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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.  All HLSPs are public immediately with no proprietary periods.  Use the filters below to discover HLSP. Search HLSP by coordinates or filenames on MAST Classic. Or, see all HLSPs in a simplified, searchable table.


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Listing Results

Results: 225
Showing 15 matching items
  • The TESS Stellar Variability Catalog (TESS-SVC)

    The TESS Stellar Variability Catalog (TESS-SVC) describes which stars, among those observed at 2-min cadence in the TESS light curve photometry, show periodic variability over the timescales of 0.01 to 13 days. The TESS-SVC includes a broad range of periodic variable stars (rotation, pulsation, eclipsing binaries, etc.) that were selected based on the photometric periodogram analysis described in Fetherolf et al. 2023. Each star in the TESS-SVC includes the measured period of photometric variability, time and amplitude of the maximum flux, significance of the detected variability signal, properties extracted from the TESS Input Catalog, and a summary figure. Each summary figure shows the full TESS light curve (left panels), Lomb-Scargle periodogram or auto-correlation function (center panels), and the light curve phase-folded on the measured photometric variability period (right panels). The periodogram results provided are extracted from a single sector of TESS PDCSAP photometry, and the method for selecting the specific sector for stars observed in multiple TESS sectors is described in Fetherolf et al. 2023.

  • Beyond Ultra-deep Frontier Fields and Legacy Observations (BUFFALO)

    The Beyond Ultra-deep Frontier Fields and Legacy Observations program (BUFFALO, Steinhardt et al. 2020, HST Program ID 15117) is a 101-orbit Cycle 25 HST program of prime ACS/WFC + parallel WFC3/IR imaging around all 6 of the clusters in the Hubble Frontier Fields program (HFF, Lotz et al. 2017). The BUFFALO program significantly expands the area imaged around each HFF cluster by a factor of about 3-4 times, in a total of 5 filters (ACS/WFC F606W and F814W, and WFC3/IR F105W, F125W, and F160W). This additional area had not previously been extensively observed by HST but was already covered by deep multi-wavelength data sets, including Spitzer and Chandra. As with the original HFF program, BUFFALO is designed to take advantage of gravitational lensing from massive clusters to simultaneously find high-redshift galaxies that would otherwise lie below HST detection limits and model foreground clusters to study the properties of dark matter and galaxy assembly. The expanded area is providing the first opportunity to study both cosmic variance at high redshift and galaxy assembly in the outskirts of the large HFF clusters.

  • Lyman-alpha Reference Sample (LARS)

    The Lyman-a Reference Sample (hereafter, LARS) collection consists of HST observations of 45 star-forming galaxies at redshifts 0.03–0.24. The products consist of reduced images, line and galaxy property maps, and tables of photometric measurements. The data used mainly come from the two LARS HST imaging programs (PIDs: 12310 and 13483). Various instruments (ACS/SBC, ACS/WFC, and WFC3/UVIS) and filters have been used to image the Lyman-alpha/H-alpha/H-beta emission and characterize the stellar populations. Apart from the reduced images the collection also contains maps of emisison lines and of derived physical quantities such as stellar age, extinction, and mass for the galaxies. In addition the collection contains tables with global photometry of the galaxies and tables with surface brightness profiles for each galaxy.

  • Fireworks Ultraviolet Survey (FUVS)

    NGC 6946, otherwise known as the Fireworks Galaxy, is a nearby star-forming spiral galaxy with 10 supernovae observed in the past century. The Fireworks UltraViolet Survey (FUVS) is an imaging survey targeting the O and B stars in NGC 6946. The catalog contains resolved stellar photometry produced from high spatial resolution, near-UV images in Hubble Space Telescope's WFC3/UVIS F336W and F275W filters. This dataset was aligned using Gaia Data Release 2- the source IDs of the Gaia-matched sources are provided.

