Contents

A&A 435, 799-810 (2005)
DOI: 10.1051/0004-6361:20041520

A sample of X-ray emitting normal galaxies from the BMW-HRI Catalogue[*]

M. Tajer1,2 - G. Trinchieri1 - A. Wolter1 - S. Campana1 - A. Moretti1 - G. Tagliaferri1


1 - INAF - Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy
2 - Università di Milano - Bicocca, Dipartimento di Fisica, P.za della Scienza 3, 20126 Milano, Italy

Received 23 June 2004 / Accepted 16 December 2004

Abstract
We obtained a sample of 143 normal galaxies with X-ray luminosity in the range 1038-1043 erg s-1 from the cross-correlation of the ROSAT HRI Brera Multi-scale Wavelet (BMW-HRI) Catalogue with the Lyon-Meudon Extragalactic Database (LEDA). We find that the average X-ray properties of this sample are in good agreement with those of other samples of galaxies in the literature. We selected a complete flux limited serendipitous sample of 32 galaxies from which we derived the $\log N-\log S$ distribution of normal galaxies in the flux range $1.1{-} 110 \times 10^{-14}$ erg cm-2 s-1. The resulting distribution is consistent with the Euclidean -1.5 slope. Comparisons with other samples, such as the Extended Medium Sensitivity Survey, the ROSAT All Sky Survey, the XMM-Newton/2dF survey, and the Chandra Deep Field Survey indicate that the $\log N-\log S$ distribution of normal galaxies is consistent with a Euclidean slope over a flux range of about 6 decades.

Key words: X-ray: galaxies - galaxies: general - surveys

1 Introduction

Detailed X-ray studies of normal galaxies have been possible only with the advent of imaging instruments aboard the Einstein observatory. The Einstein results were summarized in the catalogue and atlas published by Fabbiano et al. (1992), who constructed a large homogeneous sample of 493 galaxies, included in either A Revised Shapley-Ames Catalog of Bright Galaxies (Sandage & Tammann 1981) or in the Second Revised Catalog of Bright Galaxies (de Vaucouleurs et al. 1976), both targets and objects serendipitously detected in Einstein fields. While representative of the galaxy population (see e.g. Shapley et al. 2001; Eskridge et al. 1995), it was not constructed to be a complete, unbiased sample, so it is likely to contain unknown selection biases.

Elliptical galaxies were found to retain large amounts ( 108 -1011 $M_{\odot}$) of hot gas ( $T \sim 10^7$ K) whose thermal emission dominates their X-ray luminosities, while in normal spirals the integrated contribution of the evolved stellar sources, such as supernova remnants and X-ray binaries, is generally the dominant component (see Kim et al. 1992; Fabbiano et al. 1992; Fabbiano 1989). Extended emission from a hot, gaseous component in spiral galaxies was detected only in some cases (Vogler & Pietsch 1996; Trinchieri et al. 1988; Fabbiano & Trinchieri 1987), or associated with starburst activity.

Subsequent observations of individual sources made by ROSAT and ASCA confirmed most of the Einstein results and added interesting information on the X-ray properties of normal galaxies in the local universe (see among others Read et al. 1997; Brown & Bregman 1998; Beuing et al. 1999; Roberts & Warwick 2000).

With the launch of XMM-Newton and Chandra, the study of the X-ray properties of "normal'' galaxies at intermediate ( $z \sim 0.1$) or cosmological distances (Hornschemeier et al. 2002; Brandt et al. 2001; Georgakakis et al. 2004a; Norman et al. 2004; Georgakakis et al. 2004b; Hornschemeier et al. 2003; Georgakakis et al. 2003) was made possible, thanks to significantly improved sensitivity and spatial and spectral resolution of the instruments. In spite of the large number of papers, however, a truly complete sample of X-ray emitting normal galaxies in the local universe with a significant number of objects has not been properly discussed in the literature so far. Georgakakis et al. (2003) gave galaxy number density at $F_{0.5-2} \sim 7
\times 10^{-16}$ erg cm-2 s-1 from stacking analysis, while Georgakakis et al. (2004a) presented a sample of 26 X-ray sources detected in an area of $\sim$2.5 deg-2, of which only 2 were however classified as normal galaxies. Georgakakis et al. (2004b) only recently presented a larger sample of 11 normal galaxies detected in an area of $\sim$4.5 deg-2.

