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Interacting Galaxies: The Kinematics of NGC 4038/39 and the HI Bridge Between M81 and NGC 3077

Published online by Cambridge University Press:  14 August 2015

J.M. van der Hulst
J.M. van der Hulst*
Affiliation:
Kapteyn Astronomical Institute, University of Groningen

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Computer simulations of galaxy encounters (Toomre 1974 and references therein) have strongly supported the idea that the luminous bridges and tails in many multiple galaxies are a result of gravitational interaction. The need for an observational test of the kinematics of these models has prompted observations of NGC 4038/39 (the “antennae”) in the 21 cm line of neutral hydrogen (HI) with the Westerbork Synthesis Radio Telescope (WSRT) at an angular resolution of 100″×150″ (α×δ). A detailed description of the observations and data reduction is given elsewhere (van der Hulst, 1977). Neutral hydrogen is definitely associated with the tails as was already indicated by the filled aperture observations of Huchtmeier and Bohnenstengel (1975) at the lower resolution of 8′.7. The distribution of HI column density is shown in Figure 1 superposed on a print of a plate obtained by F. Schweizer with the 4 m telescope at Cerro Tololo. Owing to the low declination of the object (−19°) the WSRT map is affected by several sidelobes; the main effect is an attenuation of extended east-west structures, for which reason the HI along the southern tail in Fig. 1 shows a gap. Computer experiments and a comparison with the filled aperture observations show that the WSRT data are entirely consistent with an HI distribution which is uniform along this tail and increases with about a factor 2 at the extreme end, where the tail is very blue and small HII regions are present (Schweizer, elsewhere in this volume). The tails contain 2.9 × 109 M⊙ of HI (assuming a distance of 20 Mpc), 85% of which is in the southern and more prominent tail. About 1.1 × 109 M⊙ of HI is associated with the galaxies which are not spatially resolved at the present angular resolution.

Type
V: The Outskirts of Galaxies
Information
Symposium - International Astronomical Union , Volume 77: Structure and Properties of Nearby Galaxies , 1978 , pp. 269 - 277
Copyright
Copyright © Reidel 1978 

References

Barbieri, C., Bertola, F., di Tullio, G.: 1974, Astron. Astrophys. 35, 463.Google Scholar
Davies, R.D.: 1974, in The Formation and Dynamics of Galaxies, IAU Symp. No. 58, ed. Shakeshaft, J.R., p.119.Google Scholar
Davies, R.D., Wright, A.E.: 1977, Monthly Not. Roy. Astron. Soc. 180, 71.Google Scholar
Fujimoto, M., Sofue, Y.: 1976, Astron. Astrophys. 47, 263.Google Scholar
Huchtmeier, W.K., Bohnenstengel, H.D.: 1975, Astron. Astrophys. 41, 477.Google Scholar
Hulst, J.M. van der: 1977, , University of Groningen.Google Scholar
Lynden-Bell, D.: 1976, Monthly Not. Roy. Astron. Soc. 174, 695.Google Scholar
Mathewson, D.S.: 1976, Roy. Greenwich Obs. Bull. No. 182.Google Scholar
Mathewson, D.S., Schwarz, M.P.: 1976, Monthly Not. Roy. Astron. Soc. 176, 47p.CrossRefGoogle Scholar
Mathewson, D.S., Cleary, M.N., Murray, J.D.: 1974, Astrophys. J. 190, 291.Google Scholar
Mathewson, D.S., Schwarz, M.P., Murray, J.D.: 1977, Astrophys. J. Letters 217, L5.CrossRefGoogle Scholar
Roberts, M.S.: 1972, in External Galaxies and Quasi Stellar Objects, IAU Symp. no.44, ed. Evans, D.S., p.12.Google Scholar
Rots, A.H., Shane, W.W.: 1975, Astron. Astrophys. 45, 25.Google Scholar
Toomre, A.: 1974, in The Formation and Dynamics of Galaxies, IAU Symp. no.58, ed. Shakeshaft, J.R., p.347.Google Scholar
Toomre, A., Toomre, J.: 1972, Astrophys. J. 178, 623.CrossRefGoogle Scholar
Weliachew, L., Sancisi, R., Guélin, M.: 1977, Astron. Astrophys., submitted.Google Scholar