scholarly journals The Dense-gas Mass versus Star Formation Rate Relation: A Misleading Linearity?

2017 ◽  
Vol 843 (1) ◽  
pp. 7 ◽  
Author(s):  
G. Parmentier
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Dense Gas ◽  
Rate Relation

scholarly journals The dense galactic environments of the Milky Way

2018 ◽  
Vol 14 (S345) ◽  
pp. 34-38
Author(s):  
Quang Nguyen-Luong ◽  
Neal Evans ◽  
Kee-Tae Kim ◽  
Hyunwoo Kang ◽  
Keyword(s):  
Star Formation ◽  
Gas Phase ◽  
Massive Star ◽  
Milky Way ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Dense Gas ◽  
Star Forming ◽  
Star Forming Regions ◽  
Rate Relation

AbstractStar formation takes place in the dense gas phase, and therefore a simple dense gas and star formation rate relation has been proposed. With the advent of multi-beam receivers, new observations show that the deviation from linear relations is possible. In addition, different dense gas tracers might also change significantly the measurement of dense gas mass and subsequently the relation between star formation rate and dense gas mass. We report the preliminary results the DEnse GAs in MAssive star-forming regions in the Milky Way (DEGAMA) survey that observed the dense gas toward a suite of well-characterized massive star-forming regions in the Milky Way. Using the resulting maps of HCO+ 1–0, HCN 1–0, CS 2–1, we discuss the current understanding of the dense gas phase where star formation takes place.

scholarly journals THE RADIO CONTINUUM-STAR FORMATION RATE RELATION IN WSRT SINGS GALAXIES

2014 ◽  
Vol 147 (5) ◽  
pp. 103 ◽  
Author(s):  
Volker Heesen ◽  
Elias Brinks ◽  
Adam K. Leroy ◽  
George Heald ◽  
Robert Braun ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Radio Continuum ◽  
Rate Relation

scholarly journals SHAPING THE DUST MASS-STAR-FORMATION RATE RELATION

2014 ◽  
Vol 782 (2) ◽  
pp. L23 ◽  
Author(s):  
Jens Hjorth ◽  
Christa Gall ◽  
Michał J. Michałowski
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Mass Star ◽  
Dust Mass ◽  
Rate Relation

scholarly journals Modes of star formation from Herschel

2012 ◽  
Vol 8 (S292) ◽  
pp. 87-90
Author(s):  
L. Testi ◽  
E. Bressert ◽  
S. Longmore
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Mass Function ◽  
Initial Mass Function ◽  
Dense Gas ◽  
Nearby Star ◽  
Star Forming ◽  
Star Forming Regions ◽  
Massive Cluster

AbstractWe summarize some of the results obtained from Herschel surveys of nearby star forming regions and the Galactic plane. We show that in the nearby star forming regions the starless core spatial surface density distribution is very similar to that of the young stellar objects. This, taken together with the similarity between the core mass function and the initial mass function for stars and the relationship between the amount of dense gas and star formation rate, suggest that the cloud fragmentation process defines the global outcome of star formation. This “simple” view of star formation may not hold on all scales. In particular dynamical interactions are expected to become important at the conditions required to form young massive clusters. We describe the successes of a simple criterion to identify young massive cluster precursors in our Galaxy based on (sub-)millimeter wide area surveys. We further show that in the location of our Galaxy where the best candidate for a precursor of a young massive cluster is found, the “simple” scaling relationship between dense gas and star formation rate appear to break down. We suggest that in regions where the conditions approach those of the central molecular zone of our Galaxy it may be necessary to revise the scaling laws for star formation.

scholarly journals The Star Formation Rate-Dense Gas Relation in Galaxies as Measured by HCN(3-2) Emission

2008 ◽  
Vol 681 (2) ◽  
pp. L73-L76 ◽  
Author(s):  
R. S. Bussmann ◽  
D. Narayanan ◽  
Y. L. Shirley ◽  
S. Juneau ◽  
J. Wu ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Dense Gas

scholarly journals γ-ray/infrared luminosity correlation of star-forming galaxies

2020 ◽  
Vol 641 ◽  
pp. A147
Author(s):  
P. Kornecki ◽  
L. J. Pellizza ◽  
S. del Palacio ◽  
A. L. Müller ◽  
J. F. Albacete-Colombo ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Cosmic Ray ◽  
Fundamental Relation ◽  
Star Forming ◽  
Best Fitting ◽  
Power Law Index ◽  
Rate Relation ◽  
Shed Light

Context. Nearly a dozen star-forming galaxies have been detected in γ-rays by the Fermi observatory in the last decade. A remarkable property of this sample is the quasi-linear relation between the γ-ray luminosity and the star formation rate, which was obtained assuming that the latter is well traced by the infrared luminosity of the galaxies. The non-linearity of this relation has not been fully explained yet. Aims. We aim to determine the biases derived from the use of the infrared luminosity as a proxy for the star formation rate and to shed light on the more fundamental relation between the latter and the γ-ray luminosity. We expect to quantify and explain some trends observed in this relation. Methods. We compiled a near-homogeneous set of distances, ultraviolet, optical, infrared, and γ-ray fluxes from the literature for all known γ-ray emitting, star-forming galaxies. From these data, we computed the infrared and γ-ray luminosities, and star formation rates. We determined the best-fitting relation between the latter two, and we describe the trend using simple, population-orientated models for cosmic-ray transport and cooling. Results. We find that the γ-ray luminosity–star formation rate relation obtained from infrared luminosities is biased to shallower slopes. The actual relation is steeper than previous estimates, having a power-law index of 1.35 ± 0.05, in contrast to 1.23 ± 0.06. Conclusions. The unbiased γ-ray luminosity–star formation rate relation can be explained at high star formation rates by assuming that the cosmic-ray cooling region is kiloparsec-sized and pervaded by mild to fast winds. Combined with previous results about the scaling of wind velocity with star formation rate, our work provides support to advection as the dominant cosmic-ray escape mechanism in galaxies with low star formation rates.

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