Giant molecular clouds in the early-type galaxy ngc 4526

Utomo, Dyas, Blitz, Leo, Davis, Timothy ORCID: https://orcid.org/0000-0003-4932-9379, Rosolowsky, Erik, Bureau, Martin, Cappellari, Michele and Sarzi, Marc 2015. Giant molecular clouds in the early-type galaxy ngc 4526. Astrophysical Journal 803 (1) , p. 16. 10.1088/0004-637X/803/1/16

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Abstract

We present a high spatial resolution (≈20 pc) of 12CO(2 −1) observations of the lenticular galaxy NGC 4526. We identify 103 resolved giant molecular clouds (GMCs) and measure their properties: size R, velocity dispersion σv, and luminosity L. This is the first GMC catalog of an early-type galaxy. We find that the GMC population in NGC 4526 is gravitationally bound, with a virial parameter α ~ 1. The mass distribution, dN/dM ∝ M−2.39 ± 0.03, is steeper than that for GMCs in the inner Milky Way, but comparable to that found in some late-type galaxies. We find no size–line width correlation for the NGC 4526 clouds, in contradiction to the expectation from Larson's relation. In general, the GMCs in NGC 4526 are more luminous, denser, and have a higher velocity dispersion than equal-size GMCs in the Milky Way and other galaxies in the Local Group. These may be due to higher interstellar radiation field than in the Milky Way disk and weaker external pressure than in the Galactic center. In addition, a kinematic measurement of cloud rotation shows that the rotation is driven by the galactic shear. For the vast majority of the clouds, the rotational energy is less than the turbulent and gravitational energy, while the four innermost clouds are unbound and will likely be torn apart by the strong shear at the galactic center. We combine our data with the archival data of other galaxies to show that the surface density Σ of GMCs is not approximately constant, as previously believed, but varies by ~3 orders of magnitude. We also show that the size and velocity dispersion of the GMC population across galaxies are related to the surface density, as expected from the gravitational and pressure equilibrium, i.e., σv R−1/2 ∝ Σ1/2.

Item Type:	Article
Date Type:	Published Online
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Publisher:	American Astronomical Society
ISSN:	1538-4357
Last Modified:	19 Oct 2022 06:49
URI:	https://orca.cardiff.ac.uk/id/eprint/87971

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