Compact H I Clouds from the GALFA-H I Survey

Type Journal Article
Names Ayesha Begum, Snežana Stanimirović, Joshua E. Peek, Nicholas P. Ballering, Carl Heiles, Kevin A. Douglas, Mary Putman, Steven J. Gibson, Jana Grcevich, Eric J. Korpela, Min-Young Lee, Destry Saul, John S. Gallagher
Publication The Astrophysical Journal
Volume 722
Issue 1
Pages 395-411
Date October 1, 2010
Library Catalog NASA ADS
Abstract The Galactic Arecibo L-band Feed Array H I (GALFA-H I) survey is mapping the entire Arecibo sky at 21 cm, over a velocity range of -700 to +700 km s-1 (LSR), at a velocity resolution of 0.18 km s-1, and a spatial resolution of 3.5 arcmin. The unprecedented resolution and sensitivity of the GALFA-H I survey have resulted in the detection of numerous isolated, very compact H I clouds at low Galactic velocities, which are distinctly separated from the H I disk emission. In the limited area of ~4600 deg2 surveyed so far, we have detected 96 such compact clouds. The detected clouds are cold with a median T k,max (the kinetic temperature in the case in which there is no non-thermal broadening) of 300 K. Moreover, these clouds are quite compact and faint, with median values of 5 arcmin in angular size, 0.75 K in peak brightness temperature, and 5 × 1018 cm-2 in H I column density. Most of the clouds deviate from Galactic rotation at the 20-30 km s-1 level, and a significant fraction show evidence for a multiphase medium and velocity gradients. No counterparts for these clouds were found in other wave bands. From the modeling of spatial and velocity distributions of the whole compact cloud population, we find that the bulk of the compact clouds are related to the Galactic disk, and their distances are likely to be in the range of 0.1 to a few kpc. We discuss various possible scenarios for the formation and maintenance of this cloud population and its significance for Galactic interstellar medium studies.
Tags Galaxy: evolution, Galaxy: halo, ISM: clouds, ISM: kinematics and dynamics, ISM: structure, Radio Lines: ISM
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