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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, or search on HLSP metadata on a MAST Classic form here.
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HLSPs
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Listing Results
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.
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.
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.
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.
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.
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.
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).
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.
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.
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.
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.
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.
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.
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.
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.
alpha Ori Spectral Atlas (HST/GHRS)
ATLASALPHAORI is an ultraviolet atlas of Alpha Orionis (Betelgeuse) constructed by members of the HST Goddard High Resolution Spectrograph (GHRS) scientific development and calibration teams. This star was chosen because of extensive observations of it from ground-based spectrographs, photometers, and interferometers in the optical and IR spectral regions and because of the time coverage of its variations from ground sites and the IUE satellite by many observers. The spectral data were recorded on 1992 Septmber 24 using the GHRS Small Science Aperture (SSA). The atlas includes a number of plots of relative flux versus wavelength over the range 1979 to 3300 Angstroms. The data also include two-column ASCII files listing the wavelengths (in Angstroms) and flux (in units of 10^9 ergs cm^2/s/Angstrom).
Bianchi, Conti, Shiao (BCS) Catalog of Unique GALEX Sources
The GALEX spacecraft operated for over 10 years and surveyed nearly the entire sky during its lifetime. The telescope observed in both FUV (1344-1786 Angstroms) and NUV (1771-2831 Angstroms) simultaneously until May 2009, when the FUV detector failed. The NUV detector continued to operate until June 2013, when GALEX was retired and the mission ended. The standard GALEX data products at MAST include visit and coadd image files, as well as a source catalog produced by the GALEX reduction pipeline called the "MCAT". The MCAT consists of over 200 million source measurements, but, since it was run on each tile, there are multiple measurements of the same source due to tile overlaps and different surveys (AIS, MIS, DIS, Guest Investigator, etc.) To rectify the situation, Bianchi et al. have constructed a catalog of unique sources: one based on All-Sky Imaging Survey (AIS) tiles, and another based on Medium-Sky Imaging Survey (MIS) tiles. These catalogs are homogeneous in depth and quality, and are optimal for cross-matching GALEX UV fluxes with data in other bands (e.g., for source selection combining optical or IR data), or for Galactic and extragalactic population studies.
Catalogs of GALEX UV unique sources, and of UV-optical matched sources
Comprehensive catalogues of hot star candidates in the Milky Way, selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344GÇö1786 Angstroms) and near-UV (NUV; 1771GÇö2831 Angstroms) imaging. Sources are cross-matched with Sloan Digital Sky Survey Data Release 7.
Brightest of Reionizing Galaxies
The Brightest of Reionizing Galaxies (BoRG) observations were first obtained in HST Cycle 17 in program GO 11700 (PI: Michele Trenti) and continued in Cycle 19 with program GO 12572 (PI: Michele Trenti). BoRG is an ongoing pure-parallel program that obtains WFC3 imaging in four filters (F606W, F098M, F125W, F160W) on random sightlines at high Galactic latitudes (|b| > 30 degrees). BoRG also assimilates data from the similar Hubble Infrared Pure Parallel Imaging Extragalactic Survey (HIPPIES) pure-parallel program (GO 11702; PI: Yan) as well as the coordinated parallel observations acquired as part of the Cosmic Origins Spectrograph (COS) GTO program (GO 11519, 11520, 11524, 11528, 11530, 11533, 11534, 11541, 12024, and 12025).
ATLAS9 Model Atmosphere Database
BOSZ stellar atmosphere models are based on ATLAS-APOGEE ATLAS9, and cover a broad range of effective temperature, surface gravity, metallicity, carbon abundance, and alpha-element abundance. Versions at different instrumental broadenings are provided. The new BOSZ LTE models have been fit to O,B,A,F,G stars observed with HST/STIS, and those results are compared to fits for the LTE grid from Castelli & Kurucz (2004).
The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey
The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey, CANDELS (Grogin et al. 2011; Koekemoer et al. 2011), PI: S. Faber, Co-PI, H. Ferguson, is designed to document the first third of galactic evolution from z = 8 to 1.5 via deep imaging of more than 250,000 galaxies with WFC3/IR and ACS. It will also discover and characterize Type Ia SNe beyond z > 1.5 and establish their accuracy as standard candles for cosmology.
Carina Nebula
In early February 2010, mosaic images of the Herbig-Haro 901 and 902 (hereafter just HH 901) star formation sites were obtained using both the visible (UVIS) and infrared (IR) channels of the new Wide Field camera 3 (WFC3). The new WFC3 observations include four pointings in a 2x2 mosaic pattern, with small dithers within each pointing to fill the gaps between the two CCD chips, and allow for the rejection of cosmic rays and detector artifacts. A mosaic image was also obtained for a parallel field, using the Advanced Camera for Surveys. In 2005, a 43-orbit investment of Hubble observing time was awarded (HST proposals 10241 and 10475), to study the Carina Nebula in the light of Hydrogen-alpha. Although these observations cover only a small central part of the entire nebula, it resulted in one of the largest contiguous ACS images ever collected. Most of the observations are part of a large mosaic, centered on the star clusters Trumpler 14 and Trumpler 16. Many smaller nearby fields were also imaged, including the spectacular Herbig-Haro object HH666 and the nearby NGC 3324. In 2008, the Hubble Heritage Team also obtained WFPC2 mosaic data for NGC 3324 (HST proposal 11800) with the [O III] and [S II] filters (F502N and F673N).
Photometric Catalogs Surrounding Nearby Core-Collapse Supernovae
CCSNE (HST Proposal #14786) is a high-precision, photometric survey of areas surrounding historic, nearby core-collapse supernovae. The catalogs are used to infer the initial masses of the progenitors by fitting stellar evolution models to the color-magnitude distributions of the resolved stellar populations near the supernovae. Each area is observed in two filters, either F606W+F814W, F435W+F606W, or F438W+F606W. The drizzled mosaics and source catalogs are provided for all the observed fields.
chi Lupi (B9.5 pHgMn) Spectral Atlas (HST/GHRS)
A major, eight-year investigation of the extraordinarily detailed ultraviolet spectrum of the sharp-lined, non-magnetic, main-sequence chemically peculiar star chi Lupi (B9.5pHgMn + A2Vm) was undertaken as a GHRS GTO team project. The UV observations are comprised of 345 Angstroms of the spectrum acquired with the Goddard High Resolution Spectrograph on board the HST, at an average resolution of 0.023 Angstroms. The team provides an online version of their reduced data, as well as the synthetic spectra and line identification lists used to produce the figures in Brandt et al. (1999).
Cluster Lensing And Supernova survey with Hubble
By observing 25 massive galaxy clusters with HST's panchromatic imaging capabilities (Wide-field Camera 3, WFC3, and the Advanced Camera for Surveys, ACS), CLASH will accomplish four primary science goals. The CLASH Multi-Cycle Treasury program (12065 PI: Marc Postman) observed 25 clusters over a three-year period. The team was awarded a total of 524 orbits of HST to conduct this program, and provide images, catalogs, and lens models.
An ACS Treasury Survey of the Coma cluster of galaxies
The HST ACS Coma Cluster Treasury Survey is a deep, two-passband imaging survey of one of the nearest rich clusters of galaxies, the Coma cluster (Abell 1656, HST Proposal 10861). While HST data were obtained with both the ACS and NICMOS instruments, only the ACS data are included in this release. The survey was designed to cover an area of 740 square arcmin in regions of different density of both galaxies and intergalactic medium within the cluster. The ACS failure of January 27th 2007 left the survey 28% complete, with 21 ACS pointings (230 square arcmin) completed, and partial data for a further 4 pointings (44 square arcmin).
CoolCAT - A cool-star UV spectral catalog
COOLCAT is a catalog of HST STIS Echelle spectra of normal, late-type (cool) stars. The catalog includes those objects in the HST archive as of March 2003 with publicly available STIS data taken in one or more of the Echelle modes. Unusual objects like cataclysmic variables, symbiotics, and eclipsing binaries of the Zeta Aurigae class were excluded. For each Echelle observation, the individual orders from the standard pipeline processing were spliced together to form a continuous 1-D spectrum. Each spectrum was graded on a scale of A (=excellent) to E (=probably useless for analysis) by considering the cumulative distribution of signal-to-noise over the wavelength bins. If more than one observation was available in a specific Echelle mode setting, these were coadded using cross-correlation to align the exposures to a common wavelength scale. If two or more different mode settings were available, the segments were concatenated to form a broad-band spectral tracing. The flux scales of the segments were adjusted, if necessary, to match calibrated IUE NEWSIPS low- and high-resolution spectral energy distributions (as available).
Copernicus Atlases of 6 Selected Stars
During the Copernicus mission several stars were observed intensively with the high-resolution spectrometers to obtain as complete wavelength coverage as possible. Ultraviolet high resolution spectral atlases were constructed for six stars: Alpha CMa (Sirius), Alpha Lyr (Vega), Beta Ori (Rigel), Gamma Peg, Iota Her, and Tau Sco.
Cosmic Evolution Survey
COSMOS (P.I. Nicholas Scoville) is an HST Treasury Program to survey a two square degree equatorial field, centered on RA=10:00:28.6 and DEC=+02:12:21.0 with the ACS in the I band of the VIMOS equatorial field. Parallel observations with WFPC2 and NICMOS were also obtained. Several HST programs are associated with this project: (9822; 9999; 10092; 10337; 10702). The team has also assembled several publically available ancillary datasets including optical spectra, deep XMM and VLA imaging, ground-based optical/IR imaging, UV imaging from GALEX and IR data from SIRTF. MAST has archived the ACS, WFPC2, NICMOS and GALEX science products from the COSMOS project.
A Cataclysmic Variables and Related Objects Ultraviolet Spectral Catalog
A catalog of Far Ultraviolet Spectroscopic Explorer (FUSE) spectra of cataclysmic variables (CVs) and related objects (ROs). For each object there is (i) at least one FUSE spectrum, (ii) possibly a theoretical fit spectrum (when the continuum can be modeled sucessfully), and (iii) basic data about the system including figures and downloadable ASCII tables. The catalog includes all CV types and sub-types, such as dwarf novae (U Gem, Z Cam, SS Cyg, WZ Sge and SU UMa sub-types), nova-likes (VY Scl/anti-DN, UX UMa, SW Sex sub-types), magnetic systems (IPs, Polars, DQ her, AM Her sub-types). In addition, the catalog also includes miscellaneous ojbects related to CVs such as novae (all types of novae), symbiotics, and some pre-cataclysmic variables.
A Catalog and Atlas of Cataclysmic Variables
The Catalog and Atlas of Cataclysmic Variables (2001, PASP 113, 764) is a web-based version of the team's previously published catalogs (Downes and Shara 1993, PASP 105, 127; Downes, Webbink, and Shara 1997, PASP 109, 345). The data in this version supersedes that in the published catalogs, and contains the latest information on the objects. The catalog was frozen on February 1, 2006, and no new information will be added.
