AN INTENSELY STAR-FORMING GALAXY AT<i>z</i>∼ 7 WITH LOW DUST AND METAL CONTENT REVEALED BY DEEP ALMA AND<i>HST</i>OBSERVATIONS

Ouchi, Masami; Ellis, Richard S.; Ono, Yoshiyasu; Nakanishi, Koichiro; Kohno, Kotaro; Momose, Rieko; Kurono, Yasutaka; Ashby, M. L. N.; Shimasaku, Kazuhiro; Willner, S. P.; Fazio, G. G.; Tamura, Motohide; Iono, Daisuke

doi:10.1088/0004-637x/778/2/102

Cited by 218 publications

(355 citation statements)

References 93 publications

(129 reference statements)

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“…For example, Kanekar et al (2013) searched for [CII] emission from a lensed Lyman-α emitter at z ∼ 6.5, and showed a non detection. Similarly, Ouchi et al (2013) utilized ALMA to search for [CII] from Himiko, a luminous galaxy at z ∼ 6.5 that forms stars at ∼ 100 M yr −1 . These authors showed a non detection to limits L CII < 5.4 × 10 7 L .…”

Section: [Cii] Morphologies and Dynamicsmentioning

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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Section: [Cii] Morphologies and Dynamicsmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…All model variants predict dust masses approximately 0.5 dex larger than those predicted by our fiducial model for galaxies in this stellar mass range. This is driven by higher efficiencies for the condensation of dust in stellar ejecta in the 'no-acc' and 'high-cond' (2015) at z = 3, 4, and 5, and a compilation of data in Mancini et al (2015) at z = 6 and 7, taken from Kanekar et al (2013), Ouchi et al (2013), Ota et al (2014), Maiolino et al (2015), Schaerer et al (2015), and Watson et al (2015).…”

Section: Dust Masses In Galaxiesmentioning

confidence: 99%

The dust content of galaxies from z = 0 to z = 9

Popping

Somerville

Galametz

2017

Monthly Notices of the Royal Astronomical Society

237

326

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We study the dust content of galaxies from z = 0 to z = 9 in semi-analytic models of galaxy formation that include new recipes to track the production and destruction of dust. We include condensation of dust in stellar ejecta, the growth of dust in the interstellar medium (ISM), the destruction of dust by supernovae and in the hot halo, and dusty winds and inflows. The rate of dust growth in the ISM depends on the metallicity and density of molecular clouds. Our fiducial model reproduces the relation between dust mass and stellar mass from z = 0 to z = 7, the number density of galaxies with dust masses less than 10 8.3 M , and the cosmic density of dust at z = 0. The model accounts for the double power-law trend between dust-togas (DTG) ratio and gas-phase metallicity of local galaxies and the relation between DTG ratio and stellar mass. The dominant mode of dust formation is dust growth in the ISM, except for galaxies with M * < 10 7 M , where condensation of dust in supernova ejecta dominates. The dust-to-metal ratio of galaxies depends on the gasphase metallicity, unlike what is typically assumed in cosmological simulations. Model variants including higher condensation efficiencies, a fixed timescale for dust growth in the ISM, or no growth at all reproduce some of the observed constraints, but fail to simultaneously reproduce the shape of dust scaling relations and the dust mass of high-redshift galaxies.

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“…The simultaneous presence of both dust-rich and dust-(and metal-) poor objects (e.g. Ouchi et al 2013) at high redshift indicates that the transition between these two populations has to be very rapid and may take place on a Myr time-scale (Mattsson 2015). Fig.…”

Section: Elliptical Galaxies: Dust Evolution In the High Redshift Unimentioning

confidence: 99%

The cosmic dust rate across the Universe

Gioannini¹,

Matteuccí

Calura

2017

Monthly Notices of the Royal Astronomical Society

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We investigate the evolution of interstellar dust in the Universe by means of chemical evolution models of galaxies of different morphological types, reproducing the main observed features of present day galaxies. We adopt the most updated prescriptions for dust production from supernovae and asymptotic giant branch (AGB) stars as well as for dust accretion and destruction processes. Then, we study the cosmic dust rate in the framework of three different cosmological scenarios for galaxy formation: i) a pure luminosity scenario (PLE), ii) a number density evolution scenario (DE), as suggested by the classical hierarchical clustering scenario and iii) an alternative scenario, in which both spirals and ellipticals are allowed to evolve in number on an observationally motivated basis. Our results give predictions about the evolution of the dust content in different galaxies as well as the cosmic dust rate as a function of redshift. Concerning the cosmic dust rate, the best scenario is the alternative one, which predicts a peak at 2 < z < 3 and reproduces the cosmic star formation rate. We compute the evolution of the comoving dust density parameter Ω dust and find agreement with data for z < 0.5 in the framework of DE and alternative scenarios. Finally, the evolution of the average cosmic metallicity is presented and it shows a quite fast increase in each scenario, reaching the solar value at the present time, although most of the heavy elements are incorporated into solid grains, and therefore not observable in the gas phase.

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AN INTENSELY STAR-FORMING GALAXY ATz∼ 7 WITH LOW DUST AND METAL CONTENT REVEALED BY DEEP ALMA ANDHSTOBSERVATIONS

Cited by 218 publications

References 93 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

The dust content of galaxies from z = 0 to z = 9

The cosmic dust rate across the Universe

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