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Evolution of star formation and gas
Cosmology and Nongalactic Astrophysics · Submitted 25 Oct 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These two instruments will revolutionise our understanding of the interstellar medium (ISM) and associated star formation and galaxy evolution, both locally and in the distant Universe.
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The abstract, sentence by sentence
In these lectures I review observations of star-forming molecular clouds in our Galaxy and nearby galaxies to develop a physical intuition for understanding star formation in the local and high-redshift Universe. A lot of this material is drawn from early work in the field since much of the work was done two decades ago and this background is not generally available in the present literature. I also attempt to synthesise our well-developed understanding of star formation in low-redshift galaxies with constraints from theory and observations at high redshift to develop an intuitive model for the evolution of galaxy mass and luminosity functions in the early Universe. The overall goal of this contribution is to provide students with background helpful for analysis of far-infrared (FIR) observations from Herschel and millimetre/submillimetre (mm/submm) imaging with ALMA (the Atacama Large Millimetre/submillimetre Array). These two instruments will revolutionise our understanding of the interstellar medium (ISM) and associated star formation and galaxy evolution, both locally and in the distant Universe. To facilitate interpreting the FIR spectra of Galactic star-forming regions and high-redshift sources, I develop a model for the dust heating and radiative transfer in order to elucidate the observed infrared (IR) emissions. I do this because I am not aware of a similar coherent discussion in the literature.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In these lectures I review observations of star-forming molecular clouds in our Galaxy and nearby galaxies to develop a physical intuition for understanding star formation in the local and high-redshift Universe. | contribution 0.70 | 0.20 | 0.04 | asserted 0.78 |
| s1 | A lot of this material is drawn from early work in the field since much of the work was done two decades ago and this background is not generally available in the present literature. | background 0.81 | 0.07 | 0.02 | asserted 0.99 |
| s2 | I also attempt to synthesise our well-developed understanding of star formation in low-redshift galaxies with constraints from theory and observations at high redshift to develop an intuitive model for the evolution of galaxy mass and luminosity functions in the early Universe. | contribution 0.96 | 0.55 | 0.15 | asserted 0.56 |
| s3 | The overall goal of this contribution is to provide students with background helpful for analysis of far-infrared (FIR) observations from Herschel and millimetre/submillimetre (mm/submm) imaging with ALMA (the Atacama Large Millimetre/submillimetre Array). | contribution 0.73 | 0.21 | 0.05 | asserted 0.96 |
| s4 | These two instruments will revolutionise our understanding of the interstellar medium (ISM) and associated star formation and galaxy evolution, both locally and in the distant Universe. | background 0.71 | 0.05 | 0.13 | asserted 0.95 |
| s5 | To facilitate interpreting the FIR spectra of Galactic star-forming regions and high-redshift sources, I develop a model for the dust heating and radiative transfer in order to elucidate the observed infrared (IR) emissions. | method 0.83 | 0.91 | 0.05 | asserted 0.98 |
| s6 | I do this because I am not aware of a similar coherent discussion in the literature. | gap 0.98 | 0.31 | 0.03 | asserted 0.79 |
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The paper
Original abstract
In these lectures I review observations of star-forming molecular clouds in our Galaxy and nearby galaxies to develop a physical intuition for understanding star formation in the local and high-redshift Universe. A lot of this material is drawn from early work in the field since much of the work was done two decades ago and this background is not generally available in the present literature. I also attempt to synthesise our well-developed understanding of star formation in low-redshift galaxies with constraints from theory and observations at high redshift to develop an intuitive model for the evolution of galaxy mass and luminosity functions in the early Universe. The overall goal of this contribution is to provide students with background helpful for analysis of far-infrared (FIR) observations from Herschel and millimetre/submillimetre (mm/submm) imaging with ALMA (the Atacama Large Millimetre/submillimetre Array). These two instruments will revolutionise our understanding of the interstellar medium (ISM) and associated star formation and galaxy evolution, both locally and in the distant Universe. To facilitate interpreting the FIR spectra of Galactic star-forming regions and high-redshift sources, I develop a model for the dust heating and radiative transfer in order to elucidate the observed infrared (IR) emissions. I do this because I am not aware of a similar coherent discussion in the literature.
Human review
How the literature uses it
11 arXiv papers cite this in 18 sentences
Papers citing it · 12 sentences without a confident label
Uses its method or tool 1 paper
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The dust temperature, $T= 43.0 K$, is estimated using the formalism of [ref] for extremely obscured nuclear starbursts (i.e. optically thick for the IR emission of $λ100 μm$[The gas column density profile shown in Fig. [ref] confirms that indeed the central dusty region is optically thick at $λ100 μm$.]): $T_dust = 630×[L_IR/10^12L_]^1/4/R_pc^1/2 K$.
ALMA Observations of Warm Molecular Gas and Cold Dust in NGC 34 · Gas Mass and Dust Mass · 0.89
Uses its data or values 1 paper
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For the standard ISM gas-to-dust ratio $N_H / A_V = 2×10^21$ cm$^-2$, $κ_V ≃312$ cm$^2$ gr$^-1$ and for $κ_IR/κ_V ∼1/30$ [ref] , $κ_IR ≃10$ cm$^2$ gr$^-1$.
ALMA Resolves the Nuclear Disks of Arp 220 · Radiation Pressure Support · 0.99
Cites it as background 3 papers
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Since measuring CO in normal star-forming galaxies at high redshifts is challenging, there has been significant interest recently in using dust masses as a proxy for the total molecular gas contents [ref] .
Validation of the equilibrium model for galaxy evolution to z~3 through molecular gas and dust observations of lensed star-forming galaxies · Gas-to-dust ratio · 0.94
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The relationship between dust mass, dust temperature, and dust luminosity () is in general well understood (e.g., [ref] , [ref] ): when dust grains absorb UV photons from young OB stars, they are heated and re-emit their energy at IR wavelengths.
Molecular Gas, Dust and Star Formation in Galaxies: II. Dust properties and scalings in \sim\ 1600 nearby galaxies · , , and Plane · 0.99
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Star formation takes place largely if not exclusively within molecular clouds [ref] .
Two physical regimes for the Giant HII Regions and Giant Molecular Clouds in the Antennae Galaxies · Introduction · 0.94
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