Two other samples of "normal'' galaxies are available in the literature, selected in the Chandra Deep Fields (Norman et al. 2004; Hornschemeier et al. 2003). However their median redshifts (z = 0.297, Hornschemeier et al. 2003; and z = 0 to z = 1.3, Norman et al. 2004) indicates that they should not be considered as "local''.

The large database provided by ROSAT has been exploited only marginally to derive unbiased and complete sample of galaxies. Zimmermann et al. (2001) selected a sample of candidate normal galaxies from the ROSAT All Sky Survey (RASS) Bright Source Catalogue (Voges et al. 1999) above a flux limit of about 10-12 erg cm-2 s-1 ( 0.1 - 2.4 keV band). A few samples were derived from the ROSAT Position Sensitive Proportional Counter (PSPC) pointed observations, such as the WGA (White et al. 1994) and the ROSPSPC (ROSAT team 2001), and a new catalogue of galaxies is in progress (G. Peres, private communication). Here we exploited the potential of the Brera Multi-scale Wavelet (BMW-HRI) catalogue (Panzera et al. 2003) to extract a sample of normal galaxies, as we discuss in the next sections. While the PSPC is probably more efficient at detecting faint and extended sources such as galaxies, the sharp core of the HRI point spread function allows us to detect sources in more crowded fields and to measure the extent of bright, small-size sources, providing a good complement to the PSPC data.

   
2 The sample

In order to create a complete, serendipitous sample of galaxies with X-ray emission, we made use of X-ray data from the BMW ROSAT HRI catalogue and optical data from LEDA (Lyon-Meudon Extragalactic Database). The BMW-HRI catalogue consists of 29089 X-ray sources detected in 4303 ROSAT HRI pointed fields with exposure times longer than 100 s using a multiscale wavelet algorithm (Campana et al. 1999; Lazzati et al. 1999; Panzera et al. 2003). Sources detected with a significance $\geq$4.2 $\sigma$ are contained in the catalogue, which provides name, position, count rate, flux, and extension, along with the relative errors. In our study we used the full catalogue, but we excluded X-ray sources in the Trapezium field, which is a rich stellar cluster in the Milky Way where the high density of X-ray sources would prevent proper optical identifications. The BMW-HRI catalogue can be searched via the HEASARC Browse[*] or via the Brera Observatory web site[*].

Created in 1983 at Lyon Observatory, LEDA[*] was the first database of extragalactic objects and it is continuously updated. It gives a free access to the main astrophysical parameters (coordinates, morphological type, diameter and axis ratio, apparent magnitudes and colors, radial velocity, surface brightness, etc.) for about 106 galaxies over the whole sky. The completeness in apparent B-magnitude is satisfied up to mB = 15.5 (see Paturel et al. 1997).

  \begin{figure}
\par\includegraphics[width=8.8cm,clip]{1520fig1.ps}
\end{figure} Figure 1: Displacement between optical and X-ray positions for point-like sources in the total sample. The solid circle refers to thecross-correlation radius of 20 $^{\prime \prime }$; the dashed one, with 13 $^{\prime \prime }$ radius, contains about 90% of the identifications.

To obtain a representative sample of galaxies we started from the BMW-HRI catalogue and included only serendipitous detections, avoiding the targets. We chose a 3$^\prime $ radius to define the typical region of the target, and selected only sources at off-axis angles $\theta >
3$$^\prime $. In spite of this location, we had to exclude 12 additional sources that were targets of the observations. We then cross-correlated the positions of the X-ray sources in the BMW-HRI catalogue with those of galaxies present in the LEDA database version of 1999 with a tolerance of 20 $^{\prime \prime }$, which should be a reasonable guess to detect extended objects like galaxies and to avoid most of spurious coincidences. This criterium is not appropriate for very extended galaxies (e.g. M 31 or M 33), where a large number of sources are detected at distances significantly larger than our tolerance radius. Therefore we could be selecting against large galaxies, if there is no source within a distance of $\sim$20 $^{\prime \prime }$ from the nucleus. However, this should not be a concern in this study, since the surface density of large galaxies is small; in particular, in the LEDA catalog, the density of galaxies with D25 >3' is < $3 \times 10^{-2}$ deg-2, which implies about <10 in the area we surveyed.

