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dc.contributor.authorGim, Hansung B.
dc.contributor.authorBorthakur, Sanchayeeta
dc.contributor.authorMomjian, Emmanuel
dc.contributor.authorPadave, Mansi
dc.contributor.authorJansen, Rolf A.
dc.contributor.authorNelson, Dylan
dc.contributor.authorHeckman, Timothy M.
dc.contributor.authorKennicutt Jr., Robert C.
dc.contributor.authorFox, Andrew J.
dc.contributor.authorPineda, Jorge L.
dc.contributor.authorThilker, David
dc.contributor.authorKauffmann, Guinevere
dc.contributor.authorTumlinson, Jason
dc.identifier.citationGim, Hansung B., Sanchayeeta Borthakur, Emmanuel Momjian, Mansi Padave, Rolf A. Jansen, Dylan Nelson, Timothy M. Heckman et al. "DIISC-I: The Discovery of Kinematically Anomalous H i Clouds in M 100." The Astrophysical Journal 922, no. 1 (2021): 69.en_US
dc.description.abstractWe report the discovery of two kinematically anomalous atomic hydrogen (H i) clouds in M 100 (NGC 4321), which was observed as part of the Deciphering the Interplay between the Interstellar medium, Stars, and the Circumgalactic medium (DIISC) survey in H i 21 cm at 3.3 km s−1 spectroscopic and 44″ × 30″ spatial resolution using the Karl G. Jansky Very Large Array. 15 15 The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. These clouds were identified as structures that show significant kinematic offsets from the rotating disk of M 100. The velocity offsets of 40 km s−1 observed in these clouds are comparable to the offsets seen in intermediate-velocity clouds (IVCs) in the circumgalactic medium (CGM) of the Milky Way and nearby galaxies. We find that one anomalous cloud in M 100 is associated with star-forming regions detected in Hα and far-ultraviolet imaging. Our investigation shows that anomalous clouds in M 100 may originate from multiple mechanisms, such as star formation feedback-driven outflows, ram pressure stripping, and tidal interactions with satellite galaxies. Moreover, we do not detect any cool CGM at 38.8 kpc from the center of M 100, giving an upper limit of N(H i) ≤1.7 × 1013 cm−2 (3σ). Since M 100 is in the Virgo cluster, the nonexistence of neutral/cool CGM is a likely pathway for turning it into a red galaxy.en_US
dc.publisherAmerican Astronomical Societyen_US
dc.subjectkinematically anomalous cloudsen_US
dc.subjectinterstellar cloudsen_US
dc.subjectinterstellar mediumen_US
dc.subjectvirgo clusteren_US
dc.titleDIISC-I: The Discovery of Kinematically Anomalous H i Clouds in M 100en_US
mus.citation.journaltitleThe Astrophysical Journalen_US
mus.relation.collegeCollege of Letters & Scienceen_US
mus.relation.universityMontana State University - Bozemanen_US

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