BRAINE, J.; DAVOUST, E.; ZHU, M.; LISENFELD, U.; MOTCH, C.; SEAQUIST, E. R.

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BRAINE, J.
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]

DAVOUST, E.
Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées [LATT]

ZHU, M.

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Ce document a été publié dans

Astronomy and Astrophysics - A&A. 2003, vol. 408, p. L13-L16

EDP Sciences

Résumé en anglais

The Taffy Galaxies system, UGC 12914/5, contains huge amounts of molecular gas in the bridge region between the receding spirals after a direct collision. $2 - 9 \\times 10^9$M$_\\odot$ of molecular gas is present between the galaxies, more than the CO emission from the entire Milky Way! Such dense gas can only be torn off by collisions between dense clouds, in this case with relative velocities of about 800 $\\kms$, such that the remnant cloud acquires an intermediate velocity and is left in the bridge after separation of the colliding galaxies. We suggest that after ionization in the collision front, the gas cooled and recombined very quickly such that the density remained high and the gas left the colliding disks in molecular form.< Réduire

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Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804