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Title:
The Disruption and Fueling of M33
Authors:
Putman, M. E.; Peek, J. E. G.; Muratov, A.; Gnedin, O. Y.; Hsu, W.; Douglas, K. A.; Heiles, C.; Stanimirovic, S.; Korpela, E. J.; Gibson, S. J.
Affiliation:
AA(Department of Astronomy, Columbia University, New York, NY 10027, USA ), AB(Astronomy Department, University of California at Berkeley, Berkeley, CA 94720-3411, USA ), AC(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA ), AD(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA ), AE(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA ), AF(Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA ; School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK ), AG(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA ), AH(Department of Astronomy, University of Wisconsin - Madison, Madison, WI 53706-1582, USA ), AI(Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA ), AJ(Arecibo Observatory, National Astronomy and Ionosphere Center, Arecibo, PR 00612, USA ; Department of Physics and Astronomy, Western Kentucky University, Bowling Green, KY 42101, USA)
Publication:
The Astrophysical Journal, Volume 703, Issue 2, pp. 1486-1501 (2009). (ApJ Homepage)
Publication Date:
10/2009
Origin:
IOP
ApJ Keywords:
galaxies: evolution, galaxies: individual: M33, galaxies: halos, galaxies: ISM, galaxies: kinematics and dynamics, Local Group
DOI:
10.1088/0004-637X/703/2/1486
Bibliographic Code:
2009ApJ...703.1486P

Abstract

The disruption of the M33 galaxy is evident from its extended gaseous structure. We present new data from the Galactic Arecibo L-Band Feed Array H I (GALFA-H I) Survey that show the full extent and detailed spatial and kinematic structure of M33's neutral hydrogen. Over 18% of the H I mass of M33 (M_HI_{tot}=1.4 \times 10^9 M sun) is found beyond the star-forming disk as traced in the far-ultraviolet (FUV). The most distinct features are extended warps, an arc from the northern warp to the disk, diffuse gas surrounding the galaxy, and a southern cloud with a filament back to the galaxy. The features extend out to 22 kpc from the galaxy center (18 kpc from the edge of the FUV disk), and the gas is directly connected to M33's disk. Only five discrete clouds (i.e., gas not directly connected to M33 in position-velocity space) are cataloged in the vicinity of M33, and these clouds show similar properties to Galactic and M31 halo clouds. M33's gaseous features most likely originate from the tidal disruption of M33 by M31 1-3 Gyr ago as shown by an orbit analysis which results in a tidal radius <15 kpc in the majority of M33's possible orbits. M33 is now beyond the disruptive gravitational influence of M31, and the gas appears to be returning to M33's disk and redistributing its star formation fuel. M33's high mean velocity dispersion in the disk (~18.5 km s-1) may also be consistent with the previous interaction and high rate of star formation. M33 will either exhaust its star formation fuel in the next few Gyrs or eventually become star formation fuel for M31. The latter represents the accretion of a large gaseous satellite by a spiral galaxy, similar to the Magellanic Clouds' relationship to the Galaxy.
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