The Resolved Stellar Populations in the LEGUS Galaxies1
Sabbi, E; Calzetti, D; Ubeda, L; et al.Adamo, A; Cignoni, M; Thilker, D; Aloisi, A; Elmegreen, BG; Elmegreen, DM; Gouliermis, DA; Grebel, EK; Messa, M; Smith, LJ; Tosi, M; Dolphin, A; Andrews, JE; Ashworth, G; Bright, SN; Brown, TM; Chandar, R; Christian, C; Clayton, GC; Cook, DO; Dale, DA; De Mink, SE; Dobbs, C; Evans, AS; Fumagalli, M; Gallagher, JS; Grasha, K; Herrero, A; Hunter, DA; Johnson, KE; Kahre, L; Kennicutt, RC; Kim, H; Krumholz, MR; Lee, JC; Lennon, D; Martin, C; Nair, P; Nota, A; Ostlin, G; Pellerin, A; Prieto, J; Regan, MW; Ryon, JE; Sacchi, E; Schaerer, D; Schiminovich, D; Shabani, F; Van Dyk, SD; Walterbos, R; Whitmore, BC; Wofford, A
Date: 15 March 2018
Astrophysical Journal, Supplement Series
American Astronomical Society / IOP Publishing
The Legacy ExtraGalactic UV Survey (LEGUS) is a multiwavelength Cycle 21 Treasury program on the Hubble Space Telescope. It studied 50 nearby star-forming galaxies in 5 bands from the near-UV to the I-band, combining new Wide Field Camera 3 observations with archival Advanced Camera for Surveys data. LEGUS was designed to investigate ...
The Legacy ExtraGalactic UV Survey (LEGUS) is a multiwavelength Cycle 21 Treasury program on the Hubble Space Telescope. It studied 50 nearby star-forming galaxies in 5 bands from the near-UV to the I-band, combining new Wide Field Camera 3 observations with archival Advanced Camera for Surveys data. LEGUS was designed to investigate how star formation occurs and develops on both small and large scales, and how it relates to the galactic environments. In this paper we present the photometric catalogs for all the apparently single stars identified in the 50 LEGUS galaxies. Photometric catalogs and mosaicked images for all filters are available for download. We present optical and near-UV color-magnitude diagrams for all the galaxies. For each galaxy we derived the distance from the tip of the red giant branch. We then used the NUV color-magnitude diagrams to identify stars more massive than 14 Mo, and compared their number with the number of massive stars expected from the GALEX FUV luminosity. Our analysis shows that the fraction of massive stars forming in star clusters and stellar associations is about constant with the star formation rate. This lack of a relation suggests that the timescale for evaporation of unbound structures is comparable or longer than 10 Myr. At low star formation rates this translates to an excess of mass in clustered environments as compared to model predictions of cluster evolution, suggesting that a significant fraction of stars form in unbound systems.
Physics and Astronomy
College of Engineering, Mathematics and Physical Sciences
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