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A z=1.82 Analog of Local Ultra-massive Elliptical Galaxies

(2010)

Authors:

M Onodera, E Daddi, R Gobat, M Cappellari, N Arimoto, A Renzini, Y Yamada, HJ McCracken, C Mancini, P Capak, M Carollo, A Cimatti, M Giavalisco, O Ilbert, X Kong, S Lilly, K Motohara, K Ohta, DB Sanders, N Scoville, N Tamura, Y Taniguchi

HiZELS: the High Redshift Emission Line Survey with UKIRT

(2010)

Authors:

Philip Best, Ian Smail, David Sobral, Jim Geach, Timothy Garn, Rob Ivison, Jaron Kurk, Gavin Dalton, Michele Cirasuolo, Mark Casali

The NGC 404 Nucleus: Star Cluster and Possible Intermediate Mass Black Hole

(2010)

Authors:

Anil C Seth, Michele Cappellari, Nadine Neumayer, Nelson Caldwell, Nate Bastian, Knut Olsen, Robert D Blum, Victor P Debattista, Richard McDermid, Thomas Puzia, Andrew Stephens

Temporal pixel multiplexing for simultaneous high-speed, high-resolution imaging.

Nat Methods 7:3 (2010) 209-211

Authors:

Gil Bub, Matthias Tecza, Michiel Helmes, Peter Lee, Peter Kohl

Abstract:

We introduce an imaging modality that, by offsetting pixel-exposure times during capture of a single image frame, embeds temporal information in each frame. This allows simultaneous acquisition of full-resolution images at native detector frame rates and high-speed image sequences at reduced resolution, without increasing bandwidth requirements. We demonstrate this method using macroscopic and microscopic examples, including imaging calcium transients in heart cells at 250 Hz using a 10-Hz megapixel camera.

Measuring the low mass end of the Mbh - sigma relation

(2010)

Authors:

Davor Krajnovic, Michele Cappellari, Richard M McDermid, Roger L 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.