The ALPINE-ALMA [C II] Survey: [C II] 158 μm Emission Line Luminosity Functions at z ∼ 4–6

Yan, Lin; Sajina, Anna; Loiacono, F.; Lagache, G.; Béthermin, M.; Faisst, Andreas L.; Ginolfi, M.; Fèvre, O. Le; Gruppioni, C.; Capak, P.; Cassata, P.; Schaerer, D.; Silverman, John D.; Bardelli, S.; Dessauges‐Zavadsky, M.; Cimatti, A.; Hathi, N. P.; Lemaux, Brian C.; Ibar, E.; Jones, G. C.; Koekemoer, Anton M.; Oesch, Pascal; Talia, M.; Pozzi, F.; Riechers, D.; Tasca, L.; Toft, Sune; Vallini, L.; Vergani, D.; Zamorani, G.; Zucca, E.

doi:10.3847/1538-4357/abc41c

Cited by 32 publications

(45 citation statements)

References 54 publications

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“…In Figure 9, we present the number density of [C II] line emitters at z = 6, including recent [C II] line studies at z > 4 (Swinbank et al 2012;Matsuda et al 2015;Yamaguchi et al 2017;Cooke et al 2018;Hayatsu et al 2019;Decarli et al 2020;Yan et al 2020 Looze et al (2014). We find that our lower limit estimate is consistent with both the semi-analytical results and SFRF.…”

Section: [C Ii] Luminosity Functionsupporting

confidence: 76%

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ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ^⋆ Galaxy at z = 6.0719

Fujimoto

Oguri

Brammer

et al. 2021

ApJ

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Section: [C Ii] Luminosity Functionsupporting

confidence: 76%

“…have not yet been identified, due to the lack of sufficiently deep and large survey volumes (e.g., Matsuda et al 2015;Aravena et al 2016;Yamaguchi et al 2017;Hayatsu et al 2019;Decarli et al 2020;Romano et al 2020;Yan et al 2020).…”

Section: Introductionmentioning

confidence: 99%

ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ^⋆ Galaxy at z = 6.0719

Fujimoto

Oguri

Brammer

et al. 2021

ApJ

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“…where Φ(L, z) is the [CII] luminosity function derived from the UV-selected central ALPINE targets (Yan et al 2020), L lim is the luminosity corresponding to the limiting flux of each ALPINE…”

Section: Accounting For Completenessmentioning

confidence: 99%

The ALPINE-ALMA [CII] survey

Romano

Cassata

Morselli

et al. 2021

A&A

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Context. Galaxy mergers are thought to be one of the main mechanisms of the mass assembly of galaxies in the Universe, but there is still little direct observational evidence of how frequent they are at z ≳ 4. Recently, many works have suggested a possible increase in the fraction of major mergers in the early Universe, reviving the debate on which processes (e.g., cold accretion, star formation, mergers) most contribute to the mass build-up of galaxies through cosmic time. Aims. To estimate the importance of major mergers in this context, we make use of the new data collected by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey, which attempted to observe the [CII] 158 μm emission line from a sample of 75 main-sequence star-forming galaxies at 4.4 < z < 5.9. Methods. We used, for the first time, the morpho-kinematic information provided by the [CII] emission, along with archival multiwavelength data to obtain the fraction of major mergers (fMM) at z ∼ 5. By combining the results from ALPINE with those at lower redshifts from the literature, we also studied the evolution of the merger fraction through cosmic time. We then used different redshift-evolving merger timescales (TMM) to convert this fraction into the merger rate per galaxy (RMM) and in the volume-averaged merger rate (ΓMM). Results. We find a merger fraction of fMM ∼ 0.44 (0.34) at z ∼ 4.5 (5.5) from ALPINE. By combining our results with those at lower redshifts, we computed the cosmic evolution of the merger fraction which is described by a rapid increase from the local Universe to higher redshifts, a peak at z ∼ 3, and a slow decrease toward earlier epochs. Depending on the timescale prescription used, this fraction translates into a merger rate ranging between ∼0.1 and ∼4.0 Gyr−1 at z ∼ 5, which in turn corresponds to an average number of major mergers per galaxy between 1 and 8 in ∼12.5 yr (from z = 6 to the local Universe). When convolved with the galaxy number density at different epochs, the merger rate density becomes approximately constant over time at 1 < z < 4, including values from 10−4 to 10−3 Gyr−1 Mpc−3, depending on the assumed TMM. We finally compare the specific star formation and star-formation rate density with the analogous quantities from major mergers, finding a good agreement at z > 4 if we assume a merger timescale that quickly decreases with increasing redshift. Conclusions. Our new constraints on the merger fraction from the ALPINE survey at z ∼ 5 reveal the presence of a significant merging activity in the early Universe. Whether this population of mergers can provide a relevant contribution to the galaxy mass assembly at these redshifts and through the cosmic epochs is strongly dependent on the assumption of the merger timescale. However, our results show that an evolving TMM ∝ (1 + z)−2 agrees well with state-of-the-art cosmological simulations, suggesting a considerable role of mergers in the build-up of galaxies at early times.

