribution per map pixel histogram for the area around the stars, scaling it for the applied aperture size and correcting for noise correlation.
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.
The PHAT observations are grouped into 23 "bricks", each listed under a different proposal ID. Each brick consists of a 3x6 array of pointings, producing complete coverage in the UV, optical, and NIR. Each brick is observed as two 3x3 "half bricks", with observations taken ~6 months apart. In the first observing season, a 3x3 half brick of WFC3 pointings is completed in primary, while parallel observations produce a highly overlapping 3x3 tile of ACS observations in the adjacent half brick. After 6 months, the telescope can be rotated by 180 degrees from the original orientation, such that the primary WFC3 pointings cover the area that was tiled by ACS in the first season, and vice versa. Each pointing is observed for 2 orbits, using the 2 WFC3 cameras for one orbit each.
Filters: F275W+F336W (WFC3/UVIS), F475W+F814W (ACS/WFC), F110W+F160W (WFC3/IR)
Depth: UVIS data reach a magnitude limit of ~25 in F275W and F336W. ACS data reach maximum depths of ~28 magnitudes in F475W and ~27 magnitudes in F814W in the uncrowded outer disk. In these same regions, WFC3/IR data reach maximum depths of ~26.5 and ~25.5 in F110W and F160W, respectively. However, the depth is crowding limited in the optical and NIR, and thus is a strong function of radius. As a result, photometry in the inner bulge fields is far shallower.
All available catalogs are listed at http://archive.stsci.edu/vo/mast_services.html.
Pan-STARRS is a system for wide-field astronomical imaging developed and operated by the Institute for Astronomy at the University of Hawaii. Pan-STARRS1 (PS1) is the first part of Pan-STARRS to be completed and is the basis for Data Release 1 (DR1). The PS1 survey used a 1.8 meter telescope and its 1.4 Gigapixel camera (GPC1; see PS1 GPC1 camera) to image the sky in five broadband filters (g, r, i, z, y). The PS1 Science Consortium funded the operation of the Pan-STARRS1 telescope, situated at Haleakala Observatories near the summit of Haleakala in Hawaii, for the purposes of astronomical research. The PS1 consortium is made up of astronomers and engineers from 14 institutions from six countries.
The Pan-STARRS Data Release 1 Object Catalog "Best" filtered exists in the MAST holdings and is thus available through a cone search. The filtered data is a ~2billion row subset based on an object having more than 2 detections.
All available catalogs are listed at http://archive.stsci.edu/vo/mast_services.html.
Pan-STARRS is a system for wide-field astronomical imaging developed and operated by the Institute for Astronomy at the University of Hawaii. Pan-STARRS1 (PS1) is the first part of Pan-STARRS to be completed and is the basis for Data Release 1 (DR1). The PS1 survey used a 1.8 meter telescope and its 1.4 Gigapixel camera (GPC1; see PS1 GPC1 camera) to image the sky in five broadband filters (g, r, i, z, y). The PS1 Science Consortium funded the operation of the Pan-STARRS1 telescope, situated at Haleakala Observatories near the summit of Haleakala in Hawaii, for the purposes of astronomical research. The PS1 consortium is made up of astronomers and engineers from 14 institutions from six countries.
The Pan-STARRS Data Release 1 Object Catalog v3 exists in the MAST holdings and is thus available through a cone search.
All available catalogs are listed at http://archive.stsci.edu/vo/mast_services.html.
