The ALPINE-ALMA [CII] survey

Gruppioni, C.; Béthermin, M.; Loiacono, F.; Fèvre, O. Le; Capak, P.; Cassata, P.; Faisst, Andreas L.; Schaerer, D.; Silverman, John D.; Yan, Lin; Bardelli, S.; Boquien, M.; Carraro, R.; Cimatti, A.; Dessauges‐Zavadsky, M.; Ginolfi, M.; Fujimoto, Seiji; Hathi, N. P.; Jones, G. C.; Khusanova, Y.; Koekemoer, Anton M.; Lagache, G.; Lemaux, B. C.; Oesch, Pascal; Pozzi, F.; Riechers, Dominik A.; Rodighiero, G.; Romano, Michael; Talia, M.; Vallini, L.; Vergani, D.; Zamorani, G.; Zucca, E.

doi:10.1051/0004-6361/202038487

Cited by 160 publications

(255 citation statements)

References 135 publications

(173 reference statements)

Supporting

Mentioning

209

Contrasting

Order By: Relevance

“…On the other hand, the field LF seems to be quite consistent with the targets ones except in the case of the highest luminosity bin. There is agreement between the field [C II] LF and the IR-derived [C II] LF based on the ALPINE serendipitous sources detected in continuum (Gruppioni et al 2020). The agreement persists at L [C II] > 10 9.5 L for the clustered sample if the companions of the central targets are included in the IR-derived [C II] LF of Gruppioni et al (2020).…”

Section: Lfs From Alpinementioning

confidence: 58%

“…Within the sample of the serendipitous [C II] lines, there are five sources for which also the continuum has been detected (Bethermin et al 2020;Gruppioni et al 2020). It is well known that there is a correlation between the [C II] luminosity and the SFR (De Looze et al 2014).…”

Section: Relation Between [C Ii] Luminosity and Sfrmentioning

confidence: 99%

“…Thereafter, we compare our sample with the LF based on the sources serendipitously detected in the rest-frame FIR continuum (Gruppioni et al 2020;Bethermin et al 2020). The 118 ALPINE pointings have indeed revealed a wealth of serendipitous continuum emitters across a wide range of redshifts.…”

Section: Lfs From Alpinementioning

confidence: 99%

“…The 118 ALPINE pointings have indeed revealed a wealth of serendipitous continuum emitters across a wide range of redshifts. These sources were used to build a LF at 250 µm (rest-frame) and a total IR LF from z = 0.5 to z = 6 (see Gruppioni et al 2020 for details). For the purposes of our comparison, we considered the IR LF in the highest redshift interval 4.5 < z < 6, where the companions of the central targets have been removed [C II] LFs at z ∼ 5 from the serendipitous sources in ALPINE compared to other works in the literature.…”

Section: Lfs From Alpinementioning

confidence: 99%

See 3 more Smart Citations

The ALPINE–ALMA [C II] survey

Loiacono

Decarli²,

Gruppioni³

et al. 2021

A&A

View full text Add to dashboard Cite

We present the first [C II] 158 μm luminosity function (LF) at z ∼ 5 from a sample of serendipitous lines detected in the ALMA Large Program to INvestigate [C II] at Early times (ALPINE). A study of the 118 ALPINE pointings revealed several serendipitous lines. Based on their fidelity, we selected 14 lines for the final catalog. According to the redshift of their counterparts, we identified eight out of 14 detections as [C II] lines at z ∼ 5, along with two as CO transitions at lower redshifts. The remaining four lines have an elusive identification in the available catalogs and we considered them as [C II] candidates. We used the eight confirmed [C II] and the four [C II] candidates to build one of the first [C II] LFs at z ∼ 5. We found that 11 out of these 12 sources have a redshift very similar to that of the ALPINE target in the same pointing, suggesting the presence of overdensities around the targets. Therefore, we split the sample in two (a “clustered” and “field” subsample) according to their redshift separation and built two separate LFs. Our estimates suggest that there could be an evolution of the [C II] LF between z ∼ 5 and z ∼ 0. By converting the [C II] luminosity to the star-formation rate, we evaluated the cosmic star-formation rate density (SFRD) at z ∼ 5. The clustered sample results in a SFRD ∼10 times higher than previous measurements from UV–selected galaxies. On the other hand, from the field sample (likely representing the average galaxy population), we derived a SFRD ∼1.6 higher compared to current estimates from UV surveys but compatible within the errors. Because of the large uncertainties, observations of larger samples will be necessary to better constrain the SFRD at z ∼ 5. This study represents one of the first efforts aimed at characterizing the demography of [C II] emitters at z ∼ 5 using a mm selection of galaxies.

