We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.

Durham Research Online
You are in:

Resolving the ISM at the peak of cosmic star formation with ALMA : the distribution of CO and dust continuum in z ∼ 2.5 submillimeter galaxies.

Rivera, Gabriela Calistro and Hodge, J. A. and Smail, Ian and Swinbank, A. M. and Weiss, A. and Wardlow, J. L. and Walter, F. and Rybak, M. and Chen, Chian-Chou and Brandt, W. N. and Coppin, K. and Cunha, E. da and Dannerbauer, H. and Greve, T. R. and Karim, A. and Knudsen, K. K. and Schinnerer, E. and Simpson, J. M. and Venemans, B. and Werf, P. P. van der (2018) 'Resolving the ISM at the peak of cosmic star formation with ALMA : the distribution of CO and dust continuum in z ∼ 2.5 submillimeter galaxies.', Astrophysical journal., 863 (1). p. 56.


We use Atacama Large Millimeter Array (ALMA) observations of four submillimeter galaxies (SMGs) at z ~ 2–3 to investigate the spatially resolved properties of the interstellar medium (ISM) at scales of 1–5 kpc (0farcs1–0farcs6). The velocity fields of our sources, traced by the 12CO(J = 3–2) emission, are consistent with disk rotation to the first order, implying average dynamical masses of ~3 × 1011 ${M}_{\odot }$ within two half-light radii. Through a Bayesian approach we investigate the uncertainties inherent to dynamically constraining total gas masses. We explore the covariance between the stellar mass-to-light ratio and CO-to-H2 conversion factor, α CO, finding values of ${\alpha }_{\mathrm{CO}}={1.1}_{-0.7}^{+0.8}$ for dark matter fractions of 15%. We show that the resolved spatial distribution of the gas and dust continuum can be uncorrelated to the stellar emission, challenging energy balance assumptions in global SED fitting. Through a stacking analysis of the resolved radial profiles of the CO(3–2), stellar, and dust continuum emission in SMG samples, we find that the cool molecular gas emission in these sources (radii ~5–14 kpc) is clearly more extended than the rest-frame ~250 μm dust continuum by a factor >2. We propose that assuming a constant dust-to-gas ratio, this apparent difference in sizes can be explained by temperature and optical depth gradients alone. Our results suggest that caution must be exercised when extrapolating morphological properties of dust continuum observations to conclusions about the molecular gas phase of the interstellar medium (ISM).

Item Type:Article
Full text:(VoR) Version of Record
Download PDF
Publisher Web site:
Publisher statement:© 2018. The American Astronomical Society. All rights reserved.
Date accepted:25 June 2018
Date deposited:23 August 2018
Date of first online publication:09 August 2018
Date first made open access:23 August 2018

Save or Share this output

Look up in GoogleScholar