Michele Cappellari: Publications

The SAURON project - XVII. Stellar population analysis of the absorption line strength maps of 48 early-type galaxies

(2010)

Authors:

Harald Kuntschner, Eric Emsellem, Roland Bacon, Michele Cappellari, Roger L Davies, P Tim de Zeeuw, Jesús Falcón-Barroso, Davor Krajnović, Richard M McDermid, Reynier F Peletier, Marc Sarzi, Kristen L Shapiro, Remco CE van den Bosch, Glenn van de Ven

Formation of slowly rotating early-type galaxies via major mergers: a Resolution 51��

(2010)

Authors:

M Bois, F Bournaud, E Emsellem, K Alatalo, L Blitz, M Bureau, M Cappellari, RL Davies, TA Davis, PT de Zeeuw, P-A Duc, S Khochfar, D Krajnovic, H Kuntschner, P-Y Lablanche, RM McDermid, R Morganti, T Naab, T Oosterloo, M Sarzi, N Scott, P Serra, A Weijmans, LM Young

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

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

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.

51��