Contents

A&A 414, 487-496 (2004)
DOI: 10.1051/0004-6361:20031686

Optically bright active galactic nuclei in the ROSAT-Faint source catalogue[*]

M.-P. Véron-Cetty 1 - S. K. Balayan 2 - A. M. Mickaelian 2 - R. Mujica 3 - V. Chavushyan 3 - S. A. Hakopian 2 - D. Engels 4 - P. Véron 1 - F.-J. Zickgraf 4 - W. Voges 5 - D.-W. Xu 6,5


1 - Observatoire de Haute Provence, CNRS, 04870 Saint-Michel l'Observatoire, France
2 - Byurakan Astrophysical Observatory and Isaac Newton Institute of Chile, Armenian branch, Byurakan 378433, Aragatzotn province, Armenia
3 - INAOE, Apdo. postal 51 y 216, 72000 Puebla, Pue., Mexico
4 - Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
5 - Max-Planck-Institute für extraterrestrische Physik, Postfach 1312, 85741, Garching, Germany
6 - National astronomical observatories, Beijing 100012, PR China

Received 10 June 2003 / Accepted 17 October 2003

Abstract
To build a large, optically bright, X-ray selected AGN sample we have correlated the ROSAT-FSC catalogue of X-ray sources with the USNO catalogue limited to objects brighter than O=16.5 and then with the APS database. Each of the 3212 coincidences was classified using the slitless Hamburg spectra. 493 objects were found to be extended and 2719 starlike. Using both the extended objects and the galaxies known from published catalogues we built up a sample of 185 galaxies with $O_{\rm APS}<17.0$ mag, which are high-probability counterparts of RASS-FSC X-ray sources. 130 galaxies have a redshift from the literature and for another 34 we obtained new spectra. The fraction of Seyfert galaxies in this sample is 20%. To select a corresponding sample of 144 high-probability counterparts among the starlike sources we searched for very blue objects in an APS-based color-magnitude diagram. Forty-one were already known AGN and for another 91 objects we obtained new spectra, yielding 42 new AGN, increasing their number in the sample to 83. This confirms that surveys of bright QSOs are still significantly incomplete. On the other hand we find that, at a flux limit of 0.02 count s-1 and at this magnitude, only 40% of all QSOs are detected by ROSAT.

Key words: quasars: general - X-rays: galaxies - galaxies: Seyfert

1 Introduction

The ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC) is derived from the all-sky survey performed during the ROSAT mission in the energy band 0.1-2.4 keV; it contains 18811 sources down to a limiting ROSAT-PSPC count-rate of 0.05 count s-1 (Voges et al. 1999). The 2012 brightest (count-rate above 0.2 count s-1) high galactic latitude ( $\vert b\vert>30^{\rm o}$) sources of the BSC catalogue have been tentatively optically identified by Schwope et al. (2000). The ROSAT Faint Source Catalogue (FSC) (Voges et al. 2000) contains 105 924 sources and represents the faint extension of the RASS-BSC.

The Hamburg QSO Survey is a wide-angle objective prism survey for finding bright QSOs in the northern sky. The survey plates have been taken with the former Hamburg Schmidt telescope now located at the Spanish-German Center in Calar Alto (Spain). A 1 $\hbox{$.\!\!^\circ$ }$7 objective prism has been used providing unwidened spectra with a dispersion of 1390 Å mm-1 at H$\gamma$(Hagen et al. 1995). The slitless spectra allow the classification of objects brighter than about B=17.0. The first study of a sample of previously known QSOs with the ${\it Einstein~Observatory}$ has shown that, as a class, they are luminous X-ray emitters (Tananbaum et al. 1979). Bade et al. (1998) and Zickgraf et al. (2003) have described a way to identify X-ray sources by using the Hamburg survey plates; this process has been applied to a subsample of 5341 sources from the ROSAT-BSC.

In the present paper we try to find all AGN brighter than O=16.5 in a subarea of the ROSAT-FSC. As the FSC survey is only about 2.5 times deeper than the BSC survey, we do not expect a significant difference in the identification content of these two samples but, because the number of sources in the FSC survey is much larger, we expect the discovery of many additional optically bright AGN. As the ROSAT survey is a low-energy survey, it contains a relatively high fraction of Narrow-Line Seyfert 1 Galaxies (NLS1s) because they usually have a soft X-ray excess (see for instance Laor et al. 1997); we therefore expect to find new bright NLS1s.

In the following we call AGN (or Active Galactic Nuclei) QSOs, BL Lac objects, Seyfert galaxies and Liners. QSOs are defined as Seyfert 1 galaxies brighter than M B=-23.0[*].


  \begin{figure} \par\includegraphics[clip,width=7.9cm]{HISTO_FX.eps}\end{figure} Figure 1: Histogram of the logarithm of the X-ray count rates (in counts s-1) of the 29 321 ROSAT-FSC sources.

2 Analysis

2.1 The sample

In the area of the sky defined by $\delta_{1950}>$ 0$^{\rm o}$ and $\vert b\vert>30^{\rm o}$ (10 313 deg2) there are 29 321 ROSAT-FSC sources.

Figure 1 shows the histogram of the logarithm of the X-ray count rates of these sources (in counts s-1). Below 0.02 counts s-1 the survey is obviously quite incomplete, reflecting the fact that its sensitivity limit is not uniform over the sky. On the other hand 130 sources have a count rate greater than 0.05 counts s-1 but were not included in the BSC as their detected photon number was less than 15. They were included in the FSC.

Figure 2 shows the distribution over the sky of (a) the 29 321 sources and (b) the 15 848 sources with Fx>0.02 counts s-1. The second distribution is much more uniform than the first and, in the following, we shall restrict our analysis to this subsample.


  \begin{figure} \par\includegraphics[clip,width=8.2cm]{CARTE.eps}\end{figure} Figure 2: Distribution over the sky of a) the 29 321 ROSAT-FSC sources, b) the 15 848 sources brighter than 0.02 counts s-1.

2.2 Identification methodology

Our aim being to identify all bright extragalactic objects associated with a ROSAT-FSC source in the area defined above, we chose to make use of the Hamburg slitless survey of the northern sky which, in principle, allows us to determine the nature of every object brighter than $O\sim17.0$. However this would require us to visually inspect all objects within a given radius around each of the 15 848 X-ray sources in the sample. This is obviously not feasible. We therefore decided to preselect all bright objects lying near the X-ray positions in the APS database, which is a catalogue of all objects visible on the Palomar Sky Survey plates, including magnitude, colour and classification as starlike or extended. But this could not be easily done as the APS was not directly available (when we started this work). The USNO catalogue is similar to the APS catalogue except that it does not classify the listed objects as starlike or extended; but it is available on CD-ROMs. It was therefore easy to select all bright USNO objects near the X-ray positions. We then sent the list of 3776 selected objects to the University of Minnesota where a batch job was run to find their APS magnitude, colour and classification.

However, as very bright stars (O<12.0) are saturated on the DSS1 images and bright extended galaxies are poorly recognized by the automatic extraction procedures of both the USNO and APS databases, to find these objects we had to cross-correlate the X-ray catalogue with various catalogues of bright stars and galaxies. We ended up with 3212 objects found in the APS database, 685 bright stars and 91 additional galaxies.

The APS classification as "star-like" or "extended" were then evaluated by visual screening of the DSS2 images. 2719 APS objects were found to be "star-like" and 493 "extended". All 3212 APS objects were subsequently classified using the digitized objective prism spectra of the Hamburg Quasar Survey.

Follow-up observations were started for the "extended" objects and additional galaxies having $O_{\rm APS}<17.0$, showing the sample to be a mixture of galaxies containing 20% AGN.

The "star-like" objects were separated into several subsamples according to their APS colour and magnitude. A sample of 144 high-probability AGN candidates was selected. Based on literature data and our own follow-up spectroscopy, 83 of them are now confirmed AGN.


  \begin{figure} \par\includegraphics[clip,width=8cm]{ROSAT_PPM.eps}\end{figure} Figure 3: Position differences for the coincidences between ROSAT-FSC X-ray sources and PPM stars within two arcminutes. The radius of the circle is 25 $\hbox {$^{\prime \prime }$ }$.

2.3 The USNO and APS databases

To identify the X-ray sources with relatively bright optical counterparts we have cross-correlated our ROSAT sample with the USNO-A2.0 catalogue (Monet et al. 1996) from which we have extracted all objects in the magnitude range O=12.0-16.5 (4 420 441 i.e. 428 deg-2). We have found 25 549 objects located within 2 $\hbox{$^\prime$ }$ of one of the 15 848 X-ray sources.

As the USNO catalogue positions are rather poor for very bright objects, we have extracted the 1306 PPM (Positions and Proper Motions) stars (Röser & Bastian 1991) located within 120 $\hbox {$^{\prime \prime }$ }$ of a ROSAT position. The PPM star catalogue contains 181 731 stars north of declination -2 $\hbox{$.\!\!^\circ$ }$5 , brighter than about $m_{\rm pg}=11.0$. Figure 3 shows the distribution of the position differences between the ROSAT and PPM positions. The circle drawn on the figure has a radius of 25 $\hbox {$^{\prime \prime }$ }$. The number of coincidences within this circle is 704 (with 19 X-ray sources being associated with two PPM stars), while the expected number of chance coincidences is 27. There are therefore 685 X-ray sources within 25 $\hbox {$^{\prime \prime }$ }$ of at least one PPM star. We consider these 685 sources as identified; we ignored them in the following and we are left with 15 163 X-ray sources.

The histogram of the separation between the optical and X-ray positions (Fig. 4) shows that, for separations larger than 35 $\hbox {$^{\prime \prime }$ }$, there is an overwhelming majority of chance coincidences. For smaller separations, the fraction of real associations rapidly increases. This empirically defined limit is a compromise to maximize the number of real associations and minimize the number of chance coincidences. It is not straightforward to determine the fraction of real associations having a separation larger than 35 $\hbox {$^{\prime \prime }$ }$ and therefore lost by using this limit. For separations smaller than 35 $\hbox {$^{\prime \prime }$ }$, there are 3776 coincidences, half being expected by chance and half real. Including the PPM stars, about 17% of the X-ray FSC sources are therefore physically associated with a relatively bright object.

Zickgraf et al. (2003) found that the 90% error radius for the X-ray positions in the BSC is 21 $\hbox {$^{\prime \prime }$ }$. This is significantly smaller than the value of 35 $\hbox {$^{\prime \prime }$ }$ we used for the separation limit for real associations. This difference can probably be ascribed to the differences in count rates between the two samples.

In total there are 3364 X-ray sources with at least one USNO object within 35 $\hbox {$^{\prime \prime }$ }$: 2985 with a single USNO object, 348 with two, 29 with three and 2 with four.


  \begin{figure} \par\includegraphics[clip,width=8.2cm]{histo_dis.eps}\end{figure} Figure 4: Histogram of the square of the separation between the X-ray and USNO positions for the 25 549 associations in units of 100 square arcsec.

