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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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Results: 198

Hubble Space Telescope Atlases of Cluster Kinematics (HACKS) (HACKS)

A number of studies based on data collected by the Hubble Space Telescope (HST) GO-13297 program “HST Legacy Survey of Galactic Globular Clusters: Shedding UV Light on Their Populations and Formation" have investigated the photometric properties of a large sample of Galactic globular clusters and revolutionized our understanding of their stellar populations. In this project, the authors expand previous studies by focusing on the stellar clusters’ internal kinematics. The authors computed proper motions for stars in 56 globular clusters and one open cluster by combining the GO-13297 images with archival HST data. The astro-photometric catalogs released with this paper represent the most complete and homogeneous collection of proper motions of stars in the cores of stellar clusters to date, and expand the information provided by the current (and future) Gaia data releases to much fainter stars and into the crowded central regions. At the dawn of a new era in astronomy with the first light of the James Webb Space Telescope (JWST), the legacy that these proper-motion catalogs offer is further enhanced, since they can serve as an important astrometric benchmark for JWST-based data reduction and tools.

NLTE-OBGRID: New NLTE Model SEDs For OB Stars (NLTE-OBGRID)

Ivan Hubeny has updated the TLusty OB NLTE model SED grids of Lanz & Hubeny (2003) and Lanz & Hubeny (2007) using a more complete hydrogen atom to produce more realistic IR flux predictions. In particular, the new NLTE spectra have a much better description of line confluences and of the contribution to the opacity in very high series members. In addition, there are improvements in the treatment of the hydrogen and He II continua from high levels, inclusion of more scattering opacity sources, and updates to the physics of level dissolution. Each model has 29957 points at constant spectral resolution of R=5000 and a micro-turbulent velocity of 2 km/s. The Asplund et al. (2009) element abundances are used for computing the spectra. The grid contains 1082 model pairs of spectra and continua and covers effective temperature Teff in the range 15,000-55,000 K and surface gravity log(g) between 1.75 and 4.75, with steps of 0.25. The steps in Teff are 1,000 K between 15,000 and 29,000 K and 2,500 K between 30,000 and 55,000 K. As Teff rises, more of the unstable lower surface gravities are omitted. There are five metallicity values log Z=[M/H] of 0.301, 0.000, -0.301, -0.70, and -1.00, which correspond to Z=2, 1, 0.5, 0.2, and 0.1, where Z=1 is the solar value. The continuum spectra have a coarser wavelength scale than the spectra. Both ASCII text and FITS versions of the SEDs are provided. The wavelengths are in Angstroms measured in vacuum, while the fluxes are in erg/cm**2/s/Angstrom.

TESS FFI-Based Light Curves from the GSFC Team (GSFC-ELEANOR-LITE)

The TESS Full Frame Images (FFIs) present a wealth of opportunity for discovery.  The team aims to make this opportunity accessible to the entire community by providing the FFI light curves of all stars brighter than 16 mag from the primary mission (Years 1 and 2; Sectors 1–26) for public release.  This includes a total of over 150 million light curves, making it the largest set of TESS light curves released to date.  The light curves were constructed using the eleanor python library (Feinstein et al., 2019) in an offline, parallel implementation on the Discover supercomputer at the NASA Center for Climate Simulation (NCCS).  The eleanor-lite format in which they are stored allows for a relatively low memory requirement per light curve, providing for bulk storage and fast transfer of the light curves.  This format will facilitate large-scale analysis of the light curves, such as algorithmic and machine learning approaches to finding signals of interest to the user.

Jupiter Great Red Spot Velocity Fields from HST/WFC3 (GRS-WFC3)

High precision velocity fields of Jupiter's Great Red Spot (GRS) have been created by correlating sequences of WFC3/UVIS images spanning typical sequence durations of 10 hours. The analysis, results, and high-level science products are described in a paper by Wong et al. (2021), entitled 'Evolution of the Horizontal Winds in Jupiter's Great Red Spot from One Jovian Year of HST/WFC3 Maps.' Velocities were measured using the Advection Corrected Correlation Image Velocimetry (ACCIV) software, which was described in Asay-Davis et al. (2009) and is available at GitHub.

