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MAST Staff - 2025 Jul 28

Updated HLSPs

  • Mega-MUSCLES v25: SEDs for a dozen stars are now updated with DEM models for the Extreme Ultraviolet and provide model uncertainties. More details in Wilson et al. 2025.
  • SMARTS DR2 provides 1 million simulated stellar light curves designed to mimic the Kepler Bonus Background data. Includes rotational variability from star spots, stellar activity cycles, and latitudinal differential rotation for the 4-year Kepler baseline.
  • TESS-SPOC was updated with calibrated light curves and target pixel files from 200 second TESS full frame images for the following sectors:
    • Sector 75 — 159,999 targets
    • Sector 76 — 160,000 targets
  • TICA quick-look calibrated full frame images from the following orbits are now available at MAST:
    • Sector 93, complete
    • Sector 94
      • Orbit 1, complete
      • Orbit 2, Part A
  • QLP calibrated light curves from TESS full frame images for Sector 92 are now available at MAST. This Sector adds ~ 2 million targets derived from 200 second cadence FFIs
A two-panel plot comparing the Spectral Energy Distributions (SEDs) of two stars GJ 676A (orange line) and LHS 2686 (red line) to the Sun (yellow line). The x-axis in both panels shows wavelength in Angstroms. The top panel displays the stellar flux as a function of wavelength, scaled to the Earth Equivalent Instellation Distance. This represents the amount of X-ray and ultraviolet light a planet would receive in each star's habitable zone compared to Earth. The legend in the bottom right indicates stellar masses: GJ 676A has 0.63 solar masses, and LHS 2686 has 0.16 solar masses. The top of the plot labels spectral regions from left to right: X-ray, EUV (Extreme Ultraviolet), FUV (Far Ultraviolet), NUV (Near Ultraviolet), and Optical/Infrared. The bottom panel shows the ratio of each star's SED to the Solar SED. The plot highlights how much more or less flux these stars emit at different wavelengths, with differences reaching up to four orders of magnitude at shorter (X-ray) wavelengths.
Figure 7 from Wilson et al. 2025. The following description is taken directly from the paper:

Top panel: SEDs of the hottest (GJ 676A) and second coolest (LHS 2686) compared with that of the Sun (Woods et al. 2009). The spectra are scaled to the Earth Equivalent Installation Distance (EEID, Mamajek & Stapelfeldt 2023).
Bottom panel: The flux ratios of the scaled M dwarf SEDs to the Solar SED.

 

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