The ALMA Redshift 4 Survey (AR4S)

Schreiber, C.; Pannella, M.; Leiton, R.; Elbaz, D.; Wang, T.; Okumura, K.; Labbé, Ivo

doi:10.1051/0004-6361/201629155

Cited by 92 publications

(132 citation statements)

References 57 publications

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“…This result provides further theoretical support to the recent claim by Gavazzi et al (2015a) that bars are one of the main contributor of the flattening observed at high masses in the star formation rate-stellar mass correlation (Whitaker et al 2012;Magnelli et al 2014;Whitaker et al 2014;Gavazzi et al 2015b;Ilbert et al 2015;Lee et al 2015;Schreiber et al 2016).…”

Section: Discussionsupporting

confidence: 88%

Bar-driven evolution and quenching of spiral galaxies in cosmological simulations

Spinoso

Bonoli

Dotti

et al. 2016

Mon. Not. R. Astron. Soc.

109

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We analyse the output of the hi-res cosmological "zoom-in" hydrodynamical simulation ErisBH to study self-consistently the formation of a strong stellar bar in a Milky Way-type galaxy and its effect on the galactic structure as well as on the central gas distribution and star formation. The simulation includes radiative cooling, star formation, SN feedback and a central massive black hole wich is undergoing gas accretion and is heating the surroundings via thermal AGN feedback. A large central region in the ErisBH disk becomes bar-unstable after z ∼ 1.4, but a clear bar-like structure starts to grow significantly only after z ≃ 0.4, possibly triggered by the interaction with a massive satellite. At z ≃ 0.1 the bar stabilizes and reaches its maximum radial extent of l ≈ 2.2 kpc. As the bar grows, it becomes prone to buckling instability, which we quantify based on the anisotropy of the stellar velocity dispersion. The actual buckling event is observable at z ≃ 0.1, resulting in the formation of a boxy-peanut bulge clearly discernible in the edge-on view of the galaxy at z = 0. The bar in ErisBH does not dissolve during the formation of the bulge but it is long-lived and is strongly non-axisymmetric down to the resolution limit of ∼ 100 pc at z = 0. During its early growth, the bar exerts a strong torque on the gas within its extent and drives gas inflows that enhance the nuclear star formation on sub-kpc scales. Later on, as the bar reaches its maximum length and strength, the infalling gas is nearly all consumed into stars and, to a lesser extent, accreted onto the central black hole, leaving behind a gasdepleted region within the central ∼ 2 kpc. Observations would more likely identify a prominent, large-scale bar at the stage when the galactic central region has already been quenched. Bar-driven quenching may play an important role in disk-dominated galaxies at all redshift. AGN feedback is instrumental in this scenario not because it directly leads to quenching, but because it promotes a strong bar by maintaining a flat rotation curve, suppressing the density of baryons within the central kpc in the early stages of the formation of the galaxy.

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Section: Discussionsupporting

confidence: 88%

Bar-driven evolution and quenching of spiral galaxies in cosmological simulations

Spinoso

Bonoli

Dotti

et al. 2016

Mon. Not. R. Astron. Soc.

109

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“…Such temperatures are very similar to the 40±2 K found for a massive sample of z∼4 galaxies by Schreiber et al (2016) and the 40-50 K found by Sklias et al (2014) for typical z∼2-3 sources from the Herschel Lens Survey (Egami et al 2010). We remark that one might naturally expect an evolution in dust temperature given the observed evolution in the SFR surface densities observed in galaxies with cosmic time (e.g., Shibuya et al 2015) and the correlation of dust temperature with SFR surface density (e.g., Elbaz et al 2011).…”

