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천문학회지(JKAS) , Vol.54 no.1 (2021)
pp.17~35

DOI : 10.5303/JKAS.2021.54.1.017

STAR FORMATION ACTIVITY OF GALAXIES UNDERGOING RAM PRESSURE STRIPPING IN THE VIRGO CLUSTER

Jae Yeon Mun

(Department of Physics and Astronomy, Seoul National University)

Ho Seong Hwang

(Korea Astronomy and Space Science Institute)

Myung Gyoon Lee

(Department of Physics and Astronomy, Seoul National University)

Aeree Chung

(Department of Astronomy, Yonsei University)

Hyein Yoon

(Department of Astronomy, Yonsei University/Sydney Institute for Astronomy, School of Physics/ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D))

Jong Chul Lee

(Korea Astronomy and Space Science Institute)

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. We first use 48 galaxies undergoing different stages of stripping based on Hi morphology, Hi deficiency, and relative extent to the stellar disk, from the VIVA survey. We then employ a new scheme for galaxy classification which combines Hi mass fractions and locations in projected phase space, resulting in a new sample of 365 galaxies. We utilize a variety of star formation tracers, which include g - r, WISE [3.4]-[12] 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 find no clear evidence for enhancement in the integrated star formation activity of galaxies undergoing early to active stripping. 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. 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. Our results also indicate that it is possible to trace galaxies at different stages of stripping with the combination of Hi gas content and location in projected phase space, which can be extended to other galaxy clusters that lack high-resolution Hi imaging.

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