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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: 216
Showing 15 matching items

The Cosmic Evolution Early Release Science Survey (CEERS)

The Cosmic Evolution Early Release Science Survey (CEERS) covers 100 sq. arcmin of the Extended Groth Strip (EGS) field with JWST NIRCam imaging in parallel to MIRI imaging, NIRSpec and NIRCam wide-field slitless spectroscopy, all in a region supported by a rich set of HST/CANDELS multi-wavelength data. CEERS demonstrates, tests, and validates efficient extragalactic surveys with coordinated, overlapping parallel observations. The observations were obtained in two epochs in Cycle 1. In June, 2022, four pointings of MIRI imaging (F560W, F770W, F1000W, F1280W, F1500W, F1800W, and F2100W) were obtained with NIRCam imaging in parallel (F115W, F150W, F200W, F277W, F356W, F410M, F444W). In December, 2022, six pointings of NIRSpec multi-object spectroscopy with the PRISM (R~100) and medium resolution gratings (G140M/F100LP, G235M/F170LP, G395M/F290LP; R~1000) were obtained with NIRCam imaging in parallel. Four of these pointings were also observed with NIRCam slitless grism spectroscopy (R~1500) with MIRI imaging in parallel.

Low Resolution Stellar Library (LOWLIB)

"Stellar libraries" are collections of stellar spectra. Such libraries find use in population synthesis studies, stellar parameter estimation, exposure time calculators, mission planning, and education. This HLSP contains 513 stellar spectra in FITS files. The spectra are flux calibrated, dereddened, and shifted to zero velocity. Observed with three low resolution gratings from the HST Space Telescope Imaging Spectrograph(STIS) and then merged into one continuous spectrum, these spectra cover roughly 0.2 < ? < 1 µm at ?/?? about 1000. This "HST Low Resolution Stellar Library" extends and supersedes NGSL, the "Next Generation Stellar Library," and comes as a companion to the Hot Star Library (Khan & Worthey 2018, A&A, 615, 115).

CANDELS Lyman Alpha Emission at Reionization Survey (CLEAR)

The CANDELS Lyman-alpha Emission at Reionization (CLEAR) survey is a HST Cycle 23 program that obtained 12-orbit depth observations with the HST/WFC3 using the G102 grism in the IR camera in 12 fields split between the GOODS-N and GOODS-S fields from the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). Combined with existing spectroscopic data (G102 and G141) from other programs, the dataset released here includes 1D and 2D spectra over (partially- or fully-covered) 0.8-1.7 um for 6048 galaxies in GOODS-South and GOODS-North to m_H = 25. In addition, this release includes updated photometric catalogs from the 3D-HST survey, and spectroscopic catalogs that include emission line fluxes and redshifts derived from the combination of the photometry and grism spectroscopy. The primary goal of CLEAR was to characterize the evolution of the Lyman-? equivalent width distribution at 6 < z < 8 and to interpret this in the context of reionization. The CLEAR dataset also allows for studies of the stellar populations, star-formation, ionization, and chemical enrichment of galaxies in the distant universe (from redshifts 0.5 to 3).

Space Telescope and Optical Reverberation Mapping of Mrk 817 (STORM2)

Calibrated spectra and light curves are provided for the HST/COS observations of the Seyfert 1 galaxy Mrk 817 in the Space Telescope and Optical Reverberation Mapping 2 (STORM 2) campaign. The STORM 2 campaign used HST/COS, Swift, NICER, XMM-Newton, and ground-based facilities in a 15-month long reverberation-mapping experiment. HST observations were made in 165 single-orbit COS visits with a mean cadence of two days from 2020 November 24 through 2022 February 24. In each visit, the team used the G130M and G160M gratings to observe the UV spectrum over the range 1070-1750 Angstroms in eight separate exposures. Exposure times were selected to provide S/N > 100 when measured over velocity bins of ~500 km/s. During each visit, the team obtained four 60-second exposures with G130M centered at 1222 Angstroms, two exposures of 175 s and 180 s using the G160M grating centered at 1533 Angstroms, and two 195 s exposures with G160M at 1577 Angstroms. As described in Homayouni et al. (2023), the team customized the calibrations of these spectra to provide more accurate and repeatable flux calibrations. These reprocessed spectra obtained with the various central wavelength and FPPOS settings were then combined for each individual observation into single spectra for G130M and G160M, single merged G130M+G160M spectra, a merged spectrum for the whole data set, and extracted continuum and emission-line light curves.

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.