To check the goodness of our choice, we plotted the relative shifts between optical and X-ray positions in Fig. 1. We used only point-like X-ray sources because in extended sources the association with a single optical object could be misleading (e.g. in groups and pairs). About 90% of the identifications are within 13 $^{\prime \prime }$ (represented by the dashed circle in Fig. 1).

This is in good agreement with the HRI positional uncertainty, since the best attitude solution guarantees that on average known objects are detected within 10 $^{\prime \prime }$ of their catalog position, although with possible additional discrepancy mainly in declination (see the ROSAT Handbook at http://heasarc.gsfc.nasa.gov/docs/rosat/ruh/handbook/handbook.html). We verified that all X-ray sources with X-ray/optical off-set >10 $^{\prime \prime }$ are still within the galaxy (i.e. D25). We concluded that the association of the X-ray sources with galaxies found by the cross-correlation is sound on positional grounds.

The cross-correlation yielded 399 X-ray sources associated with 281 galaxies. Since constructed field-by-field, the BMW-HRI catalogue contains multiple detections of the same source. Therefore we only had 283 distinct X-ray sources associated with galaxies[*].

To check the results of the cross-correlation, we inspected HRI images for each source and obtained information from the NASA/IPAC Extragalactic Database (NED) to a) eliminate spurious coincidences [15 sources], b) eliminate AGNs [47 objects], and c) select clusters [57 objects].

a.
We eliminated a source when the obvious optical counterpart was not a LEDA galaxy, but a background or foreground object. This was checked both using NED and the X-ray/optical contour maps.

b.
We excluded objects classified in Véron-Cetty & Véron (2001) Catalogue as Seyfert 1 galaxies, QSOs, BL Lacs, or AGNs. For Seyfert 2 galaxies, the X-ray emission could have a non nuclear origin, so we eliminated them when we saw from images that the X-ray emission was point-like and well centered on the nucleus, while we retained those for which we found an extended emission. We also retained starburst galaxies, LINERs and objects that we know from the literature could have a nuclear source but also non-nuclear X-ray emission (e.g. NGC 3079).

c.
Several galaxies lie inside a cluster; we inspected X-ray images and eliminated those objects whose X-ray emission was indistinguishable from the cluster's, but we retained galaxies for which emission clearly associated with the galaxy is detected above the cluster background (see PGC 12350 in Fig. 2). We retained galaxies in poor groups even when they are the brightest member since there is still ambiguity in the literature about emission from bright early-type galaxies and groups, which are often analyzed in the same context (see among others Pildis et al. 1995; Ponman et al. 1996; Mahdavi et al. 1997; Osmond & Ponman 2004; Mulchaey & Zabludoff 1998; Jones et al. 2003; Mulchaey et al. 2003; Helsdon & Ponman 2003; Mamon 1992; Helsdon & Ponman 2000; Dell'Antonio et al. 1994).
Moreover, in 5 cases the same X-ray source was associated with two or more galaxies in a pair or in a group; since we could not discriminate on a positional basis, we chose the brightest galaxy in the pair or in the group.

These selection criteria yielded a total of 195 X-ray sources (including multiple detections) associated with 143 galaxies whose properties are listed in Table 1, which is available in electronic form. We show the first page here as an example. Col. (1) gives the BMW-HRI name of the source, Cols. (2) and (3) the position of the X-ray peak, Col. (4) the extension of the X-ray source (or "p'' if the source is point-like; asterisks label extended sources for which count rates have been estimated using ad hoc regions), Col. (5) the LEDA galaxy associated to the X-ray source, Col. (6) the name of the galaxy in other common catalogues (e.g. NGC), Col. (7) the morphological type, Col. (8) the distance of galaxy, Col. (9) the apparent B-magnitude corrected for galactic extinction, inclination and redshift effects (see Paturel et al. 1997), Col. (10) the HRI count rate with error, Col. (11) the flux with error, Col. (12) the logarithm of X-ray luminosity (count rates and fluxes have been recomputed with respect to values reported in the BMW-HRI catalogue; see Sect. 3 for details), and Col. (13) specifies whether the galaxy is in the complete subsample (c), in cluster (Cl) or in group (Gr).

