Cookies

We use cookies to ensure that we give you the best experience on our website. You can change your cookie settings at any time. Otherwise, we'll assume you're OK to continue.

Durham University

Department of Physics

Staff profile

Publication details for Professor Ian Smail

Decarli, R., Walter, F., Aravena, M., Carilli, C., Bouwens, R., da Cunha, E., Daddi, E., Ivison, R.J., Popping, G., Riechers, D., Smail, I.R., Swinbank, M., Weiss, A., Anguita, T., Assef, R.J., Bauer, F.E., Bell, E.F., Bertoldi, F., Chapman, S., Colina, L., Cortes, P.C., Cox, P., Dickinson, M., Elbaz, D., Gónzalez-López, J., Ibar, E., Infante, L., Hodge, J., Karim, A., Le Fevre, O., Magnelli, B., Neri, R., Oesch, P., Ota, K., Rix, H.-W., Sargent, M., Sheth, K., van der Wel, A., van der Werf, P. & Wagg, J. (2016). ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: CO Luminosity Functions and the Evolution of the Cosmic Density of Molecular Gas. The Astrophysical Journal 833(1): 69.

Author(s) from Durham

Abstract

In this paper we use ASPECS, the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field in band 3 and band 6, to place blind constraints on the CO luminosity function and the evolution of the cosmic molecular gas density as a function of redshift up to z ~ 4.5. This study is based on galaxies that have been selected solely through their CO emission and not through any other property. In all of the redshift bins the ASPECS measurements reach the predicted "knee" of the CO luminosity function (around 5 × 109 K km s−1 pc2). We find clear evidence of an evolution in the CO luminosity function with respect to z ~ 0, with more CO-luminous galaxies present at z ~ 2. The observed galaxies at z ~ 2 also appear more gas-rich than predicted by recent semi-analytical models. The comoving cosmic molecular gas density within galaxies as a function of redshift shows a drop by a factor of 3–10 from z ~ 2 to z ~ 0 (with significant error bars), and possibly a decline at z > 3. This trend is similar to the observed evolution of the cosmic star formation rate density. The latter therefore appears to be at least partly driven by the increased availability of molecular gas reservoirs at the peak of cosmic star formation (z ~ 2).