Journal
ASTROPHYSICAL JOURNAL
Volume 870, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aaefff
Keywords
galaxies: clusters: individual (D100); galaxies: evolution; galaxies: ISM; galaxies: peculiar; galaxies: star formation; galaxies: structure
Categories
Funding
- STScI grant [HST-GO-14361.003]
- NASA [NAS 5-26555]
- NSF [1714764]
- Chandra Award [GO6-17111X]
- Ministry of Education, Youth and Sports of the Czech Republic [LM2015067]
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Center for High-Performance Computing at the University of Utah
- Spanish MINECO [AyA2014-55216]
- STFC [ST/R000840/1] Funding Source: UKRI
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We present new HST F275W, F475W, and F814W imaging of the region of the Coma cluster around D100, a spiral galaxy with a remarkably long and narrow (60 x 1.5 kpc) ram pressure-stripped gas tail. We find blue sources coincident with the Ha tail, which we identify as young stars formed in the tail. We also determine they are likely to be unbound stellar complexes with sizes of similar to 50-100 pc, likely to disperse as they age. From a comparison of the colors and magnitudes of the young stellar complexes with simple stellar population models, we find ages ranging from similar to 1 to 50 Myr and masses ranging from 10(3) to similar to 10(5) M-circle dot. We find that the overall rate and efficiency of star formation are low, similar to 6.0 x 10(-3) M-circle dot yr(-1) and similar to 6 x 10(-12) yr(-1), respectively. The total H alpha flux of the tail would correspond to a star formation rate 7 times higher, indicating that some other mechanism for H alpha excitation is dominant. From an analysis of the colors, we track the progression of outside-in star formation quenching in the main body of D100, as well as its apparent companion, S0 D99. Finally, we observe that the dust extinction in the base of the tail has an outer envelope with remarkably smooth and straight edges and linear filamentary substructure strongly suggestive of magnetic fields. These features and the small amount of tail broadening strongly suggest gas cooling restricting broadening and the influence of magnetic fields inhibiting turbulence.
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