Information about magnitudes and redshifts are from LEDA and NED except for 3 objects that we observed ourselves (see Sect. 5). We calculated distances from redshifts, assuming H0 = 50 km s-1 Mpc-1; when the heliocentric radial velocity of galaxy was less than 3000 km s-1, however, we used distances from Nearby Galaxy Catalogue (Tully 1988) corrected for H0 = 50 km s-1 Mpc-1.

One hundred and sixteen of the 143 galaxies have redshift and magnitude (including our observations). Nineteen galaxies have mB and no z, 3 have z and no mB, and 5 have neither z nor mB. The redshift distribution ranges from z = 0 from $z \sim 0.15$, but $\sim$$ 90\%$ of the galaxies have z < 0.07.

   
2.1 The complete serendipitous subsample

To study the general properties of the sample we needed to derive a subsample with well known completeness criteria and limits. To this end we constructed a complete sample with both X-ray and optical flux limits, and had to consider both the X-ray and the optical completeness criteria. The X-ray completeness is related to the BMW-HRI catalogue that includes all sources with significance $\geq$4.2 $\sigma$. To take the optical limits into account, we excluded galaxies fainter than mB = 15.5, the completeness limit assumed for the LEDA Catalogue (see Paturel et al. 1997).

We also excluded objects at low galactic latitude ( $\vert b\vert \leq 10\hbox{$^\circ$ }$) to avoid source confusion in the galactic plane and X-ray sources with off-axis angle $\theta \ge 18\hbox{$^\prime$ }{}$ to match the circular HRI field of view used in the sky coverage computation (see Sect. 7).

The resulting sample of 96 objects is complete both in X-ray and optical at the given limits. However, since galaxies are often in agglomerates, some of them are expected to be related to the targets and therefore not be truly serendipitous. We therefore excluded all sources known to be associated with the target (e.g. galaxies in pairs, groups or clusters; 52 objects in all). When an association was not documented (e.g. from NED, LEDA) we conservatively excluded galaxies at the same redshift as the target (12 objects).

  \begin{figure}
\mbox{
\psfig{figure=1520f21.eps,height=4.5cm,width=4.5cm,clip=}\...
...{1mm}
\psfig{figure=1520f212.eps,height=4.5cm,width=4.5cm,clip=} }\end{figure} Figure 2: First page of the figure available in electronic form. It presents the X-ray contours from smoothed X-ray images superimposed onto optical images. Galaxies are generally at the center of the field. Smoothing is done with a Gaussian function of $\sigma = 5''$ for point-like sources and of $\sigma = 10''$ for extended sources.

The complete, serendipitous sample of 32 galaxies thus obtained is given in Table 3 and will be used to calculate the $\log N-\log S$ distribution in the local universe (z < 0.07), as will be described in detail in Sect. 7.