Deep HST ACS Imaging of 47 Tuc and the SMC
Kalirai et al. have observed the globular cluster 47 Tucanae for 121 orbits using the Advanced Camera for Surveys. These extremely deep images were taken in two filters: F606W (broad V-band) and F814W (I-band). Using these observations, Kalirai et al. were able to construct one of the deepest and most complete color-magnitude diagrams of a stellar population, probing down to 30th magnitude and extending from the faintest end of the main sequence to the coolest white dwarf members. As an added bonus, members of the Small Magellanic Cloud represent background sources, and these observations are able to resolve SMC targets down to 0.2 solar masses. The team have released their stacked ACS mosaics (FITS files), source catalog (ASCII text table), and artificial source lists (ASCII text table) used for testing photometry, astrometry, and completeness, as High Level Science Products.
Dusty Interacting Galaxy GADGET-SUNRISE Simulations
DIGGSS is a database of simulated galaxy merger images and associated "data" products. These simulations were created and analysed with the support of HST Theory Programs 9515, 10678 (PI Joel Primack), 10958, and 11759 (PI Patrik Jonsson). The galaxy merger simulations were produced by the N-body/SPH code GADGET (Springel & Hernquist 2002). For the details of the GADGET simulations, please refer to Cox et al. 2006, 2008. The GADGET simulations were then processed through the Monte-Carlo radiative transfer code SUNRISE (v2) to produce mock SDSS-g band images at 11 different viewing angles, including the effects of dust and new star-formation. For details of the SUNRISE code, please refer to Jonsson 2006. Finally, the mock SDSS g-band images were convolved with a PSF and added to noise map to simulate real observations. The non-parametric morphologies (Gini coefficient, M_20, Asymmetry, Concentration, Petrosian radii) and projected galaxy separations of the final images were measured by Lotz et al. 2008, 2010a, 2010b. For definitions of the non-parametric morphologies, please refer to Lotz et al. 2004.
Catalogs of B-, V-, and i-band dropout sources
Beckwith et al. (2006) have prepared catalogs of dropout sources for the GOODS North, GOODS South, and the Hubble Ultra Deep fields based on the original projects source catalogs.
HST Treasury Program on Eta Carinae
Kris Davidson is the PI for an HST Treasury Program that observed Eta Carinae. Two HST programs were associated with this project: 9420 and 9973. Data from other programs have also been included for the creation of this data set, including: 7302, 8036, 8327, 8483, 8619, 9083, and 9337. The project has produced a series of technical memorada that detail processing techniques, definitions, mathematical considerations and other details. Although the treasury program was designed to obtain data during an anticipated spectroscopic event in mid-2003, this star and its ejecta have unique characteristics that make them important to several branches of astrophysics. Observations were obtained using the HST STIS/CCD, STIS/MAMA, WFCP2 and ACS images. Currently only the STIS/CCD observations have been released by the team.
EUV Spectral Atlas of Stars
A table containing EUVE (Extreme Ultraviolet Explorer Data) spectra of 94 stars selected by Craig et al. (1997). The list is roughly representative of the sample of stars by the EUVE project during its lifetime (1992-January 2001). The EUVEATLAS contains EUVE (Extreme Ultraviolet Explorer Data) spectra of 94 stars selected by Craig et al. (1997). The list is roughly representative of the sample of stars by the EUVE project during its lifetime (1992-January 2001). These spectra were taken whenever possible with all the three bandpasses, short- (SW; 70-190 Angstroms), medium- (MW; 140-380 Angstroms), and long-wavelength (LW; 280-760 Angstroms). The spectral resolutions for these cameras are 0.5, 1, and 2 Angstroms, respectively. The stars are organized in a table by spectral type and by subcategories within each type. It is important to point out that the spectra in this atlas were only the best available at the time of the compilation. In some cases, longer exposures were made after the atlas was constructed (late in the mission lifetime) and are available in the HEASARC/MAST archives.
EPIC Variability Extraction and Removal for Exoplanet Science Targets
EVEREST is an open-source pipeline for removing instrumental systematics from K2 light curves, using a combination of pixel-level decorrelations to remove spacecraft pointing error and Gaussian processes to capture astrophysical variability. Corrected light curves have precision comparable to the original Kepler mission for targets brighter than Kp = 13, and within a factor of 2 for fainter targets. Transit injection and recovery tests have been performed to validate the pipeline, and comparisons with other K2 detrended HLSPs is performed (consult the Luger et al. 2016 paper for further details).
Formation History of Ultra-Faint Dwarf Galaxies
FHUFD (HST Proposal 12549) is a deep, high-precision, photometric survey of six ultra-faint dwarf galaxy satellites of the Milky Way, in order to discern any cosmologically-driven synchronization of their formation histories. For six ultra-faint dwarf satellites of the Milky Way (Bootes I, Coma Berenices, Canes Venatici II, Hercules, Leo IV, and Ursa Major I), the team provides ACS photometry, astrometry, and co-added (drizzled) images. The photometry and images are in two bands: F606W (broad V) and F814W (I), using the STMAG photometric system. The astrometry is given in equatorial coordinates (degrees, J2000). The drizzled images have a scale of 0.03 arcsec/pix. The images from each pointing are contained in their own FITS file. Each galaxy also has a single catalog file containing the point sources detected in the images.
AGN and Quasar Spectral Atlas (HST/FOS)
The FOS_AGN atlas provides spectral FITS data and preview files for all successful pre-COSTAR spectra using the Faint Object Spectrograph of AGNs (Active Galactic Nuclei). A discussion of the uniform flux and wavelength calibrations of these spectra, including common instrumental artifacts that can appear in FOS data, is given in Evans and Koratkar (2004). The data list includes 221 AGNs. Where possible, and in most cases, these spectra have been clipped at overlapping wavelengths and merged to form a panchromatic spectrum. The target list was compiled from a PI object description in the keywords denoted by "AGN", "quasar", "Seyfert", etc., as well as others designated by the PI as "galaxy" that should fit into these categories.
Frontier Fields
A new initiative of six deep fields centered on strong lensing galaxy clusters drawn from Abell et al. (1989) and the MACS survey (Ebeling et al. 2001), in parallel with six deep "blank fields" adjacent to these clusters.
Quasar Spectrum FUSE
This is a mean quasar spectrum from 630 to 1156 Angstroms, constructed from 128 FUSE observations of 85 AGNs with redshifts z < 0.67, as described in Scott et al. 2004 in the 1 Nov 2004 issue of The Astrophysical Journal.
FUSE Survey of Cataclysmic Variables
The FUSE Survey of Cataclysmic Variables (Froning et al. 2009) contains 178 FUSE observations of 99 targets. For each dataset, the data products were examined (images of the count rate and aperture placement for each exposure and extracted spectra for each observation) to identify any problems with the observation and to ensure that the pipeline correctly screened out bad time intervals. For time-tag data, the individual exposures in each segment were combined using the Calfuse tool "ttag_combine". Then the eight time-averaged segment spectra were combined into a single broadband spectrum using the IDL-based tool "fuse_analysis" provided on the FUSE website. Using the overlapping wavelength regions, the spectra were cross-correlated to correct for small wavelength offsets between channels and then combined the spectra, weighting by the error bars in each channel. Bad spectral regions were screened out as needed. The time-averaged spectra were binned to 0.1 Angstroms. Finally, spectra from different observations were combined if they were acquired close in time and if there were no gross changes in the spectrum between observations. The survey is described in the paper by Froning et al. 2012.
FUSE Atlas of Starburst Galaxies
The FUSE Atlas of Starburst Galaxies contains far-ultraviolet spectra of 24 nearby galaxies that were studied in the context of spectral synthesis by Pellerin (2004, PhD. Thesis, Universite Laval) and Pellerin & Robert 2007. The data are optimized for the study of stellar populations and can be useful in several contexts such as multiwavelength studies of young stellar populations. The data can be used as templates for high redshift galaxies. The galaxies were observed through the 30x30 arcsec (large) science aperture, except for NGC 5253 which has been observed through the 4x20 arcsec (medium) aperture. The data have been resampled to a resolution of 0.127 Angstroms/pixel (15-20 km/s). The final spectra were constructed with simple coadditions.
OB Stars (Galactic): FUSE Spectral Atlas
The first of the two FUSE data catalogs contains an atlas of far-ultraviolet spectra of 45 OB (O2-B3) stars in the Galaxy (see Pellerin, Fullerton, Robert et al. 2002; ) for the spectral region 920-1180 Angstroms. All data were obtained through the 30+ù30 arcsec (large) science aperture. The original data resolution and reciprocal spectral dispersion were 15-20 km/s and 0.062-0.067 Angstroms/pixel, respectively. The data were further resampled to 0.12 Angstroms/pixel for this atlas. Most spectra were obtained in a series of back-to-back exposures. Tests indicated that apparent wavelength shifts among them are less than half a resolution element. The final spectra were constructed with simple coadditions.
OB Stars (Magellanic): FUSE Spectral Atlas
This catalog serves data for 47 OB stars in the Large and Small Magellanic Clouds (see Walborn et al. 2002). This spectral atlas covers essentially the same spectral type and luminosity ranges in the FUSE_GALOB HLSP. The same observing configuration was used as for the other atlas. However, for this atlas the data have been rebinned to steps of 0.25 Angstroms. The primary difference is that the spectra are less attenuated below 1000 Angstroms by Galactic ISM and H2 extinction. The continuum is fully rectified (flat) and normalized to unity, bringing the conditioning of FUSE data to its fullest potential for immediate analysis purposes.
FUSE Magellanic Clouds Legacy Project
The FUSE Magellanic Clouds Legacy Project provides a products for those interested in the stellar and interstellar characteristics of the Magellanic Clouds, as discernible from the high resolution far ultraviolet spectral data obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite. Over its eight years in operations, FUSE was used to observe 187 hot stars in the Large Magellanic Cloud (LMC) and 100 hot stars in the Small Magellanic Cloud (SMC). The FUSE data for all objects have been reprocessed with CalFUSE 3.2, the archival version of the FUSE calibration pipeline software. The pipeline software is described in detail by Dixon et al. 2007. For each star, the FUSE data are shown in several standardized ways, highlighting a key set of interstellar absorption lines on an aligned velocity scale, showing a broader spectral section from 1028 - 1042 Angstroms that highlight the important O VI 1032 Angstrom region, and a compressed overview of the entire FUSE band that highlights the general characteristics of the stellar spectrum. In addition, the summary page for each object includes optical and infrared sight line context images, allowing further insights into the characteristics of each sight line. The optical data are from the Magellanic Cloud Emission Line Survey (MCELS) project, and the infrared images are from the Spitzer Space Telescope, with LMC data from the SAGE Survey of Meixner et al. and the SMC data from the S3MC Survey of Bolatto et al.
