J/MNRAS/436/1302 Radiation fields in star-forming galaxies (Popescu+, 2013)
Radiation fields in star-forming galaxies: the disc, thin disc and bulge.
Popescu C.C., Tuffs R.J.
<Mon. Not. R. Astron. Soc. 436, 1302 (2013)>
=2013MNRAS.436.1302P 2013MNRAS.436.1302P
ADC_Keywords: Models ; Galaxies, photometry
Keywords: radiative transfer - dust, extinction - galaxies: ISM -
galaxies: spiral - galaxies: stellar content
Abstract:
We provide a library of diffuse stellar radiation fields in spiral
galaxies derived using calculations of the transfer of stellar
radiation from the main morphological components - discs, thin discs
and bulges - through the dusty interstellar medium. These radiation
fields are self-consistent with the solutions for the integrated
panchromatic spectral energy distributions (SEDs) previously presented
using the same model. Because of this, observables calculated from the
radiation fields, such as gamma-ray or radio emission, can be
self-consistently combined with the solutions for the
ultraviolet/optical/submillimeter SEDs, thus expanding the range of
applicability of the radiation transfer model to a broader range of
wavelengths and physical quantities.
Description:
Radiative transfer model calculations of energy density of radiation
fields (RFs) are presented on a cylindrical grid (r,z). The radiation
fields are given for different values of central face-on dust opacity
in the B-band τBf, which is the only parameter of the model
shaping the spatial variation of the RFs. Since the energy densities
of the radiation fields are additive quantities, they scale with the
spatially integrated luminosity density at a given wavelength.
Therefore RFs are only calculated for a fixed reference luminosity
density (see Section 3 of journal paper). The radiation fields are
separately calculated for the disk, thin disk and bulge. For the bulge
different values of the Sersic index are considered.
In total calculations are for seven values of the central face-on dust
opacity, taufB=0.1,0.3,0.5,1.0,2.0,4.0,8.0. Solutions for other
values of taufB can be found by interpolation. Four values for the
Sersic index of the bulge are considered, n=1,2,4,8.
In total we have 7 (for taufB) x 6 (wavelengths) x 1 (disk) + 7
(for taufB) x 15 (wavelengths) x 1 ( thin disk) + 7 (for
taufB) x 6 (wavelengths) x 4 (for Sersic indices of bulge) = 315
combinations. In our model we consider the wavelength range from 912
Angstroem to 5 micron, as listed in Table E.2 of Popescu et al.
(2011, Cat. J/A+A/527/109).
Thus, the library contains a total of 315 files with two-dimensional
spatial grids of energy densities of the RFs, in files.tar file.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
models.dat 57 82896 All models values ((merged contents of
the files in "files.tar")
files.tar 1003 89145 *Individual files
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Note on files.tar: Individual files are labelled:
unitm<Mph><Band>wd01q06t<TAU>sca.dat, where <Mph> is the morphology
code (d, b, or td), <Band> is the photometric band, and is 10τ
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See also:
J/A+A/527/A109 : Dust and PAH emission SEDs of disk galaxies (Popescu+, 2011)
Byte-by-byte Description of file: models.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Mph Morphology: d=disk, b=bulge, td=thin disk
4- 7 A4 --- Band Photometric band (2)
9- 11 F3.1 --- tau [0.1/8] Central face-on dust opacity τ
in the B-band (3)
13 I1 --- n [1/8]? Sersic number (4)
16- 20 I5 pc r(pc) [0/24000] Galactocentric radial position
22- 26 I5 pc z(pc) [0/2000] Galactocentric vertical position
29- 41 E13.8 uJ/pc3/nm urad Energy density of radiation fields
(erg/pc3/Å)
45- 57 E13.8 uW/pc3/nm Eabs Energy absorbed (erg/s/pc3/Å)
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Note (2): Photometric bands are as in Popescu et al. 2011 (J/A+A/527/109):
------------------------------
uv09 91.2nm b 443nm
uv13 135nm v 564nm
uv15 150nm i 809nm
uv16 165nm
uv20 200nm j 1259nm
uv22 220nm k 2200nm
uv25 250nm
uv28 280nm nir 5000nm
uv36 365nm
------------------------------
Note (3): In all cases:
hd1=7972.02pc, zd1=272.160pc; hd2=5670.00pc, zd2=90.7200pc;
nposition in r: 22, nposition in z: 12.
The values correspond to:
* For bulge and thin disk:
τ = 0.0 ⟹ τ1 = 0.0000, τ2 = 0.0000
τ = 0.1 ⟹ τ1 = 0.0300, τ2 = 0.0700
τ = 0.3 ⟹ τ1 = 0.0800, τ2 = 0.2200
τ = 0.5 ⟹ τ1 = 0.1400, τ2 = 0.3600
τ = 1.0 ⟹ τ1 = 0.2800, τ2 = 0.7200
τ = 2.0 ⟹ τ1 = 0.5600, τ2 = 1.4400
τ = 3.5 ⟹ τ1 = 0.9800, τ2 = 2.5200
τ = 4.0 ⟹ τ1 = 1.1200, τ2 = 2.8800
τ = 8.0 ⟹ τ1 = 2.2300, τ2 = 5.7700
* For disk:
τ = 0.0 ⟹ τ1 = 0.0000, τ2 = 0.0000
τ = 0.1 ⟹ τ1 = 0.0279, τ2 = 0.0721
τ = 0.3 ⟹ τ1 = 0.0837, τ2 = 0.2163
τ = 0.5 ⟹ τ1 = 0.1395, τ2 = 0.3605
τ = 1.0 ⟹ τ1 = 0.2790, τ2 = 0.7210
τ = 2.0 ⟹ τ1 = 0.5580, τ2 = 1.4420
τ = 3.5 ⟹ τ1 = 0.9800, τ2 = 2.5200
τ = 4.0 ⟹ τ1 = 1.1160, τ2 = 2.8840
τ = 8.0 ⟹ τ1 = 2.2320, τ2 = 5.7680
Note (4): Sersic number (1,2,4,8) only for bulges and refers to the Sersic
index of the projected stellar emissivity of bulges (see Section 3 of
the paper).
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Acknowledgements:
Cristina Popescu, cpopescu(at)uclan.ac.uk
(End) Patricia Vannier [CDS] 19-Sep-2013