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KPG 390: A pair of trailing spirals.

Published online by Cambridge University Press:  12 August 2011

P. Repetto ,
M. Rosado ,
R. Gabbasov  and
I. Fuentes-Carrera
P. Repetto
Affiliation:
Instituto de Astronomía, Universidad Nacional Autonoma de México (UNAM), Apdo. Postal 70-264, 04510, México, D.F., México. email: prepetto@astroscu.unam.mx.
M. Rosado
Affiliation:
Instituto de Astronomía, Universidad Nacional Autonoma de México (UNAM), Apdo. Postal 70-264, 04510, México, D.F., México. email: prepetto@astroscu.unam.mx.
R. Gabbasov
Affiliation:
Instituto de Astronomía, Universidad Nacional Autonoma de México (UNAM), Apdo. Postal 70-264, 04510, México, D.F., México. email: prepetto@astroscu.unam.mx.
I. Fuentes-Carrera
Affiliation:
Department of Physics, Escuela Superior de Física y Matemáticas, IPN, U.P. Adolfo López Mateos, C.P. 07738, Mexico city IPN, México.
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Abstract

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In this study we present scanning Fabry-Perot Hα observations of the isolated interacting galaxy pair NGC 5278/79. We derived velocity fields, various kinematic parameters and rotation curves for both galaxies. These kinematical results together with the fact that dust lanes have been detected in both galaxies, as well as the analysis of surface brightness profiles along the minor axis, allowed us to determine univocally that both components of the interacting pair are trailing spirals. We have also estimated the mass of NGC 5278 fitting its rotation curve with a disk-halo component. We have tested three different types of halo (pseudo-isothermal, Hernquist and Navarro Frenk White) and we have obtained that the rotation curve can be fitted either with a pseudo-isothermal, an Hernquist halo or a Navarro Frenk White halo component, although in the first case the amount of dark matter required is about ten times smaller than for the other two halo distributions.

Keywords

Instrumentation: interferometersmethods: data analysistechniques: image processingtechniques: interferometrictechniques: radial velocitiesastrometrygalaxies: interactionsgalaxies: kinematics and dynamicsgalaxies: spiral(cosmology): dark matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 127 - 134
Copyright
Copyright © International Astronomical Union 2011

References

Marcelin, M., Lecoarer, E., Boulesteix, J., Georgelin, Y., & Monnet, G. 1987, A&A, 179, 101Google Scholar
Amram, P., Mendes de Oliveira, C., Plana, H., Balkowski, C., Boulesteix, J. & Carignan, C. 2002, Ap&SS, 281, 389Google Scholar
Fuentes-Carrera, I., Rosado, M., Amram, P., Salo, H. & Laurikainen, E. 2007, A&A, 466, 847Google Scholar
Rubin, V. C., Peterson, C. J. & Ford, W. K. Jr. 1976, BAAS, 8, 297Google Scholar
Bosma, A., van der Hulst, J. M. & Sullivan, W. T. III 1977, A&A, 57, 373Google Scholar
Blais-Ouellette, S., Amram, P. & Carignan, C. 2001, AJ, 121, 1952CrossRefGoogle Scholar
van Albada, T. S., Bahcall, J. N., Begeman, K. & Sancisi, R. 1985, ApJ, 295, 305CrossRefGoogle Scholar
Reshetnikov, V. P. & Klimanov, S. A. 2003, Astron. Lett., 29, 429CrossRefGoogle Scholar
Windhorst, R. A., et al. 2002, ApJS, 143, 113CrossRefGoogle Scholar
Byrd, G. G., Thomasson, M., Donner, K. J., Sundelius, B., Huang, T. Y. & Valtonen, M. J. 1989, Celestial Mechanics, 45, 31CrossRefGoogle Scholar
Keel, W. C. 1991, ApJ, 375, L5CrossRefGoogle Scholar
Athanassoula, E. 1978, A&A, 69, 395Google Scholar
Thomasson, M., Donner, K. J., Sundelius, B., Byrd, G. G., Huang, T.-Y. & Valtonen, M. J. 1989, A&A, 211, 25Google Scholar
Freeman, K. C. 1970, ApJ, 160, 811CrossRefGoogle Scholar
Hernquist, L. 1990, ApJ, 356, 359CrossRefGoogle Scholar
Navarro, J. F., Frenk, C. S. & White, S. D. M. 1996, ApJ, 462, 563CrossRefGoogle Scholar
Sharp, N. A. & Keel, W. C. 1985, AJ, 90, 469CrossRefGoogle Scholar
Väisänen, P., Ryder, S., Mattila, S. & Kotilainen, J. 2008, ApJ, 689, L37CrossRefGoogle Scholar
Mazzarella, J. M. & Boroson, T. A. 1993, ApJS, 85, 27CrossRefGoogle Scholar
Paturel, G., Petit, C., Prugniel, P., Theureau, G., Rousseau, J., Brouty, M., Dubois, P., & Cambrésy, L. 2003, A&A, 412, 45Google Scholar
Rosado, M., et al. 1995, Rev. Mexicana AyA, 3, 263Google Scholar
Repetto, P., Rosado, M., Gabbasov, R. & Fuentes-Carrera, I. 2010, AJ, 139, 1600CrossRefGoogle Scholar