FUSE Spectral Atlas of Wolf-Rayet Stars
The FUSE Wolf-Rayet Atlas is taken from the paper by Willis et al. 2004. This paper presents full FUSE wavelength coverage for 21 Wolf-Rayet stars distributed among WN and WC types and located in the Galaxy or either of the Magellanic Clouds. As in other FUSE MAST HLSP O-star atlases, the emphasis in the companion paper (see Willis et al. 2005) and in the figures included herein is in the presentation of data for many resonance lines from ions spanning a wide range of ionization potential. The data were obtained through the 30 X 30 arcsec (large) science aperture. The data have been processed beyond the pipeline stage to produce a single merged spectrum for each star. The post-processing steps include suppression of nightglow emission lines (by using only orbital-night data for these wavelengths), correction for the LiF1B channel "worm" by using continuum information from the LiF1A channel, use of guiding channel fluxes and generated errors to assign relative weights to fluxes in wavelength regions where channel data overlap, and a binning of the data to 0.1 Angstroms (15 pixels). The resulting spectra have a signal to noise in the range of 20 to 50 per wavelength bin. The wavelength scales of the spectra are heliocentric. No attempt has been made to rectify the stellar continuum fluxes.
Detailed Far-UV Spectral Atlas of B Main Sequence Stars
The Far-UV Spectral Atlas of B stars (Smith 2010) contains high resolution data in the far-UV wavelength region (defined here as the range 949-1225 Angstroms) for 10 B stars near the main sequence. The spectrum for type B0 is taken, with permission from the author, from the still classic Copernicus satellite atlas of tau Scorpii (Rogerson and Upson 1977). For all other types the spectra were obtained from the MAST/FUSE data archives (Far Ultraviolet Spectroscopic Explorer) in the range 949-1188 Angstroms, and from the archives of either the HST/STIS or IUE archives for wavelengths above 1188 Angstroms. Whenever both data sources were available the STIS spectrum was selected. With respect to the data in the MAST archives, the altas spectra are enhanced, first, in that wavelength irregularities for the FUSE Side 1 and Side 2 spectra have been removed to the greatest extent possible and corrections made for the stars' radial velocities. The spectra were then resampled to restore the wavelength zeropoints and increments of the original spectra. Second, the depressed fluxes in the FUSE 1B LiF detector segment due to the primary "worm" have been corrected by means of the quasi-continuum fluxes in the 2A LiF segment. Third, a star/ISM flag vector was added to the FITS files to designate those wavelengths for which the fluxes are dominated by local molecular hydrogen lines.
Detailed Far-UV Atlas of O Main Sequence Stars
The Far-UV Spectral Atlas of O Stars (Smith 2012) contains high resolution data in the far-UV wavelength region (defined here as the range 930-1188 Angstroms) for 25 O stars in the Galaxy and Magellanic clouds between spectral types O2 and O9.5, obtained from the MAST FUSE data archives. The star list consists of three parallel spectral type sequences, Galactic main sequence (luminosity classes III-I), Galactic supergiants, and low metallicity stars in the Small or Large Magellanic clouds. FITS data files of 25 stars are provided, comprised of merged spectra in each of the two FUSE detector sides, each representing the spectrum sampled in the original wavelength sampling (0.075 Angstroms). Of these stars, six spectral templates were chosen for detailed study. The identified lines are all the photospheric and Interstellar Medium atomic and molecular features in the far-UV spectrum. These lists were compiled from line synthesis of model atmospheres appropriate to the stars' spectral types from a theoretical and empirical set of line libraries. The atlas spectra are enhanced with respect to the data in the MAST archives, first, in that wavelength irregularities for the FUSE Side 1 and Side 2 spectra have been removed to the extent possible and corrections made for the stars' radial velocities. The spectra were then resampled to restore the wavelength zeropoints and increments of the original spectra. Second, the depressed fluxes in the FUSE 1B LiF detector segment due to the primary "worm" have been corrected by means of the quasi-continuum fluxes in the 2A LiF segment.
A Correction to the GALEX Spectral Fluxes Using CALSPEC and IUE
GALEX-FLUXCAL is a collection of 18 IUE spectral energy distributions (SEDs) on the CALSPEC scale that provide a correction to GALEX spectral fluxes. This HLSP also includes the correction in 50 Angstrom bins from 1300 - 3000 Angstroms. While GALEX spectrophotometry is repeatable to only 10-20% in regions of good sensitivity, the average flux correction presented here has a precision of ~3%.
GALEX Atlas of Nearby Galaxies
The GALEX Atlas of Nearby Galaxies was prepared by A. Gil de Paz, S. Boissier, B.F. Madore, M. Seibert and associated members of the GALEX Team. The team presents images, integrated photometry, surface-brightness, and color profiles for a total of 1034 nearby galaxies observed by the GALEX satellite in its far-ultraviolet (FUV; 1516 Angstroms) and near-ultraviolet (NUV; 2267 Angstroms) bands.
GALEX Unique Source Catalogs
GALEX undertook a number of surveys covering large areas of the sky at a variety of depths. However, making use of this large data set can be difficult because the standard GALEX database contains all of the detected sources, which include many duplicate observations of the same sources, as well as numerous spurious low signal-to-noise sources. At the same time, the sky footprint associated with GALEX observations has not been well defined or presented in an easily usable format. Seibert et al. have constructed three catalogs of GALEX unique source measurements; namely the GALEX All-Sky Survey Source Catalog (GASC), the GALEX Medium Imaging Survey Catalog (GMSC), and the Kepler GCAT. The team's intention is that these catalogs will provide the primary reference catalog useful for matching GALEX measurements with other large surveys of the sky at other wavelengths.
GEMS: Galaxy Evolution from Morphologies and SEDs
GEMS is a large-area (800 arcmin^2) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the Hubble Space Telescope. Centered on the Chandra Deep Field-South, it covers an area of ~ 28'x28', or about 120 HDF areas, to a depth of MAB(F606W) = 28.5(5-sigma) for compact sources. In its central ~1/4, GEMS incorporates ACS imaging from the GOODS project. Focusing on the redshift range ~ 0.2 < z < 1.1, GEMS provides morphologies and structural parameters for nearly 10,000 galaxies where redshift estimates, luminosities, and SEDs exist from COMBO-17. At the same time, GEMS contains detectable host galaxy images for several hundred faint active galactic nuclei. The science goals, the experiment design, the data reduction, and science analysis plan for GEMS are described in Rix et.al. (2004).
Galaxy Halos, Outer disks, Substructure, Thick disks and Star clusters Survey
The GHOSTS survey (P.I. Roelof de Jong, Space Telescope Science Institute) provides HST analysis of extra-planar stellar populations of nearby disk galaxies (programs 9765, 10523, and 10889). The survey provides HST analysis of extra-planar stellar populations of nearby disk galaxies. Using deep ACS, WFPC2 and WFC3 images the project targets several edge-on galaxies covering a range of masses (Vrot = 80-260 km/s).
Grayscale of Time Variations of gamma Cas Near SiIV Doublet (HST)
GHRS_GAMMACAS is an ultraviolet grayscale timeseries of difference spectra for gamma Cas in the neighborhood of the SiIV resonance lines. The spectral data were recorded for over 21 hours while gamma Cas was in HST's continuous viewing zone on 1996 March 14-15 using the GHRS 2 arcsecond Large Science Aperture (LSA). The observations covered 1045 out of a total of 1280 minutes. The data were obtained at a cadence of one spectrum per second in the ACCUM mode (8100 counts per second per pixel) with the G160M grating and were later rebinned to 1 spectrum per minute. The ACCUM mode permitted only a modest resolution (30 km/s) but provided the ability to integrate fluxes unobstructed by an aperture and construct a pseudo-continuum light curve from "non-line pixels". The spectral range covers approximately 1382--1417 Angstroms. Several instrumental effects had to be removed to obtain the final spectra. These effects included included fixed pattern noise artifacts from the detector, differential spacecraft velocities, and shifts of the spectrum in both detector coordinates caused by changes in the Geomagnetic field (so-called "GIMP") as the spacecraft traced its orbit. Photometric variations 140 pixels to the red of the Si IV line complex were removed and are presented as a separate data file. Finally, a maximum-spectrum template was obtained from the spectra by submtracting the maximum flux at each pixel from each spectrum of the time series. The data shown are from difference spectra from that template in units of continuum = 1. The spectra were taken as part of a simultaneous campaign with the RXTE satellite and contemporaneously with IUE and optical observations two months earlier.
Grism Lens-Amplified Survey from Space
GLASS is a cycle-21 large program (Program 13459) with the Hubble Space Telescope, targeting 10 massive clusters, including the 6 Frontier Fields, using the WFC3 and ACS grisms. The program consists of 140 primary orbits (with the G102 and G141 grisms) and 140 parallel orbits (with the G800L grism). Using the clusters as cosmic telescopes, GLASS obtains spectra of faint background galaxies with enhanced sensitivity and angular resolution.
GOODS: The Great Observatories Origins Deep Survey
GOODS unites extremely deep observations from NASA's Great Observatories, ESA's XMM-Newton, and the most powerful ground-based facilities, to survey the distant universe to the faintest flux limits accross the broadest range of wavelengths.
GOODS NICMOS Archival Data
As a part of the HST 10937 Archival Research proposal, PI Rychard Bouwens and colleagues retrieved and process nearly all NICMOS Camera 3 F110W and F160W data taken over the GOODS North and South fields. All data were process using the NICMOS data reduction pipeline "NICRED". The NICRED pipeline includes nine processing steps from basic calibration to generating final co-added registered mosaics. Among these nine steps are procedures for successfully handling three of the most common NICMOS anomalies: electronic ghosting, the pedestal effect and cosmic-ray persistence.
Grism-ACS Program for Extragalactic Science
GRAPES is a project which was conducted in the Hubble Ultra-Deep Field (HUDF) during HST Cycle 12, over the period 2004 September to 2005 January. Sangeeta Malhotra is the PI for proposal 9793 for which 40 orbits were allocated. Slitless spectra in the Ultra-Deep Field were obtained with the Advanced Camera for Surveys (ACS) with the Wide Field Camera (WFC) over the field of 204x204 arcsec. The G800L grism provides slitless spectra with a dispersion of about 40 Angstroms per pixel. The release constitutes 1400 1D extracted spectra from the GRAPES dataset that were selected to have i < 27.0 mag.
GALEX-SDSS-WISE Legacy Catalog
GSWLC is a catalog of physical properties for 700,000 galaxies with SDSS redshifts z < 0.3, using data from GALEX, SDSS, and WISE. The galaxy properties (stellar mass, dust attenuation, star formation rates) are obtained via UV/optical SED fitting using a Bayesian framework. The catalog contains galaxies within GALEX footprints regardless of a UV detection. Mid-IR star formation rates are derived from WISE 22 micron data.
