Galaxy kinematics from counter-dispersed imaging
Astrophysics
2009-10-30 v1
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.
Keywords
Cite
@article{arxiv.astro-ph/9809049,
title = {Galaxy kinematics from counter-dispersed imaging},
author = {N. G. Douglas and K. Taylor},
journal= {arXiv preprint arXiv:astro-ph/9809049},
year = {2009}
}
Comments
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