Publications by Michele Cappellari


A precise benchmark for cluster scaling relations: fundamental plane, mass plane and IMF in the coma cluster from dynamical models

Monthly Notices of the Royal Astronomical Society Oxford University Press (0)

S Shetty, M Cappellari, RM McDermid, D Krajnovic, PT de Zeeuw, RL Davies, C Kobayashi


First Gaia dynamical model of the Milky Way disc with six phase space coordinates: a test for galaxy dynamics

Monthly Notices of the Royal Astronomical Society Oxford University Press (0)

M Nitschai, M Cappellari, N Neumayer


An Oxford SWIFT Integral Field Spectroscopy study of 14 early-type galaxies in the Coma cluster

ArXiv (0)

N Scott, RCW Houghton, RL Davies, M Cappellari, N Thatte, FJ Clarke, M Tecza

As a demonstration of the capabilities of the new Oxford SWIFT integral field spectrograph, we present first observations for a set of 14 early-type galaxies in the core of the Coma cluster. Our data consist of I- and z-band spatially resolved spectroscopy obtained with the Oxford SWIFT spectrograph, combined with r-band photometry from the SDSS archive for 14 early- type galaxies. We derive spatially resolved kinematics for all objects from observations of the calcium triplet absorption features at \sim 8500 {AA} . Using this kinematic information we classify galaxies as either Fast Rotators or Slow Rotators. We compare the fraction of fast and slow rotators in our sample, representing the densest environment in the nearby Universe, to results from the ATLAS3D survey, finding the slow rotator fraction is \sim 50 per cent larger in the core of the Coma cluster than in the Virgo cluster or field, a 1.2 {\sigma} increase given our selection criteria. Comparing our sample to the Virgo cluster core only (which is 24 times less dense than the Coma core) we find no evidence of an increase in the slow rotator fraction. Combining measurements of the effective velocity dispersion {\sigma_e} with the photometric data we determine the Fundamental Plane for our sample of galaxies. We find the use of the average velocity dispersion within 1 effective radius, {\sigma_e}, reduces the residuals by 13 per cent with respect to comparable studies using central velocity dispersions, consistent with other recent integral field Fundamental Plane determinations.


Circumnuclear Keplerian disks in galaxies

ASTR SOC P 182 (1999) 229-230

JG Funes, F Bertola, M Cappellari, EM Corsini, A Pizzella, JCV Beltran


Searching for low-mass supermassive black holes

IAU SYMP (1999) 422-423

M Cappellari, F Bertola, EM Corsini, JG Funes, A Pizzella, JCV Beltran


Circumnuclear Keplerian disks in galaxies

ASTROPHYSICAL JOURNAL 509 (1998) L93-L96

F Bertola, M Cappellari, JG Funes, EM Corsini, A Pizzella, JCV Beltran


UV imaging of the galaxy cluster CL0939+72 at z similar to 0.4

ASTR SOC P 146 (1998) 488-491

LM Buson, F Bertola, M Cappellari, C Chiosi, A Dressler, A Oemler


The variable UV central spike of NGC 4552

ASTR SOC P 117 (1997) 545-549

M Cappellari, D Burstein, LM Buson, SD Alighieri, L Greggio, A Renzini, J Funes, F Bertola

The nature of the UV-bright spike at the center of the otherwise normal galaxy NGC 4552 is investigated by means of both Hubble Space Telescope (HST) imaging (FOC) and spectroscopy (FOS). This central feature-which underwent a recent dramatic UV flare-provides a potential new tool for revealing the presence of massive black holes in normal galaxies. In particular the sub-arcsec FOS spectra of the nucleus suggest that NGC 4552 does harbor an object with mass M > 4 x 10(8) M. within the central 2 pc.


AN ULTRAVIOLET FLARE AT THE CENTER OF THE ELLIPTIC GALAXY NGC4552

NATURE 378 (1995) 39-41

A RENZINI, L GREGGIO, SD ALIGHIERI, M CAPPELLARI, D BURSTEIN, F BERTOLA


Anisotropic Jeans models of stellar kinematics: second moments including proper motions and radial velocities

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M Cappellari

This is an addendum to the paper by Cappellari (2008, MNRAS, 390, 71), which presented a simple and efficient method to model the stellar kinematics of axisymmetric stellar systems. The technique reproduces well the integral-field kinematics of real galaxies. It allows for orbital anisotropy (three-integral distribution function), multiple kinematic components, supermassive black holes and dark matter. The paper described the derivation of the projected second moments and we provided a reference software implementation. However only the line-of-sight component was given in the paper. For completeness we provide here all the six projected second moments, including radial velocities and proper motions. We present a test against realistic N-body galaxy simulations.


Voronoi binning: Optimal adaptive tessellations of multi-dimensional data

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MICHELE Cappellari

We review the concepts of the Voronoi binning technique (Cappellari & Copin 2003), which optimally solves the problem of preserving the maximum spatial resolution of general two-dimensional data, given a constraint on the minimum signal-to-noise ratio (S/N). This is achieved by partitioning the data in an adaptive fashion using a Voronoi tessellation with nearly hexagonal lattice. We review astrophysical applications of the method to X-ray data, integral-field spectroscopy, Fabry-Perot interferometry, N-body simulations, standard images and other regularly or irregularly sampled data. Voronoi binning, unlike adaptive smoothing, produces maps where the noise in the data can be visually assessed and spurious artifacts can be recognized. The method can be used to bin data according to any general criterion and not just S/N. It can be applied to higher dimensions and it can be used to generate optimal adaptive meshes for numerical simulations.


Dynamical modeling of SAURON galaxies

Proceedings of IUTAM Symposia and Summer Schools IUTAM 3 (0)

M Cappellari, RCEVD Bosch, EK Verolme, R Bacon, M Bureau, Y Copin, RL Davies, E Emsellem, D Krajnovic, H Kuntschner, R McDermid, BW Miller, RF Peletier, PTD Zeeuw

<p style="text-align:justify;"> We describe our program for the dynamical modeling of early-type galaxies observed with the panoramic integral-field spectrograph SAURON. We are using Schwarzschild's numerical orbit superposition method to reproduce in detail all kinematical and photometric observables, and recover the intrinsic orbital structure of the galaxies. Since catastrophes are the most prominent features in the orbital observables, two-dimensional kinematical coverage is essential to constrain the dynamical models. </p>


The sixteenth data release of the Sloan Digital Sky Surveys: first release from the APOGEE-2 Southern Survey and full release of eBOSS spectra

Astrophysical Journal Supplement American Astronomical Society (0)

R Ahumada, C Allende Prieto, A Almeida, M Bureau, M Cappellari, R Davies, E-M Mueller, R Smethurst, SDSS-IVC SDSS-IV Collaboration

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