NGC 1132. We extracted spectra in four contiguous, concentric annuli, with
outer radii 0.8', 1.6', 2.4', and 3.7' (21, 43, 66, and 100 kpc),
respectively. In order to obtain interesting constraints, we tied the
abundances in all four annuli. We found a roughly flat temperature profile
(kT ~= 1.0 keV) when only one hot gas component was used. We found a
slight improvement in the fit if two hot gas components (kT = 0.8 and 1.6
keV) were used in the central bin. Our best-fitting abundance within the
4' radius was in good agreement with previous ASCA determinations (Buote
2000b; Mulchaey & Zabludoff 1999). Recent XMM measurements show evidence
of a significant abundance gradient (Gastaldello et al. 2004, F.
Gastaldello et al. 2006, in preparation); within ~4', our abundance
determination is in good agreement with XMM.
The bright X-ray source (Bauer et al. 2000), low FIR/radio ratio based
on Knapp et al. (1989) FIR limits, and NVSS radio lobes extending well
beyond galaxy of stars all indicate that the radio source is powered
by an AGN.
NGC 1132. - No features are found in this galaxy. ASCA observations
indicate that this galaxy is surrounded by a large, grouplike,
X-ray-emitting halo (Mulchaey & Zabludoff 1999).
Double system 02 49.8 -01 30 = NGC 1126 and 02 49.9 -01 29 at 8.3 preceding
and 6.9 preceding, 0.9 x 0.2, early spiral and 0.9 x 0.3, spiral, separation
1.5, m=15.4 and 15.7
Companion 3.4, 345, 0.3 x 0.3, faint
See UGC 02345