In the APS database (Cabanela et al. 2003), the objects are classified as starlike or resolved (galaxies). The photometric calibration for the starlike objects uses a magnitude-diameter relation derived from photoelectric calibrating sequences. The O magnitudes have a mean rms of 0.15-0.20 mag over the range 14-20 mag. These magnitudes are not as reliable for objects brighter than 12th mag because of the diffraction pattern. For objects brighter than 8th mag, photometry is not available. For galaxies, the integrated magnitudes are obtained from a density-to-intensity conversion. APS derived galaxy magnitudes show no systematic photometric errors and a typical rms scatter of 0.2 to 0.3 magnitudes. The $O_{\rm APS}$ and B magnitudes for stars are equal on average with a dispersion of 0.26 mag (Mickaelian et al. 1999).

In contrast, the USNO catalogue makes no distinction between starlike and extended objects. As a consequence, the magnitudes derived for galaxies are unreliable. The typical photometric error for starlike objects is about 0.31 mag rms (Mickaelian et al. 2001). Bright objects tend to saturate. The magnitudes reported for such objects are generally too high.

Figure 5 shows the comparison of the USNO and APS O magnitudes for starlike objects (left panel) and for galaxies (right panel). While the agreement between the two sets of magnitudes is reasonably good for starlike objects, it is very poor for galaxies.


  \begin{figure} \par\includegraphics[clip,width=8.6cm]{MAG_MAG.eps}\end{figure} Figure 5: Comparison of the USNO and APS O magnitudes for starlike objects ( left panel) and for galaxies ( right panel). The solid lines represent the best linear fits between the two sets of data; the dotted lines have a slope of unity.

Figure 6 shows the comparison of the USNO and APS O magnitudes with the NPM1 O magnitudes (Klemola et al. 1987) for 95 galaxies and 81 stars. The least square solutions for galaxies are:
$O_{\rm NPM1G} = 0.47\times O_{\rm USNO}$ + 11.3 ($\sigma$ = 0.54 mag)
$O_{\rm NPM1G} = 0.90\times O_{\rm APS}$ - 0.29 ($\sigma$ = 0.50 mag).


  \begin{figure} \par\includegraphics[clip,width=8.5cm]{COMP_MAG.eps}\end{figure} Figure 6: Comparison of the USNO and APS O magnitudes with the NPM1 O magnitudes for 95 galaxies (filled squares) and 81 stars (open circles). The dotted lines have a slope of unity.

This confirms that, for galaxies, the APS magnitudes are more reliable than the USNO magnitudes. We therefore extracted from the APS database objects within 10 $\hbox {$^{\prime \prime }$ }$ from the 3776 USNO objects, brighter than O=19.0. A number of these have no APS counterpart because the required plates were not available and 49 because there was no match. We checked these 49 USNO objects on the DSS2 images (Lasker et al. 1996) and found that all of them, except one, have a starlike appearance. There are 3212 coincidences between USNO and APS objects (the 3212 sample), 2652 with starlike and 560 with extended objects.

As the APS classification based on DSS1 is not always correct, all 3212 images have been checked on the DSS2 plates. Of these, 2719 were classifd as starlike and 493 as extended. Out of the 560 APS galaxies, 135 have been reclassified as starlike; 45 of them appear as binaries so that in the APS they appear as extended. On the other hand, 68 APS starlike objects have an extended image on the DSS2.

2.4 The Hamburg database

All 3212 objects have been tentatively classified using the Hamburg slitless plates on the basis of a classification scheme introduced during the ROSAT-BSC identification program (Bade et al. 1998). The statistics of this classification is given in Table 1. Of the 493 objects classified as extended, based on direct images of the DSS2 plates, four could not be classified spectroscopically because of overlapping spectra. Based on their continua the 489 remaining objects were classified as "galaxy" (red continuum),"blue galaxy" (blue continuum) or "AGN" (prominent UV excess). Sixty one of the galaxies are member of a pair (23) or of a group (38). Among the starlike objects, 2181 were classified as stars due to absorption features in their spectra. The bright saturated objects ( $O_{\rm APS}<12.0$) were also considered as stars. Moreover 383 starlike objects, too weak for the study of absorption features, were classified on the basis of their continuum: red (RED-WK), blue (BLUE-WK) and extremely blue (EBL-WK). These objects have typically $O_{\rm APS}>16.0$. Twenty two starlike objects were classified as QSOs due to the presence of a prominent UV excess and/or of emission lines. Fifty five objects could not be classified because of overlapping spectra and one more because its spectrum did not fit the classification scheme.


 

 
Table 1: Statistics of the HQS type of 3212 optical associations with 2982 ROSAT FSC sources.
HQS types Number %
AGN 6 0.2
Blue galaxy 215 6.7
Galaxy 268 8.3
QSO 22 0.7
EBL-WK 84 2.6
BLUE-WK 212 6.6
RED-WK 87 2.8
W-Dwarf 20 0.6
Star-BA 137 4.3
Star-FG 1325 41.3
Star-K 674 21.0
Star-M 25 0.8
Saturated 81 2.5
Overlap 55 1.7
Unidentified 1 0.0
Total 3212 100.0


The HQS classifications have been checked with already known objects. In our sample there are 107 confirmed QSOs. Two could not be classified with the Hamburg material because of overlapping spectra. Seventeen have been classified as QSOs, one as an AGN, 56 as EBL-WK, 22 as BLUE-WK, two as RED-WK (J15563+0309, a low luminosity QSO with MB=-23.2 and KUV 16355+4146 at z=0.765, with (O-E)=1.60) and seven as blue galaxies. These blue galaxies are in fact low luminosity QSOs ( MB>-24.0). On the other hand eleven EBL-WK objects have been shown to be stars, as well as 21 BLUE-WK and two RED-WK objects. Clearly the EBL-WK objects are good QSO candidates as well as the BLUE-WK, although to a lesser degree. When they are not QSOs, they usually turn out to be WDs or CVs.

3 Galaxies

To find Seyfert galaxies we turned our attention to the 493 objects extended on the DSS2, found within 35 $\hbox {$^{\prime \prime }$ }$ of an FSC source. If there were no real association, the number of coincidences within 15 $\hbox {$^{\prime \prime }$ }$ would be 0.184 times the number of coincidences within 35 $\hbox {$^{\prime \prime }$ }$ (the ratio of the respective areas). On the other hand, if all associations were real, Fig. 4 shows that almost all identifications would be located within 35 $\hbox {$^{\prime \prime }$ }$ and about 50% within 15 $\hbox {$^{\prime \prime }$ }$. In a sample in which the fraction of coincidences within 15 $\hbox {$^{\prime \prime }$ }$ is x, the fraction y of true associations would be y=(x-0.184)/(0.5-0.184). 218 (x=44) of the 493 galaxies are within 15 $\hbox {$^{\prime \prime }$ }$ of an X-ray source which shows that a large fraction of them ($y\sim 80$%) are genuine associations.

As we have seen above, sixty eight of the objects found to be extended on the DSS2 were classified as starlike in the APS data base. Three of them (NGC 1085, IC 2439 and KUG 2323+85) were previously found to be bright galaxies and are included in Table 2. The 65 others are probably compact galaxies; 47 are classified as "blue galaxies" on the slitless HQS spectra (in fact, ten of them are already known to be Seyfert 1s or low luminosity QSOs).

As the spectroscopic observations took place before we had the opportunity to check the APS classification on the DSS2 images (which is a rather tedious procedure as it is done visually rather than automatically), these 65 objects were not included in our original list of galaxy candidates.

Of the 493 extended objects, 155 are brighter than $O_{\rm APS}=17.0$. Ninety four of them were classified as galaxies in the APS database. To these 94 galaxies we added 91 bright galaxies not appearing in the USNO or APS databases but found by cross-correlating the ROSAT FSC with catalogues of bright galaxies (NGC, UGC, NPM1G, Mark, Zw, etc.). As the surface density in these catalogues is small, we accepted as identification all coincidences within 35 $\hbox {$^{\prime \prime }$ }$. These 185 galaxy candidates are listed in Table 2. The redshift of 130 of them were known from the literature.


  \begin{figure} \par\includegraphics[clip,width=8.4cm]{SP_OHP.eps}\end{figure} Figure 7: Spectra of the six Seyfert 1, the three Seyfert 2 and three of the five starburst galaxies confirmed by our spectroscopic observations at BAO and OHP.

We have observed 34 of the galaxies without a previously known redshift at the BAO and OHP observatories. The BAO observations were made during the period March 3 to 10, 2002 with the 2.6-m telescope using the SCORPIO spectral camera attached to the prime focus. The combination of the detector, a $2063\times2058$ $16\times16$ $\mu$m pixel Loral Lick3 CCD, with a 600 g mm-1grism resulted in the spectral range 3900-7400 Å with a dispersion of 1.7 Å pixel-1. The slit width was 1 $\hbox{$.\!\!^{\prime\prime}$ }$8 (4.3 pixels) and was oriented EW. The spectral resolution was 5 Å FWHM. The exposure time was usually 45 min. The OHP observations were made between April 15 and 19, 2002 with the 1.93-m telescope and the spectrograph CARELEC (Lemaître et al. 1989) attached to the Cassegrain focus. The detector was a $2048\times1024$ $13.5\times13.5$ $\mu$m pixel EEV CCD. The dispersion was 1.75 Å pixel-1 and the spectral range 4075-7715 Å. The slit width was 2 $\hbox{$.\!\!^{\prime\prime}$ }$0, corresponding to 3.7 pixels, and the resolution was 5.7 Å FWHM. The exposure time was usually 20 min. We found 13 absorption line galaxies, five starburst galaxies, six Seyfert 1, three Seyfert 2 and seven unclassifiable weak emission line galaxies. Figure 7 shows the spectra of the Seyfert 1 and 2 galaxies and of three starburst galaxies.

In total the redshift of 164 of the galaxies is known. We have computed their 0.1-2.4 keV X-ray luminosity. Sixty-three are smaller than 1042 erg s-1and forty-five, greater than 1042.5 erg s-1. As there are probably no starburst galaxies having an 0.1-2.4 keV X-ray luminosity substantially higher than 1042 erg s-1 (Moran et al. 1996; Condon et al. 1998), most of the 45 high X-ray luminosity galaxies must be AGN. Among the 16 which have been classified, four are starbursts and 12 AGN. The 63 low X-ray luminosity galaxies could possibly be absorbed Seyfert 2s, low-luminosity AGN as well as starbursts, or elliptical galaxies with hot gas (Hornschemeier et al. 2001; 2003; Comastri et al. 2003; Severgnini et al. 2003). Several of our low X-ray luminosity sources have been classified as Liners, Seyfert 2s, Seyfert 1.9 or 1.8.

