High-redshift star formation in the ALMA era

Hodge, Jacqueline A.; da Cunha, Elisabete

doi:10.48550/arxiv.2004.00934

Cited by 27 publications

(38 citation statements)

References 391 publications

(722 reference statements)

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“…Furthermore, recent studies have found a spectroscopically-confirmed population of massive, quiescent galaxies already at 3 𝑧 4 (Glazebrook et al 2017;Tanaka et al 2019;Valentino et al 2020). The properties of the quiescent populations both at low and intermediate redshifts suggest that their progenitors should belong to the star-forming population at 𝑧 3 (McDermid et al 2015;Belli et al 2017;Hodge & da Cunha 2020). The matching number densities, stellar masses and sizes of the massive star-forming at 𝑧 4 and quiescent populations at lower redshifts seem to support this picture (Toft et al 2012;Valentino et al 2020).…”

Section: Introductionmentioning

confidence: 77%

Dynamical properties of z $\sim 4.5$ dusty star-forming galaxies and their connection with local early type galaxies

Rizzo,

Vegetti,

Fraternali

et al. 2021

Preprint

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There is a large consensus that gas in high-𝑧 galaxies is highly turbulent, because of a combination of stellar feedback processes and gravitational instabilities driven by mergers and gas accretion. In this paper, we present the analysis of a sample of five Dusty Star Forming Galaxies (DSFGs) at 4 𝑧 5. Taking advantage of the magnifying power of strong gravitational lensing, we quantified their kinematic and dynamical properties from ALMA observations of their [CII] emission line. We combined the dynamical measurements obtained for these galaxies with those obtained from previous studies to build the largest sample of 𝑧 ∼ 4.5 galaxies with high-quality data and sub-kpc spatial resolutions, so far. We found that all galaxies in the sample are dynamically cold, with rotation-to-random motion ratios, 𝑉/𝜎, between 7 to 15. The relation between their velocity dispersions and their star-formation rates indicates that stellar feedback is sufficient to sustain the turbulence within these galaxies and no further mechanisms are needed. In addition, we performed a rotation curve decomposition to infer the relative contribution of the baryonic (gas, stars) and dark matter components to the total gravitational potentials. This analysis allowed us to compare the structural properties of the studied DSFGs with those of their descendants, the local early type galaxies. In particular, we found that five out of six galaxies of the sample show the dynamical signature of a bulge, indicating that the spheroidal component is already in place at 𝑧 ∼ 4.5.

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Section: Introductionmentioning

confidence: 77%

Dynamical properties of z $\sim 4.5$ dusty star-forming galaxies and their connection with local early type galaxies

Rizzo,

Vegetti,

Fraternali

et al. 2021

Preprint

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“…In this framework, a primary source of confusion stems from the relatively limited amount of information available for sizable samples of high-redshift galaxies, homogeneously selected on and above the main sequence. While a fine sampling of the far-IR spectral energy distribution (SED) has now become more accessible and a fundamental source to derive properties as the dust mass, temperature, and luminosity (e.g., Simpson et al 2014;Scoville et al 2016;Dunlop et al 2017;Brisbin et al 2017;Strandet et al 2017;Franco et al 2018;Zavala et al 2018;Liu et al 2019a;Dudzevičiūtė et al 2019;Simpson et al 2020;Hodge & da Cunha 2020, to mention a few recent high-resolution surveys in the (sub)mm), direct spectroscopic measurements of the cold gas in distant galaxies remain remarkably time consuming. As a result, systematic investigations of the gas properties focused on either one line transition in large samples of galaxies (e.g., Le Fèvre et al 2019;Freundlich et al 2019;Tacconi et al 2018Tacconi et al , 2020, or several lines in sparser samples, often biased towards the brightest objects as (lensed) SMGs or quasars (e.g., Carilli & Walter 2013;Bothwell et al 2013;Spilker et al 2014;Yang et al 2017;Cañameras et al 2018;Dannerbauer et al 2019).…”

Section: Introductionmentioning

confidence: 99%

CO emission in distant galaxies on and above the main sequence

Valentino,

Daddi,

Puglisi

et al. 2020

Preprint

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We present the detection of multiple carbon monoxide CO line transitions with ALMA in a few tens of infrared-selected galaxies on and above the main sequence at z = 1.1 − 1.7. We reliably detected the emission of CO (5 − 4), CO (2 − 1), and CO (7 − 6)+[C I]( 3 P 2 − 3 P 1 ) in 50, 33, and 13 galaxies, respectively, and we complemented this information with available CO (4 − 3) and [C I]( 3 P 1 − 3 P 0 ) fluxes for part of the sample, and modeling of the optical-to-mm spectral energy distribution. We retrieve a quasi-linear relation between L IR and CO (5 − 4) or CO (7 − 6) for main-sequence galaxies and starbursts, corroborating the hypothesis that these transitions can be used as star formation rate (SFR) tracers. We find the CO excitation to steadily increase as a function of the star formation efficiency (SFE), the mean intensity of the radiation field warming the dust ( U ), the surface density of SFR (Σ SFR ), and, less distinctly, with the distance from the main sequence (∆MS). This adds to the tentative evidence for higher excitation of the CO+[C I] spectral line energy distribution (SLED) of starburst galaxies relative to that for main-sequence objects, where the dust opacities play a minor role in shaping the high-J CO transitions in our sample. However, the distinction between the average SLED of upper main-sequence and starburst galaxies is blurred, driven by a wide variety of intrinsic shapes. Large velocity gradient radiative transfer modeling demonstrates the existence of a highly excited component that elevates the CO SLED of high-redshift main-sequence and starbursting galaxies above the typical values observed in the disk of the Milky Way. This excited component is dense and it encloses ∼ 50% of the total molecular gas mass in main-sequence objects. We interpret the observed trends involving the CO excitation as mainly driven by a combination of large SFRs and compact sizes, as large Σ SFR are naturally connected with enhanced dense molecular gas fractions and higher dust and gas temperatures, due to increasing UV radiation fields, cosmic ray rates, and dust/gas coupling. We release the full data compilation and the ancillary information to the community.