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“…Over the last year many results based on the ALPINE survey have been presented, describing the interstellar medium (ISM) properties of normal star-forming galaxies at z ∼ 5 (the [CII]-SFR relation: Schaerer et al 2020;the [CII] (Jones et al 2020;Romano et al 2020;Ginolfi et al 2020a) or presenting statistical studies at z ∼ 5, including the [CII] luminosity function for ultraviolet (UV) and serendipitously detected line emitters (Yan et al 2020;Loiacono et al 2021), the infrared (IR) luminosity function (Gruppioni et al 2020), and the cosmic star formation rate density (SFRD, Khusanova et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The ALPINE-ALMA [CII] survey

Pozzi¹,

Calura²,

Fudamoto

et al. 2021

A&A

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Aims. The dust content of normal galaxies and the dust mass density (DMD) at high-z (z > 4) are unconstrained given the source confusion and the sensitivity limitations of previous observations. The ALMA Large Program to INvestigate [CII] at Early times (ALPINE), which targeted 118 ultra-violet (UV)-selected star-forming galaxies at 4.4 < z < 5.9, provides a new opportunity to tackle this issue for the first time with a statistically robust dataset. Methods. We exploited the rest-frame far-infrared (FIR) fluxes of 23 galaxies individually detected in their continuum emission, as well as stacked continuum images, to measure the dust content of the 118 UV-selected ALPINE galaxies. We focused on the dust scaling relations and, by comparison with predictions from chemical evolution models, we probed the evolutionary stage of UV-selected galaxies at high-z. By using the observed correlation between the UV luminosity and the dust mass, we estimated the DMD of UV-selected galaxies at z ∼ 5, weighting the galaxies by means of the UV luminosity function. The derived DMD is compared with the value we estimated from ten ALPINE galaxies blindly detected in the FIR continuum, at the redshift of the ALPINE targets. Results. Our ALMA survey allows the exploration for the first time of the dust content in normal star-forming galaxies at z > 4 in a statistically robust sample of sources. The comparison of the observed dust scaling relations with chemical evolution models suggests that ALPINE galaxies are not likely progenitors of disc galaxies, but of intermediate- and low-mass proto-spheroids, resulting in present-day bulges of spiral or elliptical galaxies. Interestingly, this conclusion is in line with the independent morphological analysis that shows that the majority (∼70%) of the dust-continuum detected galaxies have a disturbed morphology. The DMD obtained at z ∼ 5 from UV-selected sources is ∼30% of the value obtained from blind FIR-selected sources, showing that the UV selection misses the most dust-rich, UV-obscured galaxies.

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The ALPINE-ALMA [C II] Survey: [C II] 158 μm Emission Line Luminosity Functions at z ∼ 4–6

Cited by 32 publications

References 54 publications

ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ^⋆ Galaxy at z = 6.0719

ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ^⋆ Galaxy at z = 6.0719

The ALPINE-ALMA [CII] survey

The ALPINE-ALMA [CII] survey

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The ALPINE-ALMA [C II] Survey: [C II] 158 μm Emission Line Luminosity Functions at z ∼ 4–6

Cited by 32 publications

References 54 publications

ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ⋆ Galaxy at z = 6.0719

ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ⋆ Galaxy at z = 6.0719

The ALPINE-ALMA [CII] survey

The ALPINE-ALMA [CII] survey

Contact Info

Product

Resources

About

ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ^⋆ Galaxy at z = 6.0719

ALMA Lensing Cluster Survey: Bright [C ii] 158 μm Lines from a Multiply Imaged Sub-L ^⋆ Galaxy at z = 6.0719