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.

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Listing Results

Results: 174

Hubble UV Legacy Library of Young Stars as Essential Standards (ULLYSES)

The Hubble UV Legacy Library of Young Stars as Essential Standards ('ULLYSES') is a Director's Discretionary program devoting ~1,000 HST orbits to the production of an ultraviolet spectroscopic library of young high- and low-mass stars in the local universe. The ULLYSES program uniformly samples the fundamental astrophysical parameter space for each mass regime -- including spectral type, luminosity class, and metallicity for massive OB stars (in the Magellanic Clouds and two other lower-metallicity nearby galaxies) and the mass, and disk accretion rate for low-mass T Tauri stars (in eight young Galactic star forming regions). The data will be gathered over a three-year period, from Cycle 27 through Cycle 29 (2020-2022). The data products are combined from individual, extracted and calibrated spectra obtained with the COS and STIS instruments on-board HST. Products are made using both archival HST data and new HST observations obtained through the ULLYSES program.

TESS Light Curves From Full Frame Images (TESS-SPOC)

Since the start of the TESS Mission, the TESS Science Processing Operations Center (SPOC) pipeline has been used to calibrate full-frame images (FFI) and to assign world-coordinate system information to the FFI data delivered to the MAST. The SPOC pipeline has generated target pixel files, light curves, and associated products from two-minute cadence target data, but not from FFIs (Jenkins, et al. 2016). Data provided with this release extend the SPOC pipeline processing to include targets selected from the FFIs to create target pixel and light curve files for up to 160,000 targets per sector. Targets are selected from the FFIs using the TESS Input Catalog (TIC; Stassun et al. 2019) with a maximum of 10,000 targets per Sector on each of the sixteen TESS CCDs. Selection criteria include all two-minute cadence targets, targets bright in the near-infrared (H magnitude <=10), targets within 100 parsecs, and targets with TESS magnitude <=13.5. Details of the target selection are given in (Caldwell et al. 2020). The data products for the TESS-SPOC FFI targets are the same as for the two-minute cadence targets: calibrated target pixel files, simple aperture photometry flux time series, presearch data conditioning corrected flux time series, and cotrending basis vectors (CBV) sampled at the FFI cadence. The initial release includes TESS-SPOC FFI data products for the TESS northern hemisphere Sectors 14-26.

TESS Lightcurves From The MIT Quick-Look Pipeline (QLP)

The Transiting Exoplanet Survey Satellite (TESS) is the first high-precision full-sky photometry survey in space. The MIT QLP team produced light curves from a magnitude limited (TESS Magnitude smaller than 13.5) set of stars and other stationary luminous objects from the TESS Full Frame Images. The QLP light curves cover the full two-year TESS Primary Mission and include 14,773,977 and 9,602,103 individual light curve segments in the Southern and Northern ecliptic hemispheres, respectively. The photometric precision roughly follows the theoretical predictions pre-launch. The data reduction process is described in the primary reference (Huang et al. 2020). Additional pages in the full QLP data validation report provide additional metrics for decision-making. These plots are useful for diagnosing whether the source of transit-like variability is on target or from a nearby blended source, which is particularly important for FFI data. Some of these data validation pages are available on the MIT TOI Portal. The first data release consists of light curves for targets in Sectors 1-26. Future deliveries of extended mission light curve data with 10 minute cadence are expected to be released in the near future, starting with Sector 27.

Pure-Hydrogen White Dwarf Models (WD-GRID)

NLTE calculations of hot white dwarf (WD) model atmospheres are the cornerstone of modern flux calibrations for the Hubble Space Telescope (HST) and for the CALSPEC database. These theoretical spectral energy distributions (SEDs) provide the relative flux vs. wavelength, and only the absolute flux level remains to be set by reconciling the measured absolute flux of Vega in the visible with the Midcourse Space Experiment (MSX) values for Sirius in the mid-IR. The most recent SEDs calculated by the tlusty and tmap NLTE model atmosphere codes for the primary WDs G191B2B, GD153, and GD71 show improved agreement to 1% from 1500 Angstroms to 30 microns, in comparison to the previous 1% consistency only from 2000 Angstroms to 5 microns. These new NLTE models of hot WDs now provide consistent flux standards from the FUV to the mid-IR. Model grids from both the TLUSTY207 and TMAP2019 NLTE software codes are presented across a range of stellar parameters. Both grids contain 132 models with effective temperature (T_eff) in the range 20,000 - 95,000 K and gravity (logg) between 7.0 and 9.5, with six steps of 0.5. The steps in T_eff are 2,000 K between 20,000 and 40,000 K and 5,000 K between 40,000 and 95,000 K. The wavelengths are presented in Angstroms, measured in vaccuum. The fluxes are Eddington fluxes, with different conversions for the two model sets to needed to convert to physical fluxes. See the Bohlin et al. 2020 paper for important information on how to use and convert the fluxes from these models.

