Probing the kinematics of early-type galaxy halos using planetary nebulae
L. Coccato, O. Gerhard, M. Arnaboldi, P. Das, N. G. Douglas, K., Kuijken, M. R. Merrifield, N. R. Napolitano, E. Noordermeer, A. J., Romanowsky, M. Capaccioli, A. Cortesi, F. De Lorenzi, K. C. Freeman
TL;DR
This study uses planetary nebulae to explore the kinematics of early-type galaxy halos, revealing complex angular momentum profiles and relationships between halo velocity dispersion and galaxy properties.
Contribution
It introduces planetary nebulae as effective tracers for halo kinematics, extending analysis beyond the inner regions and providing new constraints for galaxy formation models.
Findings
Halo angular momentum varies with radius.
Halo velocity dispersion correlates with galaxy luminosity.
Planetary nebulae effectively trace outer galaxy kinematics.
Abstract
We present first results of a study of the halo kinematics for a sample of early type galaxies using planetary nebulae (PNe) as kinematical tracers. PNe allow to extend up to several effective radii (Re) the information from absorption line kinematics (confined to within 1 or 2 Re), providing valuable information and constraints for merger simulations and galaxy formation models. We find that the specific angular momentum per unit mass has a more complex radial dependence when the halo region is taken into account and that the halo velocity dispersion is related to the total galaxy luminosity, isophotal shape, and number of PNe per unit of luminosity
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