Author
Daniel Ceverino
Bio: Daniel Ceverino is an academic researcher from University of Copenhagen. The author has contributed to research in topics: Galaxy & Star formation. The author has an hindex of 4, co-authored 4 publications receiving 126 citations.
Topics: Galaxy, Star formation, Velocity dispersion, Stellar mass, Billion years
Papers
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University of Copenhagen1, Graduate University for Advanced Studies2, Paris Diderot University3, National Institutes of Natural Sciences, Japan4, California Institute of Technology5, INAF6, York University7, Aix-Marseille University8, University of Potsdam9, Leibniz Institute for Astrophysics Potsdam10, Institute for the Physics and Mathematics of the Universe11, École normale supérieure de Lyon12, University of Toulouse13
TL;DR: In this paper, the authors reported two secure (z = 3.775; 4.012) and one tentative (z ≈ 3.767) spectroscopic confirmations of massive and quiescent galaxies through K-band observations with Keck/MOSFIRE and Very Large Telescope/X-Shooter.
Abstract: We report two secure (z = 3.775; 4.012) and one tentative (z ≈ 3.767) spectroscopic confirmations of massive and quiescent galaxies through K-band observations with Keck/MOSFIRE and Very Large Telescope/X-Shooter. The stellar continuum emission, absence of strong nebular emission lines, and lack of significant far-infrared detections confirm the passive nature of these objects, disfavoring the alternative solution of low-redshift dusty star-forming interlopers. We derive stellar masses of log(M⋆/M⊙) ~ 11 and ongoing star formation rates placing these galaxies ≳ 1–2 dex below the main sequence at their redshifts. The adopted parameterization of the star formation history suggests that these sources experienced a strong (〈SFR〉 ~1200 - 3500 M⊙ yr⁻¹) and short (~50 Myr) burst of star formation, peaking ~150–500 Myr before the time of observation, all properties reminiscent of the characteristics of submillimeter galaxies (SMGs) at z > 4. We investigate this connection by comparing the comoving number densities and the properties of these two populations. We find a fair agreement only with the deepest submillimeter surveys detecting not only the most extreme starbursts but also more normal galaxies. We support these findings by further exploring the Illustris TNG cosmological simulation, retrieving populations of both fully quenched massive galaxies at z ~ 3–4 and SMGs at z ~ 4−5, with number densities and properties in agreement with the observations at z ~ 3 but in increasing tension at higher redshift. Nevertheless, as suggested by the observations, not all of the progenitors of quiescent galaxies at these redshifts shine as bright SMGs in their past, and, similarly, not all bright SMGs quench by z ~ 3, both fractions depending on the threshold assumed to define the SMGs themselves.
84 citations
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University of Copenhagen1, Graduate University for Advanced Studies2, Paris Diderot University3, National Institutes of Natural Sciences, Japan4, California Institute of Technology5, INAF6, York University7, Aix-Marseille University8, Subaru9, University of Potsdam10, Leibniz Institute for Astrophysics Potsdam11, Institute for the Physics and Mathematics of the Universe12, École normale supérieure de Lyon13, University of Toulouse14
TL;DR: In this article, the authors report two secure and one tentative confirmations of massive and quiescent galaxies through K-band observations with Keck/MOSFIRE and VLT/X-Shooter.
Abstract: We report two secure ($z=3.775, 4.012$) and one tentative ($z\approx3.767$) spectroscopic confirmations of massive and quiescent galaxies through $K$-band observations with Keck/MOSFIRE and VLT/X-Shooter. The stellar continuum emission, the absence of strong nebular emission lines and the lack of significant far-infrared detections confirm the passive nature of these objects, disfavoring the alternative solution of low-redshift dusty star-forming interlopers. We derive stellar masses of $\mathrm{log}(M_{\star}/M_\odot)\sim11$ and ongoing star formation rates placing these galaxies $\gtrsim 1-2$ dex below the main sequence at their redshifts. The adopted parametrization of the star formation history suggests that these sources experienced a strong ($\langle \rm SFR \rangle \sim 1200-3500\,M_\odot\,\mathrm{yr}^{-1}$) and short ($\sim 50$ Myr) burst of star formation, peaking $\sim 150-500$ Myr before the time of observation, all properties reminiscent of the characteristics of sub-millimeter galaxies (SMGs) at $z>4$. We investigate this connection by comparing the comoving number densities and the properties of these two populations. We find a fair agreement only with the deepest sub-mm surveys detecting not only the most extreme starbursts, but also more normal galaxies. We support these findings by further exploring the Illustris-TNG cosmological simulation, retrieving populations of both fully quenched massive galaxies at $z\sim3-4$ and SMGs at $z\sim4-5$, with number densities and properties in agreement with the observations at $z\sim3$, but in increasing tension at higher redshift. Nevertheless, as suggested by the observations, not all the progenitors of quiescent galaxies at these redshifts shine as bright SMGs in their past and, similarly, not all bright SMGs quench by $z\sim3$, both fractions depending on the threshold assumed to define the SMGs themselves.
