High Level Science Products are observations, catalogs, or models that complement, or are derived from, MAST-supported missions. These include Hubble (HST), James Webb (JWST), TESS, PanSTARRS, Kepler/K2, GALEX, Swift, XMM, and others. HLSPs can include images, spectra, light curves, maps, source catalogs, or simulations. They can include observations from other telescopes, or data that have been processed in a way that differs from what's available in the originating archive. Use the filters below to discover HLSP.



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Listing Results

Results: 148

A First Catalog of Variable Stars Measured by ATLAS

The ATLAS-VAR data release is a catalog of variable stars discovered from ATLAS data. The first data release, presented here, consists of variable stars identified from 1.4 x 108 stars down to a limiting magnitude of r ~ 18 that obtained a minimum of 100 observations during the first two years of ATLAS operations. A total of 4.7 million variable star candidates are detected, using a Lomb-Scargle periodogram and several variability metrics described in Heinze et al. (2018). The catalog is available though the MAST CasJobs SQL interface.

The ATLAS All-Sky Stellar Reference Catalog

ATLAS-REFCAT2 is an all-sky reference catalog containing nearly one billion stars down to apparent magnitude m ~19. The catalog includes PanSTARRS DR1, ATLAS Pathfinder, ATLAS re-flattened APASS, SkyMapper DR1, APASS DR9, Tycho-2, and the Yale Bright Star Catalog. Gaia DR2 serves as the source of the astrometric solution for ATLAS-REFCAT2, with typical systematic errors of < 5 mmag RMS, although this can be as much as 20 mmag near the Galactic plane. The ATLAS Pathfinder telescope was used to collect g,r,i photometry for stars brighter than the 14th magnitude bright limit of PanSTARRS, and to extend the reference system below -30 declination.

HST STIS Advanced Spectral Library

ASTRAL is a Hubble Space Telescope (HST) Large Treasury Project, whose aim is to collect high-quality ultraviolet spectra of representative bright stars utilizing the high-performance Space Telescope Imaging Spectrograph. In Cycle 18 (2010GÇô2011), ASTRAL focused on eight iconic late-type stars, devoting 146 HST orbits to the purpose. In Cycle 21 (2013GÇô2015), the program shifted gears to the warm side of the H-R diagram, to capture 21 diverse early-type objects with an allocation of 230 orbits. The main objective is to record the targets -- including well-known bright stars like Procyon, Betelgeuse, Sirius, and Vega -- with broad uninterrupted UV coverage (1150GÇô3100 Angstroms) at the highest signal-to-noise and highest echelle spectral resolution achievable within the alloted spacecraft time, and given a variety of observing constraints. These UV atlases have enormous interpretive value in their own right, and will complement efforts from ground-based observatories, which now routinely achieve comparably high resolution and S/N in optical and near-infrared spectra of bright stars.

WFPC2 Archival Parallels (Proposal 9540)

The Archival Pure Parallel Project processed and combined with state-of-the-art tools about 2,000 WFPC2 images, primarily in the wide UBVI filters, obtained in parallel with other HST instruments. The team produced combined, drizzled, cosmic-ray cleaned images for each pointing. These data can be used to address a wide range of science topics: measuring the cosmic shear on scales from 20 arcseconds to 2'; discovering ~ 50 starforming galaxies at z ~ 4; finding optical counterparts to AGNs in wide-area radio and X-ray catalogs; improving the determination of the scale length of the Galactic disk; and studying stellar populations down to 1 solar mass for about 25 separate lines of sight in the Magellanic Clouds. The images are being made available to the astronomical community for a wide variety of other investigations, thus helping realize the legacy of WFPC2 parallel images.

Auroral Planetary Imaging and Spectroscopy

Among the space-based UV observatories, the ESA/NASA Hubble Space Telescope (HST) intensively observed the outer planets (Jupiter, Saturn, Uranus) in the Far-UV (FUV) from 1993 up to now, providing thousands of images and spectra, often in the frame of combined observations with spacecraft dedicated to planetary exploration (Galileo orbiting Jupiter over 1995-2003, Cassini flyby of Jupiter in 2000, Cassini orbiting Saturn since 2004, New Horizons flyby of Jupiter in 2007, Juno in orbit around Jupiter since 2017) or Earth-based observatories (radio, IR, X-rays). Another Earth-based UV observatory is the JAXA Hisaki satellite which monitors solar system bodies on the long-term with spectro-imaging data in the Extreme UV (EUV) and FUV ranges since 2013. UV observations have also been carried in situ from spectro-imagers onboard the above-mentioned satellites. These observations now form rich databases, of interest for a a wide community, but whose use remains limited by the difficulty to access and use them. The Auroral Planetary Imaging and Spectroscopy (APIS) service aims at providing a free and simple access to processed, high-level, auroral data. Two databases can be queried by the APIS search interface so far: the primary one is built from the STSci archive of public HST planetary observations using the STIS and ACS spectro-imagers. More recently, the team have developed the possibility to query external databases such as Hisaki/EXCEED observations.

