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. Use the filters below to discover HLSP.



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Listing Results

Results: 149

Hubble eXtreme Deep Field

The XDF includes all optical and infrared data taken by Hubble covering the original Hubble Ultra-Deep Field (HUDF) program, with just a few exceptions. Small amounts of data taken with unusual or rarely used filters and spectroscopic data are not included. The XDF also includes images which only partially cover the HUDF. The data used to generate the XDF were taken over the decade from mid-2002 to the end of 2012. The total exposure on the XDF is about 1.8 million seconds using data from Hubble's two main workhorse cameras, the Advanced Camera for Surveys Wide Field Channel (ACS/WFC) and the Wide Field Camera 3 InfraRed Channel (WFC3/IR). Substantial gains accrue from using all the ACS data taken over the decade since 2002, as well as from the improved processing techniques since the HUDF was released. The gains in the XDF are equivalent to adding about 180 orbits of data to the original HUDF dataset.

A Comprehensive UV Spectral Linelist of White Dwarf G191-B2B

A team led by Simon Preval have created one of the most complete UV linelists of a white dwarf. Co-adding over 150 spectra from both HST STIS and FUSE, the team was able to identify nearly 950 absorption lines with equivalent widths as small as a few milli-Angstroms. They were able to identify every observed feature in the coadded FUSE spectrum, and nearly every feature in the coadded STIS spectrum. In addition to line identification, the team was able to measure abundances for 9 elements (C, N, O, Al, Si, P, S, Fe, Ni). At MAST, the team provides the complete linelist, as well as the spectra (both the individual and coadded versions).

Ultraviolet-bright Quasar Survey

The UV-bright Quasar Survey (UVQS) first data release (DR1) for new z~1 active galactic nuclei (AGN) across the sky contains data products and results from ground-based optical spectra of 1040 AGN candidates, selected from GALEX UV and WISE NIR color criteria. The source list contains 217 previously unreported AGN with FUV < 18 mag and redshifts generally at z > 0.5. For each source, the database includes a FITS file of the flux-calibrated, one-dimensional spectrum, a PDF plot of the spectrum with the best-fit comparison model, a redshift determination, and a PDF plot of an optical image.

All-Sky Mapping of the UV Diffuse Radiation As Observed by GALEX

Jayant Murthy has created maps of the diffuse UV radiation, in both FUV and NUV bands, using the latest GALEX all-sky data release (GR6+GR7). Tables are provided of the diffuse radiation for each GALEX visit at a resolution of 2 arcminutes, organized by galactic latitude. In addition to the diffuse background fluxes in NUV and FUV, this HLSP also provides estimates of the geocoronal and zodiacal foreground emissions for each binned pixel. A separate text table provides the estimated foreground corrections, at the observation (coadd) level, for each tile by taking the weighted average of the geocoronal and zodical emissions at the visit level. Aitoff projections of both the FUV and NUV diffuse radiation (and its variance), along with a 100-micron emission map based on the Schlegel et al. (1998) dust maps, are provided in FITS format. Finally, a table of GALEX spacecraft telemetry used to generate these data products is included.

Ultra Deep Field ACS-HRC Parallels

The ACS Ultra Deep Field (UDF) is a survey carried out using the Advanced Camera for Surveys (ACS) on HST. The UDF will consist of a single ultra-deep field (412 orbits in total) within the CDF-S GOODS area. Scientific drivers of the UDF include probing the tail of the reionization epoch, constraining the star formation history of the Universe, probing the faint end of the galaxy luminosity function, and tracking the origin, structure, and merger history of galaxies as they evolve onto and off the Hubble sequence. There is also a NICMOS companion survey designed to complete the image set with deep near-IR NICMOS images at 1.1 and 1.6 microns over a significant fraction of the UDF, providing a critical link between the HST ACS and SIRTF observations.

Ultraviolet Imaging of the UDF and the HDF

Wavelength coverage of the Hubble Ultra Deep Field (HUDF) has been been extended with deep ultraviolet wavelength observations. Observations acquired with the ACS-SBC in the Far-UV (1500 Angstroms) and WFPC2 in the Near-UV (F300W) during execution of the HST Treasury program 10403 (PI Harry Teplitz). Included with this set of data are ACS/SBC observations of the Hubble Deep Field North.

TESS-HERMES Spectroscopic Survey

The TESS-HERMES project is a spectroscopic survey using the HERMES multi-object instrument on the Anglo-Australian Telescope (AAT). So far, the survey has observed ~16,000 dwarf and subgiant stars in the southern TESS Continuous Viewing Zone (CVZ). Targets in the CVZ have overlap with every TESS sector, and thus will get a full 12 months of data. It also overlaps with the JWST CVZ, making these targets optimal for follow-up with that telescope. The TESS-HERMES project derives stellar properties (effective temperature, surface gravity, [Fe/H], v*sin(i), microturbulence, distance, extinction, mass, radius, ages) using a Bayesian approach, spectral analysis, and theoretical isochrones. This catalog of stellar parameters is available now, while the calibrated spectra are planned for a future release at MAST.