Section: Impact Of the Dust Temperaturesupporting

confidence: 85%

ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS

Bouwens

Aravena

Decarli

et al. 2016

ApJ

335

468

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We make use of deep 1.2 mm-continuum observations (12.7µJy/beam RMS) of a 1 arcmin 2 region in the Hubble Ultra Deep Field (HUDF) to probe dust-enshrouded star formation from 330 Lyman-break galaxies spanning the redshift range z = 2-10 (to ∼2-3 M ⊙ /yr at 1σ over the entire range). Given the depth and area of ASPECS, we would expect to tentatively detect 35 galaxies extrapolating the Meurer z ∼ 0 IRX-β relation to z ≥ 2 (assuming T d ∼ 35 K). However, only 6 tentative detections are found at z 2 in ASPECS, with just three at >3σ. Subdividing z = 2-10 galaxies according to stellar mass, U V luminosity, and U V -continuum slope and stacking the results, we only find a significant detection in the most massive (>10 9.75 M ⊙ ) subsample, with an infrared excess (IRX=L IR /L UV ) consistent with previous z ∼ 2 results. However, the infrared excess we measure from our large selection of sub-L * (<10 9.75 M ⊙ ) galaxies is 0.11 +0.32 −0.42 ±0.34 (bootstrap and formal uncertainties) and 0.14 +0.15 −0.14 ±0.18 at z = 2-3 and z = 4-10, respectively, lying below even an SMC IRX-β relation (95% confidence). These results demonstrate the relevance of stellar mass for predicting the IR luminosity of z 2 galaxies. We find that the evolution of the IRX-stellar mass relationship depends on the evolution of the dust temperature. If the dust temperature increases monotonically with redshift (∝ (1 + z) 0.32 ) such that T d ∼ 44-50 K at z ≥ 4, current results are suggestive of little evolution in this relationship to z ∼ 6. We use these results to revisit recent estimates of the z ≥ 3 star-formation rate density.

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“…11 M e galaxies at z>1 in our sample, show strong AGN or starburst activity, which is also seen in other samples of massive high-z galaxies (Spitler et al 2014;Martis et al 2016;Schreiber et al 2017). Also, as expected, the Herschel galaxies fall on the red side of the starforming population, and the radio galaxy (ES1C_55) plots among the quiescent objects.…”

Section: Discussionsupporting

confidence: 86%

A Subarcsecond Near-infrared View of Massive Galaxies at z > 1 with Gemini Multi-conjugate Adaptive Optics

Lacy

Nyland

Mao

et al. 2018

ApJ

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We present images taken using the Gemini South Adaptive Optics Imager (GSAOI) with the Gemini Multiconjugate Adaptive Optics System (GeMS) in three 2 arcmin 2 fields in the Spitzer Extragalactic Representative Volume Survey. These GeMS/GSAOI observations are among the first ≈0 1 resolution data in the near-infrared spanning extragalactic fields exceeding 1 5 in size. We use these data to estimate galaxy sizes, obtaining results similar to those from studies with the Hubble Space Telescope, though we find a higher fraction of compact starforming galaxies at z>2. To disentangle the star-forming galaxies from active galactic nuclei (AGNs), we use multiwavelength data from surveys in the optical and infrared, including far-infrared data from Herschel, as well as new radio continuum data from the Australia Telescope Compact Array and Very Large Array. We identify ultraluminous infrared galaxies (ULIRGs) at z∼1-3, which consist of a combination of pure starburst galaxies and AGN/starburst composites. The ULIRGs show signs of recent merger activity, such as highly disturbed morphologies and include a rare candidate triple-AGN. We find that AGNs tend to reside in hosts with smaller scale sizes than purely star-forming galaxies of similar infrared luminosity. Our observations demonstrate the potential for MCAO to complement the deeper galaxy surveys to be made with the James Webb Space Telescope.

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The ALMA Redshift 4 Survey (AR4S)

Cited by 92 publications

References 57 publications

Bar-driven evolution and quenching of spiral galaxies in cosmological simulations

Bar-driven evolution and quenching of spiral galaxies in cosmological simulations

ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS

A Subarcsecond Near-infrared View of Massive Galaxies at z > 1 with Gemini Multi-conjugate Adaptive Optics

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