J/ApJS/167/177 Emission lines of evolving HII regions (Dopita+, 2006)
Modeling the pan-spectral energy distribution of starburst galaxies.
III. Emission line diagnostics of ensembles of evolving H II regions.
Dopita M.A., Fischera J., Sutherland R.S., Kewley L.J., Leitherer C.,
Tuffs R.J., Popescu C.C., van Breugel W., Groves B.A.
<Astrophys. J. Suppl. Ser., 167, 177-200 (2006)>
=2006ApJS..167..177D 2006ApJS..167..177D
ADC_Keywords: Models, evolutionary ; H II regions ; Energy distributions
Keywords: galaxies: abundances - galaxies: formation - galaxies: general -
galaxies: starburst - ISM: abundances - H II regions
Abstract:
We build, as far as theory will permit, self-consistent model HII
regions around central clusters of aging stars. These produce strong
emission line diagnostics applicable to either individual HII regions
in galaxies or to the integrated emission line spectra of disk or
starburst galaxies. The models assume that the expansion and internal
pressure of individual HII regions is driven by the net input of
mechanical energy from the central cluster, be it through winds or
supernova events. This eliminates the ionization parameter as a free
variable, replacing it with a parameter that depends on the ratio of
the cluster mass to the pressure in the surrounding interstellar
medium. These models explain why HII regions with low abundances have
high excitation and demonstrate that at least part of the warm ionized
medium is the result of overlapping faint, old, large, and
low-pressure HII regions. We present line ratios (at both optical and
IR wavelengths) that provide reliable abundance diagnostics for both
single HII regions or for integrated galaxy spectra, and we find a
number that can be used to estimate the mean age of the cluster stars
exciting individual HII regions.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 22 51 Line ID and wavelength list
lineflux.dat 160 1275 Line flux ratios in HII region models for 0.05,
0.2, 0.4, 1.0 and 2.0Z☉ abundance set
(tables 3-7 of the paper)
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See also:
J/AJ/109/2503 : Synthesis model in HII regions. II. (Mayya 1995)
J/ApJ/619/755 : Modeling starbust SEDs (Dopita+, 2005)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- ID [1/51] Line ID
4- 11 A8 --- Ion Ion designation
15- 22 F8.1 0.1nm lambda Wavelength
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Byte-by-byte Description of file: lineflux.dat
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Bytes Format Units Label Explanations
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1- 4 F4.2 [Sun] Abund Model abundance value in solar abundance
6- 7 I2 [-] logR The R value (+2, +0, -2, -4, -6) (1)
9- 10 I2 --- ID The line ID number, defined in table2.dat
12- 20 E9.3 0.1nm lambda Wavelength of line in Angstroms
22- 30 E9.3 --- F0.1 The F(line)/F(Hβ) Ratio at t=0.1Myr (2)
32- 40 E9.3 --- F0.5 The F(line)/F(Hβ) Ratio at t=0.5Myr (2)
42- 50 E9.3 --- F1.0 The F(line)/F(Hβ) Ratio at t=1.0Myr (2)
52- 60 E9.3 --- F1.5 The F(line)/F(Hβ) Ratio at t=1.5Myr (2)
62- 70 E9.3 --- F2.0 The F(line)/F(Hβ) Ratio at t=2.0Myr (2)
72- 80 E9.3 --- F2.5 The F(line)/F(Hβ) Ratio at t=2.5Myr (2)
82- 90 E9.3 --- F3.0 The F(line)/F(Hβ) Ratio at t=3.0Myr (2)
92-100 E9.3 --- F3.5 The F(line)/F(Hβ) Ratio at t=3.5Myr (2)
102-110 E9.3 --- F4.0 The F(line)/F(Hβ) Ratio at t=4.0Myr (2)
112-120 E9.3 --- F4.5 The F(line)/F(Hβ) Ratio at t=4.5Myr (2)
122-130 E9.3 --- F5.0 The F(line)/F(Hβ) Ratio at t=5.0Myr (2)
132-140 E9.3 --- F5.5 The F(line)/F(Hβ) Ratio at t=5.5Myr (2)
142-150 E9.3 --- F6.0 The F(line)/F(Hβ) Ratio at t=6.0Myr (2)
152-160 E9.3 --- The F(line)/F(Hβ) Time-Averaged Ratio (2)
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Note (1): The ratio R is defined as
R = Mcl/(P/k) in M☉*104cm-3K units
where Mcl is the mass of the central cluster and
P is the pressure in the HII region.
Note (2): with respect to Hβ=1.0.
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History:
From electronic version of the journal
References:
Dopita et al., Paper I 2005ApJ...619..755D 2005ApJ...619..755D, Cat. J/ApJ/619/755
Dopita et al., Paper II 2006ApJ...647..244D 2006ApJ...647..244D
Groves et al., Paper IV 2008ApJS..176..438G 2008ApJS..176..438G
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 29-May-2008