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CO and Dust in PSS 2322+1944 at a redshift of 4.12

Cox, P. and Omont, A. and Djorgovski, S. G. and Bertoldi, F. and Pety, J. and Carilli, C. L. and Isaak, K. G. and Beelen, A. and McMahon, R. G. and Castro, S. (2002) CO and Dust in PSS 2322+1944 at a redshift of 4.12. Astronomy and Astrophysics, 387 (2). pp. 406-411. ISSN 0004-6361. doi:10.1051/0004-6361:20020382.

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Using the IRAM interferometer we have detected J = 4 → 3 and 5 → 4 CO line emission toward the radio quiet quasar PSS 2322+1944. At a redshift of z_(CO) = 4.1199 this is the fourth and strongest detection of CO at z > 4. The velocity-integrated CO J = 4 → 3 and J = 5 → 4 line fluxes are 4.21 ± 0.40 and 3.74 ± 0.56 Jy km s^(-1), and the linewidth is ≈ 300 km s^(-1). The CO J = 10 → 9 was searched for but not detected with an upper intensity limit of 30 mJy. The 1.35 mm (250 µm rest wavelength) continuum flux density is 7.5 ± 1.3 mJy, in agreement with previous bolometer measurements at 1.2 mm with the 30-m IRAM telescope. The 3 mm (580 µm rest wavelength) continuum is not detected with a 3 σ upper limit of 0.7 mJy. We also report observations of the 450 µm continuum in PSS 2322+1944 using the SCUBA array at the JCMT. The quasar was detected with a 450 µm flux density of 79 ± 19 mJy. At the angular resolution of 4."8 x 2." at 1.3 mm and 6."2 x 4."9 at 3.2 mm, the interferometer observations do not show evidence of spatial extension in the continuum or CO line emission. Assuming no gravitational magnification, we estimate a molecular gas mass of ≈ 2.5 x 10^(11) M_☉. The molecular gas is warm (40-100K) and dense (10^(3.5) 10^(4.1) cm^(-3). The infrared-to-CO luminosity ratio is ≈185 L_☉ (K km-s^(-1) pc^2)^(-1), comparable to the values found for ultraluminous infrared galaxies. The detection of CO emission in this high redshift QSO provides further evidence that the radio emission and the millimeter to submillimeter continuum emission are predominantly powered by a starburst which is coeval with the AGN activity.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Cox, P.0000-0003-2027-8221
Omont, A.0000-0002-4721-3922
Djorgovski, S. G.0000-0002-0603-3087
Bertoldi, F.0000-0002-1707-1775
Carilli, C. L.0000-0001-6647-3861
Additional Information:© 2002 ESO. Received 11 January 2002. Accepted 8 March 2002. R. Neri and M. Grewing are gratefully acknowledged for their support of this program, and D. Downes for useful discussions. We also thank R. Lucas for help with the data reduction and the referee, A. S. Evans, for comments which improved the contents of this paper. The IRAM Plateau de Bure staff is kindly acknowledged for its efficient assistance. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The JCMT is operated by JAC, Hilo, on behalf of the parent organisations of the Particle Physics and Astronomy Research Council in the UK, the National Research Council in Canada and the Scientific Research Organisation of The Netherlands. The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc. SGD and SMC acknowledge a partial support from the Bressler Foundation.
Funding AgencyGrant Number
Institut national des sciences de l'Univers (INSU)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Instituto Geográfico Nacional (IGN)UNSPECIFIED
Bressler FoundationUNSPECIFIED
Subject Keywords:galaxies: formation - quasars: emission lines - quasars: individual: PSS 2322+1944 - cosmology: observations - cosmology: early Universe - radio lines: galaxies
Issue or Number:2
Record Number:CaltechAUTHORS:20170328-125204254
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Official Citation:CO and Dust in PSS 2322+1944 at a redshift of 4.12 P. Cox, A. Omont, S. G. Djorgov ki, F. Bertoldi, J. Pety, C. L. Carilli, K. G. I aak, A. Beelen, R. G. McMahon and S. Ca tro A&A, 387 2 (2002) 406-411 DOI:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:75480
Deposited By: Ruth Sustaita
Deposited On:28 Mar 2017 21:36
Last Modified:15 Nov 2021 16:33

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