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Carilli, Anthony M.; Dempster, Gregory M.

doi:10.1023/a:1011985113936

Cited by 51 publications

(4 citation statements)

References 5 publications

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“…The adopted values are consistent with independent results of recent infrared modelling of spiral galaxies. With this model we also obtain Sf r ≃ 0.57 10 −28 F 1.4GHz (erg/s/Hz), in good agreement with the one obtained by Carilli (2001). In the analysis of a sample of compact ULIRGS (Condon et al, 1991), we adopt larger obscuration times and a visual extinction of A V =10mag, as implied by optical and UV properties of observed SEDs of a few ULIRGS.…”

supporting

confidence: 85%

FIR and Radio Emission in Star Forming Galaxies

Bressan

Granato²,

Silva

2001

QSO Hosts and Their Environments

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supporting

confidence: 85%

FIR and Radio Emission in Star Forming Galaxies

Bressan

Granato²,

Silva

2001

QSO Hosts and Their Environments

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“…Carilli et al (2010), reported the detection of the CO[1−0] and CO[2−1] lines with the Very Large Array (VLA), and CO[6−5] and CO[5−4] lines with the Plateau de Bure Interferometer (PdBI) and the Combined Array for Research in Millimeter Astronomy (CARMA) respectively. The source is detected in the Aztec 1.1 mm map and continuum emission is also measured at 2.2-, 3.3-, and 6.6 mm (Carilli et al 2011) and at 1.4 GHz with the VLA (Morrison et al 2009). GN20 is identified in all IRAC bands and at 24 µm while it appears as a B-band dropout in the ACS-HST image.…”

Section: Sample and Observationsmentioning

confidence: 98%

GOODS- HERSCHEL : GAS-TO-DUST MASS RATIOS AND CO-TO-H ₂ CONVERSION FACTORS IN NORMAL AND STARBURSTING GALAXIES AT HIGH- z

Magdis

Daddi

Elbaz

et al. 2011

ApJ

152

195

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We explore the gas-to-dust mass ratio (M gas /M d ) and the CO luminosityto-M gas conversion factor (α CO ) of two well studied galaxies in the GOODS-N field, that are expected to have different star forming modes, the starburst GN20 at z = 4.05 and the normal star-forming galaxy BzK-21000 at z = 1.52. Detailed sampling is available for their Rayleigh-Jeans emission via ground based mm interferometry (1.1 − 6.6 mm) along with Herschel PACS and SPIRE data that probe the peak of their infrared emission. Using the physically motivated Draine & Li (2007) models, as well as a modified black body function, we measure the dust mass (M dust ) of the sources and find (2.0 +0.7 −0.6 × 10 9 ) M ⊙ for GN20 and (8.6 +0.6 −0.9 × 10 8 ) M ⊙ for BzK-21000. The addition of mm data reduces the uncertainties of the derived M dust by a factor of ∼ 2, allowing the use of the local M gas /M d vs metallicity relation to place constraints on the α CO values of the -2two sources. For GN20 we derive a conversion factor of α CO < 1.0 M ⊙ pc −2 (K km s −1 ) −1 , consistent with that of local ULIRGs, while for BzK-21000 we find a considerably higher value, α CO ∼ 4.0 M ⊙ pc −2 (K km s −1 ) −1 , in agreement with an independent kinematic derivation reported previously. The implied star formation efficiency is ∼ 25 L ⊙ /M ⊙ for BzK-21000, a factor of ∼ 5 − 10 lower than that of GN20. The findings for these two sources support the existence of different disk-like and starburst star-formation modes in distant galaxies, although a larger sample is required to draw statistically robust results.

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“…Berta et al 2013). The state-of-the-art Atacama Large (Sub)Millimeter Array (ALMA) will make it possible in the next future to directly follow the molecular gas abundance as a function of redshift with blind searches of carbon monoxide (CO) rotational transitions (e.g Carilli & Walter 2013, and references therein). So far, only a handful of observational works have attempted to constrain this quantity.…”

Section: Introductionmentioning

confidence: 99%

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

Vallini

Gruppioni

Pozzi

et al. 2015

Monthly Notices of the Royal Astronomical Society: Letters

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We derive the CO luminosity function (LF) for different rotational transitions (i.e.(1-0), (3-2), (5-4)) starting from the Herschel LF by Gruppioni et al. and using appropriate L CO − L IR conversions for different galaxy classes. Our predicted LFs fit the data so far available at z ≈ 0 and 2. We compare our results with those obtained by semi-analytical models (SAMs): while we find a good agreement over the whole range of luminosities at z ≈ 0, at z ≈ 1 and z ≈ 2 the tension between our LFs and SAMs in the faint and bright ends increases. We finally discuss the contribution of luminous AGN (L X > 10 44 erg s −1 ) to the bright end of the CO LF concluding that they are too rare to reproduce the actual CO luminosity function at z ≈ 2.

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Untitled

Cited by 51 publications

References 5 publications

FIR and Radio Emission in Star Forming Galaxies

FIR and Radio Emission in Star Forming Galaxies

GOODS- HERSCHEL : GAS-TO-DUST MASS RATIOS AND CO-TO-H ₂ CONVERSION FACTORS IN NORMAL AND STARBURSTING GALAXIES AT HIGH- z

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

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Untitled

Cited by 51 publications

References 5 publications

FIR and Radio Emission in Star Forming Galaxies

FIR and Radio Emission in Star Forming Galaxies

GOODS- HERSCHEL : GAS-TO-DUST MASS RATIOS AND CO-TO-H 2 CONVERSION FACTORS IN NORMAL AND STARBURSTING GALAXIES AT HIGH- z

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

Contact Info

Product

Resources

About

GOODS- HERSCHEL : GAS-TO-DUST MASS RATIOS AND CO-TO-H ₂ CONVERSION FACTORS IN NORMAL AND STARBURSTING GALAXIES AT HIGH- z