An objective prism survey of emission line galaxies

1986 ◽  
Vol 10 (3) ◽  
pp. 181-189
Author(s):  
Liu Ji-ying ◽  
Huang Yong-wei ◽  
Feng Xing-chun
Keyword(s):  
Emission Line ◽  
Objective Prism ◽  
Emission Line Galaxies

scholarly journals An Automatic Approach for Selecting New HA Emission-Line Galaxies

1994 ◽  
Vol 161 ◽  
pp. 611-614
Author(s):  
O. Alonso ◽  
J. Zamorano ◽  
M. Rego ◽  
J. Gallego ◽  
A.G. Vitores
Keyword(s):  
Emission Line ◽  
Selection Criterion ◽  
Schmidt Telescope ◽  
Objective Prism ◽  
Emission Line Galaxies ◽  
Calar Alto ◽  
Observational Procedure

The most unambiguous way to discover new emission-line galaxies (ELGs) is directly by the presence of their lines, using objective-prism plates of adequate resolution. The first survey using this technique was developed by Smith in 1975 with the 0.6 m CTIO Curtis Schmidt Telescope. The Universidad Complutense de Madrid (UCM) is carrying out a survey of ELGs with the Schmidt Telescope at Calar Alto (Almería, Spain) using the presence of Ha in emission in IIIa-F prism plates as selection criterion. The observational procedure and results are described in Rego et al. 1989; Zamorano et al. 1990; Zamorano et al. 1993.

scholarly journals Slitless Spectroscopy by Photographic and CCD Detectors Across Large Fields

1994 ◽  
Vol 161 ◽  
pp. 709-714
Author(s):  
G. Comte ◽  
C. Surace
Keyword(s):  
Emission Line ◽  
Emission Lines ◽  
Photographic Emulsion ◽  
Subsequent Reduction ◽  
Schmidt Telescope ◽  
Ccd Array ◽  
Objective Prism ◽  
Emission Line Galaxies ◽  
Ccd Detectors

We present a new survey of emission line galaxies, performed with the ESO 1 m Schmidt telescope equipped with the 4° objective prism using IIIa-J photographic emulsion. The plates are digitized with the MAMA microdensitometer. A subsequent reduction of the block scans gives redshifts with a mean accuracy of 160 km/s−1, and spectrophotometric measurements of the intensity and equivalent widths of the principal emission lines. A brief discussion is given of the possible extension of quantitative reduction of slitless spectroscopy to archive plates and future large CCD array frames.

scholarly journals Comments on the Detection and Classification of Compact Emission-Line Galaxies

1979 ◽  
Vol 47 ◽  
pp. 151-153
Author(s):  
T. D. Kinman
Keyword(s):  
Emission Line ◽  
Emission Lines ◽  
Ultraviolet Excess ◽  
Strong Emission ◽  
The Galaxy ◽  
Objective Prism ◽  
Emission Line Galaxies

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.

Objective prism survey of emission-line galaxies. IV

1991 ◽  
Vol 15 (2) ◽  
pp. 131-142
Author(s):  
Huang Yong-wei ◽  
Liu Ji-ying ◽  
Feng Xing-chun
Keyword(s):  
Emission Line ◽  
Objective Prism ◽  
Emission Line Galaxies

New emission-line galaxies identified from an objective prism survey

1990 ◽  
Vol 170 (1-2) ◽  
pp. 353-360 ◽  
Author(s):  
J. Zamorano ◽  
M. Rego ◽  
R. Gonzalez-Riestra ◽  
G. Rodr�guez
Keyword(s):  
Emission Line ◽  
Objective Prism ◽  
Emission Line Galaxies

scholarly journals Optical and Far-Infrared Properties of UM Survey Emission-Line Galaxies

1989 ◽  
Vol 134 ◽  
pp. 400-401
Author(s):  
Gordon M. MacAlpine ◽  
John J. Salzer
Keyword(s):  
Emission Line ◽  
Selection Criterion ◽  
Line Emission ◽  
Far Infrared ◽  
University Of Michigan ◽  
Extensive Analysis ◽  
Objective Prism ◽  
Primary Selection ◽  
Emission Line Galaxies ◽  
The University

For the University of Michigan (UM) survey, the Curtis Schmidt telescope at CTIO is used with Kodak IIIa-J plates and the 1.°8 objective prism to detect emission-line galaxies (ELGs) and quasars. Line emission is the primary selection criterion. The quasar sample has been investigated by Lewis, MacAlpine, and Weedman (1979) and by MacAlpine and Feldman (1982) while a study of the ELGs was begun by Lewis (1983). Here, we report on a more extensive analysis of the 172 ELG candidates in the UM Lists IV (MacAlpine and Lewis 1978) and V (MacAlpine and Williams 1981) areas.

scholarly journals Comments on Extragalactic Objective-Prism Work

1995 ◽  
Vol 148 ◽  
pp. 456-456
Author(s):  
William P. Bidelman
Keyword(s):  
Emission Line ◽  
High Dispersion ◽  
Objective Prism ◽  
Emission Line Galaxies

I much regret not being able to attend this interesting meeting. However, I have two comments concerning useful Schmidt work on galaxies that I would like to pass on to you for further consideration.Both relate to objective-prism surveys for emission-line galaxies. The first is a suggestion that the work of Wasilewski (1983) should be continued. (Additional studies of his objects have been made by Bothun et al. (1989), Osterbrock & Shaw (1988) and Osterbrock et al. (1992)). This utilized the Burrell Schmidt with a 4° prism that gave a dispersion of some 400 Å/mm in the neighborhood of N1, N2 and Hβ. With this relatively high dispersion one can clearly separate these three lines, giving useful information on their relative strengths and widths that cannot be obtained from lower-dispersion material. It might be worthwhile to employ even somewhat higher dispersions than Wasilewski used, though this would no doubt affect the limiting magnitude somewhat. My second suggestion is that one should carry out objective-prism survey work in longer-wavelength spectral regions than are currently being used. The purpose is the detection of additional extragalactic objects in the z = 3–5 range; this search should utilize the lowest available dispersion.

scholarly journals Kiss: A New Digital Survey for Emission-Line Objects

1998 ◽  
Vol 179 ◽  
pp. 302-304 ◽  
Author(s):  
A. Kniazev ◽  
J. Salzer ◽  
V. Lipovetsky ◽  
T. Boroson ◽  
J. Moody ◽  
...  
Keyword(s):  
Emission Line ◽  
Rest Frame ◽  
Pilot Project ◽  
The North ◽  
Ccd Detector ◽  
Redshift Survey ◽  
Objective Prism ◽  
Emission Line Galaxies ◽  
Digital Survey ◽  
North Galactic

We have initiated a major new survey for emission-line galaxies (ELGs) which we call the KPNO International Spectroscopic Survey (KISS). Survey observations began in March 1994 with the 0.61-m Burrell Schmidt telescope. The technique we employ combines the benefits of a traditional photographic objective-prism survey with the advantages of using a CCD detector. The field of view of our CCD is 1.1° square, and the prism employed provides a dispersion of 19 Å/pixel at 5000 Å. The spectral range covered (4800-5500 Å) is restricted by a specially designed filter that transmits from rest-frame Hβ to just shortward of the strong night-sky line at 5577 Å; this greatly reduces the sky background. We expect KISS to be sensitive to galaxies with magnitudes as faint as B = 20m–21m, much deeper than existing photographic surveys. Our initial pilot project covers 100 square degrees (Salzer et al. 1994) and overlaps the CfA/Dartmouth Century Redshift Survey (α = 8h30m–16h45m and δ = 29°–30°) in the North Galactic cap.

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