%0 Generic %1 zheng2017discovery %A Zheng, Y. %A Werk, J. K. %A Peek, J. E. G. %A Putman, M. E. %D 2017 %K cloud high m33 velocity %T The Discovery and Origin of A Very-High Velocity Cloud Toward M33 %U http://arxiv.org/abs/1703.09730 %X We report the detection of a largely ionized very-high velocity cloud (VHVC; $v_LSR\sim-350$ km/s) toward M33 with the Hubble Space Telescope/Cosmic Origin Spectrograph. The VHVC is detected in OI, CII, SiII, and SiIII absorption along five sightlines separated by ~0.06-0.4 degree. On sub-degree scales, the velocities and ionic column densities of the VHVC remain relatively smooth with standard deviations of +/-14 km/s and +/-0.15 dex between the sightlines, respectively. The VHVC has a metallicity of OI/HI=-0.56+/-0.17 dex (Z=0.28+/-0.11 Z$_ødot$). Despite the position-velocity proximity of the VHVC to the ionized Magellanic Stream, the VHVC's higher metallicity makes it unlikely to be associated with the Stream, highlighting the complex velocity structure of this region of sky. We investigate the VHVC's possible origin by revisiting its surrounding HI environment. We find that the VHVC may be: (1) a MW CGM cloud, (2) related to a nearby HI VHVC -- Wright's Cloud, or (3) connected to M33's northern warp. Furthermore, the VHVC could be a bridge connecting Wright's Cloud and M33's northern warp, which would make it a Magellanic-like structure in the halo of M33.

@misc{zheng2017discovery, abstract = {We report the detection of a largely ionized very-high velocity cloud (VHVC; $v_{\rm LSR}\sim-350$ km/s) toward M33 with the Hubble Space Telescope/Cosmic Origin Spectrograph. The VHVC is detected in OI, CII, SiII, and SiIII absorption along five sightlines separated by ~0.06-0.4 degree. On sub-degree scales, the velocities and ionic column densities of the VHVC remain relatively smooth with standard deviations of +/-14 km/s and +/-0.15 dex between the sightlines, respectively. The VHVC has a metallicity of [OI/HI]=-0.56+/-0.17 dex (Z=0.28+/-0.11 Z$_{\odot}$). Despite the position-velocity proximity of the VHVC to the ionized Magellanic Stream, the VHVC's higher metallicity makes it unlikely to be associated with the Stream, highlighting the complex velocity structure of this region of sky. We investigate the VHVC's possible origin by revisiting its surrounding HI environment. We find that the VHVC may be: (1) a MW CGM cloud, (2) related to a nearby HI VHVC -- Wright's Cloud, or (3) connected to M33's northern warp. Furthermore, the VHVC could be a bridge connecting Wright's Cloud and M33's northern warp, which would make it a Magellanic-like structure in the halo of M33.}, added-at = {2017-03-30T15:08:41.000+0200}, author = {Zheng, Y. and Werk, J. K. and Peek, J. E. G. and Putman, M. E.}, biburl = {https://www.bibsonomy.org/bibtex/2c0e000245fabd0a15bab8b132f27a520/miki}, description = {[1703.09730] The Discovery and Origin of A Very-High Velocity Cloud Toward M33}, interhash = {5c3dda3fe992be6f2e68ba233fb9a78b}, intrahash = {c0e000245fabd0a15bab8b132f27a520}, keywords = {cloud high m33 velocity}, note = {cite arxiv:1703.09730Comment: Accepted for publication in ApJ}, timestamp = {2017-03-30T15:08:41.000+0200}, title = {The Discovery and Origin of A Very-High Velocity Cloud Toward M33}, url = {http://arxiv.org/abs/1703.09730}, year = 2017 }