Discovery of a Perseus-like cloud in the early Universe

H I-to-H₂ transition, carbon monoxide and small dust grains at z_abs≈ 2.53 towards the quasar J0000+0048^⋆

¹ Institut d’Astrophysique de Paris, CNRS-UPMC, UMR 7095, 98bis boulevard Arago, 75014 Paris, France
e-mail: noterdaeme@iap.fr
² Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark
³ Ioffe Physical-Technical Institute of RAS, Polyteknicheskaya 26, 194021 Saint-Petersburg, Russia
⁴ Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, 32611, USA
⁵ Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, 411 007 Pune, India
⁶ Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany
⁷ European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago 19, Chile
⁸ Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Melbourne, 3122 Victoria, Australia
⁹ Laboratoire d’Astrophysique de Marseille, CNRS/Aix Marseille Université, UMR 7326, 13388 Marseille, France
¹⁰ Department of Physics and Astronomy, LaserLaB, Vrije Universiteit, De Boelelaan 1081, 1081 HV Amsterdam, The Netherlands

Received: 23 June 2016
Accepted: 2 September 2016

Abstract

We present the discovery of a molecular cloud at z_abs ≈ 2.5255 along the line of sight to the quasar SDSS J 000015.17+004833.3. We use a high-resolution spectrum obtained with the Ultraviolet and Visual Echelle Spectrograph together with a deep multi-wavelength medium-resolution spectrum obtained with X-shooter (both on the Very Large Telescope) to perform a detailed analysis of the absorption lines from ionic, neutral atomic and molecular species in different excitation levels, as well as the broad-band dust extinction. We find that the absorber classifies as a Damped Lyman-α system (DLA) with log N(H i) (cm^-2) = 20.8 ± 0.1. The DLA has super-solar metallicity (Z ~ 2.5 Z_⊙, albeit to within a factor of two to three) with a depletion pattern typical of cold gas and an overall molecular fraction f = 2N(H₂)/(2N(H₂) + N(H i)) ~ 50%. This is the highest f-value observed to date in a high-z intervening system. Most of the molecular hydrogen arises from a clearly identified narrow (b ~ 0.7km s^-1), cold component in which carbon monoxide molecules are also found, with log N(CO)≈ 15. With the help of the spectral synthesis code Cloudy, we study the chemical and physical conditions in the cold gas. We find that the line of sight probes the gas deep after the H i-to-H₂ transition in a ~4−5 pc-size cloud with volumic density n_H ~ 80 cm^-3 and temperature of only 50 K. Our model suggests that the presence of small dust grains (down to about 0.001 μm) and high cosmic ray ionisation rate (ζ_H ~ a few times 10^-15 s^-1) are needed to explain the observed atomic and molecular abundances. The presence of small grains is also in agreement with the observed steep extinction curve that also features a 2175 Å bump. Interestingly, the chemical and physical properties of this cloud are very similar to what is seen in diffuse molecular regions of the nearby Perseus complex, despite the former being observed when the Universe was only 2.5 Gyr old. The high excitation temperature of CO rotational levels towards J0000+0048 betrays however the higher temperature of the cosmic microwave background. Using the derived physical conditions, we correct for a small contribution (0.3 K) of collisional excitation and obtain T_CMB(z = 2.53) ≈ 9.6 K, in perfect agreement with the predicted adiabatic cooling of the Universe.