801 research outputs found
HI and Hot Gas in the Outskirts of the M81 Group
Results are presented from a wide area, high resolution HI synthesis survey
of the outer regions of the nearby M81 group, where internal (galactic) and
external (group-related) evolution processes can be studied simultaneously in
great detail. The survey encompasses the star forming dwarf galaxies M81dwA,
UGC4483, and HoII, where evidence of ram pressure stripping was recently
discovered. The data do not reveal any intergalactic HI, but the outer parts of
HoII are reminiscent of tidal tails. We argue however that those structures are
equally consistent with the latest ram pressure models including cooling. The
case for a hot intergalactic medium in this poor, spiral-only group is thus
still open. The survey also puts tight constraints on possible counterparts to
the local high velocity cloud population in an external group, reaching a 3
sigma column density of 10^19 atom/cm^2 and a 6 sigma limiting mass of 1.5x10^5
M_sun.Comment: 6 pages, 3 figures, to be published in "Recycling Intergalactic and
Interstellar Matter," eds. P.-A. Duc, J. Braine, & E. Brinks (ASP: San
Francisco
An Interacting Galaxy System Along a Filament in a Void
Cosmological voids provide a unique environment for the study of galaxy
formation and evolution. The galaxy population in their interior have
significantly different properties than average field galaxies. As part of our
Void Galaxy Survey (VGS), we have found a system of three interacting galaxies
(VGS_31) inside a large void. VGS_31 is a small elongated group whose members
are embedded in a common HI envelope. The HI picture suggests a filamentary
structure with accretion of intergalactic cold gas from the filament onto the
galaxies. We present deep optical and narrow band H_alpha data, optical
spectroscopy, near-UV and far-UV GALEX and CO(1-0) data. We find that one of
the galaxies, a Markarian object, has a ring-like structure and a tail evident
both in optical and HI. While all three galaxies form stars in their central
parts, the tail and the ring of the Markarian object are devoid of star
formation. We discuss these findings in terms of a gravitational interaction
and ongoing growth of galaxies out of a filament. VGS_31 is one of the first
observed examples of a filamentary structure in a void. It is an important
prototype for understanding the formation of substructure in a void. This
system also shows that the galaxy evolution in voids can be as dynamic as in
high density environments.Comment: 17 pages, 8 figures, accepted for publication in A
Discovery of a Small Central Disk of CO and HI in the Merger Remnant NGC 34
We present CO(1-0) and HI(21-cm) observations of the central region of the
wet merger remnant NGC 34. The Combined Array for Research in Millimeter-wave
Astronomy (CARMA) observations detect a regularly rotating disk in CO with a
diameter of 2.1 kpc and a total molecular hydrogen mass of (. The rotation curve of this gas disk rises steeply,
reaching maximum velocities at 1" (410 pc) from the center. Interestingly, HI
observations done with the Karl G. Jansky Very Large Array show that the
absorption against the central continuum has the exact same velocity range as
the CO in emission. This strongly suggests that the absorbing HI also lies
within 1" from the center, is mixed in and corotates with the molecular gas. A
comparison of HI absorption profiles taken at different resolutions (5"-45")
shows that the spectra at lower resolutions are less deep at the systemic
velocity. This provides evidence for HI emission in the larger beams, covering
the region from 1 kpc to 9 kpc from the center. The central rapidly rotating
disk was likely formed either during the merger or from fall-back material.
Lastly, the radio continuum flux of the central source at mm wavelengths
( mJy) is significantly higher than expected from an extrapolation
of the synchrotron spectrum, indicating the contribution of thermal free-free
emission from the central starburst.Comment: Accepted for publication in A
KK246, a dwarf galaxy with extended H I disk in the Local Void
We have found that KK 246, the only confirmed galaxy located within the
nearby Tully Void, is a dwarf galaxy with an extremely extended H I disk and
signs of an H I cloud with anomalous velocity. It also exhibits clear
misalignment between the kinematical major and minor axes, indicative of an
oval distortion, and a general misalignment between the H I and optical major
axes. We measure a H I mass of 1.05 +- 0.08 x 10^8 M_sun, and a H I extent 5
times that of the stellar disk, one of the most extended H I disks known. We
estimate a dynamical mass of 4.1 x 10^9 M_sun, making this also one of the
darkest galaxies known, with a mass-to-light ratio of 89. The relative
isolation and extreme underdense environment make this an interesting case for
examining the role of gas accretion in galaxy evolution.Comment: 15 pages, 8 figures, 2 tables, accepted for publication in A
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