Mathematics – Logic
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21711501a&link_type=abstract
American Astronomical Society, AAS Meeting #217, #115.01; Bulletin of the American Astronomical Society, Vol. 43, 2011
Mathematics
Logic
Scientific paper
In recent years, both observations and simulations have shown that ICM-ISM stripping is likely an important driver of galaxy evolution. In order to understand the impact of stripping on galaxy evolution, it is vital to determine how the multi-phase ISM behaves during stripping, how long it takes to strip a galaxy, and how stripping influences star formation. We present multi-wavelength studies of three Virgo Cluster spirals undergoing active ram pressure stripping, including two with HST imaging. We estimate timescales for various stripping-related processes in the galaxies and identify signatures of stripping in the galaxies’ ISM and star formation distributions. All three have undisturbed old stellar disks and show one-sided extraplanar ISM distributions. This extraplanar ISM hosts regions of ongoing and recent star formation that has taken place within the past few hundred Myr, with some regions significantly younger. The galaxy NGC 4330 has distinct leading and trailing sides, including a striking ISM “upturn” feature at the leading edge. There are significant differences between the galaxy’s optical, UV, H α, and HI morphologies, and we use stellar population models to estimate that it has taken 200-400 Myr to strip the ISM from a radius of >8 to 5 kpc on the galaxy’s leading side. HST imaging reveals that NGC 4522 and NGC 4402 have GMC-mass dust clouds located outside of their main ISM truncation radii, showing that the most massive clouds can decouple from the rest of the ISM during stripping. Dust features with linear morphologies in both galaxies reveal the projected ICM wind direction. By identifying morphological characteristics related to the ram pressure stripping process, we constrain the physics of interactions between the ICM and the complex multi-phase ISM, and we provide a foundation for future observational and theoretical studies investigating the extent to which ICM-ISM interactions drive galaxy evolution.
Abramson Anne
Kenney Jeffrey D. P.
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