show abstract

Section: Lfs From Alpinementioning

confidence: 58%

Section: Relation Between [C Ii] Luminosity and Sfrmentioning

confidence: 99%

Section: Lfs From Alpinementioning

confidence: 99%

Section: Lfs From Alpinementioning

confidence: 99%

See 2 more Smart Citations

The ALPINE–ALMA [C II] survey

Loiacono

Decarli²,

Gruppioni³

et al. 2021

A&A

View full text Add to dashboard Cite

show abstract

“…Studying galaxy evolution throughout cosmic time is a key element of modern astrophysics and is crucial for our understanding of the life cycle of the progenitors of passive elliptical galaxies that we observe in the local Universe. Evidence suggests that the star formation rate (SFR) density has peaked around a redshift of z ≈ 2 (e.g., Hopkins & Beacom 2006;Madau & Dickinson 2014;Béthermin et al 2017;Gruppioni et al 2020), making this epoch (cosmic noon) particularly interesting. Moreover, at cosmic noon, dusty star-forming galaxies (DSFGs; e.g., Smail et al 1997;Blain et al 2002;Weiß et al 2013a;Casey et al 2014;Donevski et al 2020) contributed significantly to the star formation activity of the Universe (e.g., Chapman et al 2003Chapman et al , 2005.…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength dissection of a massive heavily dust-obscured galaxy and its blue companion at z∼2

Hamed

Ciesla

Béthermin

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We study a system of two galaxies, Astarte and Adonis, at z ∼ 2. At this time, the Universe was undergoing the peak of its star formation activity. Astarte is a dusty star-forming galaxy at the massive end of the main sequence (MS), and Adonis is a less massive companion galaxy that is bright in the ultraviolet and has an optical spectroscopic redshift. We investigate whether this ultramassive galaxy is quenching, and whether it has always been on the MS of star-forming galaxies. Methods. We used the code CIGALE to model the spectral energy distribution. The code relies on the energetic balance between the ultraviolet and the infrared. We derived some of the key physical properties of Astarte and Adonis, mainly their star formation rates (SFRs), stellar masses, and dust luminosities. We inspected the variation of the physical parameters depending on the assumed dust-attenuation law. We also estimated the molecular gas mass of Astarte from its CO emission, using different αCO and transition ratios (r31), and we discuss the implication of the various assumptions on the gas-mass derivation. Reults. We find that Astarte exhibits a MS-like star formation activity, and Adonis is undergoing a strong starburst phase. The molecular gas mass of Astarte is far lower than the gas fraction of typical star-forming galaxies at z = 2. This low gas content and high SFR result in a depletion time of 0.22 ± 0.07 Gyr, which is slightly shorter than expected for a MS galaxy at this redshift. The CO luminosity relative to the total infrared luminosity suggests a MS-like activity when we assume a galactic conversion factor and a low transition ratio. The SFR of Astarte is on the same order when different attenuation laws are used, unlike its stellar mass, which increases when shallow attenuation laws are used (∼1 × 1011 M⊙ assuming a Calzetti relation, versus ∼4 × 1011 M⊙ assuming a shallow attenuation law). We discuss these properties and suggest that Astarte might be experiencing a recent decrease in star formation activity and is quenching through the MS following a starburst epoch.

show abstract

Chemical Evolution of the Universe and its Consequences for Gravitational‐Wave Astrophysics

Chruślińska

2022

Annalen der Physik

View full text Add to dashboard Cite

We are now routinely detecting gravitational waves (GW) emitted by merging black holes and neutron stars. Those are the afterlives of massive stars that formed all across the Universe -at different cosmic times and with different metallicities (abundances of elements heavier than helium). Birth metallicity plays an important role in the evolution of massive stars. Consequently, the population properties of mergers are sensitive to the metallicity dependent cosmic star formation history (fSFR(Z,z)). In particular, within the isolated formation scenarios (the focus of this paper), a strong low metallicity preference of the formation of mergers involving black holes was found. The origin of this dependence and its consequences are discussed. Most importantly, uncertainty in the fSFR(Z,z) (substantial even at low redshifts, especially at low metallicity) cannot be ignored in the models. This poses a significant challenge for the interpretation of the observed GW source population properties. Possible paths for improvements and the role of future GW detectors are considered. Recent efforts to determine fSFR(Z,z) and the factors that dominate its uncertainty are summarized. Many of those factors are related to the properties of galaxies that are faint and distant and therefore difficult to observe. The fact that they leave imprint on the properties of mergers as a function of cosmic time makes future GW observations a promising (and complementary to electromagnetic observations) tool to study chemical evolution of galaxies.

show abstract

The ALPINE-ALMA [CII] survey

Cited by 160 publications

References 135 publications

The ALPINE–ALMA [C II] survey

The ALPINE–ALMA [C II] survey

Multiwavelength dissection of a massive heavily dust-obscured galaxy and its blue companion at z∼2

Chemical Evolution of the Universe and its Consequences for Gravitational‐Wave Astrophysics

Contact Info

Product

Resources

About