Hostname: page-component-848d4c4894-wg55d Total loading time: 0 Render date: 2024-05-16T00:16:04.478Z Has data issue: false hasContentIssue false
  • English
  • Français

HI Surveys of the Magellanic System

Published online by Cambridge University Press:  04 August 2017

D. S. Mathewson  and
V. L. Ford
D. S. Mathewson
Affiliation:
Mount Stromlo and Siding Spring Observatories, The Australian National University
V. L. Ford
Affiliation:
Mount Stromlo and Siding Spring Observatories, The Australian National University

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The global distribution of HI in the Magellanic System is shown in Figure 1. The gas covers some 1500 square degrees of sky and has a mass of 1.8 × 109 M⊙. There are four main components: the LMC, the SMC, the inter-Cloud region and the Magellanic Stream. The integrated HI of the first three components is mapped in Figure 2 with the Parkes 64-m radio telescope which has a resolution of 15 arc min. The previous surveys of McGee and Milton (1966), Hindman (1967), Mathewson et al. (1979) have been combined with a recent survey by Mathewson et al. (1983) of the outer regions of the System to give this large-scale picture of the gas distribution. The last two surveys were made with a velocity resolution of 4.12 km s−1 and a minimum detectable signal of 0.2 K. The long spurs extending from the LMC and SMC and the bridge joining the two galaxies with prominent spurs pointing to the Magellanic Stream are all compelling evidence for tidal interaction between the LMC and SMC (Mathewson 1976a, Murai and Fujimoto 1980). The detailed velocity field of the HI is given in Mathewson et al. (1983). Its large-scale features are shown in Figure 5 of Mathewson et al. (1979) which indicate that the radial velocities of the inter-Cloud region form a velocity continuum with those of the LMC and SMC. This plus the continuity of the general velocity gradient across the entire Magellanic System strongly suggest that the two galaxies are bound.

Type
Dynamics
Information
Symposium - International Astronomical Union , Volume 108: Structure and Evolution of the Magellanic Clouds , 1984 , pp. 125 - 136
Copyright
Copyright © Reidel 1984 

