ALBERT

Beschreibung: The extragalactic background light at far-infrared wavelengths comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year. These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations. A previous attempt at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model. Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 mum. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, M(min), such that log(10)[M(min)/M(middle dot in circle)] = 11.5(+0.7)(-0.2) at 350 mum, where M(middle dot in circle) is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe, and is lower than that predicted by semi-analytical models for galaxy formation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Amblard, Alexandre -- Cooray, Asantha -- Serra, Paolo -- Altieri, B -- Arumugam, V -- Aussel, H -- Blain, A -- Bock, J -- Boselli, A -- Buat, V -- Castro-Rodriguez, N -- Cava, A -- Chanial, P -- Chapin, E -- Clements, D L -- Conley, A -- Conversi, L -- Dowell, C D -- Dwek, E -- Eales, S -- Elbaz, D -- Farrah, D -- Franceschini, A -- Gear, W -- Glenn, J -- Griffin, M -- Halpern, M -- Hatziminaoglou, E -- Ibar, E -- Isaak, K -- Ivison, R J -- Khostovan, A A -- Lagache, G -- Levenson, L -- Lu, N -- Madden, S -- Maffei, B -- Mainetti, G -- Marchetti, L -- Marsden, G -- Mitchell-Wynne, K -- Nguyen, H T -- O'Halloran, B -- Oliver, S J -- Omont, A -- Page, M J -- Panuzzo, P -- Papageorgiou, A -- Pearson, C P -- Perez-Fournon, I -- Pohlen, M -- Rangwala, N -- Roseboom, I G -- Rowan-Robinson, M -- Portal, M Sanchez -- Schulz, B -- Scott, Douglas -- Seymour, N -- Shupe, D L -- Smith, A J -- Stevens, J A -- Symeonidis, M -- Trichas, M -- Tugwell, K -- Vaccari, M -- Valiante, E -- Valtchanov, I -- Vieira, J D -- Vigroux, L -- Wang, L -- Ward, R -- Wright, G -- Xu, C K -- Zemcov, M -- England -- Nature. 2011 Feb 24;470(7335):510-2. doi: 10.1038/nature09771. Epub 2011 Feb 16.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics & Astronomy, University of California, Irvine, California 92697, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21326201" target="_blank"〉PubMed〈/a〉

Beschreibung: The old, red stars that constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly as a result of accretion onto black holes. It is widely suspected, but unproved, that the tight correlation between the mass of the black hole and the mass of the stellar bulge results from the AGN quenching the surrounding star formation as it approaches its peak luminosity. X-rays trace emission from AGN unambiguously, whereas powerful star-forming galaxies are usually dust-obscured and are brightest at infrared and submillimetre wavelengths. Here we report submillimetre and X-ray observations that show that rapid star formation was common in the host galaxies of AGN when the Universe was 2-6 billion years old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 10(44) ergs per second. This suppression of star formation in the host galaxy of a powerful AGN is a key prediction of models in which the AGN drives an outflow, expelling the interstellar medium of its host and transforming the galaxy's properties in a brief period of cosmic time.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Page, M J -- Symeonidis, M -- Vieira, J D -- Altieri, B -- Amblard, A -- Arumugam, V -- Aussel, H -- Babbedge, T -- Blain, A -- Bock, J -- Boselli, A -- Buat, V -- Castro-Rodriguez, N -- Cava, A -- Chanial, P -- Clements, D L -- Conley, A -- Conversi, L -- Cooray, A -- Dowell, C D -- Dubois, E N -- Dunlop, J S -- Dwek, E -- Dye, S -- Eales, S -- Elbaz, D -- Farrah, D -- Fox, M -- Franceschini, A -- Gear, W -- Glenn, J -- Griffin, M -- Halpern, M -- Hatziminaoglou, E -- Ibar, E -- Isaak, K -- Ivison, R J -- Lagache, G -- Levenson, L -- Lu, N -- Madden, S -- Maffei, B -- Mainetti, G -- Marchetti, L -- Nguyen, H T -- O'Halloran, B -- Oliver, S J -- Omont, A -- Panuzzo, P -- Papageorgiou, A -- Pearson, C P -- Perez-Fournon, I -- Pohlen, M -- Rawlings, J I -- Rigopoulou, D -- Riguccini, L -- Rizzo, D -- Rodighiero, G -- Roseboom, I G -- Rowan-Robinson, M -- Sanchez Portal, M -- Schulz, B -- Scott, D -- Seymour, N -- Shupe, D L -- Smith, A J -- Stevens, J A -- Trichas, M -- Tugwell, K E -- Vaccari, M -- Valtchanov, I -- Viero, M -- Vigroux, L -- Wang, L -- Ward, R -- Wright, G -- Xu, C K -- Zemcov, M -- England -- Nature. 2012 May 9;485(7397):213-6. doi: 10.1038/nature11096.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK. mjp@mssl.ucl.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22575961" target="_blank"〉PubMed〈/a〉