Multiwavelength Study of Massive Galaxies at<i>z</i>∼2. I. Star Formation and Galaxy Growth

Daddi, E.; Dickinson, Mark; Morrison, G.; Chary, R.-R.; Cimatti, A.; Elbaz, D.; Frayer, David; Renzini, A.; Pope, Alexandra; Alexander, D. M.; Bauer, F. E.; Giavalisco, Mauro; Huynh, Minh; Kurk, J.; Mignoli, M.

doi:10.1086/521818

Cited by 1,584 publications

(2,493 citation statements)

References 98 publications

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“…The initial sample used to measure the tightness of the relation was a set of opticallyselected galaxies for which Hα emission line star formation rates or 24µm flux densities were available. Daddi et al (2007b) found similar results when expanding selection to dustier galaxies (i.e. 24µm-selected galaxies).…”

Section: Relationship To Normal Galaxies: the Infrared Main Sequencesupporting

confidence: 57%

“…(R-[24])≥14 mags [Vega]). In a multiwavelength analysis, a large fraction of these DOGs seemed to be "mid-IR excess" sources, or galaxies that have unusually strong rest-frame 8µm emission compared to the integrated infrared (Daddi et al, 2007b;Papovich et al, 2007;Magnelli et al, 2011). The physical origins of DOGs mid-infrared emission could have been AGN-heating or bright PAH emission lines.…”

Section: Mid-infrared Spitzer-selected Populationsmentioning

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: Relationship To Normal Galaxies: the Infrared Main Sequencesupporting

confidence: 57%

Section: Mid-infrared Spitzer-selected Populationsmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…The problem of semi-analytical models under-predicting star formation at high redshift has been commented on several times in the literature (e.g. Daddi et al 2007;Damen et al 2009;Fontanot et al 2009b;Dutton, van den Bosch & Dekel 2010;Weinmann, Neistein & Dekel 2011;Weinmann et al 2012). Similar deficiencies have also been reported in hydrodynamical simulations (e.g.…”

Section: S U M M a Ry A N D C O N C L U S I O N Smentioning

confidence: 57%

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Merson¹,

Baugh²,

González-Pérez³

et al. 2015

Mon. Not. R. Astron. Soc.

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High redshift galaxy clusters allow us to examine galaxy formation in extreme environments.Here we compile data for 15 z > 1 galaxy clusters to test the predictions from a state-of-theart semi-analytical model of galaxy formation. The model gives a good match to the slope and zero-point of the cluster red sequence. The model is able to match the cluster galaxy luminosity function at faint and bright magnitudes, but under-estimates the number of galaxies around the break in the cluster luminosity function. We find that simply assuming a weaker dust attenuation improves the model predictions for the cluster galaxy luminosity function, but worsens the predictions for the red sequence at bright magnitudes. Examination of the properties of the bright cluster galaxies suggests that the default dust attenuation is large due to these galaxies having large reservoirs of cold gas as well as small radii. We find that matching the luminosity function and colours of high redshift cluster galaxies, whilst remaining consistent with local observations, poses a challenge for galaxy formation models.

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“…The stellar and halo masses are taken directly from the model at the time of infall. For the second scenario (only increasing stellar mass due to residual star formation), we assign to each infalling galaxy a star formation rate using the observed relation between the SFR and stellar mass Daddi et al 2007) at the time of infall. By assuming that the star formation rates stay constant after accretion we compute the average increase in stellar mass for satellite galaxies since they have become a satellite.…”

Section: Caveatsmentioning

confidence: 99%

The influence of the environmental history on quenching star formation in a Λ cold dark matter universe

Hirschmann¹,

Lucia²,

Wilman³

et al. 2014

Monthly Notices of the Royal Astronomical Society

111

145

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We present a detailed analysis of the influence of the environment and of the environmental history on quenching star formation in central and satellite galaxies in the local Universe. We take advantage of publicly available galaxy catalogues obtained from applying a galaxy formation model to the Millennium simulation. In addition to halo mass, we consider the local density of galaxies within various fixed scales. Comparing our model predictions to observational data (SDSS), we demonstrate that the models are failing to reproduce the observed density dependence of the quiescent galaxy fraction in several aspects: for most of the stellar mass ranges and densities explored, models cannot reproduce the observed similar behaviour of centrals and satellites, they slightly under-estimate the quiescent fraction of centrals and significantly overestimate that of satellites. We show that in the models, the density dependence of the quiescent central galaxies is caused by a fraction of "backsplash" centrals which have been satellites in the past. The observed stronger density dependence on scales of 0.2 − 1 Mpc may, however, indicate additional environmental processes working on central galaxies. Turning to satellite galaxies, the density dependence of their quiescent fractions reflects a dependence on the time spent orbiting within a parent halo, correlating strongly with halo mass and distance from the halo centre. Comparisons with observational estimates suggest relatively long gas consumption time scales of roughly 5 Gyr in low mass satellite galaxies. The quenching time scales decrease with increasing satellite stellar mass. Overall, a change in modelling both internal processes and environmental processes is required for improving currently used galaxy formation models.

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Multiwavelength Study of Massive Galaxies atz∼2. I. Star Formation and Galaxy Growth

Cited by 1,584 publications

References 98 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

The influence of the environmental history on quenching star formation in a Λ cold dark matter universe

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