ACS Nearby Galaxy Survey

The ACS Nearby Galaxy Survey (ANGST) team undertook a systematic, complete, and carefully crafted imaging survey of all galaxies in the Local Universe outside the Local Group (GO-10915, DD-11307; PI:Dalcanton). The set of HLSP include binary FITS tables of photometry for the ANGST sample as defined in Dalcanton et al. 2009. Also included are associated reference images and raw photometry tables.

Archive of Nearby Galaxies: Reduce, Reuse, Recycle

A team headed by J. Dalcanton, K. Gilbert, and B. Williams have produced an archive of stellar photometry for non-Local Group galaxies within 5 Mpc, based on primary and parallel wide-filter UV and optical observations taken with ACS/WFC or WFPC2. This first release includes the ANGRRR Photometry Repository for 71 galaxies within 3.5 Mpc, which contains binary FITS tables of the stellar photometry. Also included are associated reference images and binary fits tables of the raw photometry.

Deep Optical Photometry of Six Fields in the Andromeda Galaxy

Using the Advanced Camera for Surveys on the Hubble Space Telescope, Thomas Brown (STScI) et al. obtained deep optical images reaching well below the oldest main sequence turnoff in six fields of the Andromeda Galaxy. The fields fall at four positions on the southeast minor axis, one position in the giant stellar stream, and one position on the northeast major axis. These data were obtained as part of three large observing programs (9453, 10265, 10816) designed to probe the star formation history of the stellar population in various structures of the galaxy.

Archival Legacy Investigations of Circumstellar Environments

The HST NICMOS instrument has been used from 1997 to 2008 to perform coronagraphic observations of about 400 targets. Most of them were part of surveys looking for substellar companions or resolved circumstellar disks to young nearby stars, making the NICMOS coronagraphic archive a valuable database for exoplanets and disks studies. The ALICE program is an HST Legacy program aiming at revaluing the NICMOS coronagraphic archive with improved detection limits, achieved with modern post-processing methods. Several advanced post-processing algorithms have been developed since 2007, making use of a library of on-sky science images to optimize starlight subtraction from a given dataset. The input data of the ALICE program are the non-polarimetric NICMOS data re-calibrated with observed dark frames and contemporary flat-field frames by the LAPLACE program, which represent 73% of the whole NICMOS non-polarimetric archive. The team delivered products for most of these LAPLACE data (15% were either bad acquisitions with the star not centered on the occulter, or data that couldn't align properly with a library, in grey in this database). To facilitate combination of these products with other surveys, the team has developed a standard FITS file format which provides all the necessary information for high-level analysis of high-contrast imaging datasets, and which aims at being compatible with any type of data (ground-based and space-based instrument, imaging, polarimetric, IFU data).

VLA-A Array AL218 Texas Survey Source Snapshots

The VLA-A Texas Survey consists of a sample of objects extracted in 1989 by Ray Lucas and Kenneth Chambers from the earlier Texas Interferometer 365 MHz Survey of radio sources covering a strip of sky from approximately -35.5 degrees declination to +71.5 degrees declination, and complete to flux densities of 0.25 Jy, with positional accuracies of ~1 arcsecond in RA and DEC. The Lucas and Chambers sample from 1989, which comprises the VLA-A Texas Survey is a subset of 71 sources drawn from the area of one optical Schmidt sky survey plate (covering ~6.5x6.5 degrees), Region S861, centered at approximately RA=190.640822109, DEC=-0.273834224277 (J2000), from the UK Schmidt SRC-J Survey. The Region S861 was initially chosen because it represented the combination of the deepest UK Schmidt plate material (the best optical survey material available at the time of our sample definition in 1989) and the highest galactic latitude, thereby emphasizing the extragalactic nature of the survey and also maximizing the likelihood of having more optical detections. Much more recently, the area of this plate has been covered by a number of important sky surveys including 2MASS, NRAO VLA FIRST, and the Sloan Digital Sky Survey (SDSS). In particular, the availability of the Sloan Survey data provides 5-band ugriz color information at optical wavelengths, to a depth of g,r=22.2.

