2010A&A...523A..78D


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.15CEST08:06:00

2010A&A...523A..78D - Astronomy and Astrophysics, volume 523, A78-78 (2010/11-2)

Exploring the physical properties of local star-forming ULIRGs from the ultraviolet to the infrared.

DA CUNHA E., CHARMANDARIS V., DIAZ-SANTOS T., ARMUS L., MARSHALL J.A. and ELBAZ D.

Abstract (from CDS):

We apply the da Cunha et al. (2008MNRAS.388.1595C) model of the spectral energy distribution (SEDs) of galaxies to a small pilot sample of purely star-forming ultra-luminous infrared galaxies (ULIRGs). We interpret the observed SEDs of 16 ULIRGs using this physically-motivated model that accounts for both the emission of stellar populations from the ultraviolet to the near-infrared and for the attenuation by dust in two components: an optically-thick starburst component and the diffuse ISM. The infrared emission is computed by assuming that all the energy absorbed by dust in these components is re-radiated at mid- and far-infrared wavelengths. This model allows us to derive statistically physical properties including star formation rates, stellar masses, the temperatures and masses of different dust components, and plausible star formation histories. We find that, although the ultraviolet-to-near-infrared emission represents only a small fraction of the total power radiated by ULIRGs, observations in this wavelength range are important for understanding the properties of the stellar populations and dust attenuation in the diffuse ISM of these galaxies. Furthermore, our analysis indicates that the use of mid-infrared spectroscopy from the infrared spectrograph on the Spitzer Space Telescope is crucial to obtain realistic estimates of the extinction to the central energy source, mainly via the depth of the 9.7-µm silicate feature, and thus accurately constrain the total energy balance. Our findings are consistent with the notion that, in the local Universe, the physical properties of ULIRGs are fundamentally different from those of galaxies with lower infrared luminosities and that local ULIRGs are the result of merger-induced starbursts. While these are well-established ideas, we demonstrate the usefulness of our SED modelling in deriving relevant physical parameters that provide clues to the star formation mode of galaxies.

Abstract Copyright:

Journal keyword(s): galaxies: evolution - galaxies: fundamental parameters - galaxies: starburst - galaxies: ISM

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 IRAS 00199-7426 G 00 22 07.0041916624 -74 09 41.587896860   17.41   16.24   ~ 31 1
2 2MASX J01515140-1830464 G 01 51 51.4246135039 -18 30 46.604977599   18.77       ~ 33 1
3 FIRST J024008.5-004203 G 02 40 08.576 -00 42 03.56           ~ 5 0
4 IRAS 04114-5117 G 04 12 44.202 -51 09 40.22   18.12   17.22   ~ 18 1
5 2MASX J05583717-7716393 G 05 58 37.176 -77 16 39.37           ~ 13 1
6 FIRST J082354.6+320212 G 08 23 54.616 +32 02 12.03           ~ 8 0
7 FF J1018+3649 BiC 10 18 34.578 +36 49 51.47           ~ 9 0
8 2XMM J105918.1+243234 LIN 10 59 18.128 +24 32 34.74   15.7       ~ 243 1
9 LEDA 39024 LIN 12 13 46.107 +02 48 41.50           ~ 315 1
10 2MASX J13150638-5509225 Sy2 13 15 06.383 -55 09 22.60   17.3       ~ 112 0
11 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2739 4
12 IRAS 16334+4630 LIN 16 34 52.1 +46 24 53   17.66       ~ 41 1
13 6dFGS gJ172322.0-001701 LIN 17 23 21.943 -00 17 00.96   15.1       ~ 379 0
14 2MASX J19322229-0400010 EmG 19 32 22.2960198723 -04 00 01.793135107   18.85   17.04   ~ 90 0
15 LEDA 90339 G 19 48 15.7 +09 52 05           ~ 33 0
16 6dFGS gJ204418.2-164017 LIN 20 44 18.186 -16 40 16.63   18.02   17.04   ~ 78 0
17 NAME South America H2G 22 51 49.307 -17 52 23.96   16.97       ~ 290 3

    Equat.    Gal    SGal    Ecl

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2021.04.15-08:06:00

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