A PSF-Based Approach To Kepler/K2 Data (PSFK2)

The Kepler/K2 mission offered to the science community the opportunity of obtaining high-precision light curves for a large variety of stellar fields, including stellar clusters. However, most Kepler/K2 data analyses reported in the literature are based on aperture photometry. Aperture photometry is perfectly suitable to investigating stars in sparse fields but it suffers from severe limitations in crowded environments like the central regions of stellar clusters. Thus, the wealth of information included in stellar clusters analyzed with the Kepler/K2 mission is often unexplored. The team has made use of their experience with undersampled Hubble Space Telescope images and developed a new method to analyze crowded regions with the Kepler/K2 data. The combination of a high-angular-resolution catalog and accurate point-spread-function (PSF) models allows them to pinpoint a star in a Kepler/K2 exposure and measure its flux after all detectable nearby stars are PSF-subtracted from the image. This PSF-based technique: (i) increases the number of analyzable objects in the field, (ii) provides an unbiased flux measurement for each source, (iii) extracts stellar light curves in a crowded environment and (iv) improves the reachable photometric precision for faint stars. This technique is designed to exploit the huge potential offered by the 'super-stamps', but it is also perfectly suitable to analyze single, isolated stamps. The team releases the light curves for stars in the open clusters M35 and NGC2158 observed during Campaign 0, and M44 and M67 in Campaign 5. They also provide the high-angular-resolution input catalogs used in their works, the lists of the variable stars identified (only for M 44 and M67 clusters) and the Kepler/K2 stacked images for each cluster.

GALEX UV Unique Source Catalogs ("GUVcat") and Cross-Matches With Gaia and SDSS ("GUVmatch") (GUVCAT)

The GALEX database contains almost 600 million source measurements in far-UV and near-UV. Some sources have repeated measurements (useful to search for variability, for example), due to repeated observations of the same field or overlap between fields. Bianchi, Shiao, and Thilker 2017 constructed catalogs of clean, unique (i.e. only one entry for each object) UV sources, useful to estimate density of sources across the sky or the number of sources with given magnitude or color ranges, or to match UV sources with other catalogs (revised version 2020). Flags are included to check for artifacts, as well as for existing multiple observations, and flags indicating whether a source is within the footprint of a large galaxy or stellar cluster where source identification and photometry may be unreliable or inconsistent across the bands. GUVcat is composed using tiles from the AIS (All-Sky Imaging Survey), with a depth of about 19.9/20.8 in FUV/NUV ABmag. Bianchi & Shiao 2020 matched the GUVcat_AIS with SDSS DR14 and Gaia DR2 databases (GUVMatch). Tags are included to identify and track multiple optical matches to UV sources.

NGC 5253 Images With Gaia DR2 Absolute Astrometry (NGC5253-DR2)

The blue compact dwarf galaxy NGC 5253 hosts a very young central starburst. The center contains intense radio thermal emission from a massive ultracompact H II region (or supernebula) and two massive and very young super star clusters (SSCs), which are seen at optical and infrared wavelengths. The spatial correspondence between the radio and HST images over an area of < 0.5 arcseconds is very uncertain because of the limitations of Guide Star Catalog II for HST absolute astrometry. Using the Gaia Data Release 2 catalog, we improve the absolute astrometry of the HST ultraviolet, optical and infrared images by a factor of ~10 and match them to the radio observations with an accuracy of 10-20 mas. We find that the radio and optical sources do not coincide and that there are three young SSCs at the center of NGC 5253. This High Level Science Product contains the HST images for the center of NGC 5253 re-mapped on to the Gaia DR2 reference frame. Full details of the images are given in Table 2 of Smith et al. 2020. The ACS/WFC F814W image was first mapped to the DR2 astrometry using the DrizzlePac function 'tweakreg' to an accuracy of +/- 10 mas. The smaller field of view ACS/HRC/SBC and NICMOS/NIC2 images were then aligned to the transformed ACS/WFC F814W image to accuracies of +/- 12 mas and +/- 20 mas, respectively.

