%0 Generic %1 loiacono2020alpinealma %A Loiacono, Federica %A Decarli, Roberto %A Gruppioni, Carlotta %A Talia, Margherita %A Cimatti, Andrea %A Zamorani, Gianni %A Pozzi, Francesca %A Yan, Lin %A Lemaux, Brian C. %A Riechers, Dominik A. %A Fèvre, Olivier Le %A Béthermin, Matthieu %A Capak, Peter %A Cassata, Paolo %A Faisst, Andreas %A Schaerer, Daniel %A Silverman, John D. %A Bardelli, Sandro %A Boquien, Médéric %A Burkutean, Sandra %A Dessauges-Zavadsky, Miroslava %A Fudamoto, Yoshinobu %A Fujimoto, Seiji %A Ginolfi, Michele %A Hathi, Nimish P. %A Jones, Gareth C. %A Khusanova, Yana %A Koekemoer, Anton M. %A Lagache, Guilaine %A Massardi, Marcella %A Oesch, Pascal %A Romano, Michael %A Vallini, Livia %A Vergani, Daniela %A Zucca, Elena %D 2020 %K library %T The ALPINE-ALMA C II survey: the luminosity function of serendipitous C II line emitters at $z5$ %U http://arxiv.org/abs/2006.04837 %X We present the first CII 158 $\mu$m luminosity function (LF) at $z5$ from a sample of serendipitous lines detected in the ALMA Large Program to INvestigate CII at Early times (ALPINE). A search performed over 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 8 out of 14 detections as CII lines at $z5$, and two as CO transitions at lower redshifts. The remaining 4 lines have an elusive identification in the available catalogs and we considered them as CII candidates. We used the 8 confirmed CII and the 4 CII candidates to build one of the first CII LFs at $z5$. 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" sub-sample) according to their redshift separation and built two separate LFs. Our estimates suggest that there could be an evolution of the CII LF between $z 5$ and $z 0$. By converting the CII luminosity to star formation rate we evaluated the cosmic star formation rate density (SFRD) at $z5$. 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 are necessary to better constrain the SFRD at $z5$. This study represents one of the first efforts aimed at characterizing the demography of CII emitters at $z5$ using a mm-selection of galaxies.

@misc{loiacono2020alpinealma, abstract = {We present the first [CII] 158 $\mu$m luminosity function (LF) at $z\sim 5$ from a sample of serendipitous lines detected in the ALMA Large Program to INvestigate [CII] at Early times (ALPINE). A search performed over 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 8 out of 14 detections as [CII] lines at $z\sim 5$, and two as CO transitions at lower redshifts. The remaining 4 lines have an elusive identification in the available catalogs and we considered them as [CII] candidates. We used the 8 confirmed [CII] and the 4 [CII] candidates to build one of the first [CII] LFs at $z\sim 5$. 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" sub-sample) according to their redshift separation and built two separate LFs. Our estimates suggest that there could be an evolution of the [CII] LF between $z \sim 5$ and $z \sim 0$. By converting the [CII] luminosity to star formation rate we evaluated the cosmic star formation rate density (SFRD) at $z\sim 5$. The clustered sample results in a SFRD $\sim 10$ 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 $\sim 1.6$ higher compared to current estimates from UV surveys but compatible within the errors. Because of the large uncertainties, observations of larger samples are necessary to better constrain the SFRD at $z\sim 5$. This study represents one of the first efforts aimed at characterizing the demography of [CII] emitters at $z\sim 5$ using a mm-selection of galaxies.}, added-at = {2020-06-11T09:22:11.000+0200}, author = {Loiacono, Federica and Decarli, Roberto and Gruppioni, Carlotta and Talia, Margherita and Cimatti, Andrea and Zamorani, Gianni and Pozzi, Francesca and Yan, Lin and Lemaux, Brian C. and Riechers, Dominik A. and Fèvre, Olivier Le and Béthermin, Matthieu and Capak, Peter and Cassata, Paolo and Faisst, Andreas and Schaerer, Daniel and Silverman, John D. and Bardelli, Sandro and Boquien, Médéric and Burkutean, Sandra and Dessauges-Zavadsky, Miroslava and Fudamoto, Yoshinobu and Fujimoto, Seiji and Ginolfi, Michele and Hathi, Nimish P. and Jones, Gareth C. and Khusanova, Yana and Koekemoer, Anton M. and Lagache, Guilaine and Massardi, Marcella and Oesch, Pascal and Romano, Michael and Vallini, Livia and Vergani, Daniela and Zucca, Elena}, biburl = {https://www.bibsonomy.org/bibtex/293d39637426b9f372293b0f9e10b6017/gpkulkarni}, description = {The ALPINE-ALMA [C II] survey: the luminosity function of serendipitous [C II] line emitters at $z\sim 5$}, interhash = {34cfb0e62fd9e189f7d114ba2f1f84e1}, intrahash = {93d39637426b9f372293b0f9e10b6017}, keywords = {library}, note = {cite arxiv:2006.04837Comment: 19 pages, 12 figures; submitted to Astronomy & Astrophysics}, timestamp = {2020-06-11T09:22:11.000+0200}, title = {The ALPINE-ALMA [C II] survey: the luminosity function of serendipitous [C II] line emitters at $z\sim 5$}, url = {http://arxiv.org/abs/2006.04837}, year = 2020 }