Abstract
The Lyα line emission of high-redshift galaxies depends on the density and temperature distribution of the gas, the kinematics and the dust content. We use a finite element method to model theLyα radiation of different 3D configurations considering complete frequency redistribution and the influence of velocity fields. Our results show that the central absorption feature of the double-peaked Lyα line profile observed in many radio galaxies with z=2-4 is probably the consequence of frequency redistribution rather than foreground absorption. The blue peak of the profile is enhanced for models with in fall motion and the red peak for models with outflow motion. In particular, we attempt to model the extendedLyα emission of high-redshift radio galaxies, where we consider results of corresponding hydrodynamical simulations to select possible model configurations. We find that Lyα photons scattered outside a jet-influenced low-density region are able to produce an extended Lyα halo.
Similar content being viewed by others
References
Ajiki, M., Taniguchi, Y., Murayama, T. et al.: 2002, ApJ 576, L25.
Binette, L, Kurk, J.D., Villar-Martín, M. and Röttgering, H.J.A.: 2000, A&A 356, 23.
Dawson, S., Spinrad, H., Stern et al.: 2002, ApJ 570, 92.
De Breuck, C., Röttgering, H., Miley, G., van Breugel, W. and Best, P.: 2000, A&A 362, 519.
Hu, E.M., Cowie, L.L., McMahon, R.G. et al: 2002, ApJ 568, L75.
Krause, M.: 2002, A&A, 368, L1.
Kurk, J.D., Röttgering, H.J.A., Miley, G.K. and Pentericci, L.: 2002, RevMexAA (Serie de Conferencias) 13, 191.
Meinköhn, E. and Richling, S.: 2002, A&A 392, 827.
Richling, S., Meinköhn, E., Kryzhevoi, N. and Kanschat, G.: 2001, A&A 380, 776.
Steidel, C.C., Adelberger, K.L., Sharply, A.E. et al.: 2000, ApJ 532, 170.
van Ojik, R., Röttgering, H.J.A., Miley, G.K. and Hunstead, R.W.: 1997, A&A 317, 358.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Richling, S. Modeling the Lyα radiation of high-redshift galaxies. Astrophysics and Space Science 284, 361–364 (2003). https://doi.org/10.1023/A:1024090313388
Issue Date:
DOI: https://doi.org/10.1023/A:1024090313388