Determining Star Formation Rates for Infrared Galaxies

Rieke, G. H.; Alonso‐Herrero, A.; Weiner, Benjamin J.; Pérez‐González, Pablo G.; Blaylock, Myra L.; Donley, J. L.; Marcillac, D.

doi:10.1088/0004-637x/692/1/556

Cited by 607 publications

(1,247 citation statements)

References 121 publications

(205 reference statements)

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“…Another set of templates used extensively by the DSFG community are those described in Rieke et al (2009). Rieke et al use detailed Spitzer observations of eleven local LIRGs and ULIRGs to construct a library of templates spanning 0.4µm-30 cm and luminosities 5×10 9 -10 13 L .…”

Section: Direct Fir-only Methodsmentioning

confidence: 99%

“…the "Santa Cruz SAM") that was combined with estimates for dust attenuation by both diffuse dust and stellar birth clouds surrounding young clusters. The energy absorbed by dust was assumed to be re-radiated in the infrared, and combined these with both theoretical SED templates by Devriendt et al (1999), as well as the locally-calibrated observed SED templates by Rieke et al (2009). These authors found that in order to reproduce the (rest) UV and optical luminosity functions at high-z, an evolving dust-to-metals ratio was necessary.…”

Section: Semi-analytic Methodsmentioning

confidence: 99%

“…Checked for consistency against Spitzer data. Rieke et al (2009) 14 templates, based on IRS and ISO spectra of eleven local LIRGs and ULIRGs connected to modified blackbodies with temperatures 38-64 K (where temperature scales with luminosity). Resulting templates span 5×10 9 -10 13 L , where most luminous sources have strongest silicate absorption.…”

Section: Empirical Templatesmentioning

confidence: 99%

“…Dale & Helou, 2002;Chary & Elbaz, 2001;Rieke et al, 2009). These templates, calibrated for z ∼ 0 LIRGs and ULIRGs, can usually be parameterized in terms of the bolometric luminosity of the galaxy, which is a readily available quantity from SAMs.…”

Section: Semi-analytic Modelsmentioning

confidence: 99%

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Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Section: Direct Fir-only Methodsmentioning

confidence: 99%

Section: Semi-analytic Methodsmentioning

confidence: 99%

Section: Empirical Templatesmentioning

confidence: 99%

Section: Semi-analytic Modelsmentioning

confidence: 99%

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Dusty star-forming galaxies at high redshift

2014

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“…We consider the theoretical approach taken in Somerville et al (2011) and Gilmore et al (2011) Charlot & Fall (2000); Dust re-emission: templates by Rieke et al (2009) (ii) Backward evolution, e.g., Franceschini et al (2008) Observed local-optical galaxy luminosity function (LF, for starburst population) and near-IR galaxy LF observed up to z = 1.4 (for elliptical and spiral populations)…”

Section: Introductionmentioning

confidence: 99%

An empirical approach to the extragalactic background light from AEGIS galaxy SED-type fractions

Domínguez

2011

Proc. IAU

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Abstract. The extragalactic background light (EBL) is of fundamental importance both for understanding the entire process of galaxy evolution and for γ-ray astronomy. However, the overall spectrum of the EBL between 0.1 and 1000 µm has never been determined directly, neither from observed luminosity functions (LFs), over a wide redshift range, nor from any multiwavelength observation of galaxy spectral energy distributions (SEDs). The evolving overall spectrum of the EBL is derived here utilizing a novel method based on observations only. It is emphasized that the local EBL seems already well constrained from the UV up to the mid-IR. Different independent methodologies such as direct measurement, galaxy counts, γ-ray attenuation and realistic EBL modelings point towards the same EBL intensity level. Therefore, a relevant contribution from Pop III stars to the local EBL seems unlikely.

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Observing Supermassive Black Holes Across Cosmic Time: From Phenomenology to Physics

Merloni

2016

Astrophysical Black Holes

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In the last decade, a combination of high sensitivity, high spatial resolution observations and of coordinated multi-wavelength surveys has revolutionized our view of extra-galactic black hole (BH) astrophysics. We now know that supermassive black holes reside in the nuclei of almost every galaxy, grow over cosmological times by accreting matter, interact and merge with each other, and in the process liberate enormous amounts of energy that influence dramatically the evolution of the surrounding gas and stars, providing a powerful self-regulatory mechanism for galaxy formation. The different energetic phenomena associated to growing black holes and Active Galactic Nuclei (AGN), their cosmological evolution and the observational techniques used to unveil them, are the subject of this chapter. In particular, I will focus my attention on the connection between the theory of high-energy astrophysical processes giving rise to the observed emission in AGN, the observable imprints they leave at different wavelengths, and the methods used to uncover them in a statistically robust way. I will show how such a combined effort of theorists and observers have led us to unveil most of the SMBH growth over a large fraction of the age of the Universe, but that nagging uncertainties remain, preventing us from fully understating the exact role of black holes in the complex process of galaxy and large-scale structure formation, assembly and evolution.

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Determining Star Formation Rates for Infrared Galaxies

Cited by 607 publications

References 121 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

An empirical approach to the extragalactic background light from AEGIS galaxy SED-type fractions

Observing Supermassive Black Holes Across Cosmic Time: From Phenomenology to Physics

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