Open AccessA fast bar in the post‐interaction galaxy NGC 1023
Author(s) -
Debattista Victor P.,
Maria Corsini Enrico,
Aguerri J. A. L.
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05269.x
Subject(s) - physics , astrophysics , bar (unit) , galaxy , radius , dwarf galaxy , dark matter halo , disc galaxy , stellar kinematics , halo , dark matter , astronomy , galaxy formation and evolution , milky way , computer security , meteorology , computer science
We measured the bar pattern speed, Ω p , of the SB0 galaxy NGC 1023 using the Tremaine–Weinberg method with stellar‐absorption slit spectroscopy. The morphology and kinematics of the H i gas outside NGC 1023 suggest it suffered a tidal interaction, sometime in the past, with one of its dwarf companions. At present, however, the optical disc is relaxed. If the disc had been stabilized by a massive dark matter halo and formed its bar in the interaction, then the bar would have to be slow. We found Ω p =5.0±1.8 km s ‐1 arcsec ‐1 , so that the bar ends near its corotation radius. It is therefore rotating rapidly and must have a maximum disc.