CO luminosity function from <i>Herschel</i>-selected galaxies and the contribution of AGN

Vallini, L.; Gruppioni, C.; Pozzi, F.; Vignali, C.; Zamorani, G.

doi:10.1093/mnrasl/slv173

Cited by 39 publications

(63 citation statements)

References 30 publications

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“…Effects of cosmic variance may have significant influences on the derived CO number densities. Vallini et al (2016) obtained indirect estimates of the CO luminosity function by applying various FIR-to-CO conversions on Herschel data. When comparing their empirical estimates of the CO luminosity function to model predictions, Vallini et al also found that theoretical models predict too few CO-bright galaxies at z = 2.…”

Section: Too Few Co-bright Galaxies At Z >mentioning

confidence: 99%

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Sub-mm emission line deep fields: CO and [C ii] luminosity functions out toz= 6

Popping

Kampen

Decarli

et al. 2016

Mon. Not. R. Astron. Soc.

114

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Now that ALMA is reaching its full capabilities, observations of sub-mm emission line deep fields become feasible. We couple a semi-analytic model of galaxy formation with a radiative transfer code to make predictions for the luminosity function of CO J=1-0 out to CO J=6-5 and [CII] at redshifts z=0-6. We find that: 1) our model correctly reproduces the CO and [CII] emission of low-and high-redshift galaxies and reproduces the available constraints on the CO luminosity function at z 2.75; 2) we find that the CO and [CII] luminosity functions of galaxies increase from z = 6 to z = 4, remain relatively constant till z = 1 and rapidly decrease towards z = 0. The galaxies that are brightest in CO and [CII] are found at z ∼ 2; 3) the CO J=3-2 emission line is most favourable to study the CO luminosity and global H 2 mass content of galaxies, because of its brightness and observability with currently available sub-mm and radio instruments; 4) the luminosity functions of high-J CO lines show stronger evolution than the luminosity functions of low-J CO lines; 5) our model barely reproduces the available constraints on the CO and [CII] luminosity function of galaxies at z 1.5 and the CO luminosity of individual galaxies at intermediate redshifts. We argue that this is driven by a lack of cold gas in galaxies at intermediate redshifts as predicted by cosmological simulations of galaxy formation.

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Section: Too Few Co-bright Galaxies At Z >mentioning

confidence: 99%

“…Observations with the Herschel Space Observatory revealed strong excitation of high-J CO lines (CO J=9-8 and higher) in nearby active galaxies (van der Werf et al 2010;Meijerink et al 2013). The high excitation lines can be explained by including the heating from X-ray radiation on top of the UV radiation.…”

Section: X-ray Driven Excitationmentioning

confidence: 99%

Sub-mm emission line deep fields: CO and [C ii] luminosity functions out toz= 6

Popping

Kampen

Decarli

et al. 2016

Mon. Not. R. Astron. Soc.

114

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“…For comparison, we include the predictions based on semi-analytical models by Lagos et al (2012) and Popping et al (2016) and on the empirical IR luminosity function of Herschel sources by Vallini et al (2016), as well as the constraints obtained by the earlier study of the HDF-N ). Our observations reach the knee of the luminosity functions in almost all redshift bins.…”

Section: Co Luminosity Functionsmentioning

confidence: 99%

“…Other low-J CO lines may be of practical interest, because these levels remain significantly excited in star-forming galaxies; and thus, the associated lines (CO(2-1), CO(3-2), CO(4-3)) are typically brighter and easier to detect than the ground-state transition CO(1-0). There have been various predictions of the CO luminosity functions both for the J=  1 0 transition and for intermediate and high-J lines, using either theoretical models (e.g., Lagos et al 2011Lagos et al , 2012Lagos et al , 2014Popping et al 2014aPopping et al , 2014bPopping et al , 2016 or empirical relations (e.g., Sargent et al 2012Sargent et al , 2014da Cunha et al 2013;Vallini et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Alma Spectroscopic Survey in the Hubble Ultra Deep Field: Co Luminosity Functions and the Evolution of the Cosmic Density of Molecular Gas

Decarli

Walter

Aravena

et al. 2016

ApJ

121

113

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In this paper we use ASPECS, the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (UDF) in band 3 and band 6, to place blind constraints on the CO luminosity function and the evolution of the cosmic molecular gas density as a function of redshift up to z ∼ 4.5. This study is based on galaxies that have been solely selected through their CO emission and not through any other property. In all of the redshift bins the ASPECS measurements reach the predicted 'knee' of the CO luminosity function (around 5 × 10 9 K km s −1 pc 2 ). We find clear evidence of an evolution in the CO luminosity function with respect to z ∼ 0, with more CO luminous galaxies present at z ∼ 2. The observed galaxies at z ∼ 2 also appear more gas-rich than predicted by recent semi-analytical models. The comoving cosmic molecular gas density within galaxies as a function of redshift shows a factor 3-10 drop from z ∼ 2 to z ∼ 0 (with significant error bars), and possibly a decline at z > 3. This trend is similar to the observed evolution of the cosmic star formation rate density. The latter therefore appears to be at least partly driven by the increased availability of molecular gas reservoirs at the peak of cosmic star formation (z ∼ 2).

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“…Otherwise, the values for φ over the given range are not unreasonable for any of our models. While no space density data for HCN emitters appear to be available, the simulated CO luminosity function values for the models in this work do not compare unfavourably to data and fits that Vallini et al (2016) and Decarli et al (2016) present in the range of L 10 9 K km s −1 pc 2 , where CO observational data are chiefly available. The overall features of the CO luminosity function, including the knee at L CO ∼ 10 10 K km s −1 pc 2 , are entirely consistent with the 1σ constraints from COPSS data given in Keating et al (2016).…”

Section: Appendixmentioning

confidence: 71%

On Estimation of Contamination from Hydrogen Cyanide in Carbon Monoxide Line-intensity Mapping

Chung

Viero

et al. 2017

ApJ

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Line-intensity mapping surveys probe large-scale structure through spatial variations in molecular line emission from a population of unresolved cosmological sources. Future such surveys of carbon monoxide line emission, specifically the CO(1-0) line, face potential contamination from a disjoint population of sources emitting in a hydrogen cyanide emission line, HCN(1-0). This paper explores the potential range of the strength of HCN emission and its effect on the CO auto power spectrum, using simulations with an empirical model of the CO/HCN-halo connection. We find that effects on the observed CO power spectrum depend on modeling assumptions but are very small for our fiducial model, which is based on current understanding of the galaxyhalo connection. Given the fiducial model, we expect the bias in overall CO detection significance due to HCN to be less than 1%.

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CO luminosity function from Herschel-selected galaxies and the contribution of AGN

Cited by 39 publications

References 30 publications

Sub-mm emission line deep fields: CO and [C ii] luminosity functions out toz= 6

Sub-mm emission line deep fields: CO and [C ii] luminosity functions out toz= 6

Alma Spectroscopic Survey in the Hubble Ultra Deep Field: Co Luminosity Functions and the Evolution of the Cosmic Density of Molecular Gas

On Estimation of Contamination from Hydrogen Cyanide in Carbon Monoxide Line-intensity Mapping

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