  • First Reionization Epoch Spectroscopically Complete Observations (FRESCO)

    The First Reionization Epoch Spectroscopically Complete Observations (FRESCO) program consists of spectroscopic and imaging observations designed to cover optimally the two CANDELS/Deep regions in the GOODS-South and -North fields, which are among the most valuable extragalactic legacy fields in the full sky. The core of FRESCO is NIRCam slitless grism observations, which result in a spectrum for every source in the field-of-view. FRESCO follows in the footsteps of numerous successful grism surveys conducted with HST but with greater sensitivity, at longer wavelength, and with spectral resolution a factor 10X higher. Three direct and out-of-field images were taken in the F444W filter to associate the spectra with individual galaxies.

  • The GLASS JWST Early Release Science Program (GLASS-JWST)

    The GLASS-JWST Early Release Science Program (hereafter GLASS-JWST ERS) has obtained the deepest observations of galaxies obtained of all Early Release Science Programs by targeting the Hubble Frontier Field, and in particular the lensing cluster Abell 2744. This high-level science product collection combines the GLASS-JWST NIRCam imaging data (ERS-1324) with NIRCam data from two other JWST programs targeting the same field: UNCOVER (GO-2561, PI: I. Labbé and R. Bezanson) and Program DD-2756 (PI: W. Chen).

  • The JWST Extragalactic Medium-band Survey (JEMS)

    The JWST Extragalactic Medium-band Survey (JEMS) is a deep Cycle 1 imaging survey program using 5 medium-band filters at 2 and 4 micron (F182M, F210M, F430M, F460M, F480M). With two NIRCam detector footprints (using all 5 filters) and one NIRISS imaging footprint (using F430M and F480M filters), the data total 15.6 square arcminutes with integration times 13915-27830 seconds, including full coverage of the Hubble Ultra Deep Field (HUDF), building on the deepest multi-wavelength public datasets available anywhere on the sky. These science-ready mosaics, which reach 5s point source limits (ABmag) of 29.2 in 2µm filters and 28.2-28.6 at 4µm. Our chosen filters create a JWST imaging survey in the UDF that enables novel analysis of a range of spectral features potentially across the redshift range of 0.3 < z < 20, including Paschen-a, Ha+[N II], and [O III]+Hbeta emission at high spatial resolution.

  • Catalog of planetary nebulae detected by GALEX and corollary optical surveys (GUVPNCAT)

    Planetary nebulae (PNe) consist of an ionized envelope surrounding a hot central star (CSPN). Ultraviolet observations provide important information on both the CSPN and the nebula. The team has matched the catalog of all confirmed and possible PNe (PNcat) with the Galaxy Evolution Explorer (GALEX) UV sky surveys, the Sloan Digital Sky Survey (SDSS) data release 16 (DR16), and the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) PS1 second release. A total of 671 PNe were observed by GALEX in far-UV (FUV; 1344-1786A) and/or near-UV (NUV; 1771-2831A) (GUVPNcat); 83 PNe were observed by SDSS (PNcatxSDSSDR16) and 1819 by Pan-STARRS (PNcatxPS1MDS). We merged these matched catalogs into GUVPNcatxSDSSDR16xPS1MDS, which contains a total of 375 PNe with UV and optical photometry over a total spectral coverage of about 1540-9610Å. GUVPNcat, PNcatxSDSSDR16, and PNcatxPS1MDS contain tags to track multiple matches, and multiple GALEX measurements, whereas GUVPNcatxSDSSDR16xPS1MDS contains a list of unique PNe with GALEX and SDSS and/or Pan-STARRS photometry (when multiple matches exist, ad hoc flags indicate so, but only the closest match is retained in the catalog). For details about the matching parameters, and catalog content in terms of extended and point-like PNe, as well as candidate binary CSPNe, see Gómez-Muñoz et al. (2023).

