Synthetic properties of starburst galaxies

Leitherer, Claus; Heckman, Timothy M.

doi:10.1086/192112

Cited by 2,020 publications

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“…Dale & Helou (2002) builds on this phenomenological approach by extending calibration at wavelengths >120 µm and correcting the Dale et al (2001) model assumptions regarding dust emissivity and radiation field intensity. Dopita et al (2005) present another modeling technique which reproduces SEDs from the ultraviolet through the far-infrared, and out through the radio by combining stellar synthesis output from STARBURST99 (Leitherer & Heckman, 1995), nebular line emission modeling, a dynamic evolution model of Hii regions and a simplified synchrotron emissivity model to construct self-consistent SEDs for solar-metallicity starbursts with durations ∼100 Myr. They Silva et al (1998) Stellar population synthesis model which accounts for dust obscuration from UV through the FIR; incorporates chemical evolution, gas fraction, metallicity, ages, relative fraction of starforming molecular gas to diffuse gas, the effect of small grains and PAHs and compares to observations from ISO.…”

Section: Employing Dust Radiative Transfer Models and Empirical Templmentioning

confidence: 99%

“…which takes the radiative transfer models of Leitherer & Heckman (1995) for continuous starbursts ranging in age from 10-100 Myr and a Salpeter IMF (Salpeter, 1955). Note importantly that this conversion does not account for AGN heating of dust in this wavelength regime, even though AGN fractional contribution is known to be non-negligible (10-30%).…”

Section: Estimating L Ir T Dust and M Dust From An Sedmentioning

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: Employing Dust Radiative Transfer Models and Empirical Templmentioning

confidence: 99%

Section: Estimating L Ir T Dust and M Dust From An Sedmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…We chose to do so with the full spectral fitting technique, using the STARLIGHT code (Cid Fernandes et al 2005) that produces a model spectrum from a linear combination of simple stellar population spectra, convolved with a kinematic kernel and corrected for extinction, to find the stellar population model that best matches an observed spectrum. STARBURST99 (Leitherer et al 1999) stellar populations were used as templates to fit the spectrum, with absolute metallicities of 0.001, 0.002, 0.008, 0.014 and 0.040 and ages between 2 Myr and 3 Gyr. We prefer instantaneous burst models, since continuous star formation models are not simple to interpret in this linear combination method, and use the Geneva tracks with zero rotation and the Kroupa (2001) IMF.…”

Section: Stellar Populationsmentioning

confidence: 99%

A young star-forming galaxy at z = 3.5 with an extended Lyman α halo seen with MUSE

Patrício¹,

Richard²,

Verhamme

2015

Proc. IAU

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Spatially resolved studies of high-redshift galaxies, an essential insight into galaxy formation processes, have been mostly limited to stacking or unusually bright objects. We present here the study of a typical (L * , M = 6 × 10 9 M ) young lensed galaxy at z = 3.5, observed with Multi Unit Spectroscopic Explorer (MUSE), for which we obtain 2D resolved spatial information of Lyα and, for the first time, of C III] emission. The exceptional signal-to-noise ratio of the data reveals UV emission and absorption lines rarely seen at these redshifts, allowing us to derive important physical properties (T e ∼ 15600 K, n e ∼ 300 cm −3 , covering fraction f c ∼ 0.4) using multiple diagnostics. Inferred stellar and gas-phase metallicities point towards a low-metallicity object (Z stellar = ∼0.07 Z and Z ISM < 0.16 Z ). The Lyα emission extends over ∼10 kpc across the galaxy and presents a very uniform spectral profile, showing only a small velocity shift which is unrelated to the intrinsic kinematics of the nebular emission. The Lyα extension is approximately four times larger than the continuum emission, and makes this object comparable to low-mass LAEs at low redshift, and more compact than the Lyman-break galaxies and Lyα emitters usually studied at high redshift. We model the Lyα line and surface brightness profile using a radiative transfer code in an expanding gas shell, finding that this model provides a good description of both observables.Key words: techniques: imaging spectroscopy -galaxies: abundances -galaxies: highredshift -galaxies: individual: SMACSJ2031.8-4036. I N T RO D U C T I O NDuring the past few decades, our understanding of galaxy formation and evolution has made significant progress thanks to the hundreds of high-redshift (z > 3) galaxies which have been detected in dedicated observing campaigns (e.g. Shapley et al. 2003;Vanzella et al. 2009;Stark et al. 2013). The main spectral feature used to confirm the distances of these galaxies is the Lyα emission, since it E-mail: vera.patricio@univ-lyon1.fr (VP); johan.richard@univ-lyon1.fr (JR) is the brightest emission line we can observe in distant sources. Unfortunately, many of these objects are too faint to show any other emission line at rest-frame UV wavelengths or, even less likely, continuum and absorption lines, offering a limited picture of the characteristics of high-redshift galaxies. The complexity of the Lyα resonant process, which depends not only on the gas dynamics but also on gas density and dust content, also requires the observation of non-resonant lines in order to robustly probe the physical properties of such galaxies.Stacking techniques, which combine spectra or images of dozens or even hundreds of objects in order to increase signal-to-noise ratio (e.g.

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“…To model our sample of galaxies we have used the Starburst99 code (Leitherer et al 1999, Vázquez & Leitherer 2005 to generate theoretical spectral energy distributions (SEDs), which in turn were used in Mappings III photoionization models to produce model galaxy spectra that could be compared to our observations. Starburst99 is an evolutionary synthesis code that can be used to generate synthetic ionizing far-ultraviolet (FUV) radiation spectra as a function of metallicity, star formation history, and the age and evolution of the stellar populations.…”

Section: Model Grid Parametersmentioning

confidence: 99%

Modeling the ISM Properties of Metal-Poor Galaxies and Gamma-Ray Burst Hosts

et al. 2008

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Abstract. Recent research has suggested that long-duration gamma-ray bursts (LGRBs) occur preferentially in low-metallicity environments, but the exact nature of this correlation is currently a matter of intense debate. We use the newest generation of the Starburst99/Mappings code to generate an extensive suite of cutting-edge stellar population synthesis models, covering a wide range of physical parameters specifically tailored for modeling the ISM environments of metal-poor galaxies and LGRB host galaxies. With our models, we generate optical emission line diagnostics, which will allow us to examine the ISM properties and stellar populations of a variety of galaxy populations in unprecedented detail. While accurately modeling low-metallicity galaxies still poses a challenge to these models, future improvements to these grids will have profound consequences for our understanding of metal-poor galaxies, their ISM environments, and the nature of their role as the hosts of LGRBs.

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Synthetic properties of starburst galaxies

Cited by 2,020 publications

References 0 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

A young star-forming galaxy at z = 3.5 with an extended Lyman α halo seen with MUSE

Modeling the ISM Properties of Metal-Poor Galaxies and Gamma-Ray Burst Hosts

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