Star formation in active dwarf galaxies

Thronson, H. A.; Telesco, C. M.

doi:10.1086/164756

Cited by 109 publications

(98 citation statements)

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“…Rubin et al 1992;DuPrie & Schneider 1996). Thronson & Telesco (1986) found a typical gas-to-dust mass ratio of ∼700 for normal spiral galaxies, which reflects the fact that the IRAS bands are not sensitive to a dust component colder than ∼20 K. The lower gas-to-dust ratio found in NGC 4550 indicates that a relatively warm dust component dominates the far infrared continuum.…”

Section: Dustmentioning

confidence: 95%

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Molecular gas and dust in NGC 4550

Wiklind

Henkel

2001

A&A

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Abstract.We report the detection of 1 × 10 7 M of molecular gas in the central region of the S0/E7 galaxy NGC 4550, inferred from observations of CO(1-0) emission. Dust is detected in HST WFPC2 images and found to be asymmetrically distributed around the nucleus, only extending to a galactocentric distance of 7 (600 pc). The shape of the CO emission profile is consistent with a molecular gas distribution following the dust. The distribution of the dust and gas in the center could be the result of an m = 1 instability, which is the fastest growing unstable mode in counterrotating stellar disks. On a global scale the molecular gas in NGC 4550 is stable against gravitational collapse but nevertheless star formation appears to be ongoing with normal star formation efficiency and gas consumption time scales. The stellar velocity dispersion in NGC 4550 resembles that of elliptical galaxies. It is therefore likely that a hot X-ray emitting plasma limits the lifetime of the molecular gas, that must arise from a recent ( 1 Gyr) accretion event.

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Section: Dustmentioning

confidence: 95%

“…Thronson & Telesco 1986), the star formation rate (SFR) becomes 0.065 M yr −1 . The ratio of L FIR /M H2 is usually taken as a measure of the star formation efficiency.…”

Section: Star Formationmentioning

confidence: 99%

Molecular gas and dust in NGC 4550

Wiklind

Henkel

2001

A&A

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“…The value of varies in the literature from 2.1 to 6.5 (Scoville & Young 1983;Thronson & Telesco 1986;Rowan-Robinson et al 1997) because of different assumptions about the duration of the starburst, different initial mass functions ( IMFs), and lower mass limits. In this paper we adopt a value of ¼ 2:1 from a ''cirrus'' model that combines very small grains and polycyclic aromatic hydrocarbons ( PAHs) with a Salpeter IMF in a starburst of OBA stars over 2 ; 10 6 yr (Thronson & Telesco 1986). Obtaining L 60 m from our model SED yields large SFRs of 480-810 M yr À1 .…”

Section: Implied Luminosities and Star Formation Ratesmentioning

confidence: 99%

The Bolocam Lockman Hole Millimeter‐Wave Galaxy Survey: Galaxy Candidates and Number Counts

Laurent

Aguirre

Glenn

et al. 2005

ApJ

105

191

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We present results of a new deep 1.1 mm survey using Bolocam, a millimeter-wavelength bolometer array camera designed for mapping large fields at fast scan rates, without chopping. A map, galaxy candidate list, and derived number counts are presented. This survey encompasses 324 arcmin 2 to an rms noise level (filtered for point sources) of 1:1 mm ' 1:4 mJy beam À1 and includes the entire regions surveyed by the published 8 mJy 850 m JCMT SCUBA and 1.2 mm IRAM MAMBO surveys. We reduced the data using a custom software pipeline to remove correlated sky and instrument noise via a principal component analysis. Extensive simulations and jackknife tests were performed to confirm the robustness of our source candidates and estimate the effects of false detections, bias, and completeness. In total, 17 source candidates were detected at a significance !3.0 , with six expected false detections. Nine candidates are new detections, while eight candidates have coincident SCUBA 850 m and /or MAMBO 1.2 mm detections. From our observed number counts, we estimate the underlying differential number count distribution of submillimeter galaxies and find it to be in general agreement with previous surveys. Modeling the spectral energy distributions of these submillimeter galaxies after observations of dusty nearby galaxies suggests extreme luminosities of L ¼ ð1:0 1:6Þ ; 10 13 L and, if powered by star formation, star formation rates of 500-800 M yr À1 .

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“…Using the dust opacity of the Large Magellanic Cloud (Galliano et al 2011), and a dust temperature of S316. Forming SSC in NGC 5253 3 46 K (Thronson & Telesco 1986) we obtain M dust = 1.5 ± 0.2 × 10 4 M . If we scale the gas-to-dust ratio, GT D, of NGC 5253 to match its Z ∼ 0.25Z metallicity, a common and reasonable assumption, we would estimate that GT D ∼ 500−700, similar to values in the Magellanic Clouds, and this would give a dust-predicted gas mass of M gas ∼ 10 7 M .…”

Section: Cloud D: a Very Dusty Cloudmentioning

confidence: 85%

Submillimeter View of Gas and Dust in the Forming Super Star Cluster in NGC 5253

Turner

2015

Proc. IAU

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Abstract. A giant molecular cloud has been detected surrounding the supernebula in NGC 5253, revealing details of the formation and feedback process in a very massive star cluster. "Cloud D" was recently mapped in CO J=3-2 with the Submillimeter Array. The cloud surrounds a currently forming massive cluster of mass ∼ 10 6 M , and luminosity ∼ 10 9 L . Cloud D is hot, clearly associated with the cluster, yet kinematically relatively quiescent. The dust mass is ∼15,000 M , for a gas-to-dust ratio of ∼50, nearly an order of magnitude lower than expected for this low metallicity galaxy. We posit that enrichment by the cluster, leading to a stalled cluster wind, has created the unusual conditions in Cloud D. The absence of current mechanical impact of the young cluster on the cloud, in spite of the presence of thousands of O stars, may permit future generations of stars to form near the massive cluster.

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Star formation in active dwarf galaxies

Cited by 109 publications

References 0 publications

Molecular gas and dust in NGC 4550

Molecular gas and dust in NGC 4550

The Bolocam Lockman Hole Millimeter‐Wave Galaxy Survey: Galaxy Candidates and Number Counts

Submillimeter View of Gas and Dust in the Forming Super Star Cluster in NGC 5253

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