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- W86012244 abstract "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." @default.
- W86012244 created "2016-06-24" @default.
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- W86012244 date "1979-01-01" @default.
- W86012244 modified "2023-10-16" @default.
- W86012244 title "Comments on the Detection and Classification of Compact Emission-Line Galaxies" @default.
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- W86012244 doi "https://doi.org/10.1017/s0252921100104117" @default.
- W86012244 hasPublicationYear "1979" @default.
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