4 QSOs

Figure 8a shows the APS O-E colour index vs. the O magnitude for the 2652 starlike objects in the 3212 sample. Figure 8b is the same for objects within 15 $\hbox {$^{\prime \prime }$ }$ of a ROSAT-FSC source. These figures were divided into four zones.


  \begin{figure} \par\includegraphics[clip,width=8.4cm]{COLMAG_BIG.eps}\end{figure} Figure 8: a) APS O-E colour indices vs. O magnitudes for all starlike candidate identifications within 35 $\hbox {$^{\prime \prime }$ }$; b) the same for coincidences within 15 $\hbox {$^{\prime \prime }$ }$; c) the same for the A to G stars (filled circles) and the K and M stars (open triangles) as classified according to the Hamburg scheme; d) the same for the BLUE-WK and EBL-WK objects (filled triangles), the RED-WK objects (open triangles) and the QSOs (filled circles).

Objects brighter than $O_{\rm APS}=13.5$ (zone I) are most probably bright stars. Indeed among the 576 objects in this zone, 84 could not be classified on the Hamburg slitless spectra because of saturation or overlap, but all others are stars (25 BA, 416 FG and 51 K). Objects located above the diagonal line (zone II) are very red and are likely to be late-type stars. Fig. 8c shows that indeed K and M stars are mostly located in this zone. Among the 709 objects in this zone, 13 are affected by overlapping or saturation, 685 are stars (including 437 K stars); 11 were too weak to be classified.


  \begin{figure} \par\includegraphics[clip,width=4.8cm]{colmag_qso.eps}\end{figure} Figure 9: APS O-E colour indices vs. O magnitudes for 68 confirmed QSOs.

We cross-correlated the FSC with the current version of the Véron-Cetty & Véron (2001) AGN catalogue. We found 76 coincidences within 35 $\hbox {$^{\prime \prime }$ }$ with a previously known AGN brighter than $O_{\rm USNO}=16.5$ (they are listed in Table 3); 68 have magnitude and colour in the APS database. Figure 9 is a plot of the APS O-E colour index vs. the O magnitude for these 68 AGN; 87% (59/68) are located in zone IV defined by $O_{\rm APS}>15.5$ and O-E<1.2. With this limit on O-E, we exclude red QSOs; this is unavoidable because of the very large number of stars with O-E>1.2. These objects can be recovered by examination of the slitless spectra. Figures 8d and 9 show that the distributions of the representative points of the EBL-WK and BLUE-WK objects on the one hand and of that of QSOs on the other hand are quite similar.


  \begin{figure} \par\includegraphics[clip,width=8.5cm]{POSCOL.eps}\end{figure} Figure 10: Position differences between the ROSAT-FSC X-ray sources and APS starlike objects located in each of the four zones previously defined. The circles have a radius of 15 $\hbox {$^{\prime \prime }$ }$ and 35 $\hbox {$^{\prime \prime }$ }$, respectively.

Figure 10 shows the differences between the X-ray and optical positions for the starlike objects in the 3212 sample in each of the four zones defined above. In the first two zones there is an obvious concentration towards the centre showing that most of the coincidences are genuine associations. In contrast the distribution of the points in zone III is quite uniform suggesting that most of these coincidences are due to chance.

In zone III, the observed fraction of coincidences within 15 $\hbox {$^{\prime \prime }$ }$ is x=0.20, suggesting that there are indeed very few true associations (y=0.05). On the other hand, in zone I and II, we found x=0.47 and 0.45 respectively showing that basically all objects (90 and 84% respectively) are real associations.

For the 212 starlike objects classified as BLUE-WK on the Hamburg slitless spectra, we found x=0.24, so the fraction of true coincidences is about 18%, while for the 84 EBL-WK objects, x=0.51 and, within the statistical uncertainties, all are genuine associations.

Out of the 2652 starlike objects, zone IV contains 476 coincidences within 35 $\hbox {$^{\prime \prime }$ }$ and 136 (x=0.28) within 15 $\hbox {$^{\prime \prime }$ }$ of an X-ray source, implying that y=0.32; therefore 153 of these coincidences are likely to be genuine associations, 76 being located within 15 $\hbox {$^{\prime \prime }$ }$. They could be blue stars (WD, CV, sd), or more probably QSOs. We have divided zone IV in two subregions (see the dotted line in Fig. 8). In the upper region (IVb), only 23% of the coincidences are within 15 $\hbox {$^{\prime \prime }$ }$ and therefore a small fraction of the 332 coincidences are genuine. In the lower region (IVa) containing the bluest objects, 41% of the coincidences are located within 15 $\hbox {$^{\prime \prime }$ }$ from the X-ray source, suggesting that $\sim$70% of the 144 objects located in this zone are real identifications. Among them are 41 known QSOs. The 103 other candidates, of which seven are known stars, are listed in Table 4. We have spectroscopically observed 91 of them. The observations were carried out during three observing runs (May and August 2002 and May 2003) with the 2.1-m telescope of the Guillermo Haro Astrophysical Observatory (OAGH) located in Cananea (Sonora, Mexico), operated by INAOE, and one run (September 2003) with the OHP 1.93-m telescope and the same instrument setting as for the observations of the galaxies (see Sect. 3). The 2.1-m telescope was equipped with the LFOSC focal reducer (Zickgraf et al. 1997). The slit mask and the lower dispersion grism were used, giving a wavelength coverage from 4200 Å to 9000 Å and a dispersion of 8.2 Å pixel-1. We found 49 stars (including a CV the spectrum of which is shown in Fig. 11), 38 QSOs, 1 Seyfert 1, two NLS1s, one BL Lac object (their spectra are displayed in Figs. 12-14). Five candidates have not yet been observed.

Altogether, there are, in region IVa, 83 confirmed AGN in a total of 139 spectroscopically observed starlike objects (60%).


  \begin{figure} \par\includegraphics[clip,width=6.9cm]{SP_RAUL_CV.eps}\end{figure} Figure 11: Spectrum of a cataclysmic variable observed at OAGH.


  \begin{figure} \par\includegraphics[clip,width=8.4cm]{SP_RAUL_1.eps}\end{figure} Figure 12: Spectra of 18 QSOs from Table 4 observed at OAGH.


  \begin{figure} \par\includegraphics[clip,width=8.4cm]{SP_RAUL_2.eps}\end{figure} Figure 13: Spectra of 18 QSOs from Table 4 observed at OAGH.


  \begin{figure} \par\includegraphics[clip,width=8.4cm]{SP_RAUL_3.eps}\par\end{figure} Figure 14: Spectra of six objects from Table 4 (one Seyfert 1, one QSO, two BL Lac objects and two NLS1s) observed at OAGH.

But only 60% (41/68) of all previously known AGN with APS colour fall in zone IVa showing the limits of the efficiency of the procedure we have adopted. The others are located in zone IVb, or not far from it, in a region where chance coincidences between stars and X-ray sources become non negligible. Here the Hamburg slitless spectra may turn out to be most useful in separating AGN from stars.

5 Discussion

5.1 Identification procedure

We have seen that the galaxies found within 35 $\hbox {$^{\prime \prime }$ }$ of a ROSAT source have a high probability of being genuine identifications ($\sim$80%) and therefore we included all of them in our spectroscopic program.

In the case of starlike objects, the situation is more complex due to the facts that a large fraction of the X-ray sources are in fact X-ray stars and that, the surface density of stars being relatively large, there is a non negligible number of chance coincidences. The use of the O-E vs. O diagram turns out to be quite efficient to eliminate bright stars and late type stars. However, although in our region IVa most objects are genuine identifications, in zones IVb and III there are many chance coincidences with main sequence stars. The use of the Hamburg slitless spectra in these zones is crucial to separate QSOs from stars. In addition, Seyfert 1 galaxies are often compact and classified as starlike in the APS. Moreover they usually have a relatively red O-E colour; as a consequence they easily escape detection by our automatic procedure and classification on the basis of the slitless spectra is necessary.

The relatively poor positional accuracy of the ROSAT survey ( $\sigma\sim15\hbox{$^{\prime\prime}$ }$) makes it difficult to identify objects weaker than $\sim$16.5; but this limiting magnitude is well fitted by the magnitude limit below which no recognition of absorption features is possible in the Hamburg slitless spectra.

5.2 Completeness of our QSO sample

We have seen that only 85% of the bright USNO objects have a counterpart in the APS due mainly to the incompleteness of the data base. Moreover only 60% of the known QSOs fall into our zone IVa to which we have restricted our search. Therefore our sample is expected to be no more than 50% complete.

On the other hand, as our aim is to find all AGN brighter than a given optical magnitude, we have to answer the following question: how many such AGN are missed if we identify all bright AGN in a flux limited X-ray survey?


 

 
Table 5: Number and percentage of radio quiet and radio loud X-ray detected QSOs in the Véron-Cetty & Véron catalogue. Columns 1 and 2: $O_{\rm USNO}$ range, Col. 3: number of QSOs, Col. 4: number of sources brighter than 0.02 count s-1 in the ROSAT catalogues, Col. 5: percentage of ROSAT detected QSOs; Col. 6 to 8: the same for the radio loud QSOs.
  Radio quiet Radio loud
$O_{\rm min}$ $O_{\rm max}$ n $n_{\rm X}$ % n $n_{\rm X}$ %
  <15.5 80 58 72 9 7 78
15.5 16.0 90 48 53 21 17 81
16.0 16.5 243 101 42 49 37 76
16.5 17.0 433 144 33 99 60 61
17.0 17.5 679 101 15 172 77 45
17.5 18.0 900 60 7 201 59 29
18.0 18.5 977 23 2 169 41 24
18.5 19.0 1040 13 1 107 11 10
19.0 19.5 475 4 1 41 5 12
19.5 20.0 87 0 0 18 5 28


The current version of the Véron & Véron QSO catalogue contains 5893 QSOs at $\delta>0^{\circ}$, $\vert b\vert>30^{\circ}$, with B<20.0 and z>0.10, found in the course of radio or optical surveys (QSOs found as the identification of a X-ray source have been ignored). Of these, 871 are located within 35 $\hbox {$^{\prime \prime }$ }$ from a ROSAT-BSC or -FSC source (stronger than 0.02 count s-1). We consider them as genuine identifications; 319 are radio loud and 552 radio quiet.


  \begin{figure} \par\includegraphics[clip,width=8.4cm]{FXFOPT.eps}\end{figure} Figure 15: Plot of log( $F_{\rm X}/F_{V}$) vs. $O_{\rm USNO}$ for 552 radio quiet QSOs. The two diagonal lines correspond to the sensitivity limits of the BSC and FSC ROSAT survey (0.05 and 0.02 count s-1, respectively).

On average, QSOs with higher optical luminosity have higher X-ray luminosity. According to Maccacaro et al. (1988), log( $F_{\rm X}/F_{V})=\log(F_{\rm X})+0.4\times V+5.37$ where $F_{\rm X}$ is the X-ray flux in the 0.3-3.5 keV band in erg cm-2 s-1 and $F_{V}=-0.4 \times V-8.42$ is the flux in the V band in the same units. For the ROSAT survey, this translates into: log( $F_{\rm X}/F_{V})=\log($PSPC counts s $^{-1}\times 10^{-11})+0.4\times V+5.37$where $F_{\rm X}$ is the X-ray flux in the 0.1-2.4 keV band, assuming a conversion factor of 1 PSPC count s-1 for a flux of 10-11 erg cm-2 s-1 in this band which corresponds to an unabsorbed source with a photon index $\Gamma=2.3$, a typical value for QSOs (Voges et al. 1999).

