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Comments on the Detection and Classification of Compact Emission-Line Galaxies
Published online by Cambridge University Press: 12 April 2016
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Four methods for finding emission-line galaxies have been compared. Method (a) uses the ultraviolet excess, as found either by filter photography (Haro 1956) or by objective prism spectra (Markarian 1967). glanco (1974) introduced a thin prism with the CTIO Schmidt (1740 Å mm-1 at Hβ) which with IIIa-J plates [Method (b)] gave enough resolution for Smith (1975) and MacAlpine et al. (1977a, 1977b) to detect and classify galaxies by strong emission lines. Following a suggestion by McCarthy that even higher dispersion might be useful, I have used the CTIO Schmidt with [Method (c)] the 4° prism, a GGl+55 filter and IIIa-J emulsion and with [Method (d)] the 10° prism, an RG630 filter and IIIa-F emulsion. These latter give about 400 Å mm-1 at Hβ and Hα respectively which improves the visibility of emission lines against the galaxy continuum so that [0111] 5007 and 4959 and Hβ can be seen on the green plates and Hα and [SII] 6725 can be seen on the red plates.
- Type
- III Criteria and Applications Outside the MK Domain
- Information
- International Astronomical Union Colloquium , Volume 47: Spectral Classification of the Future , 1979 , pp. 151 - 153
- Copyright
- Copyright © Vatican Observatory 1979
References
MacAlpine, G. M., Smith, S. B. and Lewis, D. W. (1977a). Astrophys. J. Supplement 54, 95.CrossRefGoogle Scholar
MacAlpine, G. M., Lewis, D.W. and Smith, S. B. (1977b). Astrophys. J. Supplement 35, 203.CrossRefGoogle Scholar
Smith, M. G., Aguirre, C. and Zemelman, M. (1976). Astrophys. J. Supplement 32, 217.CrossRefGoogle Scholar
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