Hubble Deep Field
The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image a typical field at high galactic latitude in four wavelength passbands as deeply as reasonably possible. In order to optimize observing in the time available, a field in the northern continuous viewing zone (CVZ) was selected and images were taken for 10 consecutive days, or approximately 150 orbits. Shorter 1-orbit images were also obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground-based telescopes. The observations were carried out from 18-30 December 1995, and the data are available to the community for study.
Hubble Deep Field South
A second Hubble Deep Field campaign was carried out between late September and October of 1998. The field is located in the Southern Continuous Viewing Zone. As was the case for HDF-N, approximately 150 consecutive orbits were devoted to a single telescope pointing. Additional flanking field observations were made surrounding the deep STIS, WFPC2 and NICMOS fields. The raw, pipeline calibrated and reprocessed data were released to the community on November 23, 1998. The rationale for undertaking a second deep field campaign followed from the wealth of information that has come out of HDF-N, and from the desire to provide a point of focus for similar studies of the distant universe from southern-hemisphere facilities. The wide public access to the HDF-N data stimulated extensive followup observations across the electromagnetic spectrum, both from major ground-based observatories and from other satellites.
Hubble Deep UV Legacy Survey
The HDUV is a 132 orbit imaging program with the WFC3/UVIS camera onboard the Hubble Space Telescope (HST) designed to obtain deep UV images in the F275W and F336W bands over a total area of ~100 arcmin^2 in the central parts of the two GOODS/CANDELS-Deep fields (Grogin et al. 2011). The survey was approved in HST Cycle 22 (program 13872). This image release also includes all the F275W imaging data taken by the CANDELS survey, which were not previously available as high-level science products due to alignment difficulties. Similarly, to facilitate the most efficient scientific exploitation this release incorporates the UVUDF v2.0 data release from Teplitz et al. (2013) and Rafelski et al. (2015).
Hubble Helix Observations
For the 14 hours of peak Leonid meteoroid flux in November 2002, the Hubble Space Telescope was pointed away from the radiant, and the solar arrays were oriented to minimize their cross-section. By coincidence, one of the nearest and largest planetary nebulae, the Helix Nebula (NGC 7293), was nearly opposite the incoming Leonids and could be observed. A Hubble Helix Team of volunteers, led by Margaret Meixner (STScI), organized a nine-orbit campaign to observe the Helix with the ACS, WFPC2, NICMOS, and STIS. A contiguous 3x3 grid of 4k by 4k-pixel ACS images covering much but not all of the Helix was exposed in two filters, Ha+[N II] (F658N) and [O III] (F502N). The WFPC2 images, obtained in parallel, covered portions of the nebula in [O I] (F631N), He II (F469N), or Ha (F656N). NICMOS/NIC3 observations were obtained at two locations on the nebula and two off NICMOS/NIC3 observations were obtained at five locations on the nebula and four off. A few of the STIS parallel observations in [O II] (F28X50OII) were located on the nebula, but most were located off the nebula.
Hubble Heritage Project
The Hubble Heritage Project and MAST maintain this repository of high-level science products associated with some of the Heritage press releases. These are the scientific data (in FITS format) used to create the Heritage color composite press release images. The data has been expertly prepared, significantly beyond the standard pipeline processing. This usually involves careful image registration, combination, and cleaning via drizzling, making it a ready for further scientific analysis and educational use. These data are typically made available at the time of the associated press release, and each include a README file with data reduction details. Their inclusion as MAST High-Level Science products (HLSP) also means these data can be found via MAST archive queries.
Hubble Infrared Pure Parallel Imaging Extragalactic Survey
HIPPIES utilizes long-duration pure parallel visits (~> 3 orbits) of HST at high Galactic latitude (|b| > 20 degrees) to take deep, multi-band images in WFC3 (since Cycle 17) and in ACS (starting Cycle 18). HIPPIES relased its best-effort, high-level image products derived from all these three programs (PIDs 11702, 12286; and 11700) after each set (i.e., field) of observations were finished, using the best HST reference files available at the time of data reduction. HIPPIES DR1 only involves the data taken in Cycle 17 by programs 11702 and 11700. These two programs used both the infrared (IR) and the UV-optical (UVIS) channels of WFC3. The IR images were taken in the same three bands in both programs, namely, F098M, F125W and F160W. Program 11702 used F600LP, while program 11700 used F606W. A few fields were observed by both programs, and thus have UVIS images in both F600LP and F606W.
The HLA Star Cluster Project
Compact star cluster catalogs are presented for 20 nearby, star-forming galaxies using observations from the Advanced Catalog for Surveys (ACS) and source lists generated by the Hubble Legacy Archive. A typical cluster luminosity function can be approximated by a power-law, with an average value for the index of -2.37 and rms scatter = 0.18. The uniform database provided by these HLA catalogs results in a small scatter (0.5 magnitude) in the correlation between the magnitude of the brightest cluster (M_brightest) and log of the number of clusters brighter than M_I = -9 (log N).
Hubble Legacy Fields
The Hubble Legacy Fields project combines exposures from Hubble's two main workhorse cameras (ACS/WFC and WFC3) for the GOODS-South (ECDF-S) region from the HST archival program AR-13252. The observations were taken over more than a decade between mid-2002 to the end of 2016. The HLF includes essentially all optical (ACS/WFC F435W, F606W, F775W, F814W and F850LP filters) and infrared (WFC3/IR F098M, F105W, F125W, F140W and F160W filters) data taken by Hubble over the original CDF-South region including the GOODS-South, CANDELS, ERS, ECDF-S and many other programs. Given that this dataset combines all images in the archive on the CDF-S to date, the AR proposal identified the product under the global name "Hubble Legacy Field". Given the large area, a global astrometric solution was bootstrapped from the smaller datasets. All the image mosaics have been produced using the same tangent point as the original GOODS-S dataset. The total incorporated in the HLF-GOODS-S is 5.8 MSec in 7211 exposures from about 2442 orbits.
Hot Star Extension to the Hubble Space Telescope Stellar Spectral Library
We present 41 low resolution spectra of 40 stars from 0.2 micrometers (ultraviolet) to 1.0 micrometers (near infrared) with excellent fluxing. The stars include normal O-type stars, helium-burning stars, and post-asymptotic giant branch (PAGB) stars. Spectra were obtained with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST) using three low resolution gratings, G230LB, G430L, and G750L. Cosmic ray hits and fringing in the red were corrected. A correction for scattered light was applied, significant only for the coolest stars. Cross-correlation was used to bring the spectra to a common, final, zero velocity wavelength scale. Finally, synthetic stellar spectra were used to estimate line of sight dust extinction to each star, and a five-parameter dust extinction model was fit, or a one-parameter fit in the case of low extinction. These spectra dovetail with the similar Next Generation Stellar Library (NGSL) spectra, extending the NGSL's coverage of stellar parameters, and extending to helium burning stars and stars that do not fuse.
HST/NICMOS Paschen-alpha Survey of the Galactic Center
The HPSGC survey maps out a region of 2253 pc^2 (416 arcmin^2) around the central supermassive black hole (Sgr A*) in the 1.87 and 1.90 micron narrow bands with a spatial resolution of 0.01 pc (0.2 arcsec full width at half-maximum) at a distance of 8 kpc.
Hubble Ultra Deep Field 2009
Hubble Ultra Deep Field 2009 (HUDF09) program observations, obtained as HST program 11563 (PI: Garth Illingworth) in Cycle 17. The program uses WFC3/IR as the prime instrument for 192 orbits to image the deep ACS fields that were obtained in the original HUDF (PI: Steven Beckwith) program and in the HUDF05 (PI: Massimo Stiavelli) program.
Hubble Ultra Deep Field 2012
The Hubble Ultra Deep Field 2012 program (HUDF12: Ellis et al. 2013; Koekemoer et al. 2013) is a large HST program awarded 128 orbits (HST Program ID 12498; PI: R. Ellis), designed to probe the contribution of early galaxies to cosmic reionization. Specifically, these observations quadruple the exposure time of F105W on the UDF main field by adding 72 new orbits to data obtained previously in program ID 11563 (PI: G. Illingworth; see Bouwens et al. 2011), as well as providing 30 orbits in the completely new F140W filter, and providing an additional 26 orbits of depth in the F160W filter.
The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters.
The Large Legacy Treasury Program (GO-13297, PI: G. Piotto, 131 orbits) is a UV-initiative proposal to complement the existing F606W and F814W database of the ACSGGCT (GO-10775, PI: A. Sarajedini, 134 orbits) by imaging a large sample of clusters through UV/blue WFC3/UVIS filters F275W, F336W and F438W. Because these three filters are sensitive to C, N, and O abundance variations, it is possible to disentangle and characterize multiple populations in globular clusters. Combination of these UV/blue filters with the optical ones also gives the opportunity to measure the helium content of each population. The resulting final database contains catalogs and astrometrised stacked images of 56 globular clusters and one open cluster observed during the GO-13297 (PI: Piotto) and the two pilot projects: GO-12311 (PI: Piotto) and GO-12605 (PI: Piotto). For each cluster there are three catalogs, one for each photometric method adopted. The catalogs contain information on the positions and on the photometry in five bands (F275W, F336W, F438W, F606W, and F814W) of each star found in the cluster field. The catalogs also include membership probability.
Calibrated First-Order HUT Spectra of White Dwarfs G191-B2B and HZ 43
During the Astro-1 mission, an aluminum filter was used to block first-order light, and two white dwarfs (G191-B2B and HZ 43) were observed in second order. The flux from these second-order observations were then subtracted from the first-order spectra of these two objects. This was the only time that such second-order corrections were applied to HUT spectra, because no second-order observations were obtained during Astro-2. Because these spectra are in a different format compared to the rest of the HUT data products on MAST, they are provided here as an HLSP.
Survey of High Redshift 3C Radio Galaxies and Quasars
Hz3C is a project that observed 22 high-redshift (1 < z < 2.5) 3C radio galaxies and QSO's with HST WFC3 in the rest-frame UV and IR. A custom data reduction strategy is used to remove cosmic rays, persistence signal, and other data artifacts to produce high-quality images of the targets and their local environments. Both F606W and F140W observations are available in FITS format. The observed targets include those with regions of UV emission indicating active star formation.
Survey of the Low-Redshift Intergalactic Medium with HST/COS
A survey of the low-redshift intergalactic medium (IGM) has been performed by Danforth et al. (2015). Using HST COS spectra of 82 UV-bright AGN, several thousand absorption lines are identified from 2,610 distinct redshift systems at z < 0.723. The spectral features were selected and measured using a semi-automated analysis to minimize bias in line identification. For each of the 82 sightlines, a coadded, continuum-fitted spectrum is provided in FITS format. Two catalogs for each sightline are presented: one catalog lists the identified spectral features sorted by wavelength, while another lists the absorption features associated with IGM systems sorted by redshift.
