H. Aceves and H. Velázquez
Instituto de Astronomía, UNAM, Apdo. Postal 877, 22800 Ensenada, B. C., México (aceves@astrosen.unam.mx; hmv@astrosen.unam.mx)
Received, 2005 May 30
Accepted 2005 August 22
]]> RESUMEN
Se presentan relaciones de escala entre la velocidad virial (V) y la dispersión de velocidades uni-dimensional central (σ0); el radio gravitacional (Rv) y el radio efectivo (Re); y la masa total (M) y la masa luminosa (ML) encontradas en simulaciones de N-cuerpos de fusiones binarias entre galaxias espirales. Estas relaciones son de la forma V2 α0σ, Rv α Reβ y M α MLγ. Los valores particulares obtenidos para {α,β,γ} dependen del método de ajuste utilizado [mínimos cuadrados ordinarios (OLS) o regresión ortogonal de distancia (ODR)], el tipo de perfil supuesto [de Vaucouleurs (deV) o de Sérsic (S)], y el tamaño del intervalo radial donde se hace el ajuste. Los índices α y γ resultan ser los más sensibles al procedimiento de ajuste, obteniéndose para el OLS un promedio (α)ols = 1.51 y (γ)ols = 0.69, mientras que para el ODR un (α)odr = 2.35 y (γ)odr = 0.76. El índice β depende más de el perfil adoptado, con (β)deV = 0.13 y (β)s = 0.27. Concluímos que los remanentes de fusiones formados de manera no disipativa tienen un rompimiento fuerte de homología estructural y cinemática.
ABSTRACT
We present scaling relations between the virial velocity (V) and the one-dimensional central velocity dispersion (σ0); the gravitational radius (Rv) and the effective radius (Re); and the total mass (M) and the luminous mass (ML) found in N-body simulations of binary mergers of spiral galaxies. These scalings are of the form V2 α0σ, Rv α Reβ y M α MLγ. The particlar values obtained for {α,β,γ} depend on the method of fitting used [ordinary least-squares (OLS) or orthogonal distance regression (ODR)], the assumed profile [de Vaucouleurs (deV) or Sérsic (S)], and the size of the radial interval where the fit is done. The α and γ indexes turn out more sensitive to the fitting procedure, resulting for the OLS in a mean (α)ols = 1.51 and (γ)ols = 0.69, while for the ODR (α)odr = 2.35 and (γ)odr = 0.76. The β index depends more on the adopted type of profile, with (β)deV = 0.13 and (β)s = 0.27. We conclude that dissipationless formed remnants of mergers have a strong breaking of structural and kinematical homology.
Key Words: Galaxies: Kinematics and dynamics — Methods: Numerical — N-body simulations.
DESCARGAR ARTÍCULO EN FORMATO PDF
REFERENCES
]]>Aceves, H., & Velázquez, H. 2005, MNRAS, 306, 50 [ Links ]
Barnes, J. E., 1998, in Galaxies: Interactions and Induced Star Formation, Saas-Fee Advance Course 26, eds. D. Friedli, L. Martinet, & D. Pfenniger (New York: Springer-Verlag) [ Links ]
Bernardi, M., Sheth, R. K., Annis J., et al. 2003a, AJ, 125,1849 [ Links ]
Bernardi, M., Sheth, R. K., Annis, J., et al. 2003b, AJ, 125,1866 [ Links ]
Bertin, G., Ciotti, L., & Del Principe, M. 2002, A&, 386, 149 [ Links ]
Binggeli, B., & Jerjen, H. 1998, A&A, 333, 17 [ Links ]
Boylan-Kolchin, M., Ma, C., & Quataert, E. 2005, astro-ph/0502495 [ Links ]
