Stellar Cartography

The Mega-MUSCLES Treasury Survey: X-ray to Infrared Spectral Energy Distributions of a Representative Sample of M dwarfs

By Keith Cowing
Status Report
astro-ph.EP
November 20, 2024
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The Mega-MUSCLES Treasury Survey: X-ray to Infrared Spectral Energy Distributions of a Representative Sample of M dwarfs
Comparison of blue-optical data of GJ 729, for which the most data is available from our sources. Top panel: Comparison of STIS G430L, CASLEO and X-shooter spectra, as well as Swift U band photometry and the PHOENIX model spectrum. Bottom panel: Ratio between the G430L and PHOENIX spectrum. Similar trends are seen at all other stars. — astro-ph.EP

We present 5-1×10^7 Angstrom spectral energy distributions (SEDs) for twelve M dwarf stars covering spectral types M0-M8. Our SEDs are provided for community use as a sequel to the Measurements of the Ultraviolet Spectral Characteristics of Low-mass Exoplanetary Systems (MUSCLES) survey.

The twelve stars include eight known exoplanet hosts and four stars chosen to fill out key parameter space in spectral type and rotation period. The SEDs are constructed from Hubble Space Telescope ultraviolet spectroscopy and XMM Newton, Chandra and/or Swift X-ray observations and completed with various model data, including Lyman alpha reconstructions, PHOENIX optical models, APEC coronal models and Differential Emission Measure models in the currently-unobservable Extreme Ultraviolet.

We provide a complete overview of the Mega-MUSCLES program, including a description of the observations, models, and SED construction. The SEDs are available as MAST High-Level Science Products and we describe the various data products here. We also present ensemble measurements from our sample that are of particular relevance to exoplanet science, including the high-energy fluxes in the habitable zone and the FUV/NUV ratio.

Combined with MUSCLES, Mega-MUSCLES provides SEDs covering a wide range of M-dwarf spectral types and ages such that suitable proxies for any M-dwarf planet host of interest may be found in our sample. However, we find that ultraviolet and X-ray fluxes can vary even between stars with similar parameters, such that observations of each exoplanet host star will remain the gold standard for interpreting exoplanet atmosphere observations.

David J. Wilson, Cynthia S. Froning, Girish M. Duvvuri, Allison Youngblood, Kevin France, Alexander Brown, Zachory Berta-Thompson, P. Christian Schneider, Andrea P. Buccino, Jeffrey Linsky, R. O. Parke Loyd, Yamila Miguel, Elisabeth Newton, J. Sebastian Pineda, Seth Redfield, Aki Roberge, Sarah Rugheimer, Mariela C. Vieytes

Comments: Updated Mega-MUSCLES SEDs available at this https URL
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR)
Cite as: arXiv:2411.07394 [astro-ph.EP] (or arXiv:2411.07394v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2411.07394
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Submission history
From: David Wilson
[v1] Mon, 11 Nov 2024 22:03:30 UTC (3,887 KB)
https://arxiv.org/abs/2411.07394

Astrobiology,

Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