A Galaxy Redshift Survey near HST/COS AGN Sight Lines
Keeney et al. (2018) present a galaxy redshift survey around 47 sight lines to UV-bright AGN observed by the Cosmic Origins Spectrograph (COS) in order to establish the connection between galaxies and UV-detected absorption systems in the local Universe. The collection of UV-detected absorption systems was released previously as a MAST HLSP ("IGM"; Danforth et al. 2015). IGM-GAL releases the galaxy spectra obtained as a part of this survey for ~9,000 individual galaxies whose redshift we measured. For most sight lines this survey is >90% complete to ~0.1 L* galaxies within ~1 Mpc of the sight line. Repeat observations imply that this survey has a redshift accuracy of 60 km/s for emission-line galaxies, 100 km/s for absorption-line galaxies, and 80 km/s for composite galaxies that show both emission and absorption.
Simulated Deep Survey Images
The Illustris Project conducts cosmological simulations of galaxy formation. By projecting a line of sight through a periodic volume, the team constructed realistic mock surveys which preserve the predicted geometry of the simulations. The Illustris Project consists of hydrodynamical simulations of galaxy formation in a volume 106.5 Mpc across, with detail resolved down to sub-kpc scales. Using the Arepo code, Illustris applied galaxy physics consisting of cooling, star formation, gas recycling, metal enrichment, supermassive black hole growth, and gas heating by feedback from supernovae and black holes. Three mock ultra deep fields, each 2.8 arcminutes across, in common wide filters used by HST, as well as in filters expected to be used widely by observers with JWST and WFIRST are provided. For HST and JWST simulations, the team provides images with and without convolution by model PSFs. For each image, the team also provides the simulation catalog from which they generated each image, enabling users to locate sources, link them to intrinsic simulation quantities, and conduct analyses across observation and theory space.
Comet C/2012 S1
A comprehensive set of Hubble Space Telescope (HST) observations of Comet ISON. Hubble Heritage program 13229 imaged the comet on 8 May 2013, using a Wide Field Camera 3 (WFC3) subarray which is half of one of the two CCDs (2K x 2K subarray). Eight identical 171-second exposures were obtained, with one dither step to mitigate bad pixels. The long-pass F350LP filter was used to maximize the signal-to-noise in one orbit. A small offset from the nominal aperture was applied to optimally position the comet and tail within the field of view. Another orbit on 30 April 2013 obtained deep fixed-pointing images of a field with Comet ISON in it, released July 16, 2013. Further details about the Heritage Comet ISON observing program are contained in the Phase II observing program.
CALSPEC-Calibrated IUE White Dwarfs
IUE-FLUXCAL is a collection spectral energy distributions (SEDs) for six white dwarfs in the HST CALSPEC database that are also observed by IUE. Composite IUE SEDs of each white dwarf are constructed by co-adding available low-resolution NEWSIPS spectra. The published paper compares the IUE to CALSPEC in 20 Angstrom bins for SWP and 40 Angstrom bins for LWP or LWR. A global average of these binned ratios across all six white dwarfs define corrections to the IUE NEWSIPS flux scale. This HLSP provides the co-added IUE SEDs of the six white dwarfs, as well as the table of IUE-to-CALSPEC flux ratios required to calibrate IUE data onto the HST standard scale.
White Dwarf Spectral Atlas: High dispersion IUE
An atlas of IUE Echelle spectra for a total of 55 white dwarfs has been created by Jay Holberg and collaborators. The project seeks to increase the signal-to-noise of white dwarf spectra by combining all observations of a given target into a single, epoch-combined spectrum.
Pre-Main Sequence Stars: IUE Spectral Atlas
This spectral catalog contains coadded IUE low-resolution spectra (from standard NEWSIPS MXLO files) of every T Tauri star (TTS) and candidate Herbig Ae/Be (HAEBE) star with useful IUE data. Processing and analysis procedures are described in Valenti, Johns-Krull, & Linsky (2000) for short wavelength (SW) data (1150-1980 Angstroms) and in Valenti, Fallon, and Johns-Krull (2003) for long wavelength (LW) data (1900-3200 Angstroms). The dereddened main-sequence templates used in the analysis of HAEBE stars are also presented. Coadded SW and LW spectra have been spliced together, when both are available, using the full extent of the lower noise SW segment.
Standard Stars: IUE
The team used the International Ultraviolet Explorer (IUE) Observatory to build a stellar atlas in the UV. The three installments of the UV stellar spectral atlas are given in Wu et al. (1983, 1991, 1997). Wu et al. (1992) further provides the archival data for stars, clusters, and galaxies which are not given in the above installments. This HLSP delivers the final products of the Complete UV Atlas of Standard Stars Project. It provides the IUE NEWSIPS (New Spectral Image Processing System) MXLO (Low-Dispersion Merged Extracted Image FITS File) spectra (graphics and wavelength-flux table) of 514 stars, grouped in two atlases.
K2 Galactic Archeology Program
K2GAP DR1 provides asteroseismology results (numax and dnu) for K2 Campaign 1 for the Galactic Archaeology Program (GAP) red giant targets. Targets were chosen to have (J-K) > 0.5 and H < 13.1 in an effort to choose red giants, many of which should exhibit solar-like oscillations with frequencies less than the ~30-minute cadence of K2 in Long Cadence mode. The catalog provides the asteroseismology parameters numax and dnu from six pipelines. The team have released their version of K2SFF detrended light curves, where a boxcar high-pass filter, 4-sigma outlier rejection, and linear interpolation over gaps are performed. They also provide a catalog of the asteroseismic parameters and preview plots of the power spectra for each target.
K2 Systematics Correction
K2SC is a K2 light curve detrending tool that uses Gaussian processes (GPs) to robustly model the systematics due to the Kepler telescope pointing jitter together with the astrophysical variability. The K2SC-detrended light curves are especially suited for studying variable stars in K2 photometry (by allowing us to remove the position-dependent systematics while keeping time-dependent variability intact), and searches for transiting planets (by allowing us to remove both the systematics and astrophysical variability). The detrended light curves available here consist of three components: position-dependent trend, time-dependent trend, and residual (detrended) flux.
K2 Extracted Lightcurves
The lightcurves from K2 contain larger systematics than the original Kepler mission, due to the reduction in pointing precision as a result of having to rely on only two reaction wheels. Vanderburg & Johnson have created a technique to correct for the pointing-dependent nature of the pixel-level fluxes. This correction improves the photometric precision by typical factors of 2-5, and results in median photometric performance of K2 targets to within a factor of two of the original, 4-wheeled mission. The team have released their extracted lightcurves (using a variety of photometric apertures), as well as diagnostic plots, for each target. The FITS lightcurves include all data points (with flags to indicate thruster firing), as well as multiple versions (each FITS extension is an extracted lightcurve for a different aperture). There are a total of twenty apertures provided: ten circular and ten based on the pixel response function. The final extension contains the summed image from all the postage stamp frames.
Astrometrically Calibrated Images of Cluster Regions Observed by K2
The K2SUPERSTAMP project consists of image data on four open clusters observed by the NASA K2 Mission. The clusters are M35, M67, Ruprecht 147, and NGC 6530 -- the Lagoon Nebula Cluster (referred to here as the Lagoon). While data for these regions were previously released by K2, it consisted of small (~50x50) target pixel file stamps. In this release, the K2SUPERSTAMP team have stitched together all small stamps for each region to create one larger image for every epoch, and subsequently fit a world coordinate system (WCS) solution to each resulting FITS file. With these products it is now possible to identify any and all stars in these open cluster regions via their right ascension and declination. Most stars that fell across the edge of the target pixel files now have spatially continous data. Each file corresponds to a single timestamp at the 30 minute long cadence of K2, and may be read in via standard FITS handling programs (e.g. IRAF and Python/astropy). This format enables the production of time series photometry for cluster stars.
K2 Variability Catalog
The lightcurves from K2 contain larger systematics than the original Kepler mission, due to the reduction in pointing precision as a result of having to rely on only two reaction wheels. Armstrong et al. have created a technique to correct for the pointing-dependent nature of the pixel-level fluxes. The team have released their extracted lightcurves (using a photometric aperture defined by the brightness of the target), as well as three plots of the resulting lightcurves: extracted, detrended, and phase-folded. The team has also released a catalog of object classification derived using supervised and unsupervised machine learning.
Kepler Extra-Galactic Survey
The light curves from K2 contain larger systematics than the original Kepler mission, due to the reduction in pointing precision as a result of having to rely on only two reaction wheels. The KEGS project creates detrended light curves for extragalactic targets observed in K2. The team determines optimal apertures that take into account background light and confusing neighboring sources while also maximizing light of the galaxies. The team constructs their own cotrending basis vectors (CBVs) using the galaxies on each channel via a PCA analysis, solving for CBV coefficients alongside the sawtooth pattern coefficients introduced by the pointing drift. Supernovae are analyzed in a similar fashion, but the light curves before and after the events are used to solve for the CBV coefficients.The team have released their extracted light curves and diagnostic plots for each target. Five versions of the light curves are available for each target, using a different number of CBVs. Diagnostic plots are provided by the KEGS team that show each target on a given Kepler module as well. These plots can be used to check for similar variability between targets, which could be indicative of false positive variability caused by uncorrected systematics. The apertures used for each target are also available within the FITS files.
Kepler Objects
This HLSP contains the detrended Kepler light curve and ground-based follow-up data (radial velocities and line bisectors) for Kepler's first five exoplanet discoveries.
Revised Kepler Stellar and Exoplanet Properties from GaiaDR2
KG-RADII provides revised stellar and exoplanet properties from the Kepler mission based on parallaxes from Gaia Data Release 2. These catalogs provide more precise stellar sizes and evolutionary states for 177,911 Kepler stars, as well as revised radii and incident fluxes for 2123 confirmed and 1922 candidate exoplanets.
Howell-Everett UBV Photometric Survey of the Kepler Field
The Howell-Everett Kepler Field UBV Survey contains a list of 4,414,002 sources observed in a survey of the NASA Kepler Mission field using Johnson/Harris U, B, and V filters in the NOAO Mosaic1.1 Camera at the WIYN 0.9m Telescope on Kitt Peak. The survey data were taken from 206 slightly-overlapping pointings that cover 191 square degrees in each of the three passbands. The area covered includes almost the entire Kepler field plus areas between the Kepler CCDs and around the perimeter of the field. The survey is estimated to be complete to magnitudes as faint as U~18.7, B~19.3, and V~19.1, but varies with location. The mean bright limits for point sources are U=10.1, B=10.6 and V=10.5.
