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Kinematics of Planetary Nebulae in M51's Tidal Tail

Published online by Cambridge University Press:  26 May 2016

John J. Feldmeier ,
J. Christopher Mihos ,
Patrick R. Durrell ,
Robin Ciardullo  and
George H. Jacoby
John J. Feldmeier
Affiliation:
Case Western Reserve University, 10900 Euclid Ave. Cleveland, OH 44106, U.S.A.
J. Christopher Mihos
Affiliation:
Case Western Reserve University, 10900 Euclid Ave. Cleveland, OH 44106, U.S.A.
Patrick R. Durrell
Affiliation:
Penn State University, 525 Davey Lab, University Park, PA 16802, U.S.A.
Robin Ciardullo
Affiliation:
Penn State University, 525 Davey Lab, University Park, PA 16802, U.S.A.
George H. Jacoby
Affiliation:
WIYN Observatory, P.O. Box 26732, Tucson AZ 85726, U.S.A.

Abstract

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The galaxy pair NGC 5194/95 (M51) is one of the closest and best known interacting systems. Despite its notoriety, however, many of its features are not well studied. Extending westward from NGC 5195 is a low surface brightness tidal tail, which can only be seen in deep broadband exposures. Our previous [O III] λ5007 planetary nebulae (PN) survey of M51 recovered this tidal tail, and presented us with a opportunity to study the kinematics of a galaxy interaction in progress. We report the results of a spectroscopy survey of the PN, aimed at determining their kinematic properties. We then use these data to constrain new self-consistent numerical models of the system.

Type
Part VIII: Planetary Nebulae as Galaxy Probes
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 633 - 634
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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