Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 466, Issue 2, Pages 1382-1398Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw3162
Keywords
ISM: molecules; galaxies: clusters: intracluster medium; galaxies: evolution galaxies: ISM; galaxies: spiral
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Funding
- National Research Foundation of Korea [2010-0027910]
- Science Fellowship of POSCO TJ Park Foundation
- NRF [2015R1D1A1A01060516]
- Smithsonian Institution
- Academia Sinica
- Alvin E. Nashman Fellowship in Theoretical Astrophysics
- National Research Foundation of Korea [2015R1D1A1A01060516, 2010-0027910] Funding Source: Korea Institute of Science & Technology Information (KISTI), National Science & Technology Information Service (NTIS)
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We present 12CO (2-1) data of three Virgo spirals - NGC 4330, NGC 4402 and NGC 4522 obtained using the Submillimeter Array. These three galaxies show clear evidence of ram pressure stripping due to the cluster medium as found in previous HI imaging studies. Using the high-resolution CO data, we investigate how the properties of the inner molecular gas disc change while a galaxy is undergoing HI stripping in the cluster. At given sensitivity limits, we do not find any clear signs of molecular gas stripping. However, both its morphology and kinematics appear to be quite disturbed as those of HI. Morphological peculiarities present in the molecular and atomic gas are closely related with each other, suggesting that the molecular gas can be also affected by strong intracluster medium (ICM) pressure even if it is not stripped. CO is found to be modestly enhanced along the upstream sides in these galaxies, which may change the local star formation activity in the disc. Indeed, the distribution of Ha emission, a tracer of recent star formation, well coincides with that of the molecular gas, revealing enhancements near the local CO peak or along the CO compression. FUV and Ha share some properties in common, but FUV is always more extended than CO/Ha in the three galaxies, implying that the star-forming disc is rapidly shrinking as the molecular gas properties have changed. We discuss how ICM pressure affects dense molecular gas and hence star formation properties while diffuse atomic gas is being removed from a galaxy.
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