Galaxy formation and evolution

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Measures of star formation rates from Infrared (Herschel) and UV (GALEX) emissions of galaxies in the HerMES fields

(2010)

Authors:

V Buat, E Giovannoli, D Burgarella, B Altieri, A Amblard, V Arumugam, H Aussel, T Babbedge, A Blain, J Bock, A Boselli, N Castro-Rodriguez, A Cava, P Chanial, DL Clements, A Conley, L Conversi, A Cooray, CD Dowell, E Dwek, S Eales, D Elbaz, M Fox, A Franceschini, W Gear, J Glenn, M Griffin, M Halpern, E Hatziminaoglou, S Heinis, E Ibar, K Isaak, RJ Ivison, G Lagache, L Levenson, CJ Lonsdale, N Lu, S Madden, B Maffei, G Magdis, G Mainetti, L Marchetti, GE Morrison, HT Nguyen, B O'Halloran, SJ Oliver, A Omont, FN Owen, MJ Page, M Pannella, P Panuzzo, A Papageorgiou, CP Pearson, I Perez-Fournon, M Pohlen, D Rigopoulou, D Rizzo, IG Roseboom, M Rowan-Robinson, M Sanchez Portal, B Schulz, N Seymour, DL Shupe, AJ Smith, JA Stevens, V Strazzullo, M Symeonidis, M Trichas, KE Tugwell, M Vaccari, E Valiante, I Valtchanov, L Vigroux, L Wang, R Ward, G Wright, CK Xu, M Zemcov
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An excess of star-forming galaxies in the fields of high-redshift QSOs

\mnras 405 (2010) 2623-2638-2623-2638

Authors:

JA Stevens, MJ Jarvis, KEK Coppin, MJ Page, TR Greve, FJ Carrera, RJ Ivison
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Infrared‐correlated 31‐GHz radio emission from Orion East

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 407:4 (2010) 2223-2229

Authors:

C Dickinson, S Casassus, RD Davies, JR Allison, R Bustos, K Cleary, RJ Davis, ME Jones, TJ Pearson, ACS Readhead, R Reeves, AC Taylor, CT Tibbs, RA Watson
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Candidate z~8-9 Galaxies from WFC3 Imaging

(2010)

Authors:

Silvio Lorenzoni, Andrew Bunker, Stephen Wilkins, Elizabeth Stanway, Matt Jarvis, Joseph Caruana
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Measuring the low mass end of the Mbh - sigma relation

AIP Conference Proceedings AIP Publishing 1240 (2010) 215

Authors:

D Krajnovic, Rm McDermid, Michele Cappellari, Roger Davies

Abstract:

We show that high quality laser guide star (LGS) adaptive optics (AO) observations of nearby early-type galaxies are possible when the tip-tilt correction is done by guiding on nuclei while the focus compensation due to the changing distance to the sodium layer is made 'open loop'. We achieve corrections such that 40% of flux comes from R<0.2 arcsec. To measure a black hole mass (Mbh) one needs integral field observations of both high spatial resolution and large field of view. With these data it is possible to determine the lower limit to Mbh even if the spatial resolution of the observations are up to a few times larger than the sphere of influence of the black hole.
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