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J/A+A/609/A130  [CII] luminosities of galaxies in G.A.S.+Cloudy (Lagache+, 2018)

The [CII] 158 micron line emission in high-redshift galaxies. Lagache G., Cousin M., Chatzikos M. <Astron. Astrophys. 609, A130 (2018)> =2018A&A...609A.130L (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary ; Galaxy catalogs ; Interstellar medium Keywords: galaxies: evolution - galaxies: high-redshift - galaxies: ISM Abstract: Gas is a crucial component of galaxies, providing the fuel to form stars, and it is impossible to understand the evolution of galaxies without knowing their gas properties. The [CII] fine structure transition at 158µm is the dominant cooling line of cool interstellar gas, and is the brightest of emission lines from star forming galaxies from FIR through meter wavelengths, almost unaffected by attenuation. With the advent of ALMA and NOEMA, capable of detecting [CII]-line emission in high-redshift galaxies, there has been a growing interest in using the [CII] line as a probe of the physical conditions of the gas in galaxies, and as a star formation rate (SFR) indicator at z≥4. In this paper, we have used a semi-analytical model of galaxy evolution (G.A.S.) combined with the photoionisation code CLOUDY to predict the [CII] luminosity of a large number of galaxies (25,000 at z~=5) at 4≤z≤8. We assumed that the [CII]-line emission originates from photo-dominated regions. At such high redshift, the CMB represents a strong background and we discuss its effects on the luminosity of the [CII] line. We studied the L[CII]-SFR and L[CII]-Zg relations and show that they do not strongly evolve with redshift from z=4 and to z=8. Galaxies with higher [CII] luminosities tend to have higher metallicities and higher star formation rates but the correlations are very broad, with a scatter of about 0.5 and 0.8dex for L[CII]-SFR and L[CII]-Zg, respectively. Our model reproduces the L[CII]-SFR relations observed in high-redshift star-forming galaxies, with [CII] luminosities lower than expected from local L[CII]-SFR relations. Accordingly, the local observed L[CII]-SFR relation does not apply at high-z (z~=5), even when CMB effects are ignored. Our model naturally produces the [CII] deficit (i.e. the decrease of L[CII]/LIR with LIR), which appears to be strongly correlated with the intensity of the radiation field in our simulated galaxies. We then predict the [CII] luminosity function, and show that it has a power law form in the range of L[CII] probed by the model with a slope α=-1. The slope is not evolving from z=4 to z=8 but the number density of [CII]-emitters decreases by a factor of 20x. We discuss our predictions in the context of current observational estimates on both the differential and cumulative luminosity functions. The outputs from the model are distributed as FITS-formatted files at the CDS. Description: One fits file per redshift (z=4, 4.7, 5.9, 6.7, 7.6) which gives for all galaxies with mass above 10^7 Msol: Log(M_star): stellar mass (Msol) Log(M_gas): gas mass (Mssol) ZgOHINDEX: gas metallicity (OH Index) Zg_MZ: gas metallicity (units of Zsol) LOG(ISRF): interstellar radiation field (unit of G0) Log(nHI): HI density (cm-3) Log(SFR): star formation rate from the model (Msol/yr) log(SFR_obs): star formation rate computed from the UV and IR luminosities (Msol/yr) log(LIR): 8-1000 micron luminosity (Lsol) Log(LCII): CII luminosity (Lsol) Log(LCII_WOA): CII luminosity without CMB attenuation (Lsol) Log(LCIIWOAWOH): CII luminosity without CMB attenuation and heating (Lsol) Log(LCII_Vallini): CII luminosity using N=2 (Eq. 11) (Lsol) Log(LAGN): AGN bolometric luminosity (Lsol) File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file gcciiz4.dat 126 10803 Outputs from the model for z=4 gcciiz5.dat 126 6175 Outputs from the model for z=4.7 gcciiz6.dat 126 2374 Outputs from the model for z=5.9 gcciiz7.dat 126 1074 Outputs from the model for z=6.7 gcciiz8.dat 126 388 Outputs from the model for z=7.6 fits/* 0 5 All tables in fits format
Byte-by-byte Description of file: gcciiz?.dat
Bytes Format Units Label Explanations
1- 8 F8.5 [Msun] logMstar Stellar mass (logMstar) 10- 17 F8.5 [Msun] logMgas Gas mass (log_Mgas) 19- 26 F8.5 --- ZgOHindex Gaz metallicity in OH index unit (ZgOHindex) 28- 36 F9.6 Sun ZgmZ Gaz metallicity (Zg_mZ) 38- 44 F7.5 --- logISRF Interstellar radiation field in G0 unit (log_ISRF) 46- 52 F7.5 [cm-3] lognHI HI density (log_nHI) 54- 62 F9.6 [Msun/yr] logSFR Star formation rate from the model (log_SFR) 64- 72 F9.6 [Msun/yr] logSFRobs Star formation rate computed from the UV and IR luminosities (logSFRobs) 74- 81 F8.5 [Lsun] logLIR 8-1000 micron luminosity (logLIR) 83- 90 F8.5 [Lsun] logLCII CII luminosity (logLCII) 92- 99 F8.5 [Lsun] logLCIIw CII luminosity without CMB attenuation (logLCII_woa) 101-108 F8.5 [Lsun] logLCIIww CII luminosity without CMB attenuation and heating (logLCIIwoawoh) 110-117 F8.5 [Lsun] logLCIIVa CII luminosity using N=2 (Eq. 11) (logLCII_Vallini) 119-126 F8.6 [Lsun] logLAGN ? AGN bolometric luminosity (logLagn)
Acknowledgements: Guilaine Lagache, guilaine.lagache(at)lam.fr
(End) Patricia Vannier [CDS] 07-Nov-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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