CaltechAUTHORS
  A Caltech Library Service

The Local [C ii] 158 μm Emission Line Luminosity Function

Hemmati, Shoubaneh and Yan, Lin and Díaz-Santos, Tanio and Armus, Lee and Capak, Peter and Faisst, Andreas and Masters, Daniel (2017) The Local [C ii] 158 μm Emission Line Luminosity Function. Astrophysical Journal, 834 (1). Art. No. 36. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20170104-114631452

[img] PDF - Published Version
See Usage Policy.

1279Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20170104-114631452

Abstract

We present, for the first time, the local [C ii] 158 μm emission line luminosity function measured using a sample of more than 500 galaxies from the Revised Bright Galaxy Sample. [C ii] luminosities are measured from the Herschel PACS observations of the Luminous Infrared Galaxies (LIRGs) in the Great Observatories All-sky LIRG Survey and estimated for the rest of the sample based on the far-infrared (far-IR) luminosity and color. The sample covers 91.3% of the sky and is complete at S_(60 μm) > 5.24 Jy. We calculate the completeness as a function of [C ii] line luminosity and distance, based on the far-IR color and flux densities. The [C ii] luminosity function is constrained in the range ~10^(7–9) L_⊙ from both the 1/V_(max) and a maximum likelihood methods. The shape of our derived [C ii] emission line luminosity function agrees well with the IR luminosity function. For the CO(1-0) and [C ii] luminosity functions to agree, we propose a varying ratio of [C ii]/CO(1-0) as a function of CO luminosity, with larger ratios for fainter CO luminosities. Limited [C ii] high-redshift observations as well as estimates based on the IR and UV luminosity functions are suggestive of an evolution in the [C ii] luminosity function similar to the evolution trend of the cosmic star formation rate density. Deep surveys using the Atacama Large Millimeter Array with full capability will be able to confirm this prediction.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/1538-4357/834/1/36DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/834/1/36/metaPublisherArticle
https://arxiv.org/abs/1611.03092arXivDiscussion Paper
ORCID:
AuthorORCID
Hemmati, Shoubaneh0000-0003-2226-5395
Yan, Lin0000-0003-1710-9339
Díaz-Santos, Tanio0000-0003-0699-6083
Armus, Lee0000-0003-3498-2973
Capak, Peter0000-0003-3578-6843
Faisst, Andreas0000-0002-9382-9832
Masters, Daniel0000-0001-5382-6138
Additional Information:© 2016. The American Astronomical Society. Received 2016 July 22; revised 2016 November 7; accepted 2016 November 9; published 2016 December 28. We wish to thank the referee for helpful comments which improved the content and presentation of this paper. SH wishes to thank Iary Davidzon and Hooshang Nayyeri for very useful discussions. AF acknowledges support from the Swiss National Science Foundation. T.D.-S. acknowledges support from ALMA-CONICYT project 31130005 and FONDECYT regular project 1151239.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Swiss National Science Foundation (SNSF)UNSPECIFIED
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)31130005
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1151239
Subject Keywords:galaxies: evolution; galaxies: luminosity function, mass function; infrared: galaxies; quasars: emission lines
Issue or Number:1
Record Number:CaltechAUTHORS:20170104-114631452
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170104-114631452
Official Citation:Shoubaneh Hemmati et al 2017 ApJ 834 36
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:73209
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:04 Jan 2017 20:59
Last Modified:03 Oct 2019 16:25

Repository Staff Only: item control page