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Measuring Galaxy Clustering and the Evolution of [C II] Mean Intensity with Far-IR Line Intensity Mapping during 0.5 < z < 1.5

Uzgil, B. D. and Aguirre, J. E. and Bradford, C. M. and Lidz, A. (2014) Measuring Galaxy Clustering and the Evolution of [C II] Mean Intensity with Far-IR Line Intensity Mapping during 0.5 < z < 1.5. Astrophysical Journal, 793 (2). Art. No. 116. ISSN 0004-637X. doi:10.1088/0004-637X/793/2/116.

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Infrared fine-structure emission lines from trace metals are powerful diagnostics of the interstellar medium in galaxies. We explore the possibility of studying the redshifted far-IR fine-structure line emission using the three-dimensional (3-D) power spectra obtained with an imaging spectrometer. The intensity mapping approach measures the spatio-spectral fluctuations due to line emission from all galaxies, including those below the individual detection threshold. The technique provides 3-D measurements of galaxy clustering and moments of the galaxy luminosity function. Furthermore, the linear portion of the power spectrum can be used to measure the total line emission intensity including all sources through cosmic time with redshift information naturally encoded. Total line emission, when compared to the total star formation activity and/or other line intensities reveals evolution of the interstellar conditions of galaxies in aggregate. As a case study, we consider measurement of [CII] autocorrelation in the 0.5 < z < 1.5 epoch, where interloper lines are minimized, using far-IR/submm balloon-borne and future space-borne instruments with moderate and high sensitivity, respectively. In this context, we compare the intensity mapping approach to blind galaxy surveys based on individual detections. We find that intensity mapping is nearly always the best way to obtain the total line emission because blind, wide-field galaxy surveys lack sufficient depth and deep pencil beams do not observe enough galaxies in the requisite luminosity and redshift bins. Also, intensity mapping is often the most efficient way to measure the power spectrum shape, depending on the details of the luminosity function and the telescope aperture.

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Additional Information:© 2014 American Astronomical Society. Received 2014 June 13; Accepted 2014 July 26; Published 2014 September 15. The authors thank Olivier Doré for useful discussions and Yan Gong for valuable comments that improved this manuscript. B.U. acknowledges support from the NASA GSRP Fellowship. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.
Group:Keck Institute for Space Studies
Funding AgencyGrant Number
NASA Graduate Student Research FellowshipUNSPECIFIED
Subject Keywords:galaxies: evolution; galaxies: ISM; infrared: ISM; large-scale structure of universe
Issue or Number:2
Record Number:CaltechAUTHORS:20160328-100432062
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Official Citation:B. D. Uzgil et al 2014 ApJ 793 116
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:65695
Deposited By: Colette Connor
Deposited On:31 Mar 2016 00:31
Last Modified:10 Nov 2021 23:48

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