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Planetary nebulae as kinematic tracers of galaxy halos

Published online by Cambridge University Press:  11 May 2017

Lodovico Coccato  and
PNS collaboration
Lodovico Coccato
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching b. München, Germany email: lcoccato@eso.org
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Abstract

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The kinematics and dynamical properties of galaxy stellar halos are difficult to measure, given the faint surface brightness that characterizes these regions. Gas-rich systems such as spiral galaxies can be probed using the radio Hi emission. Early-type galaxies contain less gas, therefore alternative kinematic tracers need to be used. Planetary Nebulae (PNe) can be easily detected far out in the halo thanks to their bright [Oiii] emission at 5007 Å. It is therefore possible to map the halo kinematics also in early-type galaxies, typically out to 5 effective radii or beyond. Thanks to the recent spectroscopic surveys targeting extra-galactic PNe, we can now rely on few tens of galaxies where the kinematics of the stellar halos are measured. I will discuss the most important results: (a) the relation of the stellar surface brightness and the PNe number density; (b) the velocity and velocity dispersion two-dimensional fields; (c) the radial profiles of angular momentum; and (d) the relation between the derived kinematics physical properties of the host galaxies.

Keywords

galaxies: generalgalaxies: haloesgalaxies: kinematics and dynamicsISM Planetary Nebulae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B , August 2015 , E12
Copyright
Copyright © International Astronomical Union 2017 

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