Volume 608, December 2017
|Number of page(s)||9|
|Section||Cosmology (including clusters of galaxies)|
|Published online||01 December 2017|
1 INAF Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34143 Trieste, Italy
2 Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa, Italy
3 INAF Osservatorio Astronomico di Roma, via Frascati 33, 00078 Monteporzio Catone, Italy
4 Universitá degli Studi di Roma “Tor Vergata”, via Orazio Raimondo 18, 00173 Roma, Italy
5 Cavendish Laboratory, University of Cambridge, 19 J.J. Thomson Ave., Cambridge CB3 0HE, UK
6 IRAM – Institut de RadioAstronomie Millimétrique, 300 rue de la Piscine, 38406 Saint Martin d’ Hères, France
7 Université Grenoble Alpes, IPAG, 38000 Grenoble, France
8 INAF Osservatorio Astronomico di Brera, via Brera 28, 20121 Milan, Italy
9 Kavli Insitute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
10 Dipartimento di Fisica e Astronomia, Universitá degli Studi di Bologna, viale Berti Pichat 6/2, 40127 Bologna, Italy
Received: 14 June 2017
Accepted: 20 September 2017
We have performed a high sensitivity observation of the UFO/BAL quasar APM 08279+5255 at z = 3.912 with NOEMA at 3.2 mm, aimed at detecting fast moving molecular gas. We report the detection of blueshifted CO(4−3) with maximum velocity (v95%) of −1340 km s-1, with respect to the systemic peak emission, and a luminosity of L′ = 9.9 × 109μ-1 K km s-1 pc-2, where μ is the lensing magnification factor. We discuss various scenarios for the nature of this emission and conclude that this is the first detection of fast molecular gas at redshift > 3. We derived a mass flow rate of molecular gas in the range Ṁ = 3−7.4 × 103M⊙/yr and momentum boost ṖOF/ṖAGN ~ 2−6, which is therefore consistent with a momentum conserving flow. For the largest ṖOF the scaling is also consistent with an energy conserving flow with an efficiency of ~10−20%. The present data can hardly discriminate between the two expansion modes. The mass loading factor of the molecular outflow η = ṀOF/SFR is ≫ 1. We also detected a molecular emission line at a frequency of 94.83 GHz corresponding to a rest-frame frequency of 465.8 GHz; we tentatively identified this frequency with the cation molecule N2H+(5−4), which would be the first detection of this species at high redshift. We discuss the alternative possibility that this emission is due to a CO emission line from the, so far undetected, lens galaxy. Further observations of additional transitions of the same species with NOEMA can discriminate between the two scenarios.
Key words: galaxies: active / quasars: emission lines / submillimeter: ISM / X-rays: individuals: APM 08279+5255 / quasars: individual: APM 08279+5255 / quasars: general
This work is based on observations carried out under project numbers S15CW and E15AF with the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).
The reduced spectrum (FITS file) is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/608/A30
© ESO, 2017
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