THE EVOLVING INTERSTELLAR MEDIUM OF STAR-FORMING GALAXIES SINCE<i>z</i>= 2 AS PROBED BY THEIR INFRARED SPECTRAL ENERGY DISTRIBUTIONS

Magdis, G.; Daddi, E.; Béthermin, M.; Sargent, M.; Elbaz, D.; Pannella, M.; Dickinson, Mark; Dannerbauer, H.; Cunha, Elisabete da; Walter, Fabian; Rigopoulou, D.; Charmandaris, V.; Hwang, Ho Seong; Kartaltepe, Jeyhan S.

doi:10.1088/0004-637x/760/1/6

Cited by 521 publications

(1,138 citation statements)

References 127 publications

(261 reference statements)

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“…At redshift z ∼ 1, luminous IR galaxies contribute about 50% to the SFRD (Murphy et al 2011), while the SFRD increases at higher redshift, z ∼ 2 because we have an important contribution from more active star-forming galaxies, or ultraluminous IR galaxies (L IR ≥ 10 12 L , Chapman et al 2005;Daddi et al 2007;Papovich et al 2007;Magdis et al 2012;Magnelli et al 2009), which are considered to be the ancestors of massive quiescent galaxies in the present epoch (e.g. Le Floc'h et al 2005).…”

Section: Introductionmentioning

confidence: 92%

TheHerschelVirgo Cluster Survey

Pappalardo

Bendo

Bianchi

et al. 2015

A&A

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Aims. We present three independent catalogs of point-sources extracted from SPIRE images at 250, 350, and 500 µm, acquired with the Herschel Space Observatory as a part of the Herschel Virgo Cluster Survey (HeViCS). The catalogs have been cross-correlated to consistently extract the photometry at SPIRE wavelengths for each object. Methods. Sources have been detected using an iterative loop. The source positions are determined by estimating the likelihood to be a real source for each peak on the maps, according to the criterion defined in the sourceExtractorSussextractor task. The flux densities are estimated using the sourceExtractorTimeline, a timeline-based point source fitter that also determines the fitting procedure with the width of the Gaussian that best reproduces the source considered. Afterwards, each source is subtracted from the maps, removing a Gaussian function in every position with the full width half maximum equal to that estimated in sourceExtractorTimeline. This procedure improves the robustness of our algorithm in terms of source identification. We calculate the completeness and the flux accuracy by injecting artificial sources in the timeline and estimate the reliability of the catalog using a permutation method. Results. The HeViCS catalogs contain about 52 000, 42 200, and 18 700 sources selected at 250, 350, and 500 µm above 3σ and are ∼75%, 62%, and 50% complete at flux densities of 20 mJy at 250, 350, 500 µm, respectively. We then measured source number counts at 250, 350, and 500 µm and compare them with previous data and semi-analytical models. We also cross-correlated the catalogs with the Sloan Digital Sky Survey to investigate the redshift distribution of the nearby sources. From this crosscorrelation, we select ∼2000 sources with reliable fluxes and a high signal-to-noise ratio, finding an average redshift z ∼ 0.3 ± 0.22 and 0.25 (16-84 percentile). Conclusions. The number counts at 250, 350, and 500 µm show an increase in the slope below 200 mJy, indicating a strong evolution in number of density for galaxies at these fluxes. In general, models tend to overpredict the counts at brighter flux densities, underlying the importance of studying the Rayleigh-Jeans part of the spectral energy distribution to refine the theoretical recipes of the models. Our iterative method for source identification allowed the detection of a family of 500 µm sources that are not foreground objects belonging to Virgo and not found in other catalogs.

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Section: Introductionmentioning

confidence: 92%

TheHerschelVirgo Cluster Survey

Pappalardo

Bendo

Bianchi

et al. 2015

A&A

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“…Saintonge et al, 2011). These results have come from both from CO inferred H 2 gas masses, as well as dust measurements (and associated dust-to-gas ratio assumptions Magdis et al, 2012a). While no study has performed a proper mass-selected study, indications from these observations are that the average gas fraction of galaxies rises toward high-redshift.…”

Section: Molecular Gas Fractionsmentioning

confidence: 99%

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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“…Le Floc'h et al (2009) built a catalog of 24 μm sources matched with the data from which the BzK sample was built. The total infrared luminosity (L IR , integrated between 8 μm and 1000 μm) is extrapolated from the 24 μm flux density using the Magdis et al (2012) templates; L IR is then converted into SFR assuming the Kennicutt (1998) conversion factor.…”

Section: Spitzer/mips Datamentioning

confidence: 99%

“…The data comes from the PACS evolutionary probe survey (PEP, Lutz et al 2011). We fitted the 100 μm and 160 μm PACS flux densities with Magdis et al (2012) templates in order to derive L IR of each galaxy and assume the same conversion factor between L IR and SFR as for MIPS. The PACS wavelengths have the advantage of being close The purple contours indicate sources with only UV-detection (i.e., having no mid/far-IR), the orange dots the MIPS-but-not-PACS-detected sources, and the red stars the PACS-detected sources.…”

Section: Herschel/pacs Datamentioning

confidence: 99%

Clustering, host halos, and environment ofz ~ 2 galaxies as a function of their physical properties

Béthermin

Kilbinger

Daddi

et al. 2014

A&A

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Using a sample of 25 683 star-forming and 2821 passive galaxies at z ∼ 2, selected in the COSMOS field following the BzK color criterion, we study the hosting halo mass and environment of galaxies as a function of their physical properties. Spitzer and Herschel allow us to obtain accurate star formation rate estimates for starburst galaxies. We measure the autocorrelation and cross-correlation functions of various galaxy subsamples and infer the properties of their hosting halos using both a halo occupation model and the linear bias at large scale. We find that passive and star-forming galaxies obey a similarly rising relation between the halo and stellar mass. The mean host halo mass of star-forming galaxies increases with the star formation rate between 30 M yr −1 and 200 M yr −1 , but flattens for higher values, except if we select only main-sequence galaxies. This reflects the expected transition from a regime of secular coevolution of the halos and the galaxies to a regime of episodic starburst. We find similar large-scale biases for mainsequence, passive, and starburst galaxies at equal stellar mass, suggesting that these populations live in halos of the same mass. However, we detect an excess of clustering on small scales for passive galaxies and showed, by measuring the large-scale bias of close pairs of passive galaxies, that this excess is caused by a small fraction (∼16%) of passive galaxies being hosted by massive halos (∼3 × 10 13 M ) as satellites. Finally, extrapolating the growth of halos hosting the z ∼ 2 population, we show that M ∼ 10 10 M galaxies at z ∼ 2 will evolve, on average, into massive (M ∼ 10 11 M ), field galaxies in the local Universe and M ∼ 10 11 M galaxies at z = 2 into local, massive, group galaxies. We also identify two z ∼ 2 populations which should end up in today's clusters: massive (>M ∼ 10 11 M ), strongly star-forming (>200 M yr −1 ), main-sequence galaxies, and close pairs of massive, passive galaxies.

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THE EVOLVING INTERSTELLAR MEDIUM OF STAR-FORMING GALAXIES SINCEz= 2 AS PROBED BY THEIR INFRARED SPECTRAL ENERGY DISTRIBUTIONS

Cited by 521 publications

References 127 publications

TheHerschelVirgo Cluster Survey

TheHerschelVirgo Cluster Survey

Dusty star-forming galaxies at high redshift

Clustering, host halos, and environment ofz ~ 2 galaxies as a function of their physical properties

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