2. QSO RX J1230.8+0115.
The data on RX J1230.8+0115 are given in Table 1. The X-ray flux was calculated assuming a neutral hydrogen column density = 2.2 x 1020 cm-2 and an X-ray spectral index .
Table 1. Data on QSO RX J1230.8+0115
The optical magnitudes were taken from the Edinburgh Multi-Colour Survey and represent mean values derived from two CCD-calibrated UK Schmidt Telescope plates in each waveband. The UKST plates were obtained in 1985 and were measured on the COSMOS machine at Edinburgh (MacGillivray & Stobie 1984). The accuracy of the averaged photographic magnitudes is 0.07 in U, B and V.
Adopting H0 = 50 km s-1 Mpc-1, q0 = 0.5 and an optical spectral index gives an absolute magnitude = -24.8 and an X-ray luminosity, (0.5-2.0keV), of 2.7 x 1043 erg s-1. The FWHMs of and present in the INT/FOS spectrum are approximately 1500 km s-1.
The INT/FOS spectrum (obtained in 1993) and a finding chart are shown in Fig 1.
2.2. One of the brightest QSOs and neighbour to 3C273
Ordering the Revised and Updated Catalog of QSOs (Hewitt & Burbidge 1993) in terms of apparent V-magnitude shows that QSO RX J1230.8+0115 is the 9th brightest QSO known (7th brightest in the B-band). It has a clearly stellar appearance on the UKST plates and given its apparent brightness and significant UV excess this object should have been an ideal candidate for earlier UVX surveys. Indeed it appears that this region of sky has been covered by at least one previous survey (Green, Schmidt & Liebert 1986). Lying only 54 arcminutes away from 3C273 makes it more remarkable that this object remained undetected until now as presumably the surrounding area will have been the target of other surveys. Interrogating SIMBAD and NED has produced no matches for this object and it does not show up in any published radio catalogues.
The discovery of RX J1230.8+0115 provides further evidence for incompleteness in existing surveys for bright QSOs as previously discussed by Goldschmidt et al. (1992, 1998). In addition, its brightness and proximity to 3C273 fortuitously provides a means for studying the spatial extent and absorption features of any intervening matter (low redshift Lyman- systems). To this end QSO RX J1230.8+0115 was the target of HST observations carried out in 1996, the results of which will be published elsewhere.
© European Southern Observatory (ESO) 1998
Online publication: June 12, 1998