Resolution Slightly Better Than FIR Murray+ (in prep.); Clark+ (2023) Herschel Far-Infrared 100, 160, 250 μm From NASA press release that came out on Monday!
Environments of Massive Stars Lindberg+ (2024) Over 42 000 massive stars found with the BEAST (M★ > 8 M☉ ) 100% of the 178 spectroscopically-identified massive stars successfully extracted
Environments of Massive Stars Lindberg+ (2024) Over 42 000 massive stars found with the BEAST (M★ > 8 M☉ ) 100% of the 178 spectroscopically-identified massive stars successfully extracted! Massive stars in the rings Massive stars between the rings
Environments of Massive Stars Lindberg+ (2024) ); Delcanton+ (2015 Previous best-resolution dust map of M31: resolution of 25 pc From measuring dust reddening of the red giant brand in the CMD
Environments of Massive Stars Lindberg+ (2024) Results from 25 pc dust map suggested that massive stars in areas with lower stellar density (ie, outside rings/arms) exhibit more extinction
Environments of Massive Stars Lindberg+ (2024) Results from 25 pc dust map suggested that massive stars in areas with lower stellar density (ie, outside rings/arms) exhibit more extinction Theory says this is what we expect if most massive stars outside the rings are runaways
Environments of Massive Stars Lindberg+ (2024) Massive stars seem to experience the same extinction (on average) regardless of location Suggests that massive stars in areas of low stellar density (ie, outside rings/arms), were born there
to Make Hi-Res BEAST Dust Maps? Lindberg+ (in prep.); Murray+ (2024) We want to turn a large number of individual point measurements of dust extinction into a map of the underlying dust structure. Can do this using Gaussian Process Regression!
to Make Hi-Res BEAST Dust Maps? Lindberg+ (in prep.); Murray+ (2024) We want to turn a large number of individual point measurements of dust extinction into a map of the underlying dust structure. Can do this using Gaussian Process Regression! Herschel PSF at 500 μm (15 pc in LMC)
(in prep.); McQuinn+ (2013,2015); Skillman+ (2013); Evans+ (2019) Leo P ACS F475W ACS F814W WFC3 F110W ISM metallicity 0.03 Z⊙ Distance 1.62 Mpc Stellar mass 105.7 M⊙ HI mass 105.9 M⊙
the BADGRs Clark+ (in prep.); Clark+ (2015,2018); Nersesian+ (2019) Star-by-star extinction mapping in these BADGRs will let us: • Probe the dust geometry at high resolution; is it clumpy? • See if dust is just far away from UV radiation sources • Measure the dust’s intrinsic emissivity, by comparing extinction to far-IR emission • Check for CO freeze-out, by comparing extinction to ALMA data • Use extinction as tracer of total gas column, and search for dark gas by comparing to HI and CO columns NGC 7793 NGC 4449
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