Sloan Digital Sky Survey Giant Arcs Survey (SGAS)

Strong gravitational lensing models for 37 galaxy clusters from the Sloan Digital Sky Survey Giant Arcs Survey (SGAS) are made available as HLSP, observed by HST GO13003 Cycle 20 large program (PI: Gladders). The lens models are constructed based on multi-band HST WFC3 imaging. The team supplemented these imaging data with ground-based imaging and spectroscopy from Magellan, Gemini, Apache Point Observatory, and the Multiple Mirror Telescope, in order to detect and spectroscopically confirm new multiply imaged lensed background sources behind the clusters. In the paper that accompanies this data release, Sharon et al. (2020), the team report the list of lensing constraints, and spectroscopic or photometric redshifts of sources in these fields, including cluster galaxies and background sources. The strong lensing mass models are constructed based on all available lensing evidence. The HLSP include lens model outputs (kappa, gamma) for the best-optimized model and a range of maps drawn from sets in the MCMC that sample the parameter space, from which one can derive lens model properties such as cluster masses, magnification, deflection, and their uncertainties. The models were produced using the parametric lens modeling LENSTOOL (Jullo et al. 2007).

Physics at High Angular resolution in Nearby GalaxieS - Catalogs (PHANGS-CAT)

The PHANGS program is building the first dataset to enable the multi-phase, multi-scale study of star formation across nearby spiral galaxies, by combining Atacama Large Millimeter/submillimeterArray (ALMA) CO(2-1) mapping, Very Large Telescope/Multi Unit Spectroscopic Explorer (VLT/MUSE) optical spectroscopy, and Hubble Space Telescope (HST) UV-optical imaging. Here, the team provides catalog products from the PHANGS survey, the HST portion of which is obtaining five band NUV-U-B-V-I imaging of the disks of 38 spiral galaxies at distances of 4-23 Mpc, and parallel V and I band imaging of their halos, to provide a census of tens of thousands of compact star clusters and associations. The combination of HST, ALMA, and VLT/MUSE observations will yield an unprecedented joint catalog of the observed and physical properties of ~100,000 star clusters, associations, HII regions, and molecular clouds. The PHANGS-CAT products (Version 1) provide compact cluster (CLUST) catalogs and multi-scale association (ASSOC) catalogs for five galaxies observed with HST as part of the PHANGS-HST project. The corresponding HST imaging products are available as the PHANGS-HST High Level Science Products. The team provides two kinds of compact cluster catalogs (CLUST products): human classified and machine learning (ML) classified. Only class 1 (symmetric, centrally concentrated, radial profile extended relative to point source), and class 2 (asymmetric, centrally concentrated, radial profile extended relative to point source) clusters are included. The multi-scale stellar associations (ASSOC products) are determined using both the HST NUV (F275W) and V-band (F555W) to independently delineate the stellar associations in each galaxy. The associations are calculated at three or four physical scale levels depending on the distance of the galaxy. The physical scale levels of the associations correspond to (8pc, 16pc, 32pc,64pc), or (16pc, 32pc, 64pc) for more distant galaxies. A flowchart of the entire cluster and multi-scale association processing pipeline (from Lee et al. 2022) illustrates the entire process.

Simulated TESS Light Curves for Measuring Rotation with Deep Learning (SMARTS)

Conventional methods of detecting stellar rotation from TESS light curves have struggled to obtain periods longer than 13.7 days due to complicated systematics related to the telescope's orbit. Machine learning has been shown to see beyond TESS's systematics and obtain long periods, but it requires large training sets with known rotation periods. SMARTS is a training set of synthetic light curves and binned wavelet transforms designed to mimic the full-frame image light curves of the TESS continuous viewing zones. The light curves were generated using physically realistic spot evolution models and include rotation, varying activity levels, magnetic cycles, spot emergence and decay, and latitudinal differential rotation. They are combined with real TESS galaxy light curves and stitched sector-to-sector to emulate TESS's systematics and noise. This HLSP contains 1 million simulations spanning rotation periods of 0.1—180 days.

