H i Kinematics along the Minor Axis of M82

Martini, Paul; Leroy, Adam K.; Mangum, Jeffrey G.; Bolatto, Alberto; Keating, Katie M.; Sandstrom, Karin; Walter, Fabian

doi:10.3847/1538-4357/aab08e

H i Kinematics along the Minor Axis of M82

Journal Article · Mon Mar 26 00:00:00 EDT 2018 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/aab08e· OSTI ID:1542019

^[1]; ^[2]; Mangum, Jeffrey G. ^[3]; Bolatto, Alberto ^[4]; Keating, Katie M. ^[5]; ^[6]; ^[7]

The Ohio State Univ., Columbus, OH (United States); DOE/OSTI
The Ohio State Univ., Columbus, OH (United States)
National Radio Astronomy Observatory, Charlottesville, VA (United States)
Univ. of Maryland, College Park, MD (United States)
Rincon Research Corp., Tucson, AZ (United States)
Univ. of California, San Diego, CA (United States)
Max Planck Inst. für Astronomie, Heidelberg (Germany)

M82 is one of the best-studied starburst galaxies in the local universe, and is consequently a benchmark for researching star formation feedback at both low and high redshift. We introduce new VLA H i observations that reveal the cold gas kinematics along the minor axis in unprecedented detail. This includes the detection of H i up to 10 kpc along the minor axis toward the south and beyond 5 kpc to the north. A surprising aspect of these observations is that the line-of-sight H i velocity decreases substantially from about 120 to $$50\,\mathrm{km}\,{{\rm{s}}}^{-1}$$ from 1.5 to 10 kpc off the midplane. The velocity profile is not consistent with the H i gas cooling from the hot wind. We determine that the velocity decrease is substantially greater than the deceleration expected from gravitational forces alone. If the H i consists of a continuous population of cold clouds, some additional drag force must be present, and the magnitude of the drag force places a joint constraint on the ratio of the ambient medium to the typical cloud size and density. We also demonstrate that the H i kinematics are inconsistent with a simple conical outflow centered on the nucleus, but instead require the more widespread launch of the H i over the ~1 kpc extent of the starburst region. Regardless of the launch mechanism for the H i gas, the observed velocity decrease along the minor axis is sufficiently great that the H i may not escape the halo of M82. The inferred H i outflow rate at 10 kpc off the midplane is much less than 1 $${M}_{\odot }$$ yr–1.

View Accepted Manuscript (DOE)

Research Organization:: The Ohio State Univ., Columbus, OH (United States)

Sponsoring Organization:: National Science Foundation (NSF); USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)

Grant/Contract Number:: SC0015525

OSTI ID:: 1542019

Journal Information:: The Astrophysical Journal (Online), Journal Name: The Astrophysical Journal (Online) Journal Issue: 1 Vol. 856; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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