Springer Link (Chiba Institute of Technology) · 2019 · 53 citations · 103 references
Natural SciencesAstronomyPhysicsAstrophysicsRadio AstronomyStar FormationGalaxy FormationInterstellar GasMolecular CloudsStar Formation In GalaxiesStellar EvolutionStellar PopulationsDense Gas TracersDense Molecular GasExtragalactic Radio ContinuumGas Density DistributionInterferometric Continuum ObservationsInterstellar Gas In Spiral ArmsRadio Continuum SurveysStar Formation Radio Continuum
It remains unclear what sets the efficiency with which molecular gas transforms into stars. Here we present a new VLA map of the spiral galaxy M 51 in 33 GHz radio continuum, an extinction-free tracer of star formation, at 3″ scales (̃100 pc). We combined this map with interferometric PdBI/NOEMA observations of CO(1-0) and HCN(1-0) at matched resolution for three regions in M 51 (central molecular ring, northern and southern spiral arm segments). While our measurements roughly fall on the well-known correlation between total infrared and HCN luminosity, bridging the gap between Galactic and extragalactic observations, we find systematic offsets from that relation for different dynamical environments probed in M 51; for example, the southern arm segment is more quiescent due to low star formation efficiency (SFE) of the dense gas, despite its high dense gas fraction. Combining our results with measurements from the literature at 100 pc scales, we find that the SFE of the dense gas and the dense gas fraction anti-correlate and correlate, respectively, with the local stellar mass surface density. This is consistent with previous kpc-scale studies. In addition, we find a significant anti-correlation between the SFE and velocity dispersion of the dense gas. Finally, we confirm that a correlation also holds between star formation rate surface density and the dense gas fraction, but it is not stronger than the correlation with dense gas surface density. Our results are hard to reconcile with models relying on a universal gas density threshold for star formation and suggest that turbulence and galactic dynamics play a major role in setting how efficiently dense gas converts into stars. The VLA map, Table A.1, and full Table A.2 are available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr/">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/625/A19">http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/625/A19</A>
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On the variation of the initial mass function
Pavel Kroupa · Monthly Notices of the Royal Astronomical Society · 2001 · 7.5K citations · Full text
Natural Sciences, Astronomy, Physics +16
STAR FORMATION IN GALAXIES ALONG THE HUBBLE SEQUENCE
Annual Review of Astronomy and Astrophysics · 1998 · 6.6K citations · Full text
Natural Sciences, Astronomy, Physics +15
Radio Emission from Normal Galaxies
J. J. Condon · Annual Review of Astronomy and Astrophysics · 1992 · 2.2K citations
Natural Sciences, Astronomy, Physics +14