Galaxy kinematics from counter-dispersed imaging

Abstract

Determining the internal kinematics of a galaxy from planetary nebulae (PN) is usually a two step process in which the candidate PN are first identified in a target galaxy and then, in a follow up run, spectra are obtained. We have implemented a new technique in which two dispersed images at the wavelength of the [OIII] emission line at 5007A are combined to yield positions, magnitudes and velocities of the PN population in a single step. A reduction in observing time of about a factor 2 is attainable. We present here the proof-of-principle results.

6 pages, LaTeX, Monthly Notices style, ps and eps included, loaded with \epsfbox submitted to Monthly Notices of the R.A.S. on July 9, 1998, lost in the mail, resubmitted September 3

References in corpus (3)

• Planetary Nebulae as standard candles XI. Application to Spiral Galaxies
• The Globular Cluster Systems of NGC 1400 and NGC 1407
• H-alpha Objective Prism Survey of Abell 1060

Cited by in corpus (7)

• Detection, photometry and slitless radial velocities of 535 planetary nebulae in the flattened elliptical galaxy NGC 4697
• The PN.S Elliptical Galaxy Survey: the dark matter in NGC 4494
• The PN.S Elliptical Galaxy Survey: Data Reduction, Planetary Nebula Catalog, and Basic Dynamics for NGC 3379
• The Planetary Nebulae Spectrograph: the green light for Galaxy Kinematics
• The Fornax Cluster VLT Spectroscopic Survey II - Planetary Nebulae kinematics within 200 kpc of the cluster core
• The Fornax Cluster VLT Spectroscopic Survey IV -- Cold kinematical substructures in the Fornax core from COSTA
• Galaxy Dynamics and the PNe Population