2006A&A...458...89L


Query : 2006A&A...458...89L

2006A&A...458...89L - Astronomy and Astrophysics, volume 458, 89-100 (2006/10-4)

Diagnostics of active galaxies. I. Modeling the infrared properties of dusty cores of starburst galaxies.

LOENEN A.F., BAAN W.A. and SPAANS M.

Abstract (from CDS):

Despite extensive observations over the last decades, the central questions regarding the power source of the large IR luminosity of Ultra Luminous Infra Red Galaxies (ULIRGs), and their evolution, are still not fully answered. In this paper we will focus on massive star formation as a central engine and present an evolutionary model for these dust-enshrouded star formation regions.An evolutionary model was created using existing star formation and radiative transfer codes (STARBURST99, RADMC and RADICAL) as building blocks. The results of the simulations are compared to data from two IRAS catalogs. From the simulations it is found that the dust surrounding the starburst region is made up from two components. There is a low optical depth (τ=0.1, which corresponds to 0.1% of the total dust mass), hot (T∼400K) non-grey component close to the starburst (scale size 10pc) and a large scale, colder grey component (100pc, 75K) with a much larger column (τ=10). The simulations also show that starburst galaxies can be powered by massive star formation. The parameters for this star forming region are difficult to determine, since the IR continuum luminosity is only sensitive to the total UV input. Therefore, there is a degeneracy between the total starburst mass and the initial mass function (IMF) slope. A less massive star formation with a shallower IMF will produce the same amount of OB stars and therefore the same amount of irradiating UV flux. Assuming the stars are formed according to a Salpeter IMF (Ψ(M)∝M–2.35), the star formation region should produce 109M of stars (either in one instantaneous burst, or in a continuous process) in order to produce enough IR radiation. Our models confirm that massive star formation is a valid power source for ULIRGs. In order to remove degeneracies and further determine the parameters of the physical environment also IR spectral features and molecular emissions need to be included.

Abstract Copyright:

Journal keyword(s): galaxies: starburst - galaxies: active - galaxies: nuclei - infrared: galaxies - infrared: ISM

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3148 2
2 IC 342 SBG 03 46 48.514 +68 05 45.98   10.5       ~ 1456 1
3 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5616 6
4 NGC 4038 GiP 12 01 53.002 -18 52 03.32   10.91   9.74 11.0 ~ 1304 1
5 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1631 0
6 NGC 4039 GiP 12 01 53.8 -18 53 06   11.08   9.77   ~ 1148 1
7 NGC 4945 Sy2 13 05 27.279 -49 28 04.44   9.31 14.40 7.55   ~ 1375 2
8 M 83 SBG 13 37 00.91920 -29 51 56.7400 8.85 8.11 7.52 7.21   ~ 2410 2
9 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2835 4
10 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1564 2

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2022.08.09-01:00:02

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