References

Ardeberg, A., and Maurice, E.: 1979, Astron. Astrophys. 77, 277.Google Scholar
Bajaja, E., and Loiseau, N.: 1982, Astron. Astrophys. Suppl. 48, 71.Google Scholar
Berkhuijsen, E., Haslam, C.G.T., and Salter, C.J.: 1971, Astron. Astrophys. 14, 252.Google Scholar
Briggs, F.H., Wolfe, A.M., Krumm, N., and Salpeter, E.E.: 1980, Astrophys. J., 238, 510.CrossRefGoogle Scholar
Brück, M.T.: 1975, Mon. Not. Roy. astr. Soc. 173, 327.Google Scholar
Carozzi, N.: 1974, Astron. Astrophys. Suppl. 16, 277.Google Scholar
Cohen, R.J.: 1981, Mon. Not. Roy. astr. Soc. 196, 835.Google Scholar
Cohen, R.J.: 1982, Mon. Not. Roy. astr. Soc. 199, 281.Google Scholar
Cohen, R.J.: 1982, Mon. Not. Roy. astr. Soc. 200, 391.Google Scholar
Davies, R.D., and Wright, A.E.: 1977, Mon. Not. Roy. astr. Soc. 180, 71.Google Scholar
Dubois, P.: 1975, Astron. Astrophys. 40, 227.Google Scholar
Feast, M.W.: 1968, Mon. Not. Roy. astr. Soc. 140, 345.Google Scholar
Feast, M.W., Thackeray, A.D., and Wesselink, A.J.: 1960, Mon. Not. Roy. astr. Soc. 121, 337.Google Scholar
Feitzinger, J.V.: 1980, Space Sci. Rev. 27, 35.Google Scholar
Feitzinger, J.V., Isserstedt, J., and Schmidt-Kaler, Th.: 1977, Astron. Astrophys. 57, 265.Google Scholar
Florsch, A., Marcout, J., and Fleck, E.: 1981, Astron. Astrophys. 96, 158.Google Scholar
Fujimoto, , and Murai, T.: 1984, this volume, p. 115.Google Scholar
Giovanelli, R.: 1981, Astron. J. 86, 1468.Google Scholar
Giovanelli, R., and Haynes, M.P.: 1979, Astrophys. J. 230, 404.Google Scholar
Hart, L., Davies, R.D., and Johnson, S.C.: 1980, Mon. Not. Roy. astr. Soc. 191, 269.Google Scholar
Haynes, M.P.: 1979, Astron. J. 84, 1173.CrossRefGoogle Scholar
Hindman, J.V.: 1964, Nature, 202, 377.Google Scholar
Hindman, J.V.: 1967, Aust. J. Phys. 20, 147.Google Scholar
Hulsbosch, A.N.M.: 1975, Astron. Astrophys. 40, 1.Google Scholar
Johnson, P.G., Meaburn, J., and Osman, A.M.I.: 1982, Mon. Not. Roy. astr. Soc. 198, 985.Google Scholar
Kunkel, W.E.: 1979, Astrophys. J., 228, 718.Google Scholar
Large, M.I., Quigley, M.J.S., and Haslam, C.G.T.: 1962, Mon. Not. Roy. astr. Soc. 124, 405.Google Scholar
Lin, D.N.C., and Lynden-Bell, D.: 1977, Mon. Not. Roy. astr. Soc. 181, 37.CrossRefGoogle Scholar
Lin, D.N.C., and Lynden-Bell, D.: 1982, Mon. Not. Roy. astr. Soc. 198, 707.Google Scholar
Lynden-Bell, D.: 1976, Mon. Not. Roy. astr. Soc. 174, 695.Google Scholar
McGee, R.X., and Milton, J.A.: 1966, Aust. J. Phys. 19, 343.Google Scholar
McGee, R.X., and Newton, L.M.: 1981, Proceedings of the Astronomical Society of Australia, 4, 189.Google Scholar
Mathewson, D.S.: 1976a, Proceedings of the Astronomical Society of Australia, 3, 20.Google Scholar
Mathewson, D.S.: 1976b, Roy. Greenwich Obs. Bull. No. 182, 217.Google Scholar
Mathewson, D.S., Cleary, M.N., and Murray, J.D.: 1975, Astrophys. J. (Letters), 195, L97.CrossRefGoogle Scholar
Mathewson, D.S., Ford, V.L., Dopita, M.A., Tuohy, I.R., Long, K.S., and Helfand, D.J.: 1983, Supernova Remnants and Their X-ray Emission, IAU Symp. #101, ed. Danziger, J. and Gorenstein, P., (Dordrecht: Reidel).Google Scholar
Mathewson, D.S., Ford, V.L., and Fisher, J.L.: 1983 (in preparation).Google Scholar
Mathewson, D.S., Ford, V.L., Schwarz, M.P., and Murray, J.D.: 1979, The Large Scale Characteristics of the Galaxy, IAU Symp. #84, ed. Burton, W. B., (Dordrecht: Reidel), p. 547.Google Scholar
Mathewson, D.S., and Schwarz, M.P.: 1976, Mon. Not. Roy. astr. Soc. 176, 47.Google Scholar
Mathewson, D.S., Schwarz, M.P., and Murray, J.D.: 1977, Astrophys. J. (Letters), 217, L5.CrossRefGoogle Scholar
Mirabel, I.F.: 1981, Astrophys. J. 250, 528.Google Scholar
Mirabel, I.F.: 1982, Astron. J. 256, 120.Google Scholar
Mirabel, I.F., and Cohen, R.J.: 1979, Mon. Not. Roy. astr. Soc., 188, 219.CrossRefGoogle Scholar
Morras, R.: 1983, Astron. J. 88, 62.Google Scholar
Murai, T., and Fujimoto, M.: 1980, Publ. astr. Soc. Japan, 32, 581.Google Scholar
Rogstad, D.H., Lockhart, I.A., and Wright, M.C.H.: 1974, Astrophys. J. 193, 309.Google Scholar
Rohlfs, K., Feitzinger, J.V., and Kreitschmann, J.: 1984, this volume, p. 395.CrossRefGoogle Scholar
Schneider, S.E., Helou, G., Salpeter, E.E., and Terzian, Y.: 1983, Astrophys. J. (in press).Google Scholar
Schweizer, F., Whitmore, B.C., and Rubin, V.C.: 1983, Astron. J. 88, 909.Google Scholar
Smith, M.G., and Weedman, D.W.: 1973, Astrophys. J., 179, 461.Google Scholar
Wannier, P., and Wrixon, G.T.: 1972, Astrophys. J. (Letters), 173, L119.Google Scholar
Weaver, H.: 1979, The Large Scale Characteristics of the Galaxy, IAU Symp. No. 84, ed. Burton, W. B., (Dordrecht: Reidel), 295.Google Scholar
Welch, D.L., and Madore, B.F.: 1984, this volume, p. 221.Google Scholar
Westerlund, B.E., and Glaspey, J.: 1971, Astron. Astrophys. 10, 1.Google Scholar