Figure 15 shows log( $F_{\rm X}/F_{V}$) vs. $O_{\rm USNO}$ for the 552 radio quiet QSOs. Table 5 gives the fraction of ROSAT detected QSOs vs. their optical magnitude for both the radio quiet and the radio loud samples.

At $O_{\rm USNO}=16.0$, about half of the optically selected QSOs are not detected in X-ray (Table 5) and therefore have log( FX/FV)<-1 . Consequently the median value of their X-ray to optical flux ratio is $\sim$-1.0. Figure 15 suggests that $\sigma\sim 0.5$.

Zickgraf et al. (2003) found that the median value of log( $F_{\rm X}/F_{V}$) for X-ray selected QSOs is 0.39. The fact that these objects are significantly stronger X-ray sources than optically selected QSOs is due to the much higher frequency of the survey. Indeed Williams & Bridle (1967) and Kellermann et al. (1968) have shown that the relative numbers of sources with given spectral indices depend on the frequency at which the sample is selected. A sample selected at a low frequency (optical) will include a greater proportion of sources with high values of the spectral index than will a similar sample selected at a high frequency (X-ray).

In the simple case where the distribution of the spectral indices $\alpha$ in a complete sample of sources selected at a wavelength $\lambda_{\rm o}$ is Gaussian with a mean spectral index $\alpha_{\rm o}$ and a standard deviation $\sigma_{\alpha}$, the distribution of the spectral indices of sources selected at another wavelength $\lambda_{\rm X}$ will also be Gaussian with the same standard deviation $\sigma_{\alpha}$, but with a mean spectral index $\alpha_{\rm X}$ given by: $\alpha_{\rm X}=\alpha_{\rm o}+\mu\times\sigma^{2}_{\alpha}\times ln(\lambda_{\rm X}/\lambda_{\rm o}$). In this expression $\mu$ is the exponent in the population law $N(S)\sim S^{-\mu}$ giving the number of sources with flux densities in excess of a specified value S (Williams & Bridle 1967). With $\mu=1.87$, $\lambda_{\rm o}=5000$ Å and $\lambda_{\rm X}=12.4$ Å (1 keV), we find that to get the observed increased value of $F_{\rm X}/F_{V}$ by a factor 25, corresponding to $\alpha_{\rm X}$- $\alpha_{\rm o}=0.54$, a value of $\sigma_{\alpha}=0.22$ is required, i.e. $\sigma=0.57$, where $\sigma=2.60\times\sigma_{\alpha}$ is the standard deviation of log( $F_{\rm X}/F_{V}$). This is in reasonable agreement with our estimated value of $\sigma\sim 0.5$.

Table 5 confirms that radio loud QSOs are brighter X-ray sources than radio quiet QSOs. In addition we found that, for BL Lac objects, the mean $F_{\rm X}/F_{V}$ ratio is larger than that of the radio loud QSOs as previously shown by Stocke et al. (1985). BL Lac brighter than 15.5 are all detected by ROSAT while at $O_{\rm APS}=20.0$, 50% are still detected.

5.3 The surface density of bright QSOs

The surface density of bright QSOs is difficult to determine because these objects are rare and therefore large areas of the sky have to be surveyed to find a substantial number. The Bright QSO Survey (BQS) of Schmidt & Green (1983) covering 10 714 deg2, contains 69 QSOs brighter than MB=-24.0 and B=16.16, corresponding to $0.0064\pm0.0008$ deg-2. A number of works suggest that this value is substantially underestimated and that the completeness of the BQS is in the range 30%-70% (Wampler & Ponz 1985; Goldschmidt et al. 1992; La Franca & Cristiani 1997; Wisotzki et al. 2000; Mickaelian et al. 2001).

Grazian et al. (2002) have undertaken a program similar to ours. They cross-correlated the ROSAT-BSC with the Digitized Sky Survey in the southern hemisphere to find all coincidences between X-ray sources and stellar objects brighter than $B_{\rm J}<15.13$. After spectroscopic observations of the candidates, they obtained a sample of 111 AGN in an area of 5660 deg2, 57 being brighter than MB=-24.0. But the distribution of absolute magnitudes is rather odd, 46 being greater than -25.0 and 5 smaller than -26.0. We checked the appearance of some of the low redshift objects on the DSS images; they are clearly galaxies; their O magnitude in the APS data base is much greater than the B magnitude given by Grazian et al. and the absolute magnitudes computed with these O magnitudes are definitely greater than -24.0. The true number of QSOs in this sample is therefore unknown, but certainly significantly smaller than 57.

There are, in our region of interest (10 313 deg2), 503 known QSOs ( MB<-24.0 i.e. MO<-24.4) brighter than $O_{\rm USNO}=16.5$, i.e. B=16.9 (on the average, the $O_{\rm USNO}$ magnitudes are brighter than the photoelectric B magnitudes: $<O_{\rm USNO}{-}B>~={-}0.38$; Mickaelian et al. 2001). 191 are associated with a BSC source, 84 with a FSC source and 228 are not detected by ROSAT. Here we use USNO rather than APS O magnitudes because the selection has been made with the USNO data base; using the APS magnitudes, our sample would not be complete to O=16.5.

These 503 QSOs correspond to a surface density of $0.041\pm0.002$QSO deg-2 brighter than B=16.9. If the integrated number-magnitude relation has a slope equal to $b=\mu/2.5=0.75$ (Sandage & Luyten 1969), the surface density of QSOs brighter than B=16.16 is 0.0114 deg-2. Of these QSOs 142 are brighter than $O_{\rm USNO}=15.8$ (B=16.2), corresponding to $0.014\pm0.001$ deg-2, in agreement with the preceding value, confirming that the value of b used is reasonable.

The QSO counts are systematically affected by the photometric errors on the magnitudes as these errors scatter many more objects toward bright magnitudes than it does toward faint magnitudes. Assuming that the error distribution is Gaussian, with a dispersion $\sigma$, the correction to be applied to the observed counts is a factor 10 $^{(b+1)\sigma^{2}/2}$ (Eddington 1940). With b=0.75 and $\sigma=0.31$, the true QSO surface density is smaller by 1.21 than the observed one or, at B=16.16, $0.011\pm0.002$ deg-2. This is already 78% larger than the original Schmidt & Green estimate.

Sixty seven of the known QSOs ( MO<-24.4) with available APS magnitudes are associated with a ROSAT-FSC source, 35 being located in zone IVa (Table 3). In this zone, we have found 33 additional such objects (see Table 4), almost doubling the number of known QSOs at this limiting magnitude.

We should note in addition that, among the 84 EBL-WK objects, 14 have not yet been spectroscopically observed, while 5 of the QSOs candidates in Table 4 have still to be observed. This may increases the number of new bright QSOs.

6 Conclusion

We have undertaken a program of systematic identification of optically bright AGN in both the BSC- and FSC-ROSAT catalogues. In this paper we present preliminary results concerning the FSC catalogue. We describe the method used which consists of first cross-correlating the USNO and APS databases with the X-ray catalogue, then checking the nature of the candidates by looking at the slitless Hamburg spectra.

Among the starlike objects brighter than B=16.9 we have recovered 35 previously known QSOs in the region of the O/(O-E) diagram containing 60% of the bluest QSOs and discovered 33 new ones confirming that, even at these relatively bright magnitudes, available surveys are significantly incomplete.

The total number of previously known QSOs brighter than B=16.2 corresponds to a surface density 78% higher than the original Schmidt & Green value. But we have shown that, in the subsample studied here i.e. the QSOs associated with a ROSAT-FSC source, the completeness is at best 50%. Although we cannot generalize this to the whole sample, it is not unlikely that the true surface density is significantly higher than the number derived here.

We found that at this magnitude and at a flux limit of 0.02 counts s-1, only 40% of all QSOs are detected by ROSAT.

Acknowledgements

R.M. and V.Ch. acknowledge CONACyT research grants J32178-E and 39560-F. This work is partly based on observations obtained with 2.6-m telescope at the Byurakan Astrophysical Observatory, Armenia, the 1.93-m telescope at the Observatoire de Haute Provence (CNRS), France and the 2.1-m at the Guillermo Haro Astrophysical Observatory, Cananea, Mexico. The authors acknowledge the hospitality of INAOE during the Guillermo Haro Workshop 2003, at which time the scientific conclusions presented here were discussed. They are grateful to Dr. J. Cabanela for his help with the use of the APS databases which are supported by the National Science Foundation, the National Aeronautics and Space Administration, and the University of Minnesota, and are available at http://aps.umn.edu/. The Digitized Sky Survey was produced at the Space Telescope Science Institute (STScI) under U.S. Government grant NAG W-2166.

References

  
7 Online Material


 

