An X-ray Loud Low Redshift QSO Near the BALQSO UM 232
Session 105 -- Broad Absorption Line Quasars
Display presentation, Saturday, January 1, 9:30-6:45, Salons I/II Room (Crystal Gateway)

## [105.01] An X-ray Loud Low Redshift QSO Near the BALQSO UM 232

V. T. Junkkarinen, T. A. Barlow, R. D. Cohen (CASS/UCSD)

We report the discovery of a low redshift, faint QSO (0020+0105, z = 0.422, V = 19.3) 2.9 arcminutes from the Broad Absorption Line QSO (BALQSO) UM 232 (0019+0107, z = 2.127, V = 17.6). This object was selected because it is near the position of the Einstein IPC X-ray source and it is UV bright on direct images of the UM 232 field taken with the KPNO No. 1 0.9m telescope and TEK2 CCD. The 1950 coordinates of 0020+0105 are RA = 00:20:01.5 and DEC = +01:05:26. A low resolution spectrum of 0020+0105 was obtained with the Lick 3m telescope and Kast double spectrograph. The emission lines in the spectrum of 0020+0105 include broad Mg II $\lambda$2798, narrow [O II] $\lambda$3727 and [O III] $\lambda \lambda$4959,5007, and weak, broad and narrow H$\beta$.

An X-ray detection of UM 232 with the Einstein IPC has been reported in the literature (Bregman, 1984, Ap. J., 276, 423). However, the low redshift QSO, 0020+0105, is only 0.5 arcminutes away from the Einstein X-ray position, while UM 232 is 2.7 arcminutes away from the Einstein X-ray position. The X-ray source is listed in the Einstein Observatory Catalog of IPC X-ray Sources'' (EOSCAT, 1993, SAO/NASA publication) as 2E0075 with a position error of 37 arcsec (90\% confidence). Given the X-Ray position and associated error, we consider the low redshift QSO to be the more likely identification for the X-ray source. There are some galaxies in the field as well, but identification with a faint cluster of galaxies is less likely since serendipitous point--like X-ray sources are identified more often with AGN (for example Stocke et al. 1991, Ap. J. Supp., 76, 813). The optical brightness (V = 19.3), X-ray flux ($\rm l_x \approx 2.5 \times 10 ^{-13}$ $\rm erg~cm^{-2}~s^{-1}$ 0.16 to 3.5 keV), and redshift (0.422) of 0020+0105 suggest that it is a fairly typical X-ray selected AGN (Stocke et al.~1991). The Einstein IPC observations only provide an upper limit to the X-ray emission from the BALQSO UM 232.

This research has been supported by NASA NAG 5$-$1630.