The ACS Survey of Galactic Globular Clusters

The ACS Globular Cluster Treasury program (PI: Ata Sarajedini, University of Florida, HST Program 10775) used the ACS/WFC instrument on board the Hubble Space Telescope to obtain uniform imaging of 65 of the nearest globular clusters to provide an extensive homogeneous dataset for a broad range of scientific investigations. In June 2013, six new clusters were added to the archive from the HST program 11586.

Spectroscopic Galaxy Evolution Survey with HST

3D-HST is a near-infrared spectroscopic survey with the Hubble Space Telescope designed to study the physical processes that shape galaxies in the distant Universe. This Treasury program was allocated 248 orbits of HST time during Cycles 18 and 19, surveying ~600 square arcminutes of well-studied extragalactic survey fields (AEGIS, COSMOS, GOODS-S, UKIDSS-UDS) with two orbits of primary WFC3/G141 grism coverage and two to four orbits with ACS/G800L coverage. 3D-HST now provides the critical third dimension - redshift - for ~10,000 galaxies at z>1. This is the epoch when ~60% of the star formation in the Universe took place, the number density of quasars peaked, the first galaxies stopped forming stars and the structural regularity that we see in galaxies today emerged. The survey is optimally designed for the study of galaxy evolution over 1 < z < 3.5. The science objectives include: disentangling the processes that regulate star-formation in massive galaxies, evaluating the role of environment and mergers in shaping the galaxy population, and resolving the growth of disks and bulges, spatially and spectrally.

HST Snapshots of 3CR Radio Galaxies

The revised 3C catalogue (3CR, Bennett 1962) forms a flux-limited sample of the most radio-powerful sources in the northern hemisphere. Over the decade and a half of HST operation, a snapshot imaging survey from the near-IR to the near-UV of a large number of these sources has been conducted. Most recently the team has completed a NICMOS 1.6 micron survey of low-redshift (z<0.3) 3CR sources (Madrid et al. 2006, Floyd et al 2008). The fully-reduced data for all 101 sources included in those papers are presented here in numerical order. This includes 90 sources from the SNAP survey and a further 11 from the NIC2 archive.

Hubble Tarantula Treasury Project

HTTP is a panchromatic imaging survey of stellar populations in the Tarantula Nebula (30 Dor) in the Large Magellanic Cloud that reaches into the sub-solar mass regime (<0.5 M_solar). HTTP utilizes the capability of the Hubble Space Telescope to operate the Advanced Camera for Surveys and the Wide Field Camera 3 in parallel to study this remarkable region in the near-ultraviolet, optical, and near-infrared spectral regions, including narrow-band H alpha images. The high sensitivity, spatial resolution and broadband coverage of HTTP allow users to dissect the stellar populations and infer an accurate description of the anatomy of the Tarantula Nebula, and therefore to reconstruct for the first time the temporal and spatial evolution of a prototypical starburst on a sub-parsec scale.

10 Lac (O9V) Spectral Atlas (HST/GHRS)

An ultraviolet atlas of 10 Lacertae constructed by members of the HST Goddard High Resolution Spectrograph (GHRS) scientific development and calibration teams. The star 10 Lac was chosen because it is unique as a bright O (O9V) star exhibiting a very sharp-lined spectrum. As a member of the Lacerta OB1 association, the star is known to have a distance of about 600 pc. The atlas consists of a number of plots of relative flux versus wavelength over the range 1181 -- 1777 Angstroms. The data were recorded by 4:1 substepping the G160M (medium resolution) grating over an angle corresponding to one pixel at the detector. Each pixel corresponds to a spectral resolution element of about 15 km/s. Fluxes of "continuum pixels" range from 32,000 to 100,000 photon counts across the total spectral range, resulting in a signal-to-noise ratio in excess of 100. The data were recorded over a total time of about 5 hours on 6 November, 1992 through the small science aperture. Note that these observations were done before the installation of the COSTAR corrective optic element. Identifications are given in the atlas for 45 interstellar lines of 17 ions.