Fabry-Perot Absorption-Line Spectroscopy of NGC 7079: Kinematics and Bar Pattern Speed

• Published in: The Astrophysical journal 2004-04, Vol.605 (2), p.714-724
• Main Authors: Debattista, Victor P, Williams, T. B
• Format: Article
• Language: English
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1086/382585

We present Fabry-Perot absorption-line spectroscopy of the SB0 galaxy NGC 7079. This is the first use of Fabry-Perot techniques to measure the two- dimensional stellar kinematics of an early-type disk galaxy. We scan the infrared Ca II line using the Rutgers Fabry-Perot (RFP), to obtain kinematic data extending to I-band surface brightness mu sub(I) ~ 21 mag arcsec super(-2), in a field of radius [approx]40[arc sec]. The kinematic data, consisting of line-of-sight velocities and velocity dispersions, are in good agreement with data obtained along the major axis of the disk with standard slit spectroscopy. Comparison of the exposure times required for slit and RFP spectroscopy to reach the same limiting magnitude shows that the RFP is significantly more efficient for mapping absorption-line galaxy kinematics. We use the velocity data, together with our own deep broadband photometry, to measure the bar pattern speed, [Omega] sub(p), of NGC 7079 with the model- independent Tremaine-Weinberg (TW) method. We find [Omega] sub(p) = 8.4 plus or minus 0.2 km s super(-1) arcsec super(-1); this is the best-constrained pattern speed ever measured for a bar using the TW method. From the rotation curve, corrected for asymmetric drift, we calculate the corotation radius and find that the bar ends just inside this radius. The two-dimensional character of these data allow us to show that the TW method is sensitive to errors in the position angle (P.A.) of the disk. For example, a P.A. error of 2 degree can give errors [approx] plus or minus 25% in [Omega] sub(p).