Mass, luminosity, and line width relations of Galactic molecular clouds

Solomon, P. M.; Rivolo, A. R.; Barrett, John W.; Yahil, A.

doi:10.1086/165493

Cited by 1,529 publications

(2,332 citation statements)

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“…Similar scaling relations have been shown to apply to structure within clouds; Solomon et al (1987) found…”

Section: Molecular Cloudssupporting

confidence: 64%

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Submillimetre Studies of Prestellar and Starless Cores in the Ophiuchus, Taurus and Cepheus Molecular Clouds

Pattle¹

2017

Springer Theses

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“…Similar scaling relations have been shown to apply to structure within clouds; Solomon et al (1987) found…”

Section: Molecular Cloudssupporting

confidence: 64%

“…where for molecular clouds η = 0.38 (Larson 1981), and for cores η = 0.5 (Solomon et al 1987), and the linewidth-mass relation, (Larson 1981), combine to give…”

Section: Relation Between Gravitational Potential Energy and Externalmentioning

confidence: 99%

Submillimetre Studies of Prestellar and Starless Cores in the Ophiuchus, Taurus and Cepheus Molecular Clouds

Pattle¹

2017

Springer Theses

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“…Within the Milky Way and Local Group (aside from the Small Magallenic Cloud [SMC]), the conversion factor appears to display a remarkably narrow range of X CO ≈ 2 − 4 × 10 20 cm −2 /K km s −1 (or α CO ≈ 3 − 6 M pc −2 (K km s −1 ) −1 Bloemen et al, 1986;Solomon et al, 1987;Blitz et al, 2007;Delahaye et al, 2011;Leroy et al, 2011;Donovan Meyer et al, 2012b,a). The independent H 2 mass measurements in these observations come from virial mass measurements, dust to gas ratio assumptions (or measurements), and γ-ray observations.…”

Section: Deriving H 2 Gas Masses From High-redshift Galaxiesmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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“…In NGC 1275, Salomé et al 2008 found that the CO line ratios indicate optically thick radiation but the observed brightness temperature of the molecular gas clumps is at least an order of magnitude below the expectation for normal, optically thick clouds. These observations can be reconciled if each molecular clump is comprised of many giant molecular clouds each with a mass of ∼ 10 6 M and a radius of ∼ 30 pc typical of those found in the Milky Way (Solomon et al 1987). Although the complexity of the structure makes a clean interpretation difficult, it is plausible that the peak absorbed fraction is significantly higher and therefore the bulk of the molecular gas in the NW and SE filaments lies on the near side of the galaxy.…”

Section: Outflowing Molecular Gas Clouds?mentioning

confidence: 99%

“…(1) where X CO = 2 × 10 20 cm −2 ( K km s −1 ) −1 in the Milky Way disk (Solomon et al 1987;Solomon & Vanden Bout 2005;Bolatto, Wolfire & Leroy 2013), D L is the luminosity distance, and z is the redshift of the BCG. However, the Galactic conversion factor is not expected or observed to be universal (eg.…”

Section: Molecular Gas Massmentioning

confidence: 99%

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

Russell

McNamara

Fabian

et al. 2016

Mon. Not. R. Astron. Soc.

105

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We present ALMA observations of the CO(1-0) and CO(3-2) line emission tracing filaments of cold molecular gas in the central galaxy of the cluster PKS 0745-191. The total molecular gas mass of 4.6±0.3×10 9 M , assuming a Galactic X CO factor, is divided roughly equally between three filaments each extending radially 3 − 5 kpc from the galaxy centre. The emission peak is located in the SE filament ∼ 1 arcsec (2 kpc) from the nucleus. The velocities of the molecular clouds in the filaments are low, lying within ±100 km s −1 of the galaxy's systemic velocity. Their FWHMs are less than 150 km s −1 , which is significantly below the stellar velocity dispersion. Although the molecular mass of each filament is comparable to a rich spiral galaxy, such low velocities show that the filaments are transient and the clouds would disperse on < 10 7 yr timescales unless supported, likely by the indirect effect of magnetic fields. The velocity structure is inconsistent with a merger origin or gravitational free-fall of cooling gas in this massive central galaxy. If the molecular clouds originated in gas cooling even a few kpc from their current locations their velocities would exceed those observed. Instead, the projection of the N and SE filaments underneath X-ray cavities suggests they formed in the updraft behind bubbles buoyantly rising through the cluster atmosphere. Direct uplift of the dense gas by the radio bubbles appears to require an implausibly high coupling efficiency. The filaments are coincident with low temperature X-ray gas, bright optical line emission and dust lanes indicating that the molecular gas could have formed from lifted warmer gas that cooled in situ.

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Mass, luminosity, and line width relations of Galactic molecular clouds

Cited by 1,529 publications

References 0 publications

Submillimetre Studies of Prestellar and Starless Cores in the Ophiuchus, Taurus and Cepheus Molecular Clouds

Submillimetre Studies of Prestellar and Starless Cores in the Ophiuchus, Taurus and Cepheus Molecular Clouds

Dusty star-forming galaxies at high redshift

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

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