   
Table 1: First page of table of the total sample, available in electronic form.
BMW-HRI name X-ray coordinates Ext. LEDA name Other name Morph. d mB Count rate F0.1 - 2 log$L_{\rm X}$ Notes
  RA (2000) Dec (2000) ('')     type (Mpc)   (10-3 count s-1) (10-13 cgs) erg s-1  
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
BMW000523.9+161307 00 05 23.83 16 13 11.3 52 PGC 0000372     698   15.74 $\pm$ 2.49 7.40 $\pm$ 1.17 43.59 Cl
BMW002055.1+215208 00 20 55.43 21 51 52.2 p PGC 0001333 IC 1543 Sbc 112 14.54 7.63 $\pm$ 1.11 3.58 $\pm$ 0.52 41.71 c
BMW002055.2+215208                        
BMW002549.3-453227 00 25 49.26 -45 32 26.5 p PGC 0143535   Sab   16.57 18.64 $\pm$ 3.16 7.64 $\pm$ 1.30    
BMW002950.2-405630 00 29 50.99 -40 56 37.9 p PGC 0130966 DUKST 294-9 Sc 241 15.35 19.06 $\pm$ 2.31 7.81 $\pm$ 0.95 42.72 c
BMW003652.3-333310 00 36 52.82 -33 33 14.7 p PGC 0002204 ESO 350-IG38 S? 123 14.96 2.74 $\pm$ 0.43 1.12 $\pm$ 0.14 41.27 c
BMW003918.5+030220 00 39 18.47 03 02 14.8 p PGC 0002362 NGC 194 E 103 13.09 14.75 $\pm$ 1.94 6.49 $\pm$ 0.85 41.89 c; Gr
BMW003948.3+032219 00 39 48.77 03 22 21.0 p PGC 0002401 UM 57       6.15 $\pm$ 0.49 2.70 $\pm$ 0.22    
BMW004242.0+405154 00 42 42.48 40 51 52.6 60 PGC 0002555 NGC 221 (M 32) E 1.05 8.18 52.44 $\pm$ 1.06 26.75 $\pm$ 0.54 38.52 Gr
BMW010716.2+323117 01 07 16.20 32 31 16.6 p PGC 0003966 NGC 379 S0 110 13.48 1.37 $\pm$ 0.35 0.67 $\pm$ 0.17 40.98 Gr
BMW010717.4+322857 01 07 17.76 32 28 57.0 p PGC 0003969 NGC 380 E 88 13.24 4.19 $\pm$ 0.50 2.06 $\pm$ 0.24 41.26 Gr
Column 1: BMW-HRI source name;
Cols. 2 and 3 : X-ray coordinates;
Col. 4: extension of X-ray source (radius of circle or axis of ellipse; asterisk labels sources for which ad hoc region have been used) or "p'' if point-like;
Col. 5: LEDA galaxy associated;
Col. 6: other galaxy name;
Col. 7: morphological galaxy type;
Col. 8: galaxy distance;
Col. 9: apparent B-magnitude;
Col. 10: X-ray count rate;
Col. 11: X-ray flux (0.1 - 2 keV band);
Col. 12: logarithm of X-ray luminosity (0.1 - 2 keV band);
Col. 13: c if the galaxy is in the complete subsample, Cl if in cluster, Gr if in group.

   
3 X-ray characterization

The BMW-HRI catalogue provides count rates derived using the wavelet algorithm in an automated way and under particular assumptions (for details, see Campana et al. 1999; Lazzati et al. 1999). We verified that, while count rates are correctly computed for point-like sources, for very extended sources such as NGC 1399, the extension and count rates given by the algorithm are underestimated. Moreover, when multiple observations are available we could improve the statistics by considering the full set of data. We therefore recalculated all count rates, using the BMW-HRI positions and original HRI data retrieved from the public archives[*] in pulse height analyzer (PHA) channels 1 - 10 to increase the signal-to-noise ratio (for a justification of this choice of PHA, see Trinchieri et al. 1997). When multiple observations of the same field are available, we summed the data if they have the same pointing coordinates and comparable exposure times. Otherwise, we typically used the longer exposures or those where the source is closer to the field's center.

3.1 Count rates

We classified sources as point-like or extended based on the radial distribution of the emission relative to the shape of the HRI point spread function (PSF; for a description of the ROSAT PSF see Boese 2000) at the corresponding off-axis angle. For the "extended sources'' counts were taken from the largest region that contains source counts, in most cases a circle of radius reported in Table 1, evaluated from the radial profile. Given the particular shape of the source, in a few cases we used ellipses to evaluate the counts and give minor and major semiaxes in Table 1. There are also a few extended sources for which ad hoc regions (neither circles nor ellipses) have been used to estimate counts: we label them with an asterisk in Table 1.