  • The JWST Advanced Deep Extragalactic Survey (JADES)

    The JWST Advanced Deep Survey (JADES) is the largest deep survey program that will be executed in the first few of years of operation of JWST. Three GTO Teams (NIRCam, NIRSpec, MIRI-U.S.) have combined time to produce a survey which will ultimately cover over 100 square arc minutes from 0.7 to 5 microns and 10 square arc minutes at 7.7 microns and produce thousands of galaxy spectra. The imaging data presented here is the first release from the survey and covers the “deep” portion with imaging acquired in September - October 2022. The area covered is approximately 25 square arc minutes with exposure times per filter ranging from ~14,000 to ~60,000 seconds. These data provide large galaxy samples for studying galaxy evolution from z~1 to at least z~13, and also to study the full diversity of galaxy characteristics. A catalog with photometry and photometric redshifts is included with this release. Additionally, “FITSMap” provides a multicolor image browser and links to the photometry.

  • The Cosmic Evolution Early Release Science Survey (CEERS)

    The Cosmic Evolution Early Release Science Survey (CEERS) covers 100 sq. arcmin of the Extended Groth Strip (EGS) field with JWST NIRCam imaging in parallel to MIRI imaging, NIRSpec and NIRCam wide-field slitless spectroscopy, all in a region supported by a rich set of HST/CANDELS multi-wavelength data. CEERS demonstrates, tests, and validates efficient extragalactic surveys with coordinated, overlapping parallel observations. The observations were obtained in two epochs in Cycle 1. In June, 2022, four pointings of MIRI imaging (F560W, F770W, F1000W, F1280W, F1500W, F1800W, and F2100W) were obtained with NIRCam imaging in parallel (F115W, F150W, F200W, F277W, F356W, F410M, F444W). In December, 2022, six pointings of NIRSpec multi-object spectroscopy with the PRISM (R~100) and medium resolution gratings (G140M/F100LP, G235M/F170LP, G395M/F290LP; R~1000) were obtained with NIRCam imaging in parallel. Four of these pointings were also observed with NIRCam slitless grism spectroscopy (R~1500) with MIRI imaging in parallel.

  • Low Resolution Stellar Library (LOWLIB)

    "Stellar libraries" are collections of stellar spectra. Such libraries find use in population synthesis studies, stellar parameter estimation, exposure time calculators, mission planning, and education. This HLSP contains 513 stellar spectra in FITS files. The spectra are flux calibrated, dereddened, and shifted to zero velocity. Observed with three low resolution gratings from the HST Space Telescope Imaging Spectrograph(STIS) and then merged into one continuous spectrum, these spectra cover roughly 0.2 < lambda < 1 µm at a resolving power of about 1000. This "HST Low Resolution Stellar Library" extends and supersedes NGSL, the "Next Generation Stellar Library," and comes as a companion to the Hot Star Library (Khan & Worthey 2018, A&A, 615, 115).

  • CANDELS Lyman Alpha Emission at Reionization Survey (CLEAR)

    The CANDELS Lyman-alpha Emission at Reionization (CLEAR) survey is a HST Cycle 23 program that obtained 12-orbit depth observations with the HST/WFC3 using the G102 grism in the IR camera in 12 fields split between the GOODS-N and GOODS-S fields from the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). Combined with existing spectroscopic data (G102 and G141) from other programs, the dataset released here includes 1D and 2D spectra over (partially- or fully-covered) 0.8-1.7 um for 6048 galaxies in GOODS-South and GOODS-North to m_H = 25. In addition, this release includes updated photometric catalogs from the 3D-HST survey, and spectroscopic catalogs that include emission line fluxes and redshifts derived from the combination of the photometry and grism spectroscopy. The primary goal of CLEAR was to characterize the evolution of the Lyman-? equivalent width distribution at 6 < z < 8 and to interpret this in the context of reionization. The CLEAR dataset also allows for studies of the stellar populations, star-formation, ionization, and chemical enrichment of galaxies in the distant universe (from redshifts 0.5 to 3).

