Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-34426
Devriendt, J; Rimes, C; Pichon, C; Teyssier, R; Le Borgne, D; Aubert, D; Audit, E; Colombi, S; Courty, S; Dubois, Y; Prunet, S; Rasera, Y; Slyz, A; Tweed, D (2010). The dusty, albeit ultraviolet bright, infancy of galaxies. Monthly Notices of the Royal Astronomical Society, 403(1):L84-L88.
View at publisher
The largest galaxies acquire their mass early on, when the Universe is still youthful. Cold streams violently feed these young galaxies a vast amount of fresh gas, resulting in very efficient star formation. Using a well resolved hydrodynamical simulation of galaxy formation, we demonstrate that these mammoth galaxies are already in place a couple of billion years after the big bang. Contrary to local star-forming galaxies, where dust re-emits a large part of the stellar ultraviolet (UV) light at infrared and sub-millimetre wavelengths, our self-consistent modelling of dust extinction predicts that a substantial fraction of UV photons should escape from primordial galaxies. Such a model allows us to compute reliably the number of high-redshift objects as a function of luminosity, and yields galaxies whose UV luminosities closely match those measured in the deepest observational surveys available. This agreement is remarkably good considering our admittedly still simple modelling of the interstellar medium physics. The luminosity functions of virtual UV luminous galaxies coincide with the existing data over the whole redshift range from 4 to 7, provided cosmological parameters are set to their currently favoured values. Despite their considerable emission at short wavelengths, we anticipate that the counterparts of the brightest UV galaxies will be detected by future sub-millimetre facilities like ALMA.
7 downloads since deposited on 02 Mar 2011
5 downloads since 12 months
|Item Type:||Journal Article, refereed, original work|
|Communities & Collections:||07 Faculty of Science > Institute for Computational Science|
|Dewey Decimal Classification:||530 Physics|
|Deposited On:||02 Mar 2011 15:42|
|Last Modified:||28 Feb 2014 12:43|
|Additional Information:||The definitive version is available at www.blackwell-synergy.com|
Users (please log in): suggest update or correction for this item
Repository Staff Only: item control page