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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.
HLSPs
Listing Results
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.
Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER)
The team provides UV-optical-NIR photometry for 22 million stars in the central ~0.1 deg^2 of M33 for the Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region ('PHATTER') survey. They use the filters F275W and F336W on the WFC3/UVIS camera, F475W and F814W on ACS/WFC, and the F110W and F160W on WFC3/IR. UVIS data reach a magnitude limit of ~25 in F275W and F336W. ACS data reach maximum depths of ~28 magnitudes in F475W and ~27 magnitudes in F814W in the uncrowded outer disk. In these same regions, WFC3/IR data reach maximum depths of ~26.5 and ~25.5 in F110W and F160W, respectively. However, the depths are crowding limited in the optical and NIR, and thus is a strong function of radius. As a result, photometry in the inner bulge fields is far shallower. The source catalogs and image mosaics from which the sources are extracted are provided by the team. The team also provides the WCS solutions for each subsection's reference image.
Measuring Young Stars in Space and Time (MYSST)
The 'Measuring Young Stars in Space and Time' (MYSST) project is a large, high spatial resolution, deep Hubble Space Telescope survey of the star forming complex N44 located in the Large Magellanic Cloud (LMC). Observing objects with masses as low as 0.09 M_sun (unreddened 1 Myr pre-main-sequence star), the project aims to draw a comprehensive picture of star formation on the scales of giant molecular clouds by quantifying the star formation history of N44 across space and in time. Observations were taken with the Advanced Camera for Surveys (Wide Field Channel) and the Wide Field Camera 3 (UVIS channel) in the broad band filters F555W and F814W, covering a field of view of approximately 12.2 x 14.7 arcmin^2 or 180 x 215 pc^2 at the distance of the LMC. This archive comprises the primary science output of the survey, i.e. the MYSST photometric catalog and the mosaic images.
Mapping the Escape Fraction of Ionizing Photons Using Resolved Stars (UVESCAPE)
The UVESCAPE team has demonstrated a new method for measuring the escape fraction of ionizing photons using HST imaging of resolved stars in NGC 4214, a local analog of high-z starburst galaxies that are thought to be responsible for cosmic reionization. Specifically, they forward model the UV through near-IR spectral energy distributions of ~83,000 resolved stars to infer their individual ionizing flux outputs using the Bayesian Extinction And Stellar Tool (BEAST; Gordon et al. 2016). They constrain the local escape fraction by comparing the number of ionizing photons produced by stars to the number that are either absorbed by dust or consumed by ionizing the surrounding neutral hydrogen in individual star-forming regions. They find substantial spatial variation in the escape fraction (0-40%). Integrating over the entire galaxy yields a global escape fraction of 25% (+16% / -15%). This value is much higher than previous escape fractions of zero reported for this galaxy. They discuss sources of this apparent tension, and demonstrate that the viewing angle and the 3D ISM geometric effects are the cause. If one assumes that NGC 4214 has no internal dust, like many high-z galaxies, they find an escape fraction of 59% (an upper limit for NGC 4214). This is the first non-zero escape fraction measurement for UV-faint (M_FUV) = -15.9 galaxies at any redshift, and supports the idea that starburst UV-faint dwarf galaxies can provide a sufficient amount of ionizing photons to the intergalactic medium. The team has made their catalog of stellar ionizing fluxes available as a High Level Science Product.
Physics at High Angular resolution in Nearby GalaxieS (PHANGS-HST)
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 data products from the PHANGS-HST Treasury survey, 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.
TESS Image CAlibrator Full Frame Images (TICA)
TESS images that serve as the input to the MIT Quick Look Pipeline (QLP) are provided here. The team uses a Python package ('tica'), to calibrate the raw pixels and apply astrometric registration in the form of World Coordinate Solutions.
Convolutional Neural Networks for Flare Identification in TESS 2-minute Data (STELLA)
Previous methods of flare detection with both Kepler and TESS data have relied on light curve detrending and using outlier detection heuristics for identifying flare events. stella is a novel way to detect flares in TESS short cadence data using convolutional neural networks (CNNs). Any TESS short cadence light curve can be run through the CNN models provided, without any detrending. The models created by the team return a probability light curve (see example figure), with values between 0-1 if a given light curve event is a flare or not. It takes < 1 minute to predict flares on a single TESS sector light curve using these models. The CNN models were created with Google's machine learning API, Tensorflow. The team has created 100 trained ensembled models to use when predicting flares in other short cadence TESS light curves. Any single model can be used on its own, however the team recommends using at least 10 models and averaging the results. The details of each model can be found in Feinstein et al. 2020. The models can be opened and explored using either Tensorflow, h5py, or any other software that can open HDF5 files.
Hubble imaging Probe of Extreme Environments and Clusters (HIPEEC)
The Hubble imaging Probe of Extreme Environments and Clusters ('HiPEEC') is a survey investigating star cluster formation in the extreme environments of six merging galaxies. The team provides the reduced, aligned and drizzled HST images (scale of 0.04 arcsec/pixel) for the six galaxies of the survey: NGC34, 1614, 4194, 3256, 3690 and 6052. There are 32 images in total and the filters cover at a minimum UBVI and H-alpha for each galaxy. The team also provides the star cluster catalog for each galaxy. Each catalog includes the position (RA, Dec), measured magnitudes, extinctions, ages and masses from fits to the spectral energy distributions. An explanation of the column contents is given at the start of each file.
Multi-Sector Light Curves From TESS Full Frame Images (DIAMANTE)
The DIAmante project provides raw and systematic-corrected multi-Sector lightcurves extracted from TESS Full Frame Images (FFIs). DIAmante exploits a new pipeline based on difference image analysis which has been specifically developed to analyze FFIs. The main targets are FGKM dwarf and sub-giant stars across the entire sky. The team provides additional supporting material as catalogs and data validation documents for specific targets of interest (e.g. transiting planets). The first data release presents the results (lightcurves and data validation documents) from a search for transiting planets in the Southern ecliptic hemisphere.