 
Table 2: List of the 185 galaxy candidates. Column 1: right ascension, Col. 2: declination, Col. 3: separation between the ROSAT and USNO positions in arcsec, Col. 4: X-ray count rate (count s-1), Col. 5: logarithm of the 0.1-2.4 keV X-ray luminosity (in erg s-1), Col. 6: magnitude $O_{\rm USNO}$, Col. 7: magnitude $O_{\rm APS}$, Col. 8: redshift, Col. 9: classification (abs: galaxies with absorption lines only; em: emission line galaxies, but too weak to make a classification possible; C stands for Composite spectrum; S or S?: the object is certainly an AGN, but the lines are too weak for a more precise classification); Col. 10: references: (1) BAO; (2) OHP, Col. 11: name.
J2000 optical position                  
h m s $^{\circ}$ ' '' sep('') c/r $L_{\rm X}$ $O_{\rm US}$ $O_{\rm APS}$ z   ref. Name
0 14 7.46 10 34 13.3 5.3 0.036   15.0 16.89        
0 19 37.80 29 56 2.0 27.2 0.042 42.02   15.37 0.024     NGC 76
0 24 30.24 13 35 50.3 2.4 0.032   12.5 16.63       NPM1G+13.0013
0 46 29.20 8 25 59.6 18.9 0.023 42.18 15.5 16.32 0.039     UGC 482
0 54 45.23 16 26 17.2 9.2 0.038 42.37 13.6 16.56 0.038     MCG+03.03.008
0 54 48.64 28 52 1.1 26.7 0.024 41.74   15.66 0.023     UGC 555
0 57 48.89 30 21 8.8 7.3 0.043 41.67   13.14 0.016 Liner   NGC 315
1 16 14.83 31 2 1.8 34.2 0.021 41.42     0.017     NGC 452
1 20 38.97 29 41 43.9 9.4 0.031 41.85 16.0 15.40 0.023     IC 1672
1 30 35.46 19 36 31.0 4.2 0.034 42.43 13.7 16.35 0.043     UGC 1077
2 43 48.71 14 53 13.1 33.8 0.027 42.39   16.49 0.046     IC 1835
2 46 25.36 3 36 27.3 7.1 0.078 42.25 12.5 14.91 0.023     NGC 1085
2 51 12.98 13 11 31.3 16.1 0.031 41.92 13.8 16.34 0.025     UGC 2337B
2 58 51.14 6 22 25.9 5.4 0.026 42.35 13.5 16.88 0.045     LEDA 074274
7 50 8.28 55 23 2.9 18.6 0.032 41.70 12.6 15.43 0.019 abs 2 UGC 4035
8 1 55.04 62 32 15.0 6.0 0.034 42.88 14.0   0.072      
8 30 29.14 69 1 42.8 12.3 0.022 41.66 13.5   0.022     Zw 331.048
8 36 45.79 48 42 0.7 30.1 0.027   13.7 16.24       MCG+08.16.019
8 39 55.44 74 5 15.9 32.2 0.024   15.1         NPM1G+74.0038
8 55 38.01 78 13 25.3 5.0 0.024 40.41     0.005 Liner   NGC 2655
9 6 44.71 3 36 0.9 28.1 0.023   14.2          
9 8 38.35 32 35 34.0 15.9 0.033 41.44 12.4 15.79 0.014     IC 2439
9 11 37.50 60 2 15.0 22.9 0.026 40.45   12.12 0.005 S   NGC 2768
9 12 38.04 75 38 55.4 13.2 0.040 42.81 12.8   0.061 H II 1, 2 NPM1G+75.0038
9 16 3.95 17 37 43.6 10.1 0.060 42.34   14.63 0.029     NGC 2795
9 16 50.01 20 11 54.6 19.8 0.021 41.85   15.04 0.028     NGC 2804
9 19 27.31 33 47 26.4 26.4 0.029 41.65 13.7 16.83 0.019     LEDA 139185
9 20 2.10 1 2 18.0 15.9 0.046 41.76   14.27 0.017     UGC 4956
9 23 25.93 22 19 1.0 20.3 0.081 42.50 13.9   0.030     UGC 4991b
9 23 24.36 22 18 47.3 5.4 0.081 42.60 13.4   0.034     UGC 4991a
9 23 29.19 25 46 9.6 13.4 0.021 42.35 12.5 15.73 0.050 S2 1, 2 Zw 121.071
9 24 14.29 49 15 14.9 32.9 0.021 40.86   14.71 0.009     NGC 2856
9 25 28.30 23 36 31.6 1.5 0.035 42.21 12.2 16.12 0.033 em 1 Zw 121.086
9 25 42.55 11 25 55.3 14.6 0.034 41.25   14.31 0.011     NGC 2872
9 32 10.13 21 30 4.4 18.1 0.030 39.71     0.002 H II   NGC 2903
9 32 16.98 9 41 0.5 28.6 0.023   14.8 16.74       NPM1G+09.0188
9 38 12.30 7 43 39.8 19.9 0.033   13.8 16.84       Zw 035.017
9 38 32.90 17 1 52.0 17.9 0.040 42.13   16.00 0.028     NGC 2943
9 45 28.84 56 32 53.4 2.1 0.046 43.58 15.8 16.91 0.139 abs 1  
9 50 21.61 72 16 44.1 22.7 0.025 40.23     0.004 S1.9   NGC 2985
9 59 39.60 0 35 12.1 24.1 0.028 42.72 13.1 16.42 0.066     UGC 5370
10 1 57.80 55 40 47.1 4.2 0.049 40.53   12.23 0.004 S2   NGC 3079
10 6 7.45 47 15 45.4 22.0 0.036 41.98   15.09 0.025     NGC 3111
10 13 50.50 38 45 53.8 27.8 0.028 41.80   14.15 0.023     NGC 3158
10 27 49.91 36 33 34.7 24.4 0.037 42.34   16.02 0.037 S2   HS 1024+3648
10 32 33.34 65 2 0.9 33.2 0.023 40.55   14.42 0.006     NGC 3259
10 47 10.14 72 50 20.9 8.5 0.025 40.94     0.009     NGC 3348
10 51 29.91 46 44 41.5 24.1 0.026   13.3 16.00       NPM1G+47.0182
10 58 13.77 1 36 6.3 8.8 0.069 42.63 16.5   0.038 abs 1 UGC 6057c
10 58 13.04 1 36 24.3 29.9 0.069 42.65 15.1   0.039     UGC 6057b
11 0 5.35 14 50 26.5 28.4 0.026 40.45 15.9   0.005     NGC 3485
11 3 11.35 27 58 21.1 7.8 0.034 40.56 12.2 13.02 0.005 H II   NGC 3504
11 8 43.37 29 13 25.3 2.7 0.022 42.76 13.4 16.49 0.078 em 1, 2 LEDA 094150
11 10 45.96 11 36 41.2 14.3 0.025 42.28 13.2 16.16 0.042 S1 1 Zw 067.027
11 15 2.23 4 5 7.4 13.4 0.024 42.19 13.4 16.48 0.039     Zw 039.090
11 24 43.64 38 45 46.3 22.1 0.051 41.03 12.9 12.50 0.007 H II   NGC 3665
11 25 45.33 24 8 24.5 28.9 0.029 41.86 12.7 15.12 0.024     Zw 126.051
11 28 2.16 78 59 40.4 16.3 0.046   14.7   0.000 H II   UGC 6456
11 34 6.64 25 33 34.8 18.9 0.029   12.8 16.55       MCG+04.27.068
11 39 14.88 17 8 37.2 4.2 0.037 41.85 13.1 16.23 0.021     UGC 6614
11 39 41.57 31 54 41.1 2.9 0.034 41.07 15.9   0.009 S1.8   NGC 3786
11 46 12.24 20 23 29.9 27.2 0.048 42.04 14.5 14.61 0.023 Liner   NGC 3884
11 47 22.16 35 1 7.5 25.9 0.044 42.87 14.4 16.60 0.063 S2   B2 1144+35B
11 49 59.31 21 20 1.1 9.2 0.026 41.88   15.32 0.026     NGC 3910
11 50 41.53 20 0 54.6 10.2 0.031 41.77   15.55 0.021     NGC 3919
11 53 26.26 35 56 53.8 15.3 0.023 42.66 12.3 16.27 0.068 S2 2 KUG 1150+362
11 59 52.16 55 32 5.4 30.6 0.024 42.83 13.7 16.96 0.081     PGC 2505536
12 4 6.25 20 14 6.2 25.5 0.028 41.72 12.9 14.99 0.021     NGC 4065
12 4 43.34 31 10 38.2 16.7 0.025 41.83   15.11 0.025 S1.9   UGC 7064
12 5 49.83 35 10 46.4 11.9 0.190 43.38 12.7 16.74 0.054 S1   Mark 646
12 8 5.56 25 14 14.1 16.0 0.034 41.89   15.32 0.023     UGC 7115
12 10 33.61 30 24 5.9 21.4 0.045 39.29   13.71 0.001 C   NGC 4150
12 14 18.10 29 31 4.5 5.0 0.021 42.57   16.96 0.064 S2   WAS 49b
12 14 48.65 59 54 22.5 23.3 0.028 42.64 14.6 15.61 0.060     NGC 4199a
12 14 51.71 59 54 30.5 4.5 0.028 42.65 16.3   0.061 abs 1 NGC 4199b
12 15 5.34 76 14 10.0 34.4 0.031 40.68     0.006     UGC 7265
12 16 0.00 12 41 1.4 5.4 0.033 42.78   16.60 0.065 S1.9   Mark 764
12 19 51.66 28 25 21.7 12.6 0.046 42.13 13.8 16.27 0.026     Zw 158.075
12 20 6.86 29 16 50.5 11.4 0.037 39.80 12.6 12.53 0.002 Liner   NGC 4278
12 22 54.89 15 49 20.7 15.6 0.042 40.65   11.30 0.005 C   NGC 4321
12 23 39.10 7 3 14.0 24.6 0.030 40.06   14.80 0.003     NGC 4342
12 23 42.85 58 14 45.9 10.3 0.037 41.55 14.5 16.93 0.015 S?   SBS 1221+585
12 26 28.02 9 1 23.0 26.7 0.029 41.86 14.7 14.58 0.024 Liner   NGC 4410
12 26 26.98 31 13 22.6 4.4 0.033 39.75 12.2 12.17 0.002 C   NGC 4414
12 28 29.49 17 5 6.0 9.8 0.039 40.91   12.21 0.007 Liner   NGC 4450
12 34 3.10 7 41 59.0 24.2 0.032 39.14   11.85 0.001 H II   NGC 4526
12 34 46.81 47 45 32.4 34.2 0.043 42.25   16.12 0.031     MCG+08.23.061
12 48 58.34 40 35 56.8 14.5 0.039 41.58 15.2 15.95 0.015     IC 3808