  • Space Telescope and Optical Reverberation Mapping of Mrk 817 (STORM2)

    Calibrated spectra and light curves are provided for the HST/COS observations of the Seyfert 1 galaxy Mrk 817 in the Space Telescope and Optical Reverberation Mapping 2 (STORM 2) campaign. The STORM 2 campaign used HST/COS, Swift, NICER, XMM-Newton, and ground-based facilities in a 15-month long reverberation-mapping experiment. HST observations were made in 165 single-orbit COS visits with a mean cadence of two days from 2020 November 24 through 2022 February 24. In each visit, the team used the G130M and G160M gratings to observe the UV spectrum over the range 1070-1750 Angstroms in eight separate exposures. Exposure times were selected to provide S/N > 100 when measured over velocity bins of ~500 km/s. During each visit, the team obtained four 60-second exposures with G130M centered at 1222 Angstroms, two exposures of 175 s and 180 s using the G160M grating centered at 1533 Angstroms, and two 195 s exposures with G160M at 1577 Angstroms. As described in Homayouni et al. (2023), the team customized the calibrations of these spectra to provide more accurate and repeatable flux calibrations. These reprocessed spectra obtained with the various central wavelength and FPPOS settings were then combined for each individual observation into single spectra for G130M and G160M, single merged G130M+G160M spectra, a merged spectrum for the whole data set, and extracted continuum and emission-line light curves.

  • The MUSE Ultra Deep Field (MUDF)

    The MUSE Ultra Deep Field (MUDF) program is a multi-wavelength imaging and spectroscopic survey targeting a unique extragalactic field with two quasars at z = 3.2 that are separated by only 500 kpc. By combining emission line studies with high resolution spectroscopy of the two quasars, the project is designed to connect the physical properties of galaxies observed in emission with their surrounding gas viewed in absorption along the sightlines to the background quasars. These multiple sightlines provide a stereoscopic view that yields constraints on the size and geometry of the absorbing gas in the interstellar and circumgalactic medium over 10 billion years of cosmic time. The team provides Hubble Space Telescope (HST) data products for this field, anchored by 90 orbits of Wide Field Camera 3 (WFC3) near-infrared imaging and grism spectroscopy (HST Program 15637) that represents the deepest HST grism survey ever conducted for a single field. The release contains custom-calibrated science data that includes WFC3 F140W, F125W, and F336W imaging, WFC3 G141 grism spectroscopy, and reprocessed Wide Field and Planetary Camera 2 (WFPC2) F702W and F450W imaging. The team supplies source catalogs with photometric and morphological measurements for 3,375 unique sources, including 1,536 objects with both imaging and spectroscopic coverage. The team provides robust spectroscopic redshifts for 419 sources between z = 0 – 6, which will enable a variety of studies focusing on galaxy formation and evolution in different environments. These High Level Science Products contain science images with plate scales of 0.06 arcsec pixel-1 that are aligned with north up to the GAIA Early Data Release 3 (EDR3) astrometric coordinate system. The provided Point Spread Function (PSF) models have identical plate scales and have their integrated flux normalized to unity, which corresponds to the zero-point magnitude in each filter. The catalogs are provided in ASCII format, along with a quick view PDF that contains a summary figure of the imaging, photometry, and spectroscopy for each object with HST spectral coverage.

  • TESS-Gaia Light Curve (TGLC)

    TESS-Gaia Light Curve (TGLC) is a PSF-based TESS full-frame image (FFI) light curve product. Using Gaia DR3 as priors, the team forward models the FFIs with the effective point spread function to remove contamination from nearby stars. The resulting light curves show a photometric precision closely tracking the pre-launch prediction of the noise level: TGLC's photometric precision consistently reaches <2% at 16th TESS magnitude even in crowded fields, demonstrating excellent decontamination and deblending power. The HLSP authors publish TGLC Aperture and PSF light curves for stars down to 16th TESS magnitude for all available sectors and will continue to deliver future light curves.