Panchromatic spectral energy distributions of Herschel sources

By S. Berta, D. Lutz, P. Santini, S. Wuyts, D. Rosario, D. Brisbin, A. Cooray, A. Franceschini, C. Gruppioni, E. Hatziminaoglou and 17 more. 2013

141 citations recorded by the source corpus.

Combining far-infrared Herschel photometry from the PACS Evolutionary Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time programs with ancillary datasets in the GOODS-N, GOODS-S, and COSMOS fields, it is possible to sample the 8–500 μm spectral energy distributions (SEDs) of galaxies with at least 7–10 bands. Extending to the UV, optical, and near-infrared, the number of bands increases up to 43. We reproduce the distribution of galaxies in a carefully selected restframe ten colors space, based on this rich data-set, using a superposition of multivariate Gaussian modes. We use this model to classify galaxies and build median SEDs of each class, which are then fitted with a modified version of the magphys code that combines stellar light, emission from dust heated by stars and a possible warm dust contribution heated by an active galactic nucleus (AGN). The color distribution of galaxies in each of the considered fields can be well described with the combination of 6–9 classes, spanning a large range of far- to near-infrared luminosity ratios, as well as different strength of the AGN contribution to bolometric luminosities. The defined Gaussian grouping is used to identify rare or odd sources. The zoology of outliers includes Herschel-detected ellipticals, very blue z ~ 1 Ly-break galaxies, quiescent spirals, and torus-dominated AGN with star formation. Out of these groups and outliers, a new template library is assembled, consisting of 32 SEDs describing the intrinsic scatter in the restframe UV-to-submm colors of infrared galaxies. This library is tested against L(IR) estimates with and without Herschel data included, and compared to eightother popular methods often adopted in the literature. When implementing Herschel photometry, these approaches produce L(IR) values consistent with each other within a median absolute deviation of 10–20%, the scatter being dominated more by fine tuning of the codes, rather than by the choice of SED templates. Finally, the library is used to classify 24 μm detected sources in PEP GOODS fields on the basis of AGN content, L(60)/L(100) color and L(160)/L(1.6) luminosity ratio. AGN appear to be distributed in the stellar mass (M_∗) vs. star formation rate (SFR) space along with all other galaxies, regardless of the amount of infrared luminosity they are powering, with the tendency to lie on the high SFR side of the “main sequence”. The incidence of warmer star-forming sources grows for objects with higher specific star formation rates (sSFR), and they tend to populate the “off-sequence” region of the M_∗ − SFR − z space.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6079f4ddaf458666882f84859f193618b475b5cb

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In Astronomy and Astrophysics

1. P. Hopkins
2. D. M. Alexander
3. L. Hernquist
4. E. Daddi
5. P. V. van Dokkum
6. R. Dav'e
7. R. Somerville
8. C. Conroy

In Instrumentation

1. P. V. van Dokkum
2. C. Conroy
3. P. Hopkins
4. E. Daddi
5. L. Hernquist
6. D. M. Alexander
7. A. Renzini
8. M. Franx

Citations in the corpus

• Active galactic nuclei: what’s in a name? (2017, methodology): “3.2.1); (4) multiple component SED fitting using sets of galaxy and AGN templates (Berta et al. 2013; Delvecchio et al. 2014, 2017; Calistro et al. 2017) (5) excess of radio luminosity relative to a tracer of the SF rate (SFR) in the host galaxy (e.g. far or total IR luminosity; Condon 1992; Del…”
• Dust spectral energy distributions of nearby galaxies: an insight from the Herschel Reference Survey (2014, methodology): “We compare our templates with the most popular IR SED libraries used in the literature, i.e. CE01, DH02, Elbaz et al. (2011), Magdis et al. (2012), Smith et al. (2012a) and Berta et al. (2013).”
• PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions (2017, background): “…mass ratio (which can be a function of metallicity, see below, e.g. Leroy et al. 2011, Rémy–Ruyer et al. 2014, Eales et al. 2012, Magdis et al. 2011, 2012a, Magnelli et al. 2012a, Santini et al. 2014, Sargent et al. 2014, Béthermin et al. 2015, Schreiber et al. 2015, Berta et al. 2013, 2016, G15).”
• The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations (2013, background): “…luminosity functions of galaxies (e.g., Gruppioni et al. 2010, 2013; Casey et al. 2012) and the examination of their spectral energy distributions (e.g., Hwang et al. 2010; Elbaz et al. 2010, 2011; Nordon et al. 2010, 2012; Magnelli et al. 2010, 2012; Symeonidis et al. 2013; Berta et al. 2013).”
• Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, methodology): “The code by Berta et al. (2013) includes the AGN component and differs from the original MAGPHYS in the model normalization approach.”
• An Older, More Quiescent Universe from Panchromatic SED Fitting of the 3D-HST Survey (2018, background): “Emission from central active galactic nuclei (AGNs) is now built into many SED-fitting models (Berta et al. 2013; Ciesla et al. 2015; Calistro Rivera et al. 2016; Leja et al. 2018).”
• The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, methodology): “For this reason, we obtained measurements of the stellar masses of our objects containing an AGN by means of the specific decomposition technique developed by Berta et al. (2013), to separate stellar and nuclear emission components.”
• The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, methodology): “Then, we recompute the stellar mass of each X-ray emitter by means of a three-component SED fitting code (sed3fit, Berta et al. 2013)6.”
• The evolution of the dust and gas content in galaxies (2013, background): “B.1 and Berta et al. 2013); by moving the data points with the largest SFR towards lower SFR values, this effect might be responsible for the shallower slope measured at high redshift.”
• A TWO-PARAMETER MODEL FOR THE INFRARED/SUBMILLIMETER/RADIO SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES AND ACTIVE GALACTIC NUCLEI (2014, unknown): “Some models do incorporate dust emission from both AGN and star formation (Siebenmorgen & Krügel 2007; Rieke et al. 2009; Berta et al. 2013), but most do not.”