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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.

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Results: 169

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, http://doi.org/10.5281/zenodo.3370324). 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.

Photometric Catalogs from Hubble Frontier Fields (HFFCATALOGS)

HFFCATALOGS presents multiwavelength photometric catalogs derived from HST, VLT, and Spitzer imaging, and catalogs of derived properties, for two Hubble Frontier Fields massive galaxy clusters, Abell 370 and RXC J2248.7-4431 (Bradac et al. 2019). These catalogs were developed by the ASTRODEEP team and used the ASTRODEEP pipeline. Photometric catalog columns include fluxes, magnitudes, and errors for HST WFC3 F160W, F140W, F125W, and F105W; ACS F814W, F606W, and F435W; Spitzer IRAC Channels 1 and 2, and VLT HAWK-I KS; as well as spectroscopic data compiled by Shipley et al. (2018). Property catalog columns include magnifications, photometric redshifts, errors, and goodness of fit, as well as derived stellar masses and star formation rates.

The K2 Bright Star Survey (HALO)

The HALO project produces calibrated light curves of stars from K2 that are brighter than the saturation limit of the detector (~11th magnitude). Light curves of 161 bright stars from K2 Campaign 4 and onwards are provided, derived from the unsaturated scattered-light 'halo' around the stars. Light curve creation relies on optimizing the weights of a linear combination of the pixel time series using a lagged Total Variation minimization, which is demonstrated to work on both saturated and unsaturated K2 targets. After flux extraction from the halo apertures, the light curves are further corrected using the 'k2sc' Gaussian Process systematics-correction code to further correct pointing residuals.

An HST Study of the Crater Stellar System (CRATER)

The Crater object is a faint star system, discovered relatively recently (Belokurov et al. 2014, Laevens et al. 2014), located in the Milky Way's outer halo. The collection presented here is based on optical imaging data of Crater taken with the Advanced Camera for Surveys on the Hubble Space Telescope. The available data includes the resulting catalog of Crater members, a catalog of artificial star tests, as well as an ACS reference image in F814W used for photometry.

A Wide-Field WFC3 Imaging Survey in the COSMOS Field (COSMOS-DASH)

COSMOS-Drift And SHift (COSMOS-DASH) is a Hubble Space Telescope WFC3 imaging survey of the COSMOS field in the F160W filter, comprising 456 WFC3 pointings covering an area of 0.49 deg^2, giving 0.66 deg^2 of total data in the archive. By taking advantage of the unique Drift And SHift (DASH) observing mode, COSMOS-DASH is the widest HST/WFC3 imaging survey in F160W, tripling the extragalactic survey area in the near-infrared at HST resolution.

Space Telescope and Optical Reverberation Mapping (STORM)

Calibrated spectra and models are provided for NGC 5548 from HST/COS observations in the Space Telescope and Optical Reverberation Mapping (STORM) Campaign. The STORM campaign used HST/COS, Swift, Chandra and ground-based facilities in a six-month long reverberation-mapping experiment during 2014. HST observations were made in single-orbit COS visits approximately daily from 2014 February 1 through July 27. Of the 179 scheduled visits. In each visit, the team used the G130M and G160M gratings to observe the UV spectrum over the range 1153—1796 Angstroms in four separate exposures. Exposure times were selected to provide S/N > 100 when measured over velocity bins of ~500 km/s. As described in De Rosa et al. (2015) the team customized the calibrations of these spectra to improve the wavelength calibration, the S/N with better flat fields, and more accurate and repeatable flux calibrations. These reprocessed spectra obtained with the various central wavelength and FPPOS settings were then combined into single spectra for G130M and G160M for each individual observation. The team have also modeled these UV spectra of NGC 5548 to correct for intervening absorption and to deblend the individual emission lines. These spectral models, described by Kriss et al. (2019) are based on merged G130M and G160M spectra for each observation that have been binned by 4 pixels (half a resolution element). Using the modeled spectra, the team produce spectra where absorption intrinsic to NGC 5548 and in the intervening interstellar medium of the Milky Way has been replaced by their emission model to remove the absorption features. Finally, modeled continuum fluxes, deblended emission line fluxes, and the strengths of absorption lines intrinsic to NGC 5548, as tabulated in Kriss et al. (2019) are collected here as well.