Axisymmetric model of the ionized gas in the Orion Nebula

Rubin, R. H.; Simpson, Janet P.; Haas, Michael R.; Erickson, E. F.

doi:10.1086/170145

Cited by 125 publications

(123 citation statements)

References 0 publications

Supporting

Mentioning

114

Contrasting

Unclassified

Order By: Relevance

“…As a result of the metal depletion onto dust grains the gas-phase elemental abundances are altered to H: 1.00, He: 9.50 Â 10 À2 , Li: 5.40 Â 10 À11 , B: 8.90 Â 10 À11 , C: 3.00 Â 10 À4 , N: 7.00 Â 10 À5 , O: 4.00 Â 10 À4 , Ne: 6.00 Â 10 À5 , Na: 3.00 Â 10 À7 , Mg: 3.00 Â 10 À6 , Al: 2.00 Â 10 À7 , Si: 4.00 Â 10 À6 , P: 1.60 Â 10 À7 , S: 1.00 Â 10 À5 , Cl: 1.00 Â 10 À7 , Ar: 3.00 Â 10 À6 , K: 1.10 Â 10 À8 , Ca: 2.00 Â 10 À8 , Ti: 5.80 Â 10 À10 , V: 1.00 Â 10 À10 , Cr: 1.00 Â 10 À8 , Mn: 2.30 Â 10 À8 , Fe: 3.00 Â 10 À6 , Ni: 1.00 Â 10 À7 , Cu: 1.50 Â 10 À9 , and Zn: 2.00 Â 10 À8 . These depleted elemental abundances are based on results of several studies of the Orion nebula (Baldwin et al 1991;Rubin et al 1991;Rubin, Dufour, & Walter 1993;Rubin et al 1992;Osterbrock, Tran, & Veilleux 1992). Note that beryllium, fluorine, scandium, and cobalt are not included in the calculations for the dusty models.…”

Section: Methodsmentioning

confidence: 99%

Iron Is Not Depleted in High-Ionization Nuclear Emission-Line Regions of Active Galactic Nuclei

Nagao

Murayama

Shioya

et al. 2003

The Astronomical Journal

View full text Add to dashboard Cite

To examine whether or not high-ionization nuclear emission-line regions (HINERs) in narrow-line regions of active galactic nuclei are dusty, we focus on two high-ionization forbidden emission lines, [Fe vii consistent with the dust-free models, while it cannot easily be explained by the dusty models. This suggests that iron is not depleted in HINERs, which implies that the HINERs are not dusty. This result is consistent with the idea that the HINERs are located closer than the dust-sublimation radius (i.e., the inner radius of dusty tori) and thus can be hidden by dusty tori when seen from a edge-on view toward the tori, which is also suggested by the AGN-type dependence of the visibility of high-ionization emission lines.

show abstract

Section: Methodsmentioning

confidence: 99%

Iron Is Not Depleted in High-Ionization Nuclear Emission-Line Regions of Active Galactic Nuclei

Nagao

Murayama

Shioya

et al. 2003

The Astronomical Journal

View full text Add to dashboard Cite

show abstract

“…Thuan et al 1996;Izotov & Thuan 1998;Pustilnik et al 2004), and can be explained by the presence of Wolf-Rayet stars (Bergvall & Östlin 2002), which inject matter enriched in N and C into the ISM. For the other elements, we use gas-phase relative abundances typical of H ii regions, based on an average of the abundances in the Orion Nebula determined by Baldwin et al (1991), Rubin et al (1991), Osterbrock et al (1992), Rubin et al (1993), and scaling them to the metallicity of Haro 11. The resulting carbon abundance is log(C/O) = −0.15, which is relatively high compared to Izotov & Thuan (1999), where log(C/O) ∼ −0.5.…”

Section: Elemental Abundancesmentioning

confidence: 99%

The nature of the interstellar medium of the starburst low-metallicity galaxy Haro 11: a multi-phase model of the infrared emission

Cormier

Lebouteiller

Madden

et al. 2012

A&A

102

138

View full text Add to dashboard Cite

Context. The low-metallicity interstellar medium (ISM) is profoundly different from that of normal systems, being clumpy with low dust abundance and little CO-traced molecular gas. Yet many dwarf galaxies in the nearby universe are actively forming stars. As the complex ISM phases are spatially mixed with each other, detailed modeling is needed to understand the gas emission and subsequent composition and structure of the ISM. Aims. Our goal is to describe the multi-phase ISM of the infrared bright low-metallicity galaxy Haro 11, dissecting the photoionised and photodissociated gas components. Methods. We present observations of the mid-infrared and far-infrared fine-structure cooling lines obtained with the Spitzer/IRS and Herschel/PACS spectrometers. We use the spectral synthesis code Cloudy to methodically model the ionised and neutral gas from which these lines originate. Results. We find that the mid-and far-infrared lines account for ∼1% of the total infrared luminosity L TIR , acting as major coolants of . Due to their different origins, the observed lines require a multi-phase modeling comprising: a compact H ii region, dense fragmented photodissociation regions (PDRs), a diffuse extended low-ionisation/neutral gas which has a volume filling factor of at least 90%, and porous warm dust in proximity to the stellar source. For a more realistic picture of the ISM of Haro 11 we would need to model the clumpy source and gas structures. We combine these 4 model components to explain the emission of 17 spectral lines, investigate the global energy balance of the galaxy through its spectral energy distribution, and establish a phase mass inventory. While the ionic emission lines of Haro 11 essentially originate from the dense H ii region component, a diffuse low-ionisation gas is needed to explain the

show abstract

“…To reach agreement between the model and the observations, t 2 values in the 0.036 to 0.058 range are needed. Similarly, the two-dimensional blister model of the Orion nebula by Rubin et al 1991 again predicts I (X4363)// (X5007) ratios considerably smaller than observed. These differences cannot be explained by the models and indicate the presence of substantial temperature variations along the line of sight probably due to shock waves.…”

Section: Galactic H II Regionsmentioning

confidence: 66%

The effect of shock waves on the spectra of H II regions and planetary nebulae

Peimbert

Sarmiento

Fierro

1991

PASP

View full text Add to dashboard Cite

Emission lines from H II regions and planetary nebulae are contaminated by shock waves produced by stellar winds and supernova remnants. This effect is studied and it is found that it could be responsible for: (a) the difference between the O/H abundances derived from the O nebular lines coupled with H II region models and those derived from the observed I (4363)// (5007) ratio, (b) the large t 2 values observed in the Orion nebula and M 8, (c) the difference between the stellar and the H II region O/H abundances in the solar neighborhood, (d) the large [S n]/Ha ratios observed in H II galaxies, and (e) the low O/H ratios and the N/O versus O/H anticorrelation found in Type I PN and shell nebulae around Population I stars.

show abstract

Axisymmetric model of the ionized gas in the Orion Nebula

Cited by 125 publications

References 0 publications

Iron Is Not Depleted in High-Ionization Nuclear Emission-Line Regions of Active Galactic Nuclei

Iron Is Not Depleted in High-Ionization Nuclear Emission-Line Regions of Active Galactic Nuclei

The nature of the interstellar medium of the starburst low-metallicity galaxy Haro 11: a multi-phase model of the infrared emission

The effect of shock waves on the spectra of H II regions and planetary nebulae

Contact Info

Product

Resources

About