Constraining the Milky Way's ultraviolet-to-infrared SED with Gaussian process regression. Issue 3 (15th September 2021)

• Record Type: Journal Article
• Authors: Fielder, Catherine E; Newman, Jeffrey A; Andrews, Brett H; Zasowski, Gail; Boardman, Nicholas F; Licquia, Tim; Masters, Karen L; Salim, Samir
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 508:Issue 3(2021)
• Page Start: 4459
• Page End: 4483
• Publication Date: 2021-09-15
• Subjects: Galaxy: fundamental parameters -- Galaxy: general -- Galaxy: structure; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab2618
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Improving our knowledge of global Milky Way (MW) properties is critical for connecting the detailed measurements only possible from within our Galaxy to our understanding of the broader galaxy population. We here train Gaussian process regression (GPR) models on SDSS (Sloan Digital Sky Survey) galaxies to map from galaxy properties (stellar mass, apparent axial ratio, star formation rate, bulge-to-total ratio, disc scale length, and bar vote fraction) to ultraviolet (UV; GALEX FUV / NUV ), optical (SDSS ugriz ), and infrared (IR; 2MASS JHKs and WISE W 1/ W 2/ W 3/ W 4) fluxes and uncertainties. With these models, we estimate the photometric properties of the MW, resulting in a full UV-to-IR spectral energy distribution (SED) as it would be measured externally, viewed face-on. We confirm that the MW lies in the green valley in optical diagnostic diagrams, but show for the first time that the MW is in the star-forming region in standard UV and IR diagnostics – characteristic of the population of red spiral galaxies. Although our GPR method predicts one band at a time, the resulting MW UV–IR SED is consistent with SEDs of local spirals with characteristics broadly similar to the MW, suggesting that these independent predictions can be combined reliably. Our UV–IR SED will be invaluable for reconstructing the MW's star formation history using the same tools employed for external galaxies, allowing comparisons of results from in situ measurements to those from the methods used for extragalactic objects.