Habitable Zones and M dwarf Activity across Time (HAZMAT)

The HAbitable Zones and M dwarf Activity across Time (HAZMAT) program assesses the lifetime exposure of planets to stellar ultraviolet (UV) radiation using GALEX data, HST COS and STIS spectra, and semi-empirical, full-wavelength models. The program quantifies the evolution of far- and near-UV (FUV; NUV) emission for early- and mid-M (HAZMAT I), late-M (HAZMAT III), and K (HAZMAT V) type stars, as well as extreme-UV (EUV) emission from early-M stars (HAZMAT VI). The data products below are high-resolution synthetic spectra (EUV – IR; 100 Angstroms to 5.5 microns) of early-M stars at five distinct ages between 10 Myr and 5 Gyr. The spectra are computed with the PHOENIX atmosphere code from one-dimensional upper atmosphere models of 0.35 and 0.45 solar mass stars (stellar parameters given in Table 1 of the HAZMAT VI paper). The wavelengths (given in Angstroms) are in vacuum and the wavelength grid has a resolution of <0.1 Angstroms. The flux densities (given in ergs/cm^2/s/Angstrom) are that at the stellar surface and are scalable to a distance D via (R_star/D)^2 where R_star is dependent on the age and mass of the star from Table 1. Downloadable data products include five spectra per 0.35 and 0.45 solar mass stars at ages of 10, 45, 120, 650, and 5000 Myr. The spectra reproduce either the minimum ('MIN'), lower quartile ('LQ'), median ('MED'), upper quartile ('UQ'), or maximum ('MAX') FUV and NUV flux density per age as calculated from the GALEX stellar sample in HAZMAT I.

Swift UVOT Open Clusters Catalog (UVOT-OC)

The UVOT-OC HLSP presents near-ultraviolet (NUV) point-source catalogs for 103 Galactic open clusters measured by the Niel Gehrels Swift Mission , as part of the Swift Ultraviolet Optical Telescope (UVOT) Stars Survey (Siegel et al. 2019). It includes 103 photometry files created using DAOPHOT and a custom calibration program. Applying a membership analysis driven by Gaia DR2 proper motions, 49 of these 103 have clear precise color-magnitude diagrams amenable to investigation. For a handful of clusters, only detections matched to the GAIA DR2 are included. The catalogs provide photometry, where available, measured from images in UVOT u, uvw1, uvm2 and uvw2 filters. These data, taken across the duration of the mission, provide a unique set of NUV point-source photometry on simple stellar populations.

eleanor FFI Light Curves From TESS (ELEANOR)

The TESS mission has been providing the community with 30-minute Full-Frame Images, which contain about a million stars observed every sector. However, individual target pixel files (TPFs) and light curves (LCs) are not being released for these stars. The purpose of eleanor is to provide the community with systematics-corrected light curves for stars brighter than I = 16, for which the pipeline can achieve 1% precision photometry. The first eleanor data product release contains time-stacked postcards as well as estimated 2D backgrounds per postcard for Sectors 1-13. The postcards, coupled with the eleanor software, can be used to create individual TPFs and LCs for a given TIC ID, set of coordinates, or Gaia ID. Future releases will include postcards from more Sectors and detrended light curves.

Kepler-Swift Active Galaxies and Stars Survey (KSWAGS)

The Kepler-Swift Active Galaxies and Stars (KSwAGS) survey of four modules of the original Kepler FOV was conducted by Swift-XRT to find new active galactic nuclei for Kepler monitoring. The X-ray survey results were reported in Smith et al. 2015. Due to the co-aligned UVOT telescope on the Swift spacecraft, an ultraviolet survey of the Kepler field was conducted simultaneously in the uvm2 filter at 2246 Angstroms. The catalog includes the full reduced UV survey. It contains more than three times as many sources as GALEX NUV archival data in the Kepler field, including 17,000 sources with Kepler 30-minute light curves.