STIS Next Generation Spectral Library (AR10659)

The Next Generation Spectral Library (NGSL) consists of spectra for 374 stars, all observed in the same way, and all spectra covering the spectral range, ~0.2-1.0 microns, at a resolving power R ~1000. As part of HST proposal AR 10659, the team worked to derive a wavelength-dependent correction to the slit throughput as a function of offset from the slit center, delivering Version 1 of the NGSL to MAST as an HLSP. In HST proposal GO/CAL 11652, the team derived an improved slit-throughput correction based on post-SM4 observations of a standard star (BD+75D325), which was stepped across the slit. In HST proposal AR 11755, the team incorporated the observed slit-throughput corrections in this new version of the Next Generation Spectral Library.

HST STIS Echelle Spectral Catalog of Stars

StarCAT is a catalog of high resolution ultraviolet spectra of objects classified as stars, recorded by Space Telescope Imaging Spectrograph (STIS) during its initial seven years of operations (1997-2004). StarCAT is based on 3184 echelle mode observations of 545 distinct targets, with a total exposure duration of 5.2 Ms. For many of the objects, broad ultraviolet coverage has been achieved by splicing together echellegrams taken in two or more FUV (1150-1700 Angstroms) and/or NUV (1600-3200 Angstroms) settings. In cases of multiple pointings on conspicuously variable sources, spectra were separated into independent epochs. In cases of nonvariable, or lightly variable, objects, different epochs were combined to enhance signal-to-noise (S/N).

STARBurst IRregular Dwarf Survey

STARBIRDS combines new and archival observations for 20 nearby, starburst and post-starburst dwarf galaxies from GALEX, Hubble, and Spitzer. The images are registered to a common world coordinate system, flux calibrated, and background-subtracted. A set of GALEX and Spitzer images are made available cropped to match the Hubble field-of-view, while another set of Hubble images are convolved with a 5-arcsecond point spread function and rebinned to the GALEX and Spitzer resolutions.

Spiral Galaxies

Holwerda et al. (2005) examined 32 HST/WFPC2 archival fields of 29 spiral galaxies (type Sab and later). The majority of the data are from the Cepheid distance scale Key Project. The explicit goal was to provide deep mosaics in both V- and I-band with a better sampling in order to identify background galaxies through the foreground disk.

Catalogs of Cosmologically Useful Type Ia Supernovae from Pan-STARRS

The Pan-STARRS Supernova (PS1 SN) Cosmology data release contains light curves, host galaxy spectra, light curve parameters, distance measurements, and cosmology fitter input files that can be used to measure the dark energy equation of state using two PS1 SN datasets. The first dataset (Scolnic et al. 2018) is the Pantheon sample, which combines spectroscopically classified PS1 SNe Ia with Sloan Digital Sky Survey, SuperNova Legacy Survey, and Low-z SNe Ia. These SNe were used to measure the dark energy equation of state in Scolnic et al. (2018), who find a value of -1.026 +/- 0.041. The second dataset (Jones et al. 2018) includes 1,174 Pan-STARRS SNe without spectroscopic classifications. Approximately 95% of these data SNe are of Type Ia, with the remainder being Core-Collapse (CC) SNe. Jones et al. (2018) use a Bayesian methodology to marginalize over CC SNe in these data and, after combining the sample with low-z SNe Ia, measure the dark energy equation of state to be -0.989 +/- 0.057.

Probing Evolution And Reionization Spectroscopically

PEARS is an HST program that was conducted in the GOODS North and GOODS South fields using the Advanced Camera for Surveys in Cycle 14. Observations were made during the period 2005 August 8 to 2006 February 17. Slitless spectra over both fields were obtained with the ACS Wide Field Camera (WFC) and the G800L grism over the 204x204 arcsec detector area. Short F606W images were also obtained to align to the GOODS astrometry and to provide the zero point of the slitless spectra. The G800L grism provides slitless spectra with a dispersion of about 40 Angstroms per pixel. The grism first order covers 5500-10500 Angstroms, with a peak sensitivity around 7500 Angstroms.

The HST Treasury Program on the Orion Nebula Cluster

The Orion Nebula hosts the richest cluster of young pre-main-sequence stars within 1 kpc from the Sun and therefore represents an ideal laboratory to understand the process of star formation. The "ORION" HLSP is an HST Treasury Program on the Orion Nebula cluster (GO-10246, PI M. Robberto) that has obtained deep multi-color photometry of thousand of sources well into the brown-dwarf regime, complemented by a rich set of ancillary data from ground-based observatories.

Kepler Light Curves Optimized For Asteroseismolog

KEPSEISMIC light curves are obtained from Kepler pixel-data files using large custom apertures that produce more stable light curves on longer time scales for seismic studies. For each pixel in the pixel-data file, a reference weighted flux value is computed as the 99.9th percentile of the flux divided by its error representing a measure of the signal-to-noise ratio. The resultant light curve is processed through the implementation of the Kepler Asteroseismic Data Analysis and Calibration Software, correcting for outliers, jumps, and drifts, and properly concatenating the independent Kepler Quarters in a star-by-star basis. It also fills the gaps shorter than 20 days in long cadence data following in-painting techniques. The resulting light curves are high-pass filtered at 20, 55, and 80 days yielding three different light curves for each target.