Burstein, D., Davies, R. L., Dressler, A., et al. 1987, ApJS, 64, 601 [ Links ]
Caon, N., Capaccioli, M., & D'Onofrio, M. 1993, MNRAS, 265, 1013 [ Links ]
Chiosi, C., & Carraro, G. 2002, MNRAS, 335, 335 [ Links ]
Ciotti, L., & Bertin G. 1999, A&A, 352, 447 [ Links ]
de Vaucouleurs, G. 1948, Ann. d'Astroph., 11, 247 [ Links ]
Efron, B., & Tibshirani, R. J. 1993, An Introduction to the Bootstrap (New York: Chappman & Hall) [ Links ]
Efstathiou, G., Lake, G., & Negroponte, J. 1982, MNRAS, 199, 1069 [ Links ]
Faber, S. M., & Jackson, R. E. 1976, ApJ, 204, 668 [ Links ]
Feigelson, E. D., & Babu, G. J. 1992, ApJ, 397, 55 [ Links ]
Giovanelli, R., Haynes, M. P., da Costa, L. N., Freudling, W., Salzer, J. J., & Wegner, G. 1997, ApJ, 477, L1 [ Links ]
González-García, A. C., & Balcells, M. 2005, MNRAS, 357, 753 [ Links ]
Graham, A. W. 1998, MNRAS, 295, 933 [ Links ]
Hernquist, L. 1993, ApJS, 86, 389 [ Links ]
Jørgensen, I., Franx, M., & Kjaergaard, P. 1996, MNRAS, 280, 167 [ Links ]
Khosroshahi, H. G., Raychaudhury, S., Ponman, T. J., Miles, T. A., & Forbes, D. A. 2004, MNRAS, 349, 527 [ Links ]
Kormendy, J. 1977, ApJ, 217, 406 [ Links ]
Mo, H. J., Mao, S., & White, S. D. M. 1998, MNRAS, 295, 319 (MMW) [ Links ]
Naab, T., & Burkert, A. 2003, ApJ, 597, 893 [ Links ]
Navarro, J. F., Frenk, C. S., & White, S. D. M. 1995, MNRAS, 275, 56 [ Links ]
----------. 1997, ApJ, 490, 493 [ Links ]
Padmanabhan, N., Seljak, U., Strauss, M. A., et al. 2004, New Astronomy, 9, 329 [ Links ]
Peebles, P. J. E. 1993, Principles of Physical Cosmology (Princeton: Princeton UP) [ Links ]
----------. 2002, in ASP Conf. Ser. Vol. 283, A New Era in Cosmology, eds. N. Metcalfe & T. Shanks (San Francisco: ASP), 351 [ Links ]
Peterson, R. C., & Caldwell, N. 1993, AJ, 105, 1411 [ Links ]
Power, C., Navarro, J. F., Jenkins, A., et al. 2003, MNRAS, 338, 14 [ Links ]
Prugniel, Ph., & Siemen, F. 1994, A&A, 282, L1 [ Links ]
----------. 1997, A&A, 321, 111 [ Links ]
Press, W. H., Teukolsy, S. A., Vetterling, W. T., & Flan-nery, B. P. 1992, Numerical Recipes (New York: Cambridge University Press) [ Links ]
Sérsic, J. L. 1968, Atlas de Galaxias Australes (Córdoba, Argentina: Observatorio Astronómico) [ Links ]
Shen, S., Mo, H. J., & Shu, C. 2002, MNRAS, 331, 251 (SMS) [ Links ]
Syer, D., Mao, S., & Mo, H. J. 1997, astro-ph/9711160 [ Links ]
Springel, V., Yoshida, N., & White S. D. M. 2001, New Astronomy, 6, 79 [ Links ]
Schweizer, F. 1998, in Galaxies: Interactions and Induced Star Formation, Saas-Fee Advance Course 26, eds. D. Friedli, L. Martinet, & D. Pfenniger (New York: Springer-Verlag) [ Links ]
Toomre, A. 1977, in The Evolution of Galaxies and Stellar Populations, eds. B. M. Tinsley & R. B. Karson (New Haven: Yale Univ. Obs.), 401 [ Links ]
Tully, R. B., & Fisher, J. R. 1977, A&A, 64, 661 [ Links ]
Trujillo, I., Burkert, A., & Bell, E. F. 2004, ApJ, 600, L39 [ Links ]
Velázquez, H., & Aguilar, L. 2003, RevMexAA, 39, 197 [ Links ]
Wu, X., Fang, L., & Xu W. 1998, A&A, 338, 813 [ Links ] ]]>