A PSF-Based Approach to TESS High Quality Data Of Stellar Clusters (PATHOS)

The PATHOS project provides a database of high-precision light curves for members of stellar clusters, obtained by extracting photometry from TESS Full Frame Images. Light curves are obtained with an innovative PSF-based approach, that involves the use of empirical Point Spread Functions (PSFs), a high-angular resolution input catalogue (Gaia DR2) and neighbor-subtraction. The PSF-based approach minimises the dilution effects in crowded environments, enabling extraction of high-precision photometry for stars in the faint regime (T > 13). The PATHOS database contains all the light curves extracted during the project, as well as light curves requested for other projects. Light curves of specific targets can be requested by contacting the project managers.

An Atlas of Active Galactic Nuclei Spectral Energy Distributions (AGNSEDATLAS)

AGNSEDATLAS presents the spectral energy distributions (SEDs) of 41 individual active galactic nuclei, derived from multiwavelength photometry and archival spectroscopy, including eight MAST-supported projects (HST, SWIFT-UVOT, GALEX, PanSTARRS, IUE, FUSE, HUT, WUPPE) plus at least nine other missions or observatories. In addition to these individual AGN SEDs, there are an additional 80 Seyfert SEDs produced by mixing the SEDs of the central regions of Seyferts with galaxy SEDs. All of the SEDs span at least 0.09 to 30 microns, but in some instances wavelength coverage extends into the X-ray, far-infrared, and radio.

Cluster Difference Imaging Photometric Survey (CDIPS)

The TESS mission has been releasing full-frame images recorded at 30 minute cadence. Using the TESS images, the CDIPS team has begun a Cluster Difference Imaging Photometric Survey (CDIPS), in which they are making light curves for stars that are candidate members of open clusters and moving groups. They have also included stars that show photometric indications of youth. Each light curve represents between 20 and 25 days of observations of a star brighter than Gaia Rp magnitude of 16. The precision of the detrended light curves is generally in line with theoretical expectations. The pipeline is called 'cdips-pipeline', and it is available for inspection as a GitHub repository, and should be cited as an independent software reference (Bhatti et al., 2019, The first CDIPS data release contains 159,343 light curves of target stars that fell on silicon during TESS Sectors 6 and 7. They cover about one sixth of the galactic plane. The target stars are described and listed in Bouma et al. 2019. They are stars for which a mix of Gaia and pre-Gaia kinematic, astrometric, and photometric information suggest either cluster membership or youth.

Hubble Catalog of Variables (HCV)

The Hubble Catalog of Variables (HCV) is the first full, homogeneous, catalog of variable sources found in the Hubble Source Catalog (HSC), which is built out of publicly available images obtained with the WFPC2, ACS and WFC3 instruments onboard the Hubble Space Telescope. The HCV is the deepest catalog of variables available. It includes variable stars in our Galaxy and nearby galaxies, as well as transients and variable active galactic nuclei. The HCV contains 84,428 candidate variable sources (out of 3.7 million HSC sources that were searched for variability) with V <= 27 mag; for 11,115 of them the variability is detected in more than one filter. The number of data points in a light curve range from 5 to 120, the time baseline ranges from under a day to over 15 years, while ~8% of variables have amplitudes in excess of 1 mag. Two catalogs are provided in this HLSP: a catalog of variables, and a catalog of objects that are 'constant' within 5-sigma of their median absolute deviation (MAD). The catalog of variables lists for each source the equatorial coordinates, MatchID, GroupID, subgroup, the pipeline classification flag, the expert-validation classification flag, the number of existing instrument and filter combinations for the source, the name of the instrument and filter combination. The filter combination includes: the filter detection flag (set to '1' if variability is detected, or '0' if not), the variability quality flag, the number of measurements in the light curve, the HSC magnitude, the corrected magnitude, the MAD value, and the reduced chi^2 value. For all multi-filter variable candidates, there are extra columns for each additional instrument and filter combination, in which the source is classified as a variable candidate. The catalog of constant sources contains the sources that fall below the 5-sigma detection threshold of the HCV pipeline. These include constant sources and low-amplitude variables that are below the detection threshold. For each source, the columns show the equatorial coordinates, the MatchID, the GroupID, the subgroup, the number of instrument and filter combinations in which individual sources are observed, follwed by the name of each instrument and filter combination for which the following data are given: the number of measurements in the light curve, the HSC magnitude, the corrected magnitude, the MAD value, and the reduced chi^2 value.