Kinematic properties of early-type galaxy haloes using planetary nebulae

By L. Coccato, O. Gerhard, M. Arnaboldi, P. Das, N. Douglas, K. Kuijken, M. Merrifield, N. Napolitano, E. Noordermeer, A. Romanowsky and 3 more. 2008

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We present new planetary nebulae (PNe) positions, radial velocities and magnitudes for six early-type galaxies obtained with the Planetary Nebulae Spectrograph (PNS), along with derived two-dimensional velocity and velocity dispersion fields, and the α parameters (i.e. the number of PNe per unit luminosity). We also present new deep absorption-line long-slit kinematics for three galaxies in the sample, obtained with the FOcal Reducer and low dispersion Spectrograph (FORS2) at the Very Large Telescope (VLT). We extend this study to include additional 10 early-type galaxies with PNe radial velocity measurements available from the literature, including previous PNS studies, in order to obtain a broader description of the outer-halo kinematics in early-type galaxies. These data extend the information derived from stellar absorption-line kinematics to typically several and up to 8 effective radii. The combination of photometry, absorption-line and PNe kinematics shows (i) a good agreement between the PNe number density distribution and the stellar surface brightness in the region where the two data sets overlap; (ii) a good agreement between PNe and absorption-line kinematics; (iii) that the mean rms velocity profiles fall into two groups, with part of the galaxies characterized by slowly decreasing profiles and the remainder having steeply falling profiles; (iv) a larger variety of velocity dispersion radial profiles; (v) that twists and misalignments in the velocity fields are more frequent at large radii, including some fast rotator galaxies; (vi) that outer haloes are characterized by more complex radial profiles of the specific angular momentum-related λ_R parameter than observed within 1 R_e; (vii) that many objects are more rotationally dominated at large radii than in their central parts and (viii) that the halo kinematics are correlated with other galaxy properties, such as total B band and X-ray luminosity, isophotal shape, total stellar mass, V/σ and α parameter, with a clear separation between fast and slow rotators. Based in part on observations made with the William Herschel Telescope operated by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos on the island of La Palma, of the Instituto de Astrofisica de Canarias, and on observations collected at the European Southern Observatory, Chile, Program: 76.B-0788(A). E-mail: lcoccato@mpe.mpg.de

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6df0cacc4797608ccc9c4eea6140dad27ed3f029

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WIDE-FIELD PRECISION KINEMATICS OF THE M87 GLOBULAR CLUSTER SYSTEM (2011, background): “…found via number density, chemical, and kinematical transitions in the halos of various nearby galaxies (Searle & Zinn 1978; Carollo et al. 2007; Coccato et al. 2009, 2010; Proctor et al. 2009; Alves-Brito et al. 2009; Forbes et al. 2011; Huxor et al. 2011; Arnold et al. 2011), but BCGs provide…”
ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED (2012, methodology): “Seven of these galaxies were chosen because of the availability of high-quality extended kinematic data using integrated stellar light spectroscopy from two recent papers (Coccato et al. 2009; Proctor et al. 2009).”
Simulations of binary galaxy mergers and the link with fast rotators, slow rotators, and kinematically distinct cores (2011, background): “New promising techniques are emerging which should allow us to explore the faint outer stellar structures of larger samples of ETGs (see e.g. Weijmans et al. 2009; Coccato et al. 2009; Proctor et al. 2009; Murphy, Gebhardt & Adams 2011, or the SAGES project).”
The ATLAS3D project - II. Morphologies, kinemetric features and alignment between photometric and kinematic axes of early-type galaxies (2011, background): “…kinematics even farther out one would start measuring larger misalignments as suggested by studies of planetary nebulae around early-type galaxies (Coccato et al. 2009), although these and similar studies also find galaxies that stay (approximately) aligned (Coccato et al. 2009; Proctor et al.…”
The ATLAS3D project – III. A census of the stellar angular momentum within the effective radius of early‐type galaxies: unveiling the distribution of fast and slow rotators (2011, background): “Galaxies with KDCs (group c) can be both discy or boxy.”
Galaxy Masses: A Review (2013, background): “2011) or planetary nebulae (Douglas et al. 2007; Romanowsky et al. 2009; Coccato et al. 2009; Napolitano et al. 2011) become essential, even though these populations are often scarce.”
On the correlations between galaxy properties and supermassive black hole mass (2011, methodology): “…the value of Vc derived from dynamical modelling (IC 1459; Samurović & Danziger 2005; NGC 1052, Binney, Davies & Illingworth 1990; NGC 3115, Bender, Saglia & Gerhard 1994; NGC 3608, Coccato et al. 2009; NGC 4314, Quillen, Frogel & Gonzalez 1994; and nine ellipticals in Kronawitter et al. 2000).”
The SLUGGS Survey: kinematics for over 2500 globular clusters in 12 early-type galaxies (2012, methodology): “…Astronomical Society Coccato, Gerhard & Arnaboldi 2010), the pioneering technique of Proctor et al. (2009) and Norris et al. (2008) that probed the 2D stellar kinematics to 3Reff , and extragalactic planetary nebulae (PNe, Coccato et al. 2009) that can probe the galaxy potential up to ∼10Reff .”
Two-dimensional kinematics of SLACS lenses – III. Mass structure and dynamics of early-type lens galaxies beyond z ≃ 0.1 (2011, background): “…stellar kinematics — different tracers such as planetary nebulae and globular cluster kinematics (e.g. Côté et al. 2003; Romanowsky et al. 2003, 2009; Coccato et al. 2009; de Lorenzi et al. 2009; Napolitano et al.2009; Rodionov & Athanassoula 2011), the occasional H I gas disk or ring (e.g.…”