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Issue A&A
Volume 428, Number 3, December IV 2004
Page(s) L21 - L24
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:200400096



A&A 428, L21-L24 (2004)
DOI: 10.1051/0004-6361:200400096

Letter

Atomic carbon in PSS 2322+1944, a quasar at redshift $\mathsf{4.12}$

J. Pety1, 2, A. Beelen3, P. Cox3, D. Downes1, A. Omont4, F. Bertoldi5 and C. L. Carilli6

1  IRAM, 300 rue de la Piscine, 38406 St-Martin-d'Hères, France
    e-mail: pety@iram.fr
2  LERMA, Observatoire de Paris, 75014 Paris, France
3  Institut d'Astrophysique Spatiale, Université de Paris Sud, 91405 Orsay Cedex, France
4  Institut d'Astrophysique de Paris, CNRS and Université de Paris VI, 98bis Bd. Arago, 75014 Paris, France
5  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
6  National Radio Astronomy Observatory, PO Box, Socorro, NM 87801, USA

(Received 22 September 2004 / Accepted 30 October 2004)

Abstract
We report the detection of the $^3{\rm P}_1\to{}^3{\rm P}_0$ fine-structure line of neutral carbon in the z=4.12 quasar PSS 2322+1944, obtained at the IRAM Plateau de Bure interferometer. The [CI] $^3{\rm P}_1-^3{\rm P}_0$ line is detected with a signal-to-noise ratio of ~6 with a peak intensity of $\approx$2.5 mJy and a velocity-integrated line flux of $\rm0.81 \pm 0.12 \, Jy \, km \, s^{-1}$ . Assuming an excitation temperature of 43 K (equal to the dust temperature), we derive a mass of neutral carbon (corrected for magnification) of $M_{\rm C \sc I} \approx 1.2 \times 10^7~M_\odot$. In PSS 2322+1944, the cooling due to C is about 6 times smaller than for CO, whereas the CO and C cooling represents $\approx$ 10-4 of the far-infrared continuum and more than half of the cooling due to C +.


Key words: galaxies: formation -- galaxies: starburst -- galaxies: high-redshift -- quasars: emission lines -- quasars: individual: PSS 2322+1944 -- cosmology: observations

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© ESO 2004


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