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“…In the last two decades, surveys in the far-infrared and submillimeter wavebands have opened up a new window for our understanding of the formation and evolution of galaxies, revealing a population of massive, dust-enshrouded galaxies forming stars at enormous rates in the early Universe (see, e.g., Blain et al 2002;Carilli & Walter 2013;Casey et al 2014;Hodge & da Cunha 2020). In particular, the extragalactic imaging surveys done with the Herschel Space Observatory (Pilbratt et al 2010), such as Herschel-ATLAS (Eales et al 2010a), HerMES (Oliver et al 2012), and PEP (Lutz et al 2011), have increased the number of dust-obscured starforming galaxies from hundreds to several hundred thousand.…”

Section: Introductionmentioning

confidence: 99%

Close-up view of a luminous star-forming galaxy at z=2.95

Berta,

Young,

Cox

et al. 2020

Preprint

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Exploiting the sensitivity of the IRAM NOrthern Extended Millimeter Array (NOEMA) and its ability to process large instantaneous bandwidths, we have studied the morphology and other properties of the molecular gas and dust in the starburst galaxy, H-ATLAS J131611.5+281219 (HerBS-89a), at z=2.95. High angular resolution (0 ′′ . 3) images reveal a partial 1 ′′ . 0 diameter Einstein ring in the dust continuum emission and the molecular emission lines of 12 CO (9-8) and H 2 O (2 02 − 1 11 ). Together with lower angular resolution (0 ′′ . 6) images, we report the detection of a series of molecular lines including the three fundamental transitions of the molecular ion OH + , namely (1 1 − 0 1 ), (1 2 − 0 1 ) and (1 0 − 0 1 ), seen in absorption; the molecular ion CH + (1 − 0) seen in absorption (and tentatively in emission); two transitions of amidogen (NH 2 ), namely (2 02 − 1 11 ) and (2 20 − 2 11 ) seen in emission; and HCN(11 − 10) and/or NH(1 2 − 0 1 ) seen in absorption. The NOEMA data are complemented with Very Large Array data tracing the 12 CO(1 − 0) emission line, which provides a measurement of the total mass of molecular gas and an anchor for a CO excitation analysis. In addition, we present Hubble Space Telescope imaging that reveals the foreground lensing galaxy in the near-infrared (1.15µm). Together with photometric data from the Gran Telescopio Canarias, we derive a photometric redshift of z phot = 0.9 +0.3 −0.5 for the foreground lensing galaxy. Modelling the lensing of HerBS-89a, we reconstruct the dust continuum (magnified by a factor µ ≃ 5.0) and molecular emission lines (magnified by µ ∼ 4 − 5) in the source plane, which probe scales of ∼ 0 ′′ . 1 (or 800 pc). The 12 CO(9 − 8) and H 2 O (2 02 − 1 11 ) emission lines have comparable spatial and kinematic distributions; the source-plane reconstructions do not clearly distinguish between a one-component and a two-component scenario, but the latter, which reveals two compact rotating components with sizes of ≈ 1 kpc, that are likely merging, more naturally accounts for the broad line widths observed in HerBS-89a. In the core of HerBS-89a, very dense gas with n H 2 ∼ 10 7−9 cm −3 is revealed by the NH 2 emission lines and the possible HCN(11 − 10) absorption line. HerBS-89a is a powerful star forming galaxy with a molecular gas mass of M mol = (2.1 ± 0.4) × 10 11 M ⊙ , an infrared luminosity of L IR = (4.6 ± 0.4) × 10 12 L ⊙ , and a dust mass of M dust = (2.6 ± 0.2) × 10 9 M ⊙ , yielding a dust-to-gas ratio δ GDR ≈ 80. We derive a star formation rate SFR = 614 ± 59 M ⊙ yr −1 and a depletion timescale τ depl = (3.4 ± 1.0) × 10 8 years. The OH + and CH + absorption lines, which trace low (∼ 100 cm −3 ) density molecular gas, all have their main velocity component red-shifted by ∆V ∼ 100 km s −1 relative to the global CO reservoir. We argue that these absorption lines trace a rare example of gas inflow towards the center of a starburst galaxy, indicating that HerBS-89a is accreting gas from its surroundings.

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High-redshift star formation in the ALMA era

Cited by 27 publications

References 391 publications

Dynamical properties of z $\sim 4.5$ dusty star-forming galaxies and their connection with local early type galaxies

Dynamical properties of z $\sim 4.5$ dusty star-forming galaxies and their connection with local early type galaxies

CO emission in distant galaxies on and above the main sequence

Close-up view of a luminous star-forming galaxy at z=2.95

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