For point-like sources the counts were obtained in a circular region centered at the peak of X-ray emission, with radius that includes about 90% of source counts according to the PSF. The PSF degrades as the angular distance from the center of field increases, so we chose a radius of r = 18 $^{\prime \prime }$ for $3\hbox{$^\prime$ }< \theta \leq 10$$^\prime $, r =25 $^{\prime \prime }$ for $10\hbox{$^\prime$ }< \theta \leq 15$$^\prime $ and r =40 $^{\prime \prime }$ for $\theta > 15$$^\prime $, following Boese (2000). We evaluated the background in an annulus concentric to the source radius with radii depending on the off-axis. When the source was particularly faint, we calculated count rates in a circle of radius corresponding to a smaller fraction of the PSF, to increase the signal-to-noise ratio. We then corrected the count rate accordingly following Boese (2000).

We then compared count rates obtained in this way with those reported in the BMW-HRI catalogue and found general agreement, except for some sources whose extension had been largely underestimated by the wavelet algorithm, as stated above. Indeed, our count rates would be equivalent to the "counted count rates'' reported in the catalogue, rather than those computed with the wavelet algorithm. In comparison with this quantity, we found a systematically higher count rate that is consistent with the larger PHA interval used (1 - 10 in our analysis and 2 - 9 in the BMW-HRI catalogue).

The resulting net count rates are given in Table 1, corrected for vignetting and lost counts due to the PSF (for point sources only).

   
3.2 Fluxes and luminosities

The count rates were converted into 0.1 - 2 keV fluxes using a conversion factor corresponding to a bremsstrahlung spectrum with kT =5 keV, plus the line of sight absorption appropriate for each source from Dickey & Lockman (1990), which is reported in Table 2. Although this spectrum might not be suitable for all kinds of sources, the flux in the ROSAT energy window depends only weakly on the spectral model assumed, while it is more dependent on low energy absorption. The resulting fluxes are in the range 10-14 - 10-11 erg cm-2 s-1.

To calculate luminosities, we used distances listed in Table 1. The corresponding range in $L_{\rm X}$ is 1038 - 1043 erg s-1.

   
4 The atlas

In Fig. 2 we provide an overlay of X-ray contours of the detected galaxies onto optical images from the Digital Sky Survey II (DSS II) available from the ESO archive[*]. This figure is available in electronic edition, we report here the first page as an example. When available, we used optical images obtained with the blue filter, otherwise we used those obtained in the red filter. For PGC 209730 only the DSS I plate is available. Galaxies, ordered in RA and generally at the center of the field, are identified by their PGC name.

X-ray contours are produced from images in the PHA range 1-10, smoothed using a Gaussian function with $\sigma = 5$ $^{\prime \prime }$ for point-like sources and with $\sigma = 10$ $^{\prime \prime }$ for extended sources.

   
5 Optical observations

In order to measure redshifts and magnitudes for some of the galaxies of our sample, we made spectroscopical and photometrical observations with the 1.52 m telescope of the Osservatorio Astronomico di Bologna, at Loiano (Italy) on the nights of the 16th and 17th October 2001. Because of bad atmospheric conditions, we were able to observe only 3 galaxies. A spectrophotometric calibration star was also observed. We present the results obtained in Appendix A, available in electronic edition.
 

 
Table 2: Galactic $N_{{\rm H}}$ and corresponding unabsorbed flux in the band 0.1-2 keV for 1 count/s, assuming a thermal bremsstrahlung spectral model with kT = 5 keV.
$N_{{\rm H}}$ (cm-2) CF (erg cm-2 count-1)
$1 \times 10^{20}$ $3.7 \times 10^{-11}$
$2 \times 10^{20}$ $4.1 \times 10^{-11}$
$5 \times 10^{20}$ $4.9 \times 10^{-11}$
$8 \times 10^{20}$ $5.5 \times 10^{-11}$
$3 \times 10^{21}$ $9.3 \times 10^{-11}$


   
6 Comparison with literature

To verify whether the total sample of 143 objects is representative of the X-ray properties of normal galaxies, we calculated X-ray luminosities where possible (Table 1) and plotted the distributions of $L_{\rm X}$, LB, the ratio $L_{\rm X}/L_B$ and the $L_{\rm X} -L_B$ relationship for spiral and early-type galaxies. For the 19 galaxies for which the redshift is not known but we have mB, the ratiowas calculated from fluxes. We compared our results with those in the literature and found a good general agreement. In particular:
1.
The bulk of the galaxies in the sample has an X-ray luminosity between 1038 erg s-1 and few 1042 erg s-1, in accordance with, e.g., Fabbiano (1989). 7 objects have $L_{\rm X} \ga 10^{43}$ erg s-1, but most of them lie in a group, so that the intergalactic medium could contribute to their luminosity; we cannot exclude the presence of an unidentified AGN for some of these objects.

