Simulations Of The Evolution Of The Gas, And The Stellar And Dark Matter Distributions, Caused By The Collision Of The Galaxy Pair NGC 3395/6 (Arp 270)

Details Simulations Of The Evolution Of The Gas, And The Stellar And Dark Matter Distributions, Caused By The Collision Of The Galaxy Pair NGC 3395/6 (Arp 270) Simulations Of The Evolution Of The Gas, And The Stellar And Dark Matter Distributions, Caused By The Collision Of The Galaxy Pair NGC 3395/6 (Arp 270)

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.1342l&link_type=abstract

American Astronomical Society, HEAD meeting #9, #13.42; Bulletin of the American Astronomical Society, Vol. 38, p.373

Astronomy and Astrophysics

Astronomy

Scientific paper

The colliding galaxy pair NGC 3395/6 (Arp 270) is observed by Chandra to have diffuse million-degree gas that is centrally located in each galaxy and is distinguishable from the many hotter point sources. The system has features indicative of a recent strong collision of two gas-rich galaxies, such as an extended tidal tail observed in HI and many star-forming knots that have been discovered in the optical and UV using HST. The hot, extended gas may have been produced in shocks in large-scale flows of in-falling gas resulting from the collision, and may have contributions from outflows produced by many SN explosions following the increased rate of star formation. We are investigating these possibilities by numerically simulating the collision between suitably constructed models of gaseous disk galaxies. We have explored the collision geometry and initial relative velocity needed to produce the currently observed configuration, using N-body simulations of the collision of an Sbc galaxy with an Sd (zero bulge) galaxy. (The mass ratio of the two galaxies is 2:1 and both have dark-matter halos with a mass approximately four times that of their respective disks.) We then use an N-body/SPH code to explore the evolution of the galaxy pair in more detail, paying particular attention to the evolution of the two gaseous disks. We look for the formation of dense clumps that would lead to star formation, for the production of the very extended tidal tail, and for the regions where large-scale shock heating of the gas takes place. We compare the results of our simulations with the available observational data. Using the observationally determined galactic masses and radii, we constrain the timescales for the production of various collision-induced features. We discuss the implications of the results for the production of the hot gas.

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