79 citations
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University of Copenhagen1, INAF2, University of Nottingham3, PSL Research University4, École normale supérieure de Lyon5, California Institute of Technology6, University of Concepción7, Institut d'Astrophysique de Paris8, University of Western Australia9, University of Toronto10, Peking University11, University of Connecticut12, University of Massachusetts Amherst13
TL;DR: In this article, the authors present a detailed analysis of a large sample of spectroscopically confirmed massive quiescent galaxies (MQGs; log(M*/M ⊙) ~ 11.5) at z ≳ 2.
Abstract: We present a detailed analysis of a large sample of spectroscopically confirmed massive quiescent galaxies (MQGs; log(M*/M ⊙) ~ 11.5) at z ≳ 2. This sample comprises 15 galaxies selected in the COSMOS and UDS fields by their bright K-band magnitudes and followed up with Very Large Telescope (VLT) X-shooter spectroscopy and Hubble Space Telescope (HST)/WFC3 H_(F160W) imaging. These observations allow us to unambiguously confirm their redshifts, ascertain their quiescent nature and stellar ages, and reliably assess their internal kinematics and effective radii. We find that these galaxies are compact, consistent with the high-mass end of the stellar mass–size relation for quiescent galaxies at z = 2. Moreover, the distribution of the measured stellar velocity dispersions of the sample is consistent with the most massive local early-type galaxies from the MASSIVE Survey, showing that evolution in these galaxies is dominated by changes in size. The HST images reveal, as surprisingly high, that 40% of the sample has tidal features suggestive of mergers and companions in close proximity, including three galaxies experiencing ongoing major mergers. The absence of velocity dispersion evolution from z = 2 to 0, coupled with a doubling of the stellar mass, with a factor of 4 size increase and the observed disturbed stellar morphologies, supports dry minor mergers as the primary drivers of the evolution of the MQGs over the last 10 billion yr.
24 citations
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TL;DR: In this paper, the isolated-galaxy simulations were performed using the HPC resources of CINES and TGCC under the allocations A0030402192>>\s and A0050402192 made by GENCI.
Abstract: This work
was partly supported by the grants France-Israel PICS, GermanyIsrael GIF I-1341-303.7/2016, Germany-Israel DIP STE1869/2-
1 GE625/17-1, I-CORE Program of the PBC/ISF 1829/12, ISF
857/14, US-Israel BSF 2014-273, and NSF AST-1405962. The isolated-galaxy simulations were performed using the HPC
resources of CINES and TGCC under the allocations A0030402192
and A0050402192 made by GENCI.
22 citations
Cited by
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01 Jan 1985
TL;DR: In this article, a reexamination is conducted of the formation of dwarf, diffuse, metal-poor galaxies due to supernova-driven winds, in view of data on the systematic properties of dwarfs in the Local Group and Virgo Cluster.
Abstract: A reexamination is conducted of the formation of dwarf, diffuse, metal-poor galaxies due to supernova-driven winds, in view of data on the systematic properties of dwarfs in the Local Group and Virgo Cluster. The critical condition for global gas loss as a result of the first burst of star formation is that the virial velocity lie below an approximately 100 km/sec critical value. This leads, as observed, to two distinct classes of galaxies, encompassing the diffuse dwarfs, which primarily originate from typical density perturbations, and the normal, brighter galaxies, including compact dwarfs, which can originate only from the highest density peaks. This furnishes a statistical biasing mechanism for the preferential formation of bright galaxies in denser regions, enhancing high surface brightness galaxies' clustering relative to the diffusive dwarfs.