2.
For spiral galaxies we found a linear relationship between X-ray and optical luminosities ( $L_{\rm X} \propto L_B^{1.0 \pm 0.2}$), in agreement with Fabbiano et al. (1992). However, in subsequent, more complete statistical analysis of the 234 "normal'' spiral and irregular galaxies reported by Fabbiano et al. (1992), Shapley et al. (2001) and Fabbiano & Shapley (2002) found that the $L_{\rm X} -L_B$ relationship is significantly steeper than linear, with a slope of about 1.5. Our study is based on a much smaller sample (32 spiral and irregular galaxies): as pointed out by Fabbiano & Shapley (2002), small number statistics could account for the discrepancy.

3.
For early-type galaxies we found a steeper relationship than for later types, $L_{\rm X} \propto L_B^{1.6 \pm 0.2}$, consistent with those obtained by Fabbiano et al. (1992) and Eskridge et al. (1995).


 

 
Table 3: Galactic column density (from Dickey & Lockman 1990), BMW count rates and fluxes for galaxies in the complete serendipitous sample, ordered by increasing flux.
LEDA name $N_{{\rm H}}$ Count rate F0.5 - 2
  (1020 cm-2) (10-3 count s-1) (10-13 erg cm-2 s-1)
0157406 4.9 0.37$\pm$0.07 0.12$\pm$0.02
0068536 2.5 1.11$\pm$0.34 0.32$\pm$0.09
0025825 4.2 1.12$\pm$0.22 0.35$\pm$0.06
0042833 2.0 1.31$\pm$0.23 0.35$\pm$0.05
0028990 0.8 1.50$\pm$0.30 0.36$\pm$0.07
0005323 3.8 1.33$\pm$0.28 0.41$\pm$0.09
0010446 3.1 1.48$\pm$0.24 0.43$\pm$0.06
0057078 2.3 1.63$\pm$0.28 0.44$\pm$0.08
0069338 8.8 1.24$\pm$0.20 0.46$\pm$0.07
0038773 2.0 1.70$\pm$0.11 0.46$\pm$0.03
0001333 4.2 1.55$\pm$0.27 0.48$\pm$0.09
0007289 5.5 1.71$\pm$0.26 0.56$\pm$0.10
0070861 2.6 2.11$\pm$0.38 0.61$\pm$0.12
0018991 5.4 2.18$\pm$0.32 0.70$\pm$0.10
0004117 4.0 2.36$\pm$0.23 0.73$\pm$0.06
0043675 3.9 2.49$\pm$0.37 0.77$\pm$0.12
0002204 1.9 3.23$\pm$0.23 0.87$\pm$0.05
0045318 1.0 3.78$\pm$0.60 0.91$\pm$0.14
0046432 3.2 3.13$\pm$0.66 0.91$\pm$0.20
0047432 2.3 3.61$\pm$0.64 0.97$\pm$0.16
0130966 2.4 4.41$\pm$0.81 1.19$\pm$0.22
0016574 5.9 3.73$\pm$0.51 1.23$\pm$0.17
0005324 3.8 4.34$\pm$0.51 1.35$\pm$0.16
0057728 1.5 5.11$\pm$0.39 1.38$\pm$0.11
0013368 1.4 7.22$\pm$1.41 1.73$\pm$0.24
0029050 0.8 10.20$\pm$0.70 2.45$\pm$0.17
0002362 2.7 9.06$\pm$0.99 2.63$\pm$0.29
0004848 6.1 9.26$\pm$2.43 3.06$\pm$0.66
0063122 7.9 11.02$\pm$1.42 3.97$\pm$0.36
0006367 3.0 14.80$\pm$0.60 4.29$\pm$0.17
0017451 7.5 15.66$\pm$1.72 5.64$\pm$0.72
0028995 4.8 34.20$\pm$2.00 10.94$\pm$0.64