NICMOS Legacy Archive PSF Library (LAPL) And Cirumstellar Environments
NICMOS coronagraphy, with well-matched template Point Spread Function subtraction, probes the closest environments of occulted targets with the highest imaging sensitivity in intrinsically high contrast fields at the smallest radial distances afforded. To obtain the best results, suitable template PSFs required to produce high-fidelity, photometrically robust, high contrast coronagraphic images are needed. To remedy this situation, the team undertook a rigorous, homogeneous, and complete recalibration and analysis of the full archival set of raw NICMOS coronagraphic images (through HST Cycle 15) to create a Legacy library of template PSFs.
Legacy ExtraGalactic UV Survey
LEGUS is a Treasury Program that imaged 50 local (closer than 12 Mpc) galaxies in multiple colors with WFC3 and ACS. Because of the proximity of all targets, the galaxies will be resolved into their main components: stars, star clusters, and associations. Mosaic images as well as source catalogs are provided.
Hubble Space Telescope ACS mosaic images of M51, the Whirlpool Galaxy
In January 2005, the Hubble Heritage Team obtained a large four-color mosaic image of the Whirlpool Galaxy NGC 5194 (M51), and its companion NGC 5195, with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST). The resulting color composite image was released to the community on April 25, 2005 to celebrate Hubble's 15th anniversary. Since the M51 mosaics produced by the Hubble Heritage Team represent a significant investment of expert processing beyond the standard archival products, these drizzle-combined FITS have been released simultaneously as a High Level Science Product via MAST.
Hubble Space Telescope ACS mosaic images of M82
In March 2006, the Hubble Heritage Team obtained a large 4-color mosaic image of the M82 with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST). See 10776 PI: Matt Mountain) for details. The resulting color composite image was released to the community on April 24, 2006 to celebrate Hubble's 16th anniversary. Since the M82 mosaics produced by the Hubble Heritage Team represent a significant investment of expert processing beyond the standard archival products, these drizzle-combined FITS have now been released as a High-Level Science Product via MAST.
M83 Mosaics
Galaxy M83 (NGC 5236) is a face-on spiral galaxy with a starburst in its nuclear region and active star formation occurring throughout its spiral arms. The M83 mosaic project, led by William Blair (Johns Hopkins University) and archived as a High Level Science Product at MAST, created mosaics spanning seven fields using WFC3-UVIS and WFC3-IR. Two of the fields used in this project were obtained during Program 11360 (PI: R. O'Connell) in 2009, while the other five fields were obtained as part of Program 12513 (PI: W. Blair) in 2012. Each of the 15 filters across the seven fields are combined into a single mosaic of M83, although the Fields 1 and 2 include additional filters, and hence the mosaics for those contain only those two fields. All of the mosaics, however, are astrometrically aligned to a common reference.
Ultraviolet Images of Nearby Galaxies
This High Level Science Product consists of a pictorial atlas of UV (2300 Angstrom) images, obtained with the Hubble Space Telescope Faint Object Camera, of the central 22+ù22 arcseconds of 110 galaxies ( Maoz et al. 1996). The observed galaxies are an unbiased selection constituting about one half of a complete sample of all large (D>6 arcmin) and nearby (V< 2000 km/s ) galaxies. The team measured the integrated ~2300 Angstrom flux in each image, and classified the UV morphology. The UV and optical parameters are given in the tables provided.
Magellanic Cloud Planetary Nebulae
MCPN is a project based on Hubble Space Telescope (HST) imaging with STIS and WFPC2, and optical and ultraviolet slitless spectroscopy. With HST, Magellanic Cloud PNs can be resolved in their sizes and shapes, and their central stars can be detected. Planetary nebulae (PNs) are the gaseous relics of the outermost red giant layers, ejected as a superwind after the Asymptotic Giant Branch (AGB) phase. The importance of studying Magellanic Cloud Planetary Nebulae (MCPN) is twofold: it allows the determination of physical parameters of PNs and their central stars, since their distances are known (as opposed to Galactic PN distances, that suffer large uncertainties); and they are the ideal probes of stellar evolution in low-metallicity galaxies.
A Hubble Space Telescope gallery of merging galaxies
The HST 18th anniversary press release contains a large gallery of interacting and merging galaxies. In association with this press release, seven of these objects have been made available as MAST High-Level Science Products (HLSP). These data were originally acquired under HST programs 6276, 10592, 11091, 11092, 11095, 11956, and 11994.
HST Moving Target Pipeline
This archival collection of Hubble Space Telescope images of Solar System objects was specially prepared using a software package designed to handle images involving moving targets. This includes images of planets, natural satellites, asteroids, comets, etc, from several HST cameras (WFPC2, ACS, WFC3). The images are optimally resampled onto a common pixel scale, and are always oriented such that north is up for easy comparison between other images. The processing consists of three steps: artifact rejection (bad pixels, cosmic rays, star trails), image drizzling, and intensity scaling (for quick-look PNG images). This first release includes HST moving target observations from 1994 (after HST Servicing Mission 1) through August 2014.
Measurements of the Ultraviolet Spectral Characteristics of Low-mass Exoplanetary Systems
MUSCLES is a spectral survey of 11 low-mass, planet-hosting stars, 7 M and 4 K dwarfs. The spectra cover wavelengths from 5 Angstroms to 5.5 microns, with emphasis on high-energy radiation. Data sources for the various regions of the spectra include 1.) X-rays: Chandra/XMM-Newton and APEC models (Smith et al. 2001) 2.) EUV: Empirical scaling relation based on Lya flux (Linsky et al. 2014) 3.) Lyman alpha: Reconstructed from model fit to line wings (Youngblood et al., 2016) 4.) FUV - blue visible: HST COS and STIS 5.) Visible - IR: Synthetic photospheric spectra from PHOENIX atmosphere models (Husser et al. 2013).
Outer Planet Atmospheres Legacy
OPAL is a project to obtain long time baseline observations of the outer planets in order to understand their atmospheric dynamics and evolution as gas giants. The yearly observations from OPAL throughout the remainder of Hubble's operation will provide a legacy of time-domain images for use by planetary scientists. The project will ultimately observe all of the giant planets in the solar system (Jupiter, Saturn, Uranus, and Neptune) in a wide range of filters. The images are processed using an ellipsoid limb-fitting technique, with an additional fringe correction applied to the narrow-band filters only (e.g., FQ889N for Jupiter 2014-2015), which amounts to a few percent correction. Mosaics are created for each observed filter in a projection that spans 360 degrees of longitude.
The HST Treasury Program on the Orion Nebula Cluster
The Orion Nebula hosts the richest cluster of young pre-main-sequence stars within 1 kpc from the Sun and therefore represents an ideal laboratory to understand the process of star formation. The "ORION" HLSP is an HST Treasury Program on the Orion Nebula cluster (GO-10246, PI M. Robberto) that has obtained deep multi-color photometry of thousand of sources well into the brown-dwarf regime, complemented by a rich set of ancillary data from ground-based observatories.
Probing Evolution And Reionization Spectroscopically
PEARS is an HST program that was conducted in the GOODS North and GOODS South fields using the Advanced Camera for Surveys in Cycle 14. Observations were made during the period 2005 August 8 to 2006 February 17. Slitless spectra over both fields were obtained with the ACS Wide Field Camera (WFC) and the G800L grism over the 204x204 arcsec detector area. Short F606W images were also obtained to align to the GOODS astrometry and to provide the zero point of the slitless spectra. The G800L grism provides slitless spectra with a dispersion of about 40 Angstroms per pixel. The grism first order covers 5500-10500 Angstroms, with a peak sensitivity around 7500 Angstroms.
The Panchromatic Hubble Andromeda Treasury
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. 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. Each pointing is observed for 2 orbits, using the 2 WFC3 cameras for one orbit each. The filter pairs are F275W+F336W (WFC3/UVIS), F475W+F814W (ACS/WFC), and F110W+F160W (WFC3/IR).
K2 Extracted Lightcurves
POLAR is a new pipeline to reduce K2 Target Pixel Files into light curves, which includes an optimised aperture for each star and a decorrelation of the systematic noise. Our pipeline is optimised for bright stars for which spectroscopic follow-up is possible. We achieve a maximum precision on 6 hours of 6 ppm. The decorrelated light curves are searched for transits with an adapted version of the CoRoT alarm pipeline. The candidates were screened and the ones that appear real were fitted with a trapezoidal model in order to divide them into planetary candidates and eclipsing binary candidates.
Procyon (FV-IV) Spectral Atlas - Chromospheric Lines (HST/GHRS)
This HLSP consists of a short series of ultraviolet spectra of chromospheric lines of Procyon (F5 IV-V) constructed and published by Dr. Brian Wood and colleagues at the University of Colorado (see Wood et al. 1996). The F5 IV star Procyon was chosen because it is a nearby star with prominent chromospheric emission lines in its spectrum. The Wood et al. atlas consists of plots of absolute flux for seven wavelength bands ranging from Si III, Lyman-alpha, and N V lines near 1200 Angstroms to the Mg H/K lines near 2800 Angstroms.
Probabilistic Classifications of Unresolved Point Sources in PanSTARRS1
Using a machine learning model, Tachibana & Miller 2018 classified ~1.5 billion sources from the PanSTARRS1 (PS1) data release 1 as either resolved, extended objects or unresolved, point sources. This PS1 point source catalog (PS1-PSC) provides a probabilistic ranking of all sources with a score of 0 corresponding to extended objects and 1 corresponding to point sources. The classifications are based on morphological properties measured in the PS1 stack images, though not every source in PS1 has a classification (see the known caveats). It has been demonstrated that this method does a far better job of selecting stars and galaxies than a single hard cut on the difference between the PSF and Kron magnitudes (see Figure to the right). A full description of the catalog is described in Tachibana & Miller 2018. Data are available as direct download or via MAST CasJobs.
Catalogs of Cosmologically Useful Type Ia Supernovae from Pan-STARRS
The Pan-STARRS Supernova (PS1 SN) Cosmology data release contains light curves, host galaxy spectra, light curve parameters, distance measurements, and cosmology fitter input files that can be used to measure the dark energy equation of state using two PS1 SN datasets. The first dataset (Scolnic et al. 2018) is the Pantheon sample, which combines spectroscopically classified PS1 SNe Ia with Sloan Digital Sky Survey, SuperNova Legacy Survey, and Low-z SNe Ia. These SNe were used to measure the dark energy equation of state in Scolnic et al. (2018), who find a value of -1.026 +/- 0.041. The second dataset (Jones et al. 2018) includes 1,174 Pan-STARRS SNe without spectroscopic classifications. Approximately 95% of these data SNe are of Type Ia, with the remainder being Core-Collapse (CC) SNe. Jones et al. (2018) use a Bayesian methodology to marginalize over CC SNe in these data and, after combining the sample with low-z SNe Ia, measure the dark energy equation of state to be -0.989 +/- 0.057.
