ALMA resolves the properties of star-forming regions in a dense gas disk at z ∼ 3

Swinbank, A.M. and Dye, S. and Nightingale, J.W. and Furlanetto, C. and Smail, Ian and Cooray, A. and Dannerbauer, H. and Dunne, L. and Eales, S. and Gavazzi, R. and Hunter, T. and Ivison, R.J. and Negrello, M. and Oteo-Gomez, I. and Smit, R. and Werf, P. van der and Vlahakis, C. (2015) ALMA resolves the properties of star-forming regions in a dense gas disk at z ∼ 3. Astrophysical Journal Letters, 806 (1). L17/1-L17/5. ISSN 2041-8213

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We exploit long baseline ALMA submillimeter observations of the lensed star-forming galaxy SDP 81 at z = 3.042 to investigate the properties of the interstellar medium (ISM) on scales of 50–100 pc. The kinematics of the 12CO gas within this system are well described by a rotationally supported disk with an inclination-corrected rotation speed, = 320 ± 20 km s−1, and a dynamical mass of = (3.5 ± 1.0)× 1010 within a radius of 1.5 kpc. The disk is gas-rich and unstable, with a Toomre parameter, Q = 0.30 ± 0.10, and so into star-forming regions with Jeans length 130 pc. We identify five star-forming regions within the ISM on these scales and show that their scaling relations between luminosity, line widths, and sizes are significantly offset from those typical of molecular clouds in local galaxies (Larson's relations). These offsets are likely to be caused by the high external hydrostatic pressure for the ISM, / × 107 K cm−3, which is ~104× higher than the typical ISM pressure in the Milky Way. The physical conditions of the star-forming ISM and giant molecular clouds appear to be similar to those found in the densest environments in the local universe, such as those in the Galactic center.

Item Type: Article
Keywords: galaxies: evolution; galaxies: high-redshift; galaxies: starburst
Schools/Departments: University of Nottingham, UK > Faculty of Science > School of Physics and Astronomy
Identification Number: 10.1088/2041-8205/806/1/L17
Depositing User: Eprints, Support
Date Deposited: 27 Apr 2017 10:31
Last Modified: 27 Apr 2017 11:25

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