Boissier, S., Boselli, A., Duc, P.-A., et al.
1994, The Structure of the Virgo Cluster of Galaxies from Rosat X-ray Images, Nature, 368, 828 2003, The Broadband Optical Properties of Galaxies with Redshifts 0.02 < z < 0.22, ApJ, 594, 186
Ram pressure stripping derivation software#
1996, SExtractor: Software for Source Extraction, A&AS, 117, 393 2010, Galaxy Luminosities, Stellar Masses, Sizes, Velocity Dispersions as a Function of Morphological Type, MNRAS, 404, 2087 2014, Galactic Star Formation Enhanced and Quenched by Ram Pressure in Groups and Clusters, MNRAS, 438, 444 2002, Passive Spiral Formation from Halo Gas Starvation: Gradual Transformation into S0s, ApJ, 577, 651 2000, The Origin of Star Formation Gradients in Rich Galaxy Clusters, ApJ, 540, 113 1999, Measuring and Modelling the Redshift Evolution of Clustering: The Hubble Deep Field North, MNRAS, 310, 540 Arnouts, S., Cristiani, S., Moscardini, L., et al.2009, The Seventh Data Release of the Sloan Digital Sky Survey, ApJS, 182, 543 2004, The Second Data Release of the Sloan Digital Sky Survey, AJ, 128, 502 Our results also indicate that it is possible to trace galaxies at different stages of stripping with the combination of H i gas content and location in projected phase space, which can be extended to other galaxy clusters that lack high-resolution H i imaging. Our results suggest that if there is any ram pressure stripping induced enhancement, it is at best locally modest, and galaxies undergoing enhancement make up a small fraction of the total sample. We are instead able to capture the overall quenching of star formation activity with increasing degree of ram pressure stripping, in agreement with previous studies. We find no clear evidence for enhancement in the integrated star formation activity of galaxies undergoing early to active stripping. We utilize a variety of star formation tracers, which include g - r, WISE - colors, and starburstiness that are defined by stellar mass and star formation rates to compare the star formation activity of galaxies at different stripping stages. We then employ a new scheme for galaxy classification which combines H i mass fractions and locations in projected phase space, resulting in a new sample of 365 galaxies.
We first use 48 galaxies undergoing different stages of stripping based on H i morphology, H i deficiency, and relative extent to the stellar disk, from the VIVA survey. We study galaxies undergoing ram pressure stripping in the Virgo cluster to examine whether we can identify any discernible trend in their star formation activity.
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