12 50 26.60 25 30 5.8 8.3 0.028 40.28   11.04 0.004 S2   NGC 4725
12 55 7.78 78 37 14.9 4.1 0.029 42.36 12.9   0.043 S1 1 NPM1G+78.0053
12 56 43.76 21 40 51.9 7.2 0.041 39.25   10.36 0.001 S   NGC 4826
12 59 39.35 38 48 56.3 16.0 0.022 42.01 13.2 16.23 0.033     IC 4003
13 0 39.13 2 30 5.3 22.4 0.027 40.02   12.98 0.003 H II   NGC 4900
13 4 40.89 43 18 35.0 20.1 0.031   14.0 16.86       NPM1G+43.0235
13 4 57.99 43 33 10.9 25.2 0.052   13.1 16.06       MCG+07.27.026
13 7 3.03 56 31 59.2 5.5 0.044 43.08 12.4 16.40 0.080 S1 1, 2 MCG+10.19.033
13 20 28.94 31 21 6.9 19.8 0.029 42.42 12.8 16.53 0.046     Zw 160.204
13 29 58.73 47 16 4.5 29.1 0.046 39.90   11.51 0.002 Liner   NGC 5195
13 32 48.62 41 52 18.9 12.3 0.038 42.07   14.08 0.027     NGC 5214
13 38 17.27 48 16 32.0 18.4 0.043 42.16   15.05 0.028 S2   Mark 266SW
13 42 8.34 35 39 15.2 15.3 0.021 40.16   13.06 0.004 S1.9   NGC 5273
13 44 1.90 25 56 27.8 28.5 0.026   12.8 17.00        
13 51 4.24 19 26 8.2 3.7 0.048 42.90 13.5 16.95 0.062 em 1, 2  
13 51 42.19 55 59 43.2 29.3 0.022   15.1 16.68       TEX 1349+562
13 53 9.75 24 22 37.4 6.6 0.027 42.26 13.5 16.85 0.056 S1 1, 2 Zw 132.035
13 53 26.69 40 16 58.9 7.7 0.048 41.12     0.008 Liner   NGC 5353
13 53 43.82 33 13 20.3 28.2 0.024 42.43 14.5 15.61 0.051     MCG +06.31.015
13 53 55.94 21 59 54.9 24.1 0.042   12.9 16.86        
13 58 19.76 7 13 15.2 27.4 0.044 42.07 15.7   0.025     Zw 046.025
14 12 36.95 39 18 53.8 21.2 0.034 41.96 16.4 15.27 0.025 S1.9   NGC 5515
14 13 23.13 24 31 56.8 24.3 0.024 42.44 12.2 16.34 0.052 abs 2 Zw 133.012
14 18 9.20 7 33 52.0 24.3 0.042 42.02   14.97 0.024     NGC 5546
14 22 55.37 32 51 2.7 2.0 0.028 42.14   15.28 0.034 S1.8   UGC 9214
14 26 2.32 8 6 40.5 34.6 0.024 41.84   16.98 0.026     Zw 047.039
14 26 18.64 26 14 52.3 13.8 0.027 42.02 16.3 15.58 0.030     IC 4423
14 28 23.06 78 53 8.2 0.2 0.047 42.03 12.1   0.023     IC 4470
14 29 40.64 0 21 59.2 13.8 0.025 42.51 14.8 16.92 0.055 abs 1 Zw 019.045
14 29 48.51 53 57 54.3 25.6 0.025 42.30 13.2 16.19 0.043     IC 1027
14 42 39.65 29 20 48.2 7.5 0.028 42.82 13.5 17.00 0.074 H II 1, 2 NPM1G+29.0326
14 50 51.40 5 6 52.0 25.9 0.025 41.92   15.29 0.028 S2   NGC 5765B
14 50 55.42 27 34 42.1 13.1 0.032 42.09   15.89 0.030     IC 4514
14 51 14.39 30 41 32.2 33.9 0.044   12.5 16.28       Zw 164.036
14 55 28.21 32 50 24.0 30.3 0.026   14.1 16.21       MCG+06.33.009
15 4 15.88 28 29 47.5 32.7 0.127 43.26   15.66 0.058     MCG+05.36.002
15 5 56.60 3 42 26.0 15.6 0.027 42.18   16.00 0.036 S1.8   Mark 1392
15 9 20.51 7 38 19.4 28.5 0.044 43.05 16.0 16.94 0.077 abs 2  
15 13 40.25 4 4 17.2 24.9 0.025 42.21 13.3 16.96 0.039 H II 2 Zw 049.061
15 20 29.00 44 58 15.3 11.5 0.046 42.89 13.9 16.86 0.063 abs 1  
15 21 20.58 30 40 15.3 15.0 0.139 43.57 14.0 16.93 0.079 abs 2 Zw 165.041
15 23 59.90 31 12 40.2 31.4 0.032 42.97   16.71 0.074     MCG+05.36.026
15 25 8.75 12 52 57.5 24.6 0.039 41.95 12.5 16.30 0.023     Zw 077.123
15 29 14.68 52 51 50.1 12.9 0.029 42.80 13.1 16.66 0.071 abs 1 UGC 9868
15 32 32.02 4 40 51.4 13.8 0.048 42.50   15.75 0.039     UGC 9886
15 32 57.19 0 26 36.1 11.4 0.044 42.41 15.8 16.11 0.037     Zw 022.010
15 33 17.73 82 13 46.2 11.3 0.036 41.87 12.9   0.022     UGC 9950
15 35 54.26 14 31 2.7 34.6 0.049 41.92   15.70 0.020 S2   Akn 479
15 38 10.00 57 36 12.0 12.1 0.034 42.90   16.20 0.074 S1   MCG+10.22.028
15 39 2.65 31 45 34.3 25.4 0.031 40.81   15.31 0.007     NGC 5974
15 47 48.93 37 1 36.0 19.9 0.040 43.01 15.1 16.60 0.077 em 2 NPM1G+37.0489
15 52 12.04 34 5 35.4 24.0 0.024 42.43 14.7   0.051 abs 2 NPM1G+34.0353
15 56 41.39 20 10 16.4 33.0 0.027   12.8 16.66        
16 4 55.53 28 9 56.9 21.8 0.047 43.08 12.1 16.54 0.077     Zw 167.022
16 5 29.18 16 25 8.8 28.3 0.041 42.53     0.044     UGC 10187B
16 5 35.57 44 12 22.0 16.9 0.056 42.65 13.5 16.33 0.043     MCG+07.33.038
16 5 36.83 17 48 8.1 32.0 0.025 42.09   16.32 0.034 H II   Mark 298
16 7 24.03 85 1 49.3 2.7 0.042 43.78 16.5   0.183 S1   S5 1616+85
16 7 35.36 13 56 37.6 28.9 0.026 42.11 13.1 16.21 0.034     NGC 6066
16 9 5.53 27 53 34.0 10.2 0.041 42.23 12.5 16.84 0.031 S2 1, 2 NPM1G+28.0373
16 9 35.18 63 58 1.2 8.2 0.047 42.75 14.0 16.82 0.053 em 1, 2 NPM1G+64.0143
16 11 11.40 61 16 4.5 13.2 0.030 42.09   14.95 0.031     NGC 6095
16 11 13.89 36 58 24.3 27.6 0.031 42.79 12.5 16.95 0.068 abs 2 KUG 1609+371A
16 12 33.72 29 29 39.1 15.5 0.043 42.28 13.6 15.07 0.032     NGC 6086
16 24 37.00 19 30 24.3 11.2 0.026 42.16     0.036     Zw 109.013
16 27 42.60 39 22 38.5 13.7 0.023 41.92 16.1   0.029     PGC 058195
16 29 44.90 40 48 41.8 6.2 0.039 42.15   14.31 0.029     NGC 6173
16 29 52.80 24 26 38.1 6.3 0.041 42.40 12.2 16.30 0.038 S1.9   Mark 883
16 32 58.03 11 43 23.8 27.5 0.038 42.71 16.3 15.65 0.056     Zw 080.046
16 33 48.87 35 53 18.8 33.3 0.022 42.13   16.57 0.038     KUG 1632+359
16 36 57.72 55 46 58.2 8.6 0.038 42.11 13.5 16.92 0.028 S? 1, 2  
16 37 20.55 41 11 20.1 16.3 0.038 42.22 13.0 16.74 0.032 abs 2 NPM1G+41.0441
16 39 4.72 8 21 30.9 11.2 0.035 42.48 13.2 16.88 0.045 em 2 NPM1G+08.0448
16 42 56.33 19 15 15.5 10.6 0.042 42.32 13.0 16.25 0.034     IC 1224
16 43 4.22 61 34 43.3 22.7 0.032 41.70 13.9 14.13 0.019     NGC 6223
16 56 1.58 21 12 42.0 10.4 0.028 42.46 15.4 16.99 0.049 S1 1 NPM1G+21.0507
16 57 45.01 68 30 53.1 13.9 0.045 42.42 13.1 15.88 0.037     NGC 6289
17 0 27.21 51 59 11.6 14.3 0.044 42.64 12.7 16.87 0.048 S1   NPM1G+52.0273
17 3 47.89 34 43 39.2 20.0 0.023   12.2          
17 12 36.58 38 1 13.3 25.4 0.040 42.37   15.40 0.037     IC 1245
17 15 58.85 36 23 23.1 15.2 0.048 43.18 13.6 16.13 0.086 S1 2 UGC 10782
17 23 22.08 32 49 55.2 16.7 0.022 42.63 13.2 16.55 0.067 H II 2  
17 37 56.34 41 38 32.0 19.9 0.023 42.68 15.1 16.39 0.070 H II 2 IRAS F17363+4140
17 38 11.38 58 42 55.3 21.7 0.034 42.09   15.85 0.029 S1   NGC 6418
22 21 47.39 2 54 36.2 24.5 0.028   13.2 16.72        
22 28 29.51 16 46 59.6 11.6 0.034 42.23 12.9 15.01 0.034     NGC 7291
22 32 30.68 8 12 33.0 18.2 0.034 41.96 12.5 16.08 0.025 S1   Akn 557
22 35 40.82 1 29 5.9 26.2 0.293 43.64 14.3 16.63 0.059     LEDA 087323
22 41 34.22 4 53 10.7 34.3 0.047 42.97   16.90 0.068 S?   NPM1G+04.0574
22 49 54.69 11 36 30.1 23.7 0.054 42.19   14.35 0.026     NGC 7385
22 58 1.97 13 8 4.4 10.7 0.021 41.75   15.08 0.025     NGC 7432
23 13 58.36 3 42 54.4 5.6 0.031 42.62 13.0 16.42 0.056     Zw 380.012
23 20 42.29 8 13 2.5 7.2 0.035 41.26     0.011 Liner   NGC 7626
23 25 51.50 8 47 11.2 6.6 0.025   14.3 16.46       KUG 2323+085
23 31 50.20 25 32 40.0 6.7 0.038   13.3 16.59       KUG 2329+252
23 36 14.10 2 9 18.6 3.5 0.021 40.86     0.009 H II   NGC 7714
23 56 1.96 7 31 23.4 3.1 0.049 42.53 13.6 16.84 0.040 S1   Mark 541



