J/ApJ/619/755 Modeling starburst SEDs (Dopita+, 2005)
Modeling the pan-spectral energy distribution of starburst galaxies.
I. The role of ISM pressure and the molecular cloud dissipation timescale.
Dopita M.A., Groves B.A., Fischera J., Sutherland R.S., Tuffs R.J.,
Popescu C.C., Kewley L.J., Reuland M., Leitherer C.
<Astrophys. J., 619, 755-778 (2005)>
=2005ApJ...619..755D 2005ApJ...619..755D
ADC_Keywords: Models ; Interstellar medium ; Galaxies, IR
Keywords: dust, extinction - galaxies: general - galaxies: starburst -
H II regions - infrared: galaxies - radio continuum: galaxies -
ultraviolet: galaxies
Abstract:
In this paper, we combine the stellar spectral synthesis code
STARBURST99, the nebular modeling code MAPPINGS IIIq, a
one-dimensional dynamical evolution model of H II regions around
massive clusters of young stars, and a simplified model of synchrotron
emissivity to produce purely theoretical self-consistent synthetic
spectral energy distributions (SEDs) for (solar metallicity)
starbursts lasting ∼108yr. These SEDs extend from the Lyman limit to
beyond 21cm. We present detailed SED fits to Arp 220 and NGC 6240,
and we give the predicted colors for starburst galaxies derived from
our models for the IRAS and the Spitzer Space Telescope MIPS and IRAC
instruments. Our models reproduce the spread in observed colors of
starburst galaxies. Finally, we present absolute calibrations to
convert observed fluxes into star formation rates in the UV (GALEX),
at optical wavelengths (H), and in the IR (IRAS or Spitzer).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 172 3162 Model starburst SEDs
table7.dat 116 1054 Galex, IRAS, and Spitzer filter functions
table8.dat 25 817 Attenuation curve for the models presented in
the paper
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 3 E3.1 cm-3.K P/k ISM pressure
5- 15 E11.5 Hz Freq Frequency
17- 32 F16.9 um Lambda Wavelength
34- 42 E9.4 mW/m2 nuFnu1 The 1Myr model νf(ν) (1)
44- 52 E9.4 mW/m2 nuFnu2 The 2Myr model νf(ν) (1)
54- 62 E9.4 mW/m2 nuFnu4 The 4Myr model νf(ν) (1)
64- 72 E9.4 mW/m2 nuFnu8 The 8Myr model νf(ν) (1)
74- 82 E9.4 mW/m2 nuFnu16 The 16Myr model νf(ν) (1)
84- 92 E9.4 mW/m2 nuFnu32 The 32Myr model νf(ν) (1)
94-102 E9.4 mW/m2 nuFnuL Linear combination model νf(ν) (1)
104-112 E9.4 mW/m2/Hz Fnu1 The 1Myr model f(ν) (2)
114-122 E9.4 mW/m2/Hz Fnu2 The 2Myr model f(ν) (2)
124-132 E9.4 mW/m2/Hz Fnu4 The 4Myr model f(ν) (2)
134-142 E9.4 mW/m2/Hz Fnu8 The 8Myr model f(ν) (2)
144-152 E9.4 mW/m2/Hz Fnu16 The 16Myr model f(ν) (2)
154-162 E9.4 mW/m2/Hz Fnu32 The 32Myr model f(ν) (2)
164-172 E9.4 mW/m2/Hz FnuL Linear combination model f(ν) (2)
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Note (1): In units of erg/cm2/s.
Note (2): In units of erg/cm2/s/Hz.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 8 E8.2 Hz Freq Frequency
10- 25 F16.9 um Lambda Wavelength
27- 34 F8.6 --- Galex1500A Galex 1500 Angstrom filter transmission
36- 43 F8.6 --- Galex2300A Galex 2300 Angstrom filter transmission
45- 49 F5.3 --- IRAS100um IRAS 100 micron filter transmission
51- 55 F5.3 --- IRAS60um IRAS 60 micron filter transmission
57- 61 F5.3 --- IRAS25um IRAS 25 micron filter transmission
63- 67 F5.3 --- IRAS12um IRAS 12 micron filter transmission
69- 74 F6.4 --- IRAC3.5um IRAC 3.5 micron filter transmission
76- 81 F6.4 --- IRAC4.5um IRAC 4.5 micron filter transmission
83- 88 F6.4 --- IRAC5.7um IRAC 5.7 micron filter transmission
90- 95 F6.4 --- IRAC7.9um IRAC 7.9 micron filter transmission
97-102 F6.4 --- MIPS160um MIPS 160 micron filter transmission
104-109 F6.4 --- MIPS70um MIPS 70 micron filter transmission
111-116 F6.4 --- MIPS24um MIPS 24 micron filter transmission
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 12 F12.7 um Lambda Wavelength
14- 25 F12.9 --- Atten The E(Lambda-V)/E(B-V) attenuation
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 23-Aug-2005