Mock Image Training Sets for DeepMerge (DEEPMERGE)

To investigate the use of Convolutional Neural Networks (CNNs) for distinguishing between simulated distant (z=2) merging and non-merging galaxies, the authors created two versions of mock data mimicking Hubble Space Telescope and James Webb Space Telescope observations: pristine (simulated galaxy images with PSF blurring) and noisy (simulated galaxy images with PSF and observational noise). The accuracy of the CNN model on the test set is 79% (76%) on the pristine (noisy) mock data. The CNN outperforms a Random Forest classifier (Snyder et al. 2019), which was shown to be superior to conventional one- or two-dimensional statistical methods (Concentration, Asymmetry, the Gini, M20 statistics etc.), which are commonly used when classifying merging galaxies. These data were derived from the z=2 snapshot of the Illustris-1 simulation from the Illustris Project.

Kepler Improved Resolution Image Subtraction (IRIS)

The open clusters NGC 6791 and NGC 6819 both lay in the Kepler mission's field of view --- however, due to crowding, the majority of stars in and around the clusters were not individually targeted for long or short cadence photometry during the mission. Instead, both clusters were targeted with 200x200 target pixel files, known as "superstamps." The team presents long cadence light curves for all 9,150 KIC targets that fall on the superstamps, including cluster members and field stars. This data release includes light curves for 8,427 new targets with no previously available photometry, and an extended time series baseline for 382 long cadence targets. The team produced these light curves using an image subtraction photometry pipeline, described in Colman et al. 2021, which is optimized for variability and reducing noise on crowded targets. There are at most 17 quarters (1--17) of photometry available for NGC 6791, and 14 (1--5, 7--9, 11--13, 15--17) for NGC 6819. Due to detector drift between seasons, targets towards the edges of the superstamps may not have all quarters available.

Lyman Continuum Galaxy Candidates in COSMOS (LCGCOSMOS)

Deep Hubble Space Telescope rest-frame UV Wide Field Camera 3 (WFC3)/F336W and Advanced Camera for Surveys (ACS)/F435W imaging (GO 15100, PI Cooke, 30 orbits) are used for the detection of Lyman Continuum Galaxy (LCG) candidates in the COSMOS field. LCGs are individual sources that emit ionizing flux below the Lyman break (< 912 Angstroms) and can be used to constrain cosmic reionization parameters. The team made several improvements to the standard Space Telescope Science Institute (STScI) WFC3/UVIS reduction pipeline, to clean and calibrate the images beyond what was previously available from MAST. The team also developed and applied additional, novel calibrations to the charge transfer efficiency (CTE)-corrected single-exposure calibrated images (called FLCs). This HLSP contains the final reduced and aligned WFC3/F336W images (with the new calibrations) and ACS/F435W images. The mosaics are mapped onto a larger reference image and aligned to COSMOS coordinates. The images have pixel scales 0.03 arcsec, pixels aligned north, and all pointings for each filter combined into a single image for each band. The pointings span ~40 arcmin^2 total and have an average depth of ~29 mag at 5-sigma. The point spread functions (PSF) for each pointing are also provided.

Kepler Bonus Aperture Light Curves (KBONUS-APEXBA)

NASA's Kepler mission observed background regions across its field of view for more than three consecutive years using custom-designed super apertures (EXBA masks). Since these apertures were designed to capture a region of the sky rather than single targets, the Kepler Science Data Processing pipeline produced Target Pixel Files (TPFs), but did not produce light curves for the sources within these background regions. For this data set, the team produced light curves for 9,327 sources observed in the EXBA masks. These light curves are generated using aperture photometry estimated from the instrument's Pixel Response Function (PRF) profile computed from Kepler's full-frame images (FFIs). The PRF models enable the creation of apertures that follow the characteristic shapes of the PSF in the image and the computation of flux completeness and contamination metrics. A full description of this dataset can be found in Martinez-Palomera et al. 2021, as well as the Python library kepler-apertures that was used to extract the light curves for the EXBA sources.

