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Title:
Continuum observations of M 51 and M 83 at 1.1 mm with AzTEC
Authors:
Wall, W. F.; Puerari, I.; Tilanus, R.; Israel, F. P.; Austermann, J. E.; Aretxaga, I.; Wilson, G.; Yun, M.; Scott, K. S.; Perera, T. A.; Roberts, C. M.; Hughes, D. H.
Affiliation:
AA(Instituto Nacional de Astrofísica, Óptica, y Electrónica, Apdo. 51 y 216, Puebla, Puebla, México ), AB(Instituto Nacional de Astrofísica, Óptica, y Electrónica, Apdo. 51 y 216, Puebla, Puebla, México), AC(Leiden Observatory, Leiden University, NL-2300 RA Leiden, the Netherlands), AD(Leiden Observatory, Leiden University, NL-2300 RA Leiden, the Netherlands), AE(NIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USA), AF(Instituto Nacional de Astrofísica, Óptica, y Electrónica, Apdo. 51 y 216, Puebla, Puebla, México), AG(Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA), AH(Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA), AI(North American ALMA Science Center, NRAO, 520 Edgemont Rd, Charlottesville, VA 22903, USA), AJ(CNS C 007C, Illinois Wesleyan University, Bloomington, IL 61702-2900, USA), AK(Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA), AL(Instituto Nacional de Astrofísica, Óptica, y Electrónica, Apdo. 51 y 216, Puebla, Puebla, México)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 459, Issue 2, p.1440-1467 (MNRAS Homepage)
Publication Date:
06/2016
Origin:
OUP
Astronomy Keywords:
galaxies: individual: M 51, M 83, galaxies: ISM, galaxies: spiral
Abstract Copyright:
2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stw687
Bibliographic Code:
2016MNRAS.459.1440W

Abstract

We observed the spiral galaxies M 51 and M 83 at 20 arscec spatial resolution with the bolometer array Aztronomical Thermal Emission Camera (AzTEC) on the JCMT in the 1.1 mm continuum, recovering the extended emission out to galactocentric radii of more than 12 kpc in both galaxies. The 1.1 mm-continuum fluxes are 5.6 ± 0.7 and 9.9 ± 1.4 Jy, with associated gas masses estimated at 9.4 × 109 M&sun; and 7.2 × 109 M&sun; for M 51 and M 83, respectively. In the interarm regions of both galaxies, the N(H2)/I(CO) (or X-factor) ratios exceed those in the arms by factors of ˜1.5-2. In the inner discs of both galaxies, the X-factor is about 1 × 1020 cm- 2 (K km s- 1)- 1. In the outer parts, the CO-dark molecular gas becomes more important. While the spiral density wave in M 51 appears to influence the interstellar medium and stars in a similar way, the bar potential in M 83 influences the interstellar medium and the stars differently. We confirm the result of Foyle et al. that the arms merely heighten the star formation rate (SFR) and the gas surface density in the same proportion. Our maps reveal a threshold gas surface density for an SFR increase by two or more orders of magnitude. In both galaxy centres, the molecular gas depletion time is about 1 Gyr climbing to 10-20 Gyr at radii of 6-8 kpc. This is consistent with an inside-out depletion of the molecular gas in the discs of spiral galaxies.
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