4.
Values of the X-ray-to-optical ratio in our sample cover roughly the same range $(-4 < \log~(L_{\rm X} /L_B) < 0$ with $L_{\rm X}$ and LB in erg s-1) as the spiral galaxies in Shapley et al. (2001) and the early-type galaxies in Eskridge et al. (1995), but their distributions are different. Figure 3 shows the histogram of the X-ray-to-optical ratio of the total sample of 143 galaxies. We will analyze this subject in greater detail in Sect. 7.1.


  \begin{figure}
\par\includegraphics[width=8.2cm,clip]{1520fig3.ps}
\end{figure} Figure 3: X-ray-to-optical ratio distribution for the total sample. Both fluxes are in units of erg cm-2 s-1.

   
7 The log N - log S distribution

The complete serendipitous sample of galaxies derived in Sect. 2.1 (listed in Table 3) was used to calculate the integral flux distribution ( $\log N-\log S$) of normal galaxies with X-ray emission above the X-ray flux limit of the BMW-HRI Catalogue and B-magnitude $\leq$15.5.

The sensitivity of the HRI instrument is not uniform over the entire field of view. Moreover the observing time is different for different fields so we calculated the area surveyed at any given flux (sky coverage).

In the BMW-HRI catalogue the published sky coverage was calculated by means of simulations (see Panzera et al. 2003). In this work we used a sky coverage calculated with the same procedure, but with parameters that reflect our source selection criteria, including therefore only fields with galactic latitude $\vert b\vert \geq 10\hbox{$^\circ$ }$. We considered only an annular region with $3\hbox {$^\prime $ }\leq \theta \leq 18$$^\prime $: the lower limit accounts for the target region; the upper limit is the largest radius within the field of view of the detector in the assumption of circular symmetry; and we assumed a bremsstrahlung spectrum with kT = 5 keV plus the line of sight absorption.

The resulting sky coverage is plotted in Fig. 4. The maximum area is $\sim$314 deg2 and corresponds to fluxes above $\sim$10-12 erg cm-2 s-1. The surveyed area is $\sim$196 deg2 at 10-13 erg cm-2 s-1 and $\sim$3 deg2 at $\sim$ $ 1.1 \times 10^{-14}$ erg cm-2 s-1 (the lowest flux for the galaxies in our sample).

  \begin{figure}
\par\includegraphics[width=8.4cm,clip]{1520fig4.ps}
\end{figure} Figure 4: Sky coverage for the fields at galactic latitude $\vert b\vert \geq $ 10$^\circ $ and off-axis angle $3\hbox {$^\prime $ }\leq \theta \leq 18$$^\prime $, computed by assuming a thermal bremsstrahlung spectrum with kT = 5 keV and galactic line of sight absorption.

For consistency with the sky coverage calculation, fluxes given in Table 3 are derived from the original count rates estimated in the BMW-HRI catalogue, using the wavelet algorithm and PHA channels of HRI from 2 to 9, which are corrected for vignetting and PSF according to Campana et al. (1999) and computed for the energy band 0.5 - 2 keV, the BMW-HRI Catalogue standard.

The integral $\log N-\log S$ distribution of the sample is shown in Fig. 5 and covers two decades in flux, from $\sim$1.1 to $\sim$ $ 110 \times 10^{-14}$ erg cm-2 s-1. The overall distribution could be approximated with a slope of $\sim$-1.1 (solid line in Fig. 5). However the Euclidean slope of -1.5 (dashed line) is also consistent with the data: the excess of galaxies at the highest fluxes is small and consistent within the limited statistics. Moreover, at the lower fluxes, there could be some problems with incompleteness, as we discuss below.

   
7.1 Comparison with the literature: X-ray-to-optical ratio distribution

Before comparing our $\log N-\log S$ distribution with those of other samples in the literature, we need to investigate the X-ray-to-optical ratio distribution of our complete sample more throughly. We consider samples derived from ROSAT and Einstein observations that cover a flux range similar to ours; samples derived from XMM-Newton and