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. This HLSP contains the drizzled mosaic products as well as derived morphological information for galaxies in the mosaic.

The All-Sky PLATO Input Catalog (ASPIC)

The ESA PLAnetary Transits and Oscillations of stars (PLATO) mission will search for terrestrial planets in the habitable zone of solar-type stars. Because of telemetry limitations, PLATO targets need to be pre-selected. We present an all sky catalog that will be fundamental to select the best PLATO fields and the most promising target stars, derive their fundamental parameters, analyze the instrumental performances, and then plan and optimize follow-up observations. This catalog also represents a valuable resource for the general definition of stellar samples optimized for the search of transiting planets. The first public release of the all sky PLATO Input catalogue (asPIC version 1.1) contains a total of 2,675 ,539 stars, among which are 2,378,177 FGK dwarfs and subgiants and 297,362 M dwarfs. It was produced using Gaia Data Release 2 (DR2) astrometry and photometry and 3D maps of the local interstellar medium.

Cutouts from Wide-area TESS Coadded Images (TESS-COADD-CUTOUTS)

TESS has a simple unobstructed light path, with four cameras each housing seven lenses; fast optics, with a focal ratio of f/1.4; and wide-field detectors, with four cameras each having a 24 x 96 degree field of view. This design is in principle ideal for studies of the low-surface brightness (LSB) environments of Galaxies. A major complication in such studies is, however, the impact of stray light in the images. This project aimed to investigate this issue. The processing was performed on the Amazon Elastic Cloud 2 with the Montage image mosaic engine (http://montage.ipac.caltech.edu) using data from Sectors 1-21. On spatial scales of 1 to 2 degrees, cutouts of four test galaxies indicate the background is smooth and that even with extensive stray light, the TESS co-added images can be exploited for LSB studies. The team provides coadded images in FITS format to make cutouts out of, and provide a Jupyter notebook for deriving cutouts of these co-added images for any position or resolvable object name.

A Panchromatic Spectrum Of LHS 3844 (MSTARPANSPEC)

The team presents a panchromatic spectrum, from 1 Angstrom to 10 microns, of the nearby, planet-hosting M dwarf LHS 3844. This data product is motivated by high-energy measurements of LHS 3844 in the ultraviolet with the Cosmic Origins Spectrograph on board the Hubble Space Telescope (HST/COS), and an upper limit on the soft X-ray flux from Swift's X-ray Telescope (Swift-XRT). Ten orbits of HST and 31.8ks of Swift-XRT were used to obtain these data. The HST/COS data cover the far and near ultraviolet (FUV and NUV) with the G130M, G160M, and G230L gratings. During one of the FUV (G130M) observations the team observed a flare with an absolute energy of 8.96 +/- 0.77 x 10^28 erg in the FUV and an equivalent duration of 355 +/- 31 seconds. The team excises this flare from the UV spectral data and produce panchromatic spectra for both the quiescent and flare cases of the star. Due to the large aperture of COS the prominent Lyman-alpha line is obscured by geocoronal emission. The team employs the UV-UV line correlations developed by the MUSCLES program to estimate the Lyman-α flux using measured UV emission lines in the rest of the COS data. For the rest of the high-energy spectrum, which is not measured directly, the team employs a differential emission measure (DEM) to fill in the gaps. Redward of the NUV the team uses a PHOENIX model and a blackbody curve to fill out the spectrum. The data products presented here are designed to be similar to those provided by the MUSCLES survey, such that users of MUSCLES data can easily access the spectrum of LHS 3844 and vice versa.