Stellar and Gaseous Abundances in M82

Origlia, L.; Ranalli, P.; Comastri, A.; Maiolino, R.

doi:10.1086/383018

Cited by 67 publications

(84 citation statements)

References 47 publications

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“…They attributed the weakness of the nitrogen-bearing molecules to the low nitrogen abundance in these galaxies, based on the observed trend in the HCN/HCO + ratio with metallicity. The weak J HCN 4 3 =  emission observed in M82 may be a similar effect, as there is some evidence of sub-solar metallicity for this galaxy (e.g., Origlia et al 2004;Nagao et al 2011).…”

Section: Variation In the Infrared-molecular Line Luminosity Ratiomentioning

confidence: 71%

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

Tan

Gao

Zhang

et al. 2018

ApJ

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We present J HCN 4 3 =  and J HCO 4 3 =  + maps of six nearby star-forming galaxies, NGC 253, NGC 1068, IC 342, M82, M83, and NGC 6946, obtained with the James Clerk Maxwell Telescope as part of the MALATANG survey. All galaxies were mapped in the central 2′×2′region at 14″ (FWHM) resolution (corresponding to linear scales of ∼0.2-1.0 kpc). The L IR -L′ dense relation, where the dense gas is traced by the J HCN 4 3 =  and the J HCO 4 3 =  + emission, measured in our sample of spatially resolved galaxies is found to follow the linear correlation established globally in galaxies within the scatter. We find that the luminosity ratio, L IR /L′ dense , shows systematic variations with L IR within individual spatially resolved galaxies, whereas the galaxy-integrated ratios vary little. A rising trend is also found between L IR /L′ dense ratio and the warm-dust temperature gauged by the 70 μm/100 μm flux ratio. We find that the luminosity ratios of IR/HCN (4-3) and IR/HCO + (4-3), which can be taken as a proxy for the star formation efficiency (SFE) in the dense molecular gas

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Section: Variation In the Infrared-molecular Line Luminosity Ratiomentioning

confidence: 71%

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

Tan

Gao

Zhang

et al. 2018

ApJ

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“…Origlia et al (2004) measured the nuclear gaseous and stellar metallicities by using X-ray and near-infrared spectroscopic observations, and they found that both metallicities are close to or slightly less than the solar metallicity in M 82. Taking the metallicity gradient into account, these metallicities (based also on diagnostics little affected by dust extinction) are consistent with the metallicity inferred through the far-IR fine-structure diagnostics.…”

Section: Comparison With Observational Datamentioning

confidence: 99%

Metallicity diagnostics with infrared fine-structure lines

Nagao

Maiolino

Marconi

et al. 2011

A&A

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109

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Although measuring the gas metallicity in galaxies at various redshifts is crucial to constrain galaxy evolutionary scenarios, only rest-frame optical emission lines have been generally used to measure the metallicity. This has prevented us to accurately measure the metallicity of dust-obscured galaxies, and accordingly to understand the chemical evolution of dusty populations, such as ultraluminous infrared galaxies. Here we propose diagnostics of the gas metallicity based on infrared fine-structure emission lines, which are nearly unaffected by dust extinction even the most obscured systems. Specifically, we focus on fine-structure lines arising mostly from Hii regions, not in photo-dissociation regions, to minimize the dependence and uncertainties of the metallicity diagnostics from various physical parameters. Based on photoionization models, we show that the emission-line flux ratio of ([Oiii] .21 can be used to measure and, therefore, account for the dependences on the gas density and ionization parameter, respectively. We show that these diagnostic fine-structure lines are detectable with Herschel in luminous infrared galaxies out z ∼ 0.4. Metallicity measurements with these fine-structure lines will be feasible at relatively high redshift (z ∼ 1 or more) with SPICA, the future infrared space observatory.

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“…In this paper, we focus on stars with solar initial composition (X = 0.7, Z = 0.02). This choice is partly motivated by the high metallicity of the starburst galaxy M 82 -with Z Z (McLeod et al 1993;Origlia et al 2004;Mayya et al 2006) -which contains one of the most promising candidate ULXs, M 82 X-1, and that may host a black hole of intermediate mass, as argued by e.g. Ptak & Griffiths (1999); Kaaret et al (2001); Matsumoto et al (2001); Strohmayer & Mushotzky (2003), but see Okajima et al (2006) for arguments in favour of a stellar mass black hole in M 82 X-1.…”

Section: Introductionmentioning

confidence: 99%

On the evolution and fate of super-massive stars

Yungelson

Heuvel²,

Vink

et al. 2007

A&A

107

114

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Context. We study the evolution and fate of solar composition super-massive stars in the mass range 60-1000 M . Our study is relevant for very massive objects observed in young stellar complexes as well as for super-massive stars that could potentially form through runaway stellar collisions. Aims. We predict the outcomes of stellar evolution by employing a mass-loss prescription that is consistent with the observed Hertzsprung-Russell Diagram location of the most massive stars. Methods. We compute a series of stellar models with an appropriately modified version of the Eggleton evolutionary code. Results. We find that super-massive stars with initial masses up to 1000 M end their lives as objects less massive than 150 M . These objects are expected to collapse into black holes (with M < ∼ 70 M ) or explode as pair-instability supernovae. Conclusions. We argue that if ultraluminous X-ray sources (ULXs) contain intermediate-mass black holes, these are unlikely to be the result of runaway stellar collisions in the cores of young clusters.

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Stellar and Gaseous Abundances in M82

Cited by 67 publications

References 47 publications

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

Metallicity diagnostics with infrared fine-structure lines

On the evolution and fate of super-massive stars

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Stellar and Gaseous Abundances in M82

Cited by 67 publications

References 47 publications

The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO+ J = 4 → 3

The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO+ J = 4 → 3

Metallicity diagnostics with infrared fine-structure lines

On the evolution and fate of super-massive stars

Contact Info

Product

Resources

About

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3