Gas Mass Fractions and Disk Regrowth Potential in Local Blue-Sequence E/S0s

Details Gas Mass Fractions and Disk Regrowth Potential in Local Blue-Sequence E/S0s Gas Mass Fractions and Disk Regrowth Potential in Local Blue-Sequence E/S0s

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21532902w&link_type=abstract

American Astronomical Society, AAS Meeting #215, #329.02; Bulletin of the American Astronomical Society, Vol. 42, p.426

Astronomy and Astrophysics

Astronomy

Scientific paper

Recent work has identified a population of local E/S0 galaxies that lie on the blue sequence in color vs. stellar mass parameter space, where spiral galaxies typically reside. While high-mass blue-sequence E/S0s may often be young merger/interaction remnants likely to fade to the red sequence, we focus on blue-sequence E/S0s with lower stellar masses (M* < few times 1010 M&sun;), which are characterized by fairly regular morphology and low density field environments where fresh gas infall is possible. This population may provide an evolutionary link between traditional early type galaxies and spirals through disk regrowth. Based on new GBT and VLA data for a representative sample of E/S0s, the atomic gas to stellar mass ratios for most blue-sequence E/S0s range from 0.1 to 1.0, comparable to those of spiral and irregular galaxies. Assuming that the HI is accessible for star formation, we find that at least half of our blue-sequence E/S0s can increase their stellar masses by 10-60% in 3 Gyr. We present evidence that star formation in these galaxies is bursty and likely involves externally triggered gas inflows. We also present CARMA CO 1-0 maps of select blue-sequence E/S0s and discuss these maps' implications for the disk regrowth scenario.

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