 

 
Table 3: List of the 76 known AGN brighter than $O_{\rm USNO}=16.5$, located within 35 $\hbox {$^{\prime \prime }$ }$ of a ROSAT-FSC source. Column 1: right ascension, Col. 2: declination, Col. 3: separation between the ROSAT and USNO positions in arcsec, Col. 4: X-ray count rate (count s-1), Col. 5: magnitude $O_{\rm USNO}$, Col. 6: magnitude $O_{\rm APS}$, Col. 7: APS O-E colour, Col. 8: redshift, Col. 9: absolute magnitude computed by using the $O_{\rm USNO}$ magnitude ( $H_{\rm o}=50$ km s-1 Mpc-1), Col. 10: classification, Col. 11: name.
J2000 USNO position                  
h m s $^{\circ}$ ' '' '' c/r $O_{\rm US}$ $O_{\rm APS}$ O-E z $M_{\rm abs}$   Name

0

 6 23.08 12 35 53.2 20.8 0.030 15.8 16.26 0.36 0.98 -28.4 Q RGB J0006+125
0 24 44.10 0 32 21.4 9.7 0.047 16.2 16.92 0.58 0.404 -25.8 Q PB 5932
0 36 12.50 5 49 52.0 9.1 0.064 16.3 16.88 0.28 0.41 -25.7 Q HS 0033+0533
0 52 5.57 0 35 38.4 28.6 0.024 16.3 16.80 1.04 0.399 -25.7 Q Q 0049+0019A
0 57 9.93 14 46 10.4 26.7 0.246 15.9 16.11 1.12 0.171 -24.0 Q PHL 909
1 20 17.29 21 33 46.6 25.0 0.023 15.5 15.80 0.54 1.500 -29.7 Q PG 0117+213
1 39 55.80 6 19 22.5 8.4 0.031 15.7 16.55 0.60 0.396 -26.5 Q PHL 1092
1 40 35.02 23 44 51.1 25.1 0.029 16.1 16.64 0.98 0.32 -25.4 Q HS 0137+2329
1 41 59.60 6 12 5.5 2.7 0.049 16.3 16.27 0.56 0.345 -27.2 Q PHL 1106
3 18 25.57 15 59 56.7 11.2 0.033 16.3 16.58 0.02 0.515 -25.9 Q US 3828
3 39 9.60 3 45 52.5 23.7 0.038 16.4 17.55 0.44 0.199 -24.0 Q RXS J03391+0346
4 24 46.85 0 36 6.4 7.4 0.052 16.1 16.75 1.26     BL PKS 0422+00
8 15 59.21 41 44 57.1 17.9 0.021 15.8 15.97 0.32 1.28 -29.3 Q KUV 08126+4154
8 22 36.88 54 18 36.4 33.7 0.042 16.3 16.65 1.12 0.086 -22.3 S1 SBS 0818+544
8 43 49.78 26 19 11.1 19.4 0.068 16.4 17.23 0.20 0.258 -24.7 Q HS 0840+2630
8 59 24.35 46 37 17.3 22.3 0.047 16.5 16.89 0.74 0.923 -27.5 Q US 2068
9 0 47.30 74 44 26.3 16.6 0.045 16.1     0.77 -27.4 Q HS 0855+7456
9 19 57.63 51 6 9.1 17.1 0.039 15.8 16.35 -0.80 0.553 -27.0 Q SBS 0916+513
9 25 14.35 54 44 27.2 10.4 0.048 15.9 16.66 -0.12 0.476 -26.3 Q SBS 0921+549
9 29 9.82 46 44 24.1 15.9 0.025 15.6 15.66 0.18 0.240 -25.3 Q US 645
9 36 25.45 39 49 33.7 24.8 0.033 16.1 16.81 0.82 1.25 -28.7 Q KUV 09333+4003
9 37 1.93 34 25 0.0 12.7 0.031 16.0 16.55 0.22 0.908 -28.1 Q Ton 1078
9 41 33.72 59 48 11.3 13.2 0.045 16.3 16.70 0.36 0.966 -27.9 Q SBS 0938+600
9 56 49.89 25 15 16.0 8.0 0.048 16.2 16.92 0.84 0.712 -27.2 Q OK 290
10 4 20.10 5 13 0.6 22.1 0.021 16.2 16.55 0.26 0.161 -23.8 Q PG 1001+054
10 13 30.20 53 15 59.6 6.7 0.025 16.2 16.64 0.36 1.495 -29.1 Q SBS 1010+535
10 15 57.04 1 9 13.7 16.1 0.082 16.3 16.97 0.94 0.779 -27.2 Q Q 1013+0124
10 33 59.50 35 55 9.0 14.9 0.046 16.3 16.76 0.92 0.169 -23.8 Q CSO 275
10 43 55.52 56 27 57.0 18.6 0.028 16.3 16.81 -0.40 1.951 -29.6 Q SBS 1040+567
11 17 6.41 44 13 33.8 8.1 0.023 14.8 15.06 0.40 0.144 -24.9 Q PG 1114+445
11 30 4.76 41 16 19.5 23.2 0.035 15.7 16.20 0.10 1.530 -29.5 Q KUV 11274+4133
11 33 35.40 9 39 1.8 24.6 0.029 16.4 17.05 0.06 0.379 -25.5 Q RX J11335+0939
11 43 47.71 11 28 48.1 20.6 0.046 15.5 16.38 0.80 0.118 -23.8 Q RX J11437+1128
11 52 51.90 33 7 18.8 2.7 0.033 16.1 16.30 0.40 1.389 -28.8 Q CSO 373
11 55 7.62 52 1 29.4 6.4 0.036 16.4 16.46 1.08 0.156 -23.5 Q SBS 1152+523
11 59 6.78 53 6 43.5 6.1 0.043 16.5 17.19 0.36 0.482 -25.9 Q MS 11565+5323
12 7 4.53 38 40 24.6 3.7 0.045 16.3 16.64 0.00 0.572 -26.4 Q RXS J12070+3840
12 17 40.83 49 31 17.9 1.1 0.049 16.5 17.62 0.18 0.730 -26.6 Q SBS 1215+497
12 22 10.01 27 19 2.3 6.4 0.046 15.9 16.90 0.52 0.442 -26.3 Q RXS J12221+2719
12 23 0.23 55 40 0.3 9.4 0.057 16.5 17.48 0.48 0.905 -27.5 Q SBS 1220+559
12 28 24.97 31 28 37.7 24.8 0.024 15.6 16.28 0.28 2.219 -30.4 Q B2 1225+31
12 30 50.04 1 15 22.6 6.4 0.041 14.4 14.81 0.16 0.117 -24.8 Q RX J12308+0115
12 33 26.05 45 12 23.1 11.2 0.032 16.5 16.91 -0.24 1.958 -29.4 Q HS 1231+4528
12 44 10.82 17 21 4.5 16.3 0.027 15.7 16.58 0.74 1.283 -28.8 Q PG 1241+176
13 6 5.72 80 8 20.5 10.9 0.035 16.3 18.35 1.01 1.183 -28.3 Q S5 1305+80
13 13 21.39 78 21 53.9 11.9 0.026 15.6 15.86 0.22 2.00 -30.3 Q HS 1312+7837
13 19 56.24 27 28 8.4 23.4 0.031 15.5 16.54 0.22 1.014 -28.7 Q CSO 873
13 41 0.81 41 23 14.2 17.0 0.022 16.4 16.36 -0.02 1.204 -28.3 Q PG 1338+416
13 47 19.40 59 2 32.5 10.3 0.025 16.2 16.48 0.22 0.768 -27.3 Q SBS 1345+592
13 47 37.45 30 12 52.4 20.5 0.035 15.7 16.12 0.68 0.118 -23.6 Q Q J1347+3012
13 51 28.30 1 3 38.5 17.5 0.040 16.5 17.35 0.58 1.086 -27.9 Q Q 1348+0118
14 2 44.52 15 59 56.2 1.9 0.031 16.3 16.66 1.56 0.245 -24.5 BL MC 1400+162
14 27 35.60 26 32 14.5 26.8 0.040 15.4 15.18 -0.72 0.366 -26.6 Q PG 1425+267
14 36 45.79 63 36 37.6 32.1 0.038 15.7 16.61 -0.22 2.066 -30.4 Q S4 1435+63
14 50 26.68 58 39 44.7 9.9 0.046 15.8 16.13 1.14 0.210 -23.8 Q Mark 830
14 51 53.63 72 14 46.8 5.8 0.027 16.3 16.96 0.16 0.75 -27.1 Q HS 1451+7227
15 27 28.64 65 48 10.3 14.0 0.046 16.2 16.77 0.56 0.345 -25.5 Q FBS 1526+659
15 50 43.65 11 20 47.4 23.7 0.040 16.3 16.33 0.14 0.436 -25.9 Q MC 1548+114
15 51 58.16 58 6 44.7 4.5 0.036 16.2 16.74 1.14 1.320 -28.7 Q SBS 1550+582
16 19 40.54 25 43 23.3 13.1 0.035 16.4 16.62 1.36 0.268 -24.7 Q RX J16196+2543
16 23 19.93 41 17 2.7 26.3 0.030 16.5 16.88 0.32 1.618 -28.9 Q KUV 16217+4124
16 26 37.28 58 9 17.2 6.0 0.044 16.2 16.52 0.83 0.751 -27.2 Q SBS 1625+582
16 28 25.70 8 33 0.1 10.1 0.031 16.4 17.22 0.32 0.44 -25.8 Q HS 1626+0839
16 31 43.83 52 53 43.8 5.7 0.048 16.5 16.81 0.44 0.352 -25.2 Q SBS 1630+530
16 32 1.11 37 37 50.0 14.5 0.034 16.0 16.60 0.54 1.478 -29.4 Q PG 1630+377
16 32 34.68 73 59 43.0 3.2 0.030 16.1 17.97 1.30 0.208 -24.4 Q RXS J16325+7359
16 34 29.01 70 31 32.3 1.2 0.049 14.9 15.26 1.03 1.337 -30.1 Q PG 1634+706
16 37 7.53 41 40 26.9 17.0 0.028 16.2 16.28 1.60 0.765 -27.3 Q KUV 16355+4146
17 1 0.62 64 12 9.3 19.0 0.035 15.9 16.03 0.18 2.736 -31.2 Q HS 1700+6416
17 4 41.39 60 44 30.5 8.4 0.042 15.6 15.86 0.76 0.371 -26.3 Q 3C 351.0
17 6 48.06 32 14 22.9 17.0 0.029 16.2 16.94 0.66 1.070 -28.2 Q RGB J1706+322
17 19 34.18 25 10 58.6 16.9 0.039 16.4 16.87 1.34 0.579 -26.4 Q RX J17195+2510
22 53 7.37 19 42 34.7 21.5 0.039 16.4 16.75 0.92 0.284 -24.9 Q HS 2250+1926
23 7 45.62 19 1 20.8 11.6 0.033 16.4 17.13 0.98 0.313 -25.0 Q PKS 2305+18
23 11 59.50 9 26 1.4 7.4 0.048 16.3 17.51 0.16 0.479 -26.1 Q RX J23119+0925
23 50 10.07 8 12 55.3 16.6 0.025 16.4 18.19 1.00 1.70 -29.1 Q HS 2347+0756



 

 
Table 4: List of 103 QSO candidates identified with a ROSAT-FSC source and located in zone IVa. Column 1: right ascension, Col. 2: declination, Col. 3: separation between the ROSAT and USNO positions in arcsec, Col. 4: X-ray count rate (count s-1), Col. 5: magnitude $O_{\rm USNO}$, Col. 6: magnitude $O_{\rm APS}$, Col. 7: APS O-E colour, Col. 8: redshift, Col. 9: absolute $O_{\rm USNO}$ magnitude, Col. 10: classification: DA, DN, WD: white dwarfs; *: stars; CV: cataclysmic variable; BL: BL Lac object; S1: Seyfert 1 galaxy; S1n: Narrow Line Seyfert 1; Q: QSO; Col. 11: reference: (1) OAGH and (2) OHP observations, Col. 12: name.
J2000 USNO position                    
h m s $^{\circ}$ ' '' '' c/r $O_{\rm US}$ $O_{\rm APS}$ O-E z $M_{\rm abs}$   Ref. Name

