Annu. Rev. Astron. Astrophys. 1978. 16: 103-39
Copyright © 1978 by . All rights reserved

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2. MEASUREMENT OF THE DISTRIBUTION AND KINEMATICS OF THE GAS

When one applies the restriction that observations should provide information over an appreciable fraction of the galaxy disk, one finds that there are relatively few published results from absorption-line measurements of the stellar component. In this section we therefore concentrate on the available data for the gas and compare the results obtained from the various methods of observation.

In Table 1 we list references to observations that satisfy the selection criteria. References to emission-line slit-spectra are limited to those resulting in velocity data extending over a large part of the galaxy image. The Fabry-Perot data provide such information in a single observation, so the reference list is intended to include all papers on those results. References to radio-HI data are restricted to those providing the highest relative resolution; information on the general characteristics of the HI distribution and velocity field require beamwidths of at most about one-tenth of the Holmberg diameter, and even higher resolution is needed in order to separate spiral arms (Allen 1975a). References to earlier work (prior to about 1969) and to less extensive observations of galaxy kinematics can be found in the reviews by Burbidge & Burbidge (1975) and by Roberts (1975a, b), in the I.A.U. Reports on Astronomy for Commission 28, in the circulars of the I.A.U. Working Group on Internal Motions in Galaxies, and, in the case of the LMC and SMC, in the proceedings of a conference on "The Magellanic Clouds" (Muller 1971). Observations of kinematics in the nuclear regions are referenced by Burbidge (1972) and Ulrich (1974), and are briefly discussed in Section 4.1 below.

Table 1. List of galaxies for which the velocity field has been measured by sampling many points over a large fraction of their disks

NGC Type Slit spectra of optical emission lines Halpha Fabry-Perot interferometry H I 21-cm observations with good resolution

224(M31) Sb Rubin & Ford 1970, 1971 Deharveng & Pellet 1975a, b Argyle 1965
        Roberts 1966
        Davies & Gottesman 1970
        Gottesman & Davies 1970
        Guibert 1973, 1974
        Emerson 1974, 1976
        Roberts & Whitehurst 1975
        Roberts et at. 1978
        Shane 1978
        Newton & Emerson 1977
253 Sc Demoulin & Burbidge 1970 Deharveng 1971 Combes et al. 1977
    Ulrich 1978    
300 Sd     Shobbrook & Robinson 1967
598 (M33) Scd Mayall & Aller 1942 Carranza et al. 1968 de Jager & Davies 1971
      de Vaucoulers & Gordon 1971
      de Vaucoulers 1971 Wright et at. 1972
        Warner et al. 1973
        Huchtmeier 1973
        Rogstad et al. 1976
628 Sc   Monnet & Deharveng 1977  
1068 Sb Walker 1968    
1569 Irr   de Vaucoulers et al. 1974  
2043 Scd   Deharveng & Pellet 1970 Burns & Roberts 1971
        Shostak & Rogstad 1973
        Shostak 1973
2685 Spec Ulrich 1975   Shane 1977
        Shane & Bystedi 1978
2715 Sc van der Kruit & Bosma 1978b    
2782 Sb van der Kruit 1977b    
2841 Sb     Bosma 1978b
2903 Sbc Simkin 1975a    
3031 (M81) Sab Goad 1974, 1976   Rots & Shane 1975
        Gottesman & Weliachew 1975
        Allen 1976
3067 Sab Danziger & Chromey 1972    
3079 SBc Carozzi 1977    
3198 Sc     Bosma 1978b
3310 Sbc, pec van der Kruit 1976a    
3351 SBb Rubin et al. 1975    
    Peterson et al. 1976    
3359 SBc     Seifert et al. 1975
3675 Sb van der Kruit 1975    
4027 SBd de Vaucouleurs et at. 1968    
4151 Sab Simkin 1975b   Bosma et al. 1977a
4236 Sm     Shostak & Rogstad 1973
4258 Sbc van der Kruit 1974b Courtes 1972 van Albada & Shane 1975
4449 Irr   Crillon & Monnet 1969a van Woerden et al. 1975
4490 / 85 Irr   Boulesteix et al. 1970  
4631 Sd   Crillon & Monnet 1969b Winter 1975, Weliachew et al. 1978
4736 Sab van der Kruit 1974a, 1976c   Bosma et al. 1977b
5033 Sc van der Kruit & Bosma 1978b   Bosma 1978b
5055 Sbc van der Kruit & Bosma 1978b   Bosma 1978b
5194 (M51) Sbc Burbidge & Burbidge 1964 Carranza et al. 1969 Weliachew & Gottesman 1973
      Tully 1974a Shane 1975
        Segalovitz 1976
5236 (M83) Sc     Rogstad et al. 1974
5383 SBb Peterson et al. 1978   Allen et al. 1973a
5457 (M101) Scd   de Vaucoulers & Rogstad & Shostak 1971
      de Vaucoulers 1971 Rogstad 1971
        Allen et al. 1973a, b
        Allen 1975a, b, 1976
6574 Sbc Demoulin & Tung Chan 1969    
6946 Scd     Rogstad et al 1973
7331 Sb     Bosma 1978b
7640 Sc     Seielstad & Wright 1973
LMCa SBm   Georgelin & Monnet 1970 McGee & Milton 1966
      Smith & Weedman 1971  
      Chériguène & Monnet 1972  
SMCb Irr Feast 1970 Carranza et al. 1971 Hindman 1967
      Smith & Weedman 1973 Erkes et al. 1973
IC10 Irr     Shostak 1974
IC342 Scd     Rogstad et al. 1973
IC2574 Sm     Seielstad & Wright 1973
Holm I Irr     Tully et al. 1978
Holm II Irr     Cottrell 1976b
DDO 125 Irr     Tully et al. 1978
Maffei II Sb?     Shostak & Weliachew 1971
        Love 1972

a Detailed kinematical studies of te LMC have also been made for the planetary nebulae (Smith & Weedman 1972), blue globular clusters (Andrews & Evans 1972), and supergiants (Prevot 1973).
b A detailed kinematical study of the SMC has also been made for the supergiants (Dubois 1975).

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