1,253 citations
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TL;DR: The main advances ALMA has helped bring about in understanding of the dust and gas properties of high-redshift (z≳1) star-forming galaxies during these first 9 years of its science operations are reviewed, and the interesting questions that may be answered by ALMA in the years to come are highlighted.
Abstract: The Atacama Large Millimetre/submillimetre Array (ALMA) is currently in the process of transforming our view of star-forming galaxies in the distant (z≳1) universe. Before ALMA, most of what we kne...
116 citations
01 Oct 1999
TL;DR: In this article, the authors describe version 90 (C90) of the code, paying particular attention to changes in the atomic database and numerical methods that have affected predictions since the last publicly available version, C84.
Abstract: ABSTRACT CLOUDY is a large‐scale spectral synthesis code designed to simulate fully physical conditions within an astronomical plasma and then predict the emitted spectrum. Here we describe version 90 (C90) of the code, paying particular attention to changes in the atomic database and numerical methods that have affected predictions since the last publicly available version, C84. The computational methods and uncertainties are outlined together with the direction future development will take. The code is freely available and is widely used in the analysis and interpretation of emission‐line spectra. Web access to the Fortran source for CLOUDY, its documentation Hazy, and an independent electronic form of the atomic database is also described.
111 citations
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California Institute of Technology1, University of Toulouse2, University of Geneva3, University of California, Davis4, University of Padua5, INAF6, Aix-Marseille University7, University of Copenhagen8, Institute for the Physics and Mathematics of the Universe9, University of Tokyo10, Space Telescope Science Institute11, University of La Serena12, University of Antofagasta13, University of Bologna14, Valparaiso University15, University of Cambridge16, Max Planck Society17, Cornell University18, Leiden University19
TL;DR: The ALMA Large Program to Investigate C⁺ at Early Times (ALPINE) survey is the first large multi-wavelength survey that aims at characterizing the gas and dust properties of 118 main-sequence galaxies at redshifts 4.4 3.5σ.
Abstract: We present the ancillary data and basic physical measurements for the galaxies in the ALMA Large Program to Investigate C⁺ at Early Times (ALPINE) survey—the first large multiwavelength survey that aims at characterizing the gas and dust properties of 118 main-sequence galaxies at redshifts 4.4 3.5σ) and the surrounding far-infrared continuum in conjunction with a wealth of optical and near-infrared data. We outline in detail the spectroscopic data and selection of the galaxies as well as the ground- and space-based imaging products. In addition, we provide several basic measurements including stellar masses, star formation rates (SFR), rest-frame ultra-violet (UV) luminosities, UV continuum slopes (β), and absorption line redshifts, as well as Hα emission derived from Spitzer colors. We find that the ALPINE sample is representative of the 4 < z < 6 galaxy population selected by photometric methods and only slightly biased toward bluer colors (Δβ ~ 0.2). Using [C II] as tracer of the systemic redshift (confirmed for one galaxy at z = 4.5 out of 118 for which we obtained optical [O III]λ3727A emission), we confirm redshifted Lyα emission and blueshifted absorption lines similar to findings at lower redshifts. By stacking the rest-frame UV spectra in the [C II] rest frame, we find that the absorption lines in galaxies with high specific SFR are more blueshifted, which could be indicative of stronger winds and outflows.
100 citations
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TL;DR: In this paper, the authors study the efficiency of galactic feedback in the early Universe by stacking the [C II] 158 um emission in a large sample of normal star-forming galaxies at 4 4.
Abstract: We study the efficiency of galactic feedback in the early Universe by stacking the [C II] 158 um emission in a large sample of normal star-forming galaxies at 4 4. From the stacking analysis of the datacubes, we find that the combined [C II] core emission (|v|< 200 km/s) of the higher-SFR galaxies is extended on physical sizes of ~ 30 kpc (diameter scale), well beyond the analogous [C II] core emission of lower-SFR galaxies and the stacked far-infrared continuum. The detection of such extended metal-enriched gas, likely tracing circumgalactic gas enriched by past outflows, corroborates previous similar studies, confirming that baryon cycle and gas exchanges with the circumgalactic medium are at work in normal star-forming galaxies already at early epochs.
100 citations