0

 11 19.46 28 17 50.8 18.7 0.023 15.5 15.88 0.12     * 1  
0 13 4.80 10 11 28.6 5.8 0.023 16.0 16.25 0.32 0.239 -24.9 Q 1  
0 40 46.17 18 54 24.3 17.0 0.026 16.0 16.71 -0.12 0.153 -23.3 Q 1  
1 7 37.51 22 22 32.3 33.7 0.042 16.2 16.89 0.68     * 2  
1 20 46.96 23 31 40.1 28.7 0.047 15.9 16.27 0.54     * 2  
1 37 37.24 30 2 49.1 13.1 0.035 13.5 16.90 0.36     DN   TX Tri
2 55 30.70 7 25 57.1 19.4 0.030 16.3 16.97 0.66 0.707 -27.0 Q 1  
3 53 15.60 9 56 35.1 24.0 0.030 16.0 16.49 -0.82     * 2  
8 23 46.65 24 53 51.2 18.5 0.039 15.6 15.83 -0.40     WD 1 TON 316
8 39 34.28 23 34 10.4 12.8 0.041 15.8 16.49 -0.52     DA   PG 0836+237
8 45 51.14 60 9 13.7 13.3 0.027 16.0 16.30 -0.46     DA   PG 0841+603
8 50 20.09 54 33 50.5 17.3 0.038 16.4 16.78 0.62     * 1  
8 56 32.44 50 41 14.1 5.1 0.027 15.8 15.57 -0.58 0.235 -25.0 Q 1  
9 3 32.62 16 26 1.4 21.7 0.037 16.2 16.59 0.24     * 1 LB 9181
9 10 35.38 31 27 45.9 27.0 0.048 16.3 16.21 0.42     * 1  
9 10 37.97 53 12 2.8 19.3 0.030 16.4 16.82 0.52     * 1  
9 12 15.50 1 19 59.3 3.8 0.041 16.5 16.76 -0.50     * 1  
9 20 47.61 51 25 38.8 33.1 0.021 15.7 15.65 0.12     * 1  
9 30 6.76 52 28 4.0 12.0 0.039 15.8 16.37 -0.02     *   PG 0926+527
9 30 21.87 23 53 30.1 19.2 0.027 16.0 16.70 0.14 0.243 -24.3 Q 1  
9 30 34.46 20 44 16.9 5.2 0.045 16.1 17.09 0.64 1.169 -28.4 Q 1  
9 45 13.97 15 10 11.7 17.9 0.057 15.8 17.66 0.86     * 1  
9 46 34.50 13 50 58.3 34.4 0.027 15.8 16.75 0.10     CV 1  
9 49 39.77 17 52 49.5 12.0 0.021 16.3 18.65 0.60          
9 52 45.70 2 9 38.7 17.1 0.025 15.2 16.32 -0.76     DA   PG 0950+024
9 56 49.88 29 50 14.6 10.7 0.046 15.4 16.09 -0.10 0.845 -28.5 Q 1 TON 465
9 57 11.78 63 10 10.2 3.8 0.024 16.4 16.25 -0.06 0.918 -27.6 Q 1  
10 6 14.64 44 19 7.1 15.6 0.030 16.5 16.93 -0.30     DA    
10 34 53.07 44 57 23.1 20.5 0.023 16.1 16.57 0.38 1.422 -29.0 Q 1  
10 35 27.50 49 58 27.7 22.8 0.021 16.5 17.44 0.36 1.427 -28.5 Q 1  
10 44 19.33 19 57 47.9 24.2 0.039 15.6 15.90 0.44     * 1  
10 46 42.30 39 20 18.2 8.3 0.043 16.4 17.16 0.22 0.390 -25.3 Q 1  
10 47 30.55 10 17 28.9 17.7 0.228 15.4 15.81 0.08 0.145 -24.3 Q 1  
11 8 42.46 16 50 40.2 31.2 0.030 15.6 16.48 0.04     * 1  
11 14 1.95 52 27 11.6 29.8 0.023 15.5 15.62 0.40     * 1  
11 15 7.70 2 37 57.7 7.6 0.024 16.5 17.08 -0.04 0.564 -26.1 Q 1  
11 26 16.19 32 59 53.7 29.3 0.029 16.2 15.66 0.24     * 1  
11 33 31.23 58 57 47.8 19.9 0.025 15.9 15.98 0.44     * 1  
11 34 25.08 23 16 8.8 24.0 0.039 16.3 16.66 0.64     * 1  
11 38 36.32 47 55 10.0 13.3 0.046 16.1 17.53 -0.48     * 1  
11 41 52.82 25 35 33.5 10.8 0.042 16.3 16.82 -0.96     * 1  
11 47 47.34 26 0 49.0 10.9 0.042 15.5 15.84 0.00     * 1  
12 19 57.97 27 8 57.2 9.5 0.023 16.1 17.17 0.76     * 1  
12 31 25.72 25 55 59.8 5.7 0.032 15.8 16.16 0.54     * 1  
12 32 54.28 36 44 7.4 32.5 0.022 16.0 16.61 -0.08     WD 1 CBS 353
12 52 30.85 14 26 9.3 24.3 0.029 16.3 17.30 0.10          
12 57 37.02 16 30 48.6 13.5 0.035 16.1 16.95 0.66 1.017 -28.2 Q 1  
12 59 38.22 60 38 59.4 15.9 0.039 16.3 16.47 -0.48     * 1 SBS 1257+609
12 59 44.45 68 4 0.8 30.9 0.022 16.3 16.64 -0.72     * 1 FBS 1257+683
13 0 6.40 44 42 50.9 13.9 0.036 16.2 16.06 0.46     * 1  
13 10 11.30 7 58 16.5 21.2 0.030 15.8 16.52 -0.08 0.578 -27.0 Q 1  
13 13 15.90 9 18 20.4 27.7 0.021 16.4 17.34 0.10 1.790 -29.2 Q 1  
13 14 30.78 13 7 45.8 23.8 0.044 16.3 17.00 0.24 0.741 -27.1 Q 1  
13 20 1.10 7 18 17.1 21.1 0.038 16.5 16.97 0.74 0.866 -26.9 Q 1  
13 20 22.53 30 56 22.4 19.8 0.029 16.4 17.22 -0.04 1.587 -28.1 Q 1 US 583
13 24 47.70 3 24 32.9 15.5 0.040 16.5 16.84 0.54 0.303 -24.9 Q 1  
13 32 51.09 15 29 30.9 23.9 0.042 15.5 15.56 0.14     * 1  
13 33 45.80 5 38 42.6 22.2 0.028 15.5 15.74 0.10     * 1  
13 40 59.95 60 26 11.8 17.6 0.034 16.2 16.48 -0.68     DA   SBS 1339+606
13 42 46.90 18 44 43.8 22.4 0.039 16.4 16.69 0.12 0.382 -25.5 Q 1  
13 50 13.97 14 35 47.4 30.4 0.023 16.4 16.93 0.48     * 1  
13 51 25.25 19 5 33.4 10.8 0.027 16.4 16.89 0.64     * 1  
13 54 48.82 49 13 37.1 19.8 0.028 15.5 15.68 0.32     * 1  
13 55 43.99 20 12 31.8 19.9 0.030 15.6 16.11 0.30     * 1  
13 58 41.50 2 49 12.5 21.1 0.046 16.2 16.85 -0.08     * 1  
14 6 58.74 14 42 38.6 13.0 0.034 15.4 15.84 0.34 0.264 -25.7 Q 1  
14 9 39.24 28 16 49.9 25.2 0.035 16.1 16.93 0.34 0.165 -23.9 Q 1  
14 10 57.74 64 33 10.6 18.8 0.041 16.4 16.83 0.06 0.462 -25.9 Q 1  
14 17 30.16 13 0 1.6 11.6 0.021 15.7 16.00 0.38     * 1  
14 19 25.77 38 2 49.0 12.7 0.039 16.2 17.22 0.08 0.517 -26.3 Q 1  
14 31 10.98 14 23 8.3 3.7 0.022 16.1 15.91 -0.04 1.425 -29.0 Q 1  
14 47 50.12 38 5 30.3 12.2 0.023 15.8 16.28 0.04     * 1  
15 0 31.80 48 36 47.0 16.0 0.021 16.4 16.72 0.48 1.031 -27.9 Q 1  
15 5 27.62 29 47 18.7 8.7 0.036 15.0 15.65 -0.34 0.527 -27.6 Q 1 CSO 1080
15 8 32.28 67 42 43.4 9.0 0.032 16.0 17.12 0.14 0.336 -25.8 Q 1  
15 12 44.60 9 31 0.8 23.0 0.037 15.9 16.61 0.56     * 1  
15 16 32.30 12 13 50.5 10.6 0.028 16.2 17.26 0.78     BL 1  
15 44 3.76 26 48 38.6 21.7 0.023 16.4 17.15 0.74     * 1  
15 45 53.50 9 36 20.6 19.6 0.032 16.1 16.40 -0.22          
15 48 33.03 44 22 26.1 12.7 0.021 16.3 16.97 0.48 0.322 -25.2 Q 1  
15 51 9.60 45 42 52.1 22.5 0.036 15.6 15.95 0.32          
15 51 52.45 19 11 4.1 34.9 0.034 15.8 16.31 0.50          
15 53 4.93 35 48 28.6 25.2 0.033 16.1 17.20 0.72 0.722 -26.8 Q 1  
15 56 9.90 3 9 22.5 9.6 0.037 16.3 16.80 0.48 0.131 -23.2 S1n 1  
16 5 19.72 14 48 52.5 15.5 0.040 16.2 16.51 0.00 0.371 -25.7 Q 1  
16 9 47.80 7 12 33.2 27.8 0.021 16.4 16.95 0.64     * 1  
16 11 36.58 15 20 54.6 18.8 0.030 16.3 16.69 0.40 1.309 -28.6 Q 1  
16 17 42.10 6 2 23.8 20.4 0.078 15.5 15.69 0.42     * 1  
16 28 35.38 45 20 43.3 34.1 0.022 16.4 17.00 0.68     * 1  
16 30 9.65 45 16 37.9 21.7 0.022 16.5 16.96 0.32     * 1  
16 31 10.46 38 44 49.6 7.8 0.036 15.8 15.97 0.48     * 1  
16 45 20.15 61 35 9.7 3.8 0.023 16.4 16.89 0.64 0.410 -25.5 Q 1  
16 46 15.52 25 41 43.3 15.7 0.047 16.4 17.26 0.56 0.188 -23.9 Q 1  
17 18 28.97 57 34 22.3 6.4 0.039 15.9 16.07 0.48 0.100 -22.9 S1n 1  
17 20 13.19 49 55 26.4 28.8 0.027 16.0 15.89 0.36     * 1  
17 21 45.75 57 16 56.7 31.5 0.021 15.8 15.87 0.24     * 1  
17 28 13.44 32 22 5.8 10.8 0.022 16.4 17.08 0.34 0.563 -26.3 Q 1  
17 29 35.53 52 30 47.5 3.0 0.029 16.2 15.96 0.02 0.278 -25.0 Q 1  
17 49 12.30 55 12 8.9 28.7 0.023 16.3 16.58 0.44     WD 1  
22 37 31.84 10 19 4.0 3.8 0.024 16.5 16.77 -0.46 0.103 -22.5 S1 1  
22 37 33.28 10 18 42.7 26.3 0.024 15.9 16.10 0.50     * 1  
23 7 13.30 4 32 2.5 29.8 0.079 15.9 17.25 -0.92     * 1  
23 15 52.73 11 33 2.1 21.4 0.036 16.5 17.20 0.24 0.567 -26.2 Q 1 KUV 23134+1117



Copyright ESO 2004