Quasar Spectrum HST/FOS
This is a mean quasar spectrum, between 350 and 3000 Angstroms, constructed from 284 FOS observations of 101 quasars with redshifts z > 0.33, as described in Zheng et al. 1997.
Reionization Lensing Cluster Survey
RELICS obtained HST infrared imaging of 41 massive galaxy clusters to efficiently search for brightly lensed high-redshift galaxies in time for JWST Cycle 1. The clusters include 21 of the 34 most massive known based on Planck data. Observations of each cluster are split into two epochs, enabling supernova searches in addition to our high-redshift and cluster science. For each cluster, the team observes up to 5-orbit depth with ACS and WFC3/IR. They obtain 3 orbits of ACS imaging in F435W, F606W, and F814W (minus existing archival imaging) and 2 orbits of WFC3/IR imaging in F105W, F125W, F140W, F160W. Five of the clusters require two WFC3/IR pointings. For the 19 clusters with no existing ACS archival imaging, the team also obtains 3-orbit images of blank parallel fields with WFC3/IR F105W, F125W, F140W, F160W (2 orbits) and WFC3/UVIS F350LP (1 orbit) to search for additional high-redshift candidates as in the BoRG and HIPPIES surveys.
Surveying the Agents of a Galaxy's Evolution
SAGE traces the life cycle of observable matter that drives the evolution of a galaxy's appearance. The study consists of Spitzer Space Telescope images of the Large Magellanic Cloud (SAGE-LMC) and the Small Magellanic Cloud and Magellanic Bridge (SAGE-SMC) in addition to Spitzer spectroscopy of the dust composition in the Large Magellanic Cloud (SAGE-Spec, 30 Doradus) and Small Magellanic Cloud (SMC-Spec). The emission from the coldest dust is traced by the Herschel Observatory in the imaging program HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) in the Magellanic Clouds. The source catalogs are available as a High Level Science Product.
Neptunes Dark Vortex
A new dark vortex was discovered on Neptune in 2015 observations by WFC3, as part of the OPAL program. A Mid-Cycle 23 program (GO-14492) confirmed the dark spot with higher SNR imaging, as described in a 2016 STScI press release. Data processing and HLSP formats are described in Wong et al. (2018) and in the README file on the project's HLSP webpage. OPAL 2017 images gave the final views of SDS-2017, as it seemed to fade away.
Spiral Galaxies
Holwerda et al. (2005) examined 32 HST/WFPC2 archival fields of 29 spiral galaxies (type Sab and later). The majority of the data are from the Cepheid distance scale Key Project. The explicit goal was to provide deep mosaics in both V- and I-band with a better sampling in order to identify background galaxies through the foreground disk.
Swift Optical/Ultraviolet Supernova Archive
SOUSA is a project to reprocess all Swift supernova data using Breeveld et al. (2012) zeropoints and applying time-dependent sensitivity correction on the same system. Data were originally retrieved from the HEASARC Swift archive, then searched on a given supernova's position to ensure all images of the field are obtained. A total of 253 supernova are included in this archive, each with multiple UVOT filters. The image portion of SOUSA is hosted at MAST as an HLSP.
Space Telescope A901/902 Galaxy Evolution Survey
STAGES is a a large area (~0.5x0.5 degree) survey of the complex Abell 901(a,b)/902 multiple-cluster system at z=0.165. An 80-tile imaging mosaic in F606W was conducted in Cycle 13 under GO program 10395 (PI: M. Gray). With multiwavelength data available from COMBO-17, HST, Spitzer, XMM-Newton, GALEX, 2dF and GMRT the survey goals include simultaneously linking galaxy morphology with other observables such as age, star-formation rate, nuclear activity, and stellar mass. The data products available at MAST include the reduced HST/ACS images for each of the 80 tiles in the F606W ACS mosaic, as well as postage stamps for all objects in the field and the complete output of GALFIT profile fitting.
STARBurst IRregular Dwarf Survey
STARBIRDS combines new and archival observations for 20 nearby, starburst and post-starburst dwarf galaxies from GALEX, Hubble, and Spitzer. The images are registered to a common world coordinate system, flux calibrated, and background-subtracted. A set of GALEX and Spitzer images are made available cropped to match the Hubble field-of-view, while another set of Hubble images are convolved with a 5-arcsecond point spread function and rebinned to the GALEX and Spitzer resolutions.
HST STIS Echelle Spectral Catalog of Stars
StarCAT is a catalog of high resolution ultraviolet spectra of objects classified as stars, recorded by Space Telescope Imaging Spectrograph (STIS) during its initial seven years of operations (1997-2004). StarCAT is based on 3184 echelle mode observations of 545 distinct targets, with a total exposure duration of 5.2 Ms. For many of the objects, broad ultraviolet coverage has been achieved by splicing together echellegrams taken in two or more FUV (1150-1700 Angstroms) and/or NUV (1600-3200 Angstroms) settings. In cases of multiple pointings on conspicuously variable sources, spectra were separated into independent epochs. In cases of nonvariable, or lightly variable, objects, different epochs were combined to enhance signal-to-noise (S/N).
STIS Next Generation Spectral Library (AR10659)
The Next Generation Spectral Library (NGSL) consists of spectra for 374 stars, all observed in the same way, and all spectra covering the spectral range, ~0.2-1.0 microns, at a resolving power R ~1000. As part of HST proposal AR 10659, the team worked to derive a wavelength-dependent correction to the slit throughput as a function of offset from the slit center, delivering Version 1 of the NGSL to MAST as an HLSP. In HST proposal GO/CAL 11652, the team derived an improved slit-throughput correction based on post-SM4 observations of a standard star (BD+75D325), which was stepped across the slit. In HST proposal AR 11755, the team incorporated the observed slit-throughput corrections in this new version of the Next Generation Spectral Library.
Data Products From TESS Data Alerts
The TESS mission successfully launched on 18 April 2018 and began science operations on 25 July 2018. Observations of science Sector 1 were performed from 25 July to 22 August, during which pixel data from nearly 16,000 objects were collected at two-minute cadence. These data were sent to the Science Processing Operations Center (SPOC) at NASA Ames for calibration, reduction, cotrending, and transit detection. The potential planet signatures, in the form of Threshold Crossing Events (TCEs), were reviewed by the TESS Science Office to identify targets for imaging and spectroscopic follow-up. A total of 44 high-quality planet candidates in Sector 1 were initially selected from the two-minute cadence data for follow-up observations by the TESS Follow-Up Program (TFOP). Additional deliveries of alerts are provided as more Sectors and multi-Sector searches are conducted by the team.
TESS-HERMES Spectroscopic Survey
The TESS-HERMES project is a spectroscopic survey using the HERMES multi-object instrument on the Anglo-Australian Telescope (AAT). So far, the survey has observed ~16,000 dwarf and subgiant stars in the southern TESS Continuous Viewing Zone (CVZ). Targets in the CVZ have overlap with every TESS sector, and thus will get a full 12 months of data. It also overlaps with the JWST CVZ, making these targets optimal for follow-up with that telescope. The TESS-HERMES project derives stellar properties (effective temperature, surface gravity, [Fe/H], v*sin(i), microturbulence, distance, extinction, mass, radius, ages) using a Bayesian approach, spectral analysis, and theoretical isochrones. This catalog of stellar parameters is available now, while the calibrated spectra are planned for a future release at MAST.
Search Field from a Search for Kuiper Belt Objects
The "TNO Search Field" images are the sidereally summed images of a search for trans-Neptunian objects (TNOs) using the Wide Field Camera of the HST/ACS instrument. The observations were taken under Cycle 11 program GO-9433. The TNO search consisted of approximately 96x400 s exposures in the F606W filter for each of six contiguous ACS fields of view. The exposures were spread over a 15-day period in Jan-Feb 2003, with a complex sequence optimized for the discovery of the slowly-moving TNOs. The images provided are the sidereal-image templates that were subtracted from the search-field exposures.
A FUV Atlas of Low-Resolution HST spectra of T Tauri Stars
This HLSP consists of a spectral atlas in the far-ultraviolet of 91 pre-main-sequence stars. Yang et al. (2012) describe data processing procedures and present flux measurements of strong emission features as well as correlation analysis of FUV and optical accretion diagnostics. The atlas mainly contains the STIS G140L spectra of 24 stars and ACS/SBC PR130L prism of 54 stars. The atlas also include the STIS E140M spectra of eight stars, the GHRS G160M grating of two stars, and the IUE SWP spectra of six stars.
Hubble Ultra Deep Field Follow-on
PI Massimo Stiavelli obtained an HST Cycle 14 (Program 10632), whose objective is to search for galaxies at z > 6.5 in the Hubble Ultra Deep Field. The program was conceived as a follow-on program to the Hubble Ultra Deep Field (HUDF) and was designed to obtain deep ACS (F606W, F775W, F850LP) imaging in the area of the original HUDF NICMOS parallel fields. In addition, deep NICMOS (F110W, F160W) images within the original HUDF field were made as simultaneous parallel observations.
Ultra Deep Field ACS-HRC Parallels
The ACS Ultra Deep Field (UDF) is a survey carried out using the Advanced Camera for Surveys (ACS) on HST. The UDF will consist of a single ultra-deep field (412 orbits in total) within the CDF-S GOODS area. Scientific drivers of the UDF include probing the tail of the reionization epoch, constraining the star formation history of the Universe, probing the faint end of the galaxy luminosity function, and tracking the origin, structure, and merger history of galaxies as they evolve onto and off the Hubble sequence. There is also a NICMOS companion survey designed to complete the image set with deep near-IR NICMOS images at 1.1 and 1.6 microns over a significant fraction of the UDF, providing a critical link between the HST ACS and SIRTF observations.
Ultra Deep Field - ACS-WFC
The ACS Ultra Deep Field (UDF) is a survey carried out using the Advanced Camera for Surveys (ACS) on HST. The UDF will consist of a single ultra-deep field (412 orbits in total) within the CDF-S GOODS area. Scientific drivers of the UDF include probing the tail of the reionization epoch, constraining the star formation history of the Universe, probing the faint end of the galaxy luminosity function, and tracking the origin, structure, and merger history of galaxies as they evolve onto and off the Hubble sequence. There is also a NICMOS companion survey designed to complete the image set with deep near-IR NICMOS images at 1.1 and 1.6 microns over a significant fraction of the UDF, providing a critical link between the HST ACS and SIRTF observations.
Ultra Deep Field NICMOS Parallels
The ACS Ultra Deep Field (UDF) is a survey carried out using the Advanced Camera for Surveys (ACS) on HST. The UDF will consist of a single ultra-deep field (412 orbits in total) within the CDF-S GOODS area. Scientific drivers of the UDF include probing the tail of the reionization epoch, constraining the star formation history of the Universe, probing the faint end of the galaxy luminosity function, and tracking the origin, structure, and merger history of galaxies as they evolve onto and off the Hubble sequence. There is also a NICMOS companion survey designed to complete the image set with deep near-IR NICMOS images at 1.1 and 1.6 microns over a significant fraction of the UDF, providing a critical link between the HST ACS and SIRTF observations.
Ultra Deep Field NICMOS-Treasury
The ACS Ultra Deep Field (UDF) is a survey carried out using the Advanced Camera for Surveys (ACS) on HST. The UDF will consist of a single ultra-deep field (412 orbits in total) within the CDF-S GOODS area. Scientific drivers of the UDF include probing the tail of the reionization epoch, constraining the star formation history of the Universe, probing the faint end of the galaxy luminosity function, and tracking the origin, structure, and merger history of galaxies as they evolve onto and off the Hubble sequence. There is also a NICMOS companion survey designed to complete the image set with deep near-IR NICMOS images at 1.1 and 1.6 microns over a significant fraction of the UDF, providing a critical link between the HST ACS and SIRTF observations.
Ultraviolet Imaging of the UDF and the HDF
Wavelength coverage of the Hubble Ultra Deep Field (HUDF) has been been extended with deep ultraviolet wavelength observations. Observations acquired with the ACS-SBC in the Far-UV (1500 Angstroms) and WFPC2 in the Near-UV (F300W) during execution of the HST Treasury program 10403 (PI Harry Teplitz). Included with this set of data are ACS/SBC observations of the Hubble Deep Field North.
Hyperspectra Images of Uranus with STIS
Uranus-STIS is a collection of hyperspectral cubes of Uranus, constructed from HST/STIS observations which were obtained in 2002, 2012, and 2015. These data cover half the extent of Uranus with a spatial sampling of 0.0277 arcsec/pixel, and a spectral coverage from 300.4GÇö1020.0 nm with a sampling of 0.4 nm/pixel. The data provided in this collection were obtained with the STIS 0.10 arcsecond long-slit, which was aligned with the planet's polar axis and stepped across the disk at intervals of 0.152 arcseconds from center to edge. This observing pattern was executed for both the G430L and G750L gratings. The data were pipeline processed, extracted, calibrated, and combined (see Sromovsky et al. 2018 and references therein), with the uniform spatial and spectral sampling noted above.
USNO-KEPLER Catalog
Karen Kinemuchi has provided this USNO-Kepler catalog, a table of every object in the USNO B1.0 catalog found within the Kepler field-of-view, covering roughly 105 square degrees in the sky. For convenience, the team omits stars that fall on the gaps between the CCD chips that make up the Kepler photometer. The data table has the proper motion information as well as the photographic plate magnitudes in approximate B, R and I passbands. The USNO B1.0 catalog has a confusion limit of V = 21st mag (Monet et al. 2003).
All-Sky Mapping of the UV Diffuse Radiation As Observed by GALEX
Jayant Murthy has created maps of the diffuse UV radiation, in both FUV and NUV bands, using the latest GALEX all-sky data release (GR6+GR7). Tables are provided of the diffuse radiation for each GALEX visit at a resolution of 2 arcminutes, organized by galactic latitude. In addition to the diffuse background fluxes in NUV and FUV, this HLSP also provides estimates of the geocoronal and zodiacal foreground emissions for each binned pixel. A separate text table provides the estimated foreground corrections, at the observation (coadd) level, for each tile by taking the weighted average of the geocoronal and zodical emissions at the visit level. Aitoff projections of both the FUV and NUV diffuse radiation (and its variance), along with a 100-micron emission map based on the Schlegel et al. (1998) dust maps, are provided in FITS format. Finally, a table of GALEX spacecraft telemetry used to generate these data products is included.
Swift Optical/Ultraviolet Telescope GRB Afterglow Catalog
The Swift Ultra-Violet/Optical Telescope (UVOT) gamma-ray burst (GRB) afterglow catalog greatly expands on the first Swift UVOT GRB afterglow catalog. This second catalog is constructed from a database containing over 120,000 independent UVOT observations of 538 GRBs first detected by Swift, HETE2, INTEGRAL, IPN, Fermi, and AGILE. The catalog covers GRBs discovered from 2005 Jan 17 to 2010 Dec 25. Using photometric information in three UV bands, three optical bands, and a "white" or open filter, the catalog provides positional, temporal, and photometric information for each burst, as well as Swift BAT and XRT GRB parameters.
Swift UVOT Serendipitous Source Catalogue
Version 1.1 of the Swift UVOT Serendipitous Source Catalogue has been produced by processing the data between 10th Jan 2005 and 1st Oct 2010. The data processing was performed at the Mullard Space Science Laboratory (MSSL, University College London, U.K.) using Swift FTOOLS from NASAGÇÖs High Energy Astrophysics Software (HEASOFT), with some customizing of the UVOT packages in order to get more complete source detection and to apply quality flags to the sources. The catalogue contains positions, photometry in three UV and three optical bands, morphological information and quality flags. The total number of observations included in the catalogue is 23,059, giving 6,200,016 sources of which 2,027,265 have multiple entries in the source table because they have been detected in more than one observation.
Ultraviolet-bright Quasar Survey
The UV-bright Quasar Survey (UVQS) first data release (DR1) for new z~1 active galactic nuclei (AGN) across the sky contains data products and results from ground-based optical spectra of 1040 AGN candidates, selected from GALEX UV and WISE NIR color criteria. The source list contains 217 previously unreported AGN with FUV < 18 mag and redshifts generally at z > 0.5. For each source, the database includes a FITS file of the flux-calibrated, one-dimensional spectrum, a PDF plot of the spectrum with the best-fit comparison model, a redshift determination, and a PDF plot of an optical image.
Ultraviolet Imaging of the HUDF with WFC3
The Hubble UltraDeep Field (UDF) previously had deep observations at Far-UV, optical (B-z), and NIR wavelengths, but only comparatively shallow near-UV (u-band) imaging from WFPC2. With this new UVUDF project (Teplitz et al. 2013), we fill this gap in UDF coverage with deep near-ultraviolet imaging with WFC3-UVIS in F225W, F275W, and F336W. The HLSP provides science quality mosaics, photometric catalogs, and improved photometric redshifts to enable a wide range of research by the community. Data were obtained in three observing Epochs, each using one of two observing modes. Epochs 1 and 2 together obtained about 15 orbits of data per filter, and Epoch 3 obtained another 15 orbits per filter.
A Comprehensive UV Spectral Linelist of White Dwarf G191-B2B
A team led by Simon Preval have created one of the most complete UV linelists of a white dwarf. Co-adding over 150 spectra from both HST STIS and FUSE, the team was able to identify nearly 950 absorption lines with equivalent widths as small as a few milli-Angstroms. They were able to identify every observed feature in the coadded FUSE spectrum, and nearly every feature in the coadded STIS spectrum. In addition to line identification, the team was able to measure abundances for 9 elements (C, N, O, Al, Si, P, S, Fe, Ni). At MAST, the team provides the complete linelist, as well as the spectra (both the individual and coadded versions).
WFC3 Galactic Bulge Treasury Program
The WFC3 Galactic Bulge Treasury Program provide WFC3 photometry, astrometry, proper motions, and co-added (drizzled) images for four fields in the Galactic bulge (Stanek, SWEEPS, Baade, and OGLE29). The photometry and images are in five bands: F390W (Washington C), F555W (V), F814W (I), F110W (J), and F160W (H), using the STMAG photometric system. The astrometry is given in pixel coordinates (matching the scale in the drizzled images) and equatorial coordinates (degrees, J2000). The drizzled images have a scale of 0.03 arcsec/pix, rotated with North at the top of each image.
Wide Field Camera 3 Early Release Science Program
WFC3 is a panchromatic camera that was installed in HST as part of Servicing Mission 4. WFC3 has two cameras covering, respectively, ultraviolet and visual wavelengths (200 to 1,000 nm; the UVIS channel) and near-infrared wavelengths (900 to 1,700 nm; the IR channel). The STScI director allocated ~210 orbits of Director's Discretionary time to the WFC3 SOC for challenging science programs designed to test key capabilities of both the UVIS and IR channels. These orbits were distributed between programs 11359 and 11360. The combined dataset from these programs is referred to as the "WFC3 Early Release Science (ERS) Program". The ERS products made available here are based on custom processing of the original dataset. In some cases, this involved the use of more contemporary calibration files than were publicly available at a given time. In others, the team employed specialized software to extract measurements of general interest from the images.
Wide Field Juno Coverage
WFCJ is a Hubble Space Telescope program that uses WFC3/UVIS to take regional- and global-scale images of Jupiter to complement ongoing observations by the Juno spacecraft in situ. In addition to maps of the planet in multiple filters, zonal wind profiles are also calculated and made available. Data are sorted based on "perijove" number (each periastron passage by the Juno spacecraft).
WFC3 Infrared Spectroscopic Parallel Survey
WISP is a large HST pure-parallel program using the WFC3 G102 and G141 grisms to obtain images, spectra, and catalogs of star forming galaxies between redshifts 0.5 to 2.5. The primary science goals are to measure the star formation history over the last ~10 billion years, probe galaxy clustering on Mpc scales at redshifts 1 < z < 2, constrain the evolution of dust extinction and metallicity as functions of mass and luminosity, and to conduct a serendeipitous search for highly luminous Lyman alpha emitters beyond redshifts z > 6. Currently there are 390 different fields with products available.
STScI Outreach Imaging
This is a collection of High Level Science Products produced by the Outreach Imaging Team at STScI. This team conducts observations primarily intended for high-impact press releases, often associated with Hubble's anniversaries or other special events. Although driven by outreach purposes, the team follows the same best practices for observing and data processing as any science program, and also provides their expertly-prepared data as High Level Science Products for archival research.
Hubble eXtreme Deep Field
The XDF includes all optical and infrared data taken by Hubble covering the original Hubble Ultra-Deep Field (HUDF) program, with just a few exceptions. Small amounts of data taken with unusual or rarely used filters and spectroscopic data are not included. The XDF also includes images which only partially cover the HUDF. The data used to generate the XDF were taken over the decade from mid-2002 to the end of 2012. The total exposure on the XDF is about 1.8 million seconds using data from Hubble's two main workhorse cameras, the Advanced Camera for Surveys Wide Field Channel (ACS/WFC) and the Wide Field Camera 3 InfraRed Channel (WFC3/IR). Substantial gains accrue from using all the ACS data taken over the decade since 2002, as well as from the improved processing techniques since the HUDF was released. The gains in the XDF are equivalent to adding about 180 orbits of data to the original HUDF dataset.