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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
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-a 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.
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.
Hubble Tarantula Treasury Project (30DOR) (HTTP)
HTTP is a panchromatic imaging survey of stellar populations in the Tarantula Nebula (30 Dor) in the Large Magellanic Cloud that reaches into the sub-solar mass regime (<0.5 M_solar). HTTP utilizes the capability of the Hubble Space Telescope to operate the Advanced Camera for Surveys and the Wide Field Camera 3 in parallel to study this remarkable region in the near-ultraviolet, optical, and near-infrared spectral regions, including narrow-band H alpha images. The high sensitivity, spatial resolution and broadband coverage of HTTP allow users to dissect the stellar populations and infer an accurate description of the anatomy of the Tarantula Nebula, and therefore to reconstruct for the first time the temporal and spatial evolution of a prototypical starburst on a sub-parsec scale
Targeting Extremely Magnified Panchromatic Lensed Arcs and their Extended Star formation (TEMPLATES)
The TEMPLATES program is designed to obtain high signal-to-noise NIRSpec and MIRI IFU spectroscopy, with accompanying imaging, for 4 gravitationally lensed galaxies at 1<z<4. This program aims to spatially resolve the star formation in galaxies across the peak of cosmic star formation, in an extinction-robust manner. Lensing magnification pushes JWST to the highest spatial resolutions possible at these redshifts, to map the key spectral diagnostics of star formation and dust extinction: H-alpha, Pa-alpha, and 3.3um PAH within individual distant galaxies. The targets are among the brightest, best-characterized lensed systems known, and span a wide range of specific star formation rate, extinction, and luminosity. They have extensive ancillary datasets. The TEMPLATES science goals are: 1) demonstrate extinction-robust star formation rate diagnostics for distant galaxies; 2) determine the physical scales of star formation in distant galaxies, in an extinction-robust way; 3) measure specific star formation rates and compare the spatial distribution of the young and old stars; and 4) measure the physical conditions of star formation and their spatial variation.
James Webb Space Telescope Early Release Observations (JWST-ERO)
The James Webb Space Telescope (JWST) Early Release Observations (EROs) are a set of science products created to mark the end of commissioning and the beginning of science operations for JWST. Colloquially known as the "Webb First Images and Spectra", these products were intended to demonstrate to the global public that JWST is ready for science and is capable of producing spectacular results. The package was released on 12 July 2022, and included images and spectra of the galaxy cluster SMACS J0723.3-7327 and distant lensed galaxies, the interacting galaxy group Stephan's Quintet, NGC 3324 in the Carina star-forming complex, the Southern Ring planetary nebula NGC 3132, and the transiting hot Jupiter WASP-96 b.
HST Photometry and Astrometry of the Bootes I Ultrafaint Dwarf Galaxy (BOOCATS)
Bootes I is a nearby, relatively bright ultrafaint dwarf galaxy. This dataset consists of two catalogs of sources in the line-of-sight to this ultrafaint galaxy, produced from deep, optical imaging in three fields, taken with the Hubble Space Telescope Advanced Camera for Surveys, Wide Field Camera. The first catalog contains photometry for the sources while the second catalog contains astrometric measurements, providing relative proper motions for the brighter sources.
Illustris Simulated Deep Fields (ILLUSTRIS)
This page hosts synthetic deep survey images from the Illustris Project cosmological simulations of galaxy formation. By projecting a line of sight through a periodic volume, the team constructed realistic mock surveys which preserve the predicted geometry of the simulations. With the emergence of large hydrodynamical simulations of galaxy formation, the team can now create these mock galaxy surveys with detail down to the size scales and distances revealed by HST, and in the future, those JWST and WFIRST will reveal. The Illustris Project consists of hydrodynamical simulations of galaxy formation in a volume 106.5 Mpc across, with detail resolved down to sub-kpc scales. Using the Arepo code, Illustris applied galaxy physics consisting of cooling, star formation, gas recycling, metal enrichment, supermassive black hole growth, and gas heating by feedback from supernovae and black holes. By converting simulations like these into synthetic observations, the team interprets HST observations with complex models of galaxy assembly, plan ahead for future missions, and directly contrast valuable survey data with our theoretical understanding of the physics behind the formation of galaxies. Here, the team presents "mock ultra-deep fields", each 2.2 to 19 arcminutes across, in common wide filters used by HST and JWST, as well as in filters expected to be used widely by observers with the Nancy Grace Roman space telescope (formerly "WFIRST"). The team presents mock lightcones from both the original Illustris-1 simulation, as well as from the IllustrisTNG suite of simulations. For each image, the team also provides the simulation catalog from which they generated each image, enabling users to locate sources, link them to intrinsic simulation quantities, and conduct analyses across observation and theory space.
WISE + Pan-STARRS1 Source Types and Redshifts with Machine Learning (WISE-PS1-STRM)
WISE-PS1-STRM is a neural network source classification and photometric redshift catalog extracted from a cross-match between the WISE All-Sky and PS1 3p DR2 source catalogs. The resulting catalog has 354,590,570 objects, significantly fewer than the parent PS1 catalog, but its combination of optical and infrared colors facilitate both better source classification and photometric redshift estimation. A neural network classified objects into galaxies, quasars, and stars, then another network estimated photometric redshifts for the galaxies. The star sample purity and quasar sample completeness measures improve substantially, and the resulting photo-z ’s are significantly more accurate in terms of statistical scatter and bias than those calculated from PS1 properties alone. See the README file and the primary reference paper for a detailed description of the catalog metadata.
COS Legacy Archive Spectroscopic SurveY (CLASSY)
The COS Legacy Spectroscopic SurveY (CLASSY) is a treasury survey that builds on the Hubble Space Telescope (HST) archive to construct the first high-quality, high-resolution far-ultraviolet (far-UV) spectral database of 45 nearby star-forming galaxies. The survey combines 177 orbits of archival observations with 135 new orbits (312 total orbits) of HST observations, or more than 600 total spectral images taken with the Cosmic Origins Spectrograph (COS). The CLASSY Treasury sample contains 45 star-forming galaxies selected to span similar properties as seen at high redshift, with a large range of masses, metallicities, ionization parameters, and densities, but enhanced star formation rates. The CLASSY spectral atlas contains a suite of emission and absorption features that enable investigations of the massive stellar population properties, the physical properties of large-scale outflows that regulate star formation, and the chemical abundance patterns of the gas and stars. Further, CLASSY will improve the diagnostic power of the rest-frame UV lines for use by future JWST/ELT surveys, providing a long-lasting legacy to the astronomical community for decades to come.
BlueTides Mock Image Catalogue (BLUETIDES)
The BlueTides Mock Image Catalogue is a catalogue of mock images of roughly 100,000 MUV= -22.5 to -19.6 mag galaxies from the BlueTides hydrodynamical simulation at z=7, 8, 9, 10, 11 and 12. This includes mock images of these galaxies with the James Webb, Hubble, Roman, and Euclid Space Telescopes, as well as Subaru and VISTA, in a range of near- and mid-infrared filters. These images are created from the stellar particle distribution of BlueTides galaxies, as determined through the detailed hydrodynamics of the cosmological simulation. Each star particle in each galaxy is assigned an SED based on its age and metallicity, and nebular continuum, line emission, and dust attenuation are modelled. Fluxes are taken from a convolution of the SEDs with the various filter transmission curves. The images show the 6x6 or 10x10 kpc fields of view surrounding each galaxy, depending on the telescope. The images are binned onto a pixel scale of 0.5 times the native pixel scale of each instrument. These images are convolved with model PSFs, to produce realistic estimates of what true images with these telescopes would look like, although non-convolved images are also available. The catalogue images have no noise, so that they can be adapted for specific use cases. Software for adding noise is available on GitHub, alongside software for accessing and visualising the catalogue data.
Neptune's Dark Vortex NDS-2018 (NDS-2018)
A Northern Dark Spot discovered in 2018 (NDS-2018) was detected in the annual observations of Neptune from the OPAL program. Once 2019 OPAL data showed that the spot was drifting very close to the equator, additional observing programs were conducted to understand how the dark vortex was changing on shorter time scales, and to capture finer detail by taking a higher number of blue (F467M) images in each HST orbit. Dark spots require high spatial resolution at blue wavelengths to be observed, so no ground-based observatory has yet published a detection of one. Only the Voyager 2 spacecraft and Hubble have made published observations of dark vortices on Neptune. Wong et al. (2022) reviews the overall collection of HST imaging data from the WFC3/UVIS instrument. These have been processed to correct for geometric distortion, cosmic ray hits, and fringing (at narrowband red wavelengths), then navigated to define latitude, longitude, emission, and incidence angles for each pixel. Frames have been corrected for loss of contrast due to scattered light from the wings of the point spread function, and limb darkening and large-scale zonal brightness variation were removed by constructing difference images. The team prepared stacks of coadded difference images to maximize PSF sampling and to reduce noise from pixel instability.
Roman Strongly Lensed Supernova Simulations (RSLSS)
Using anticipated characteristics of the Roman Space Telescope Type Ia supernova (SN Ia) survey, the team has constructed mock catalogs of expected resolved lensing systems and strongly lensed Type Ia and core-collapse (CC) SN light curves, including microlensing effects. The data products include mock catalogs for four Roman SN Ia survey variants and the High Latitude Survey (HLS), as well as 2.4 million simulated light curves (600k for each of 4 SN classes: Ia, Ibc, IIn, IIP) based on the Hounsell et al. 2018 "Allz" strategy. These products were used to predict that Roman will find ~11 lensed SNIa and ~20 CCSN for the fiducial SN Ia surveys, with a time delay precision of ~2 and 3 days (measured with the SNTD package: https://sntd.readthedocs.io/), respectively. The predicted parameters were then used to construct Fisher matrices, also included, and derive projected constraints on cosmological parameters for each SN Ia survey strategy.
Hubble Space Telescope Atlases of Cluster Kinematics (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.
TESS Eclipsing Binaries (TESS-EBS)
TESS-EBs is a catalog containing locations, ephemerides and basic light curve properties for eclipsing binary stars found in data from the Transiting Exoplanet Survey Satellite (TESS). Prša et al. 2022 discuss the selection criteria for eclipsing binary candidates, the detection of hither-to unknown eclipsing systems, the determination of ephemerides, the validation and triage process, and the derivation of heuristic estimates for the ephemerides. They also present statistical properties of the sample and qualitative estimates of completeness. Instead of keeping to the widely used discrete classes, the authors propose a binary star morphology classification based on a dimensionality reduction algorithm. The catalog will continue to be updated with new sectors of data as they become available. The deliverables presented here are curated by the TESS Eclipsing Binary Working Group, an open group of professional and citizen scientists.