Dust in starburst nuclei and ULIRGs - SED models for observers

By R. Siebenmorgen, E. Kruegel. 2006

164 citations recorded by the source corpus.

Aims. We provide a library of some 7000 SEDs for the nuclei of starburst and ultra luminous galaxies. Its purpose is to quickly ob tain estimates of the basic parameters, such as luminosity, size and dust or gas mass and to predict the flux at yet unobserved wavelengths . The procedure is simple and consists of finding an element in the library that m atches the observations. The objects may be in the local universe or at high z. Methods. We calculate the radiative transfer in spherical symmetry for a stellar cluster permeated by an interstellar medium with standard (Milky Way) dust properties. The cluster contains two stellar populations: old bulge stars and OB stars. Because the latter are young, a certain fraction of them will be embedded in compact clouds which constitute hot spots that determine the MIR fluxes. Results. We present SEDs for a broad range of luminosities, sizes and obscurations. We argue that the assumption of spherical symmetry and the neglect of clumpiness of the medium are not severe shortcomings for computing the dust emission. The validity of the approach is demonstrated by matching the SED of seven of the best studied galaxies, including M82 and Arp220, by library elements. In all cases, one finds an element which fits the observed SED very well, and the p arameters defining the element are in full accord with what is known about the galaxy from detailed studies. We also compare our method of computing SEDs with other techniques described in the literature.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/cb6df9f8b08b65186165ac838db43a8594b99eca

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Citations in the corpus

Star formation and mass assembly in high-redshift galaxies (2009, methodology): “A variety of different libraries are used for this purpose (e.g., Chary & Elbaz 2001; Dale & Helou 2002; Lagache et al. 2003; Siebenmorgen & Krügel 2007, and so on).”
Panchromatic spectral energy distributions of Herschel sources (2013, methodology): “Modeling from the ultraviolet (UV) to FIR, making use of radiative transfer and ray tracing techniques (e.g. Siebenmorgen & Krügel 2007; Piovan et al. 2006; Dopita et al. 2005; Efstathiou et al. 2000; Silva et al. 1998), provides extensive information on the physical properties of star-forming…”
Modelling the spectral energy distribution of galaxies - V. The dust and PAH emission SEDs of disk galaxies (2010, background): “Models for starburst galaxies can befound in Rowan-Robinson & Efstathiou 1993, Krügel & Siebenmorgen 1994, Silva et al. 1998, Efstathiou et al. 2000, Takagi et al. 2003,Dopita et al. 2005, Siebenmorgen & Krügel 2007, Groves et al. 2008.”
Photometric redshifts in the SWIRE Survey (2008, background): “…that the estimate of the infrared bolometric luminosity is uncertain by a factor of ∼2 due to uncertainties in the correct template fit (RowanRobinson et al 2005, Siebenmorgen and Krugel 2007; Reddy et al (2006) quote 2-3), and this applies also to derived quantities like the star-formation rate.”
Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. IV. The Controlling Parameters of the Starburst SED (2007, methodology): “In connection with this is the total luminosity of Arp 220, which is log L∗ = 12.16(L⊙) in our models, close to the value of 12.1 of Tagaki et al. (2003b) and Siebenmorgen & Krügel (2007), and just below the 12.4 from Silva et al. (1998).”
Fitting the integrated spectral energy distributions of galaxies (2010, methodology): “Like da Cunha et al. (2008) and Siebenmorgen and Krügel (2007) it provides physical templates with as few parameters as possible.”
Far-infrared spectral energy distribution fitting for galaxies near and far (2012, methodology): “While the Siebenmorgen & Krügel (2007) work contains ∼7000 SEDs, we limit ourselves to the 120 most luminous SEDs, consistent with ULIRG infrared luminosities.”
GOODS-HERSCHEL AND CANDELS: THE MORPHOLOGIES OF ULTRALUMINOUS INFRARED GALAXIES AT z ∼ 2 (2011, methodology): “The vast majority of the sources were best fit using the Siebenmorgen & Krügel (2007) library, which is based on radiative transfer models and spans a wide range of template shapes.”
A TWO-PARAMETER MODEL FOR THE INFRARED/SUBMILLIMETER/RADIO SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES AND ACTIVE GALACTIC NUCLEI (2014, methodology): “The colors for local actively star-forming galaxies (filled squares) shown in Figure 5 come from Siebenmorgen & Krügel (2007), the colors for normal star-forming galaxies (open circles) are from Dale et al. (2012), and the colors for the local AGN M 87 (filled triangle) are from NED; the…”
A CHANDRA PERSPECTIVE ON GALAXY-WIDE X-RAY BINARY EMISSION AND ITS CORRELATION WITH STAR FORMATION RATE AND STELLAR MASS: NEW RESULTS FROM LUMINOUS INFRARED GALAXIES (2010, background): “The obscuration to these star-forming regions can be very significant (AV >∼ 50 mag; e.g., Genzel et al. 1998; Siebenmorgen & Krügel 2007) and can attenuate emission over the 2–10 keV bandpass.”
Dusty Star Forming Galaxies at High Redshift (2014, background): “…the complex dust infrared emission from stars, molecular clouds and dust grains over a wide range of galaxy geometries and luminosities (Silva et al., 1998; Chary and Elbaz, 2001; Dale et al., 2001; Dale and Helou, 2002; Abel and Wandelt, 2002; Siebenmorgen and Krügel, 2007; Draine and Li, 2007).”
DETERMINING STAR FORMATION RATES FOR INFRARED GALAXIES (2008, background): “Existing libraries of SED templates (e.g., Chary & Elbaz 2001; Dale & Helou 2002; Siebenmorgen & Krügel 2007) show a strong pattern of behavior with bolometric luminosity.”