THE INTERSTELLAR MEDIUM IN DISTANT STAR-FORMING GALAXIES: TURBULENT PRESSURE, FRAGMENTATION, AND CLOUD SCALING RELATIONS IN A DENSE GAS DISK AT z = 2.3

By A. M. Swinbank, P. Papadopoulos, P. Cox, M. Krips, R. Ivison, I. Smail, A. Thomson, R. Neri, J. Richard, H. Ebeling. 2011

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We have used the Institut de Radioastronomie Millimétrique (IRAM) Plateau de Bure Interferometer and the Expanded Very Large Array to obtain a high-resolution map of the CO(6–5) and CO(1–0) emission in the lensed, star-forming galaxy SMM J2135−0102 at z = 2.32. The kinematics of the gas are well described by a model of a rotationally supported disk with an inclination-corrected rotation speed, vrot = 320 ± 25 km s−1, a ratio of rotational-to-dispersion support of v/σ = 3.5 ± 0.2, and a dynamical mass of (6.0 ± 0.5) × 1010 M☉ within a radius of 2.5 kpc. The disk has a Toomre parameter, Q = 0.50 ± 0.15, suggesting that the gas will rapidly fragment into massive clumps on scales of LJ ∼ 400 pc. We identify star-forming regions on these scales and show that they are ∼10 × denser than those in quiescent environments in local galaxies, and significantly offset from the local molecular cloud scaling relations (Larson's relations). The large offset compared to local molecular cloud line-width–size scaling relations implies that supersonic turbulence should remain dominant on scales ∼100× smaller than in the kinematically quiescent interstellar medium (ISM) of the Milky Way, while the molecular gas in SMM J2135 is expected to be ∼50× denser than that in the Milky Way on all scales. This is most likely due to the high external hydrostatic pressure we measure for the ISM, Ptot/kB ∼ (2 ± 1) × 107 K cm−3. In such highly turbulent ISM, the subsonic regions of gravitational collapse (and star formation) will be characterized by much higher critical densities, ncrit > = 108 cm−3, a factor ≳1000× more than the quiescent ISM of the Milky Way.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ec48639a4a40a4a92cabd44ec24b12c3c0230d29

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