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27 April 2024 |
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The Disruption and Fueling of M33 | | M.E. Putman
; J.E.G. Peek
; A. Muratov
; O. Gnedin
; W. Hsu
; K.A. Douglas
; C. Heiles
; S. Stanimirovic
; E.J. Korpela
; S.J. Gibson
; | | Date: |
12 Dec 2008 | | 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 HI
(GALFA-HI) Survey that show the full extent and detailed spatial and kinematic
structure of M33’s neutral hydrogen. Over 18% of the HI mass of M33
(M_HI_tot=1.4 x 10^9 Msun) is found beyond the star forming disk. 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 extraplanar 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 gaseous disk. The extraplanar features most likely originate
from the tidal disruption of M33 by M31 1-3 Gyr ago as shown from 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 extraplanar gas appears to be returning to M33’s disk and
redistributing its star formation fuel. The returning gas may be falling
towards M33’s central regions due to the loss of angular momentum as it
interacted with a diffuse gaseous M31 halo during the closest approach. M33
will eventually become fuel for M31, representing the accretion of a large
satellite by a spiral galaxy, similar to the Magellanic Clouds’ relationship to
the Galaxy. | | Source: | arXiv, 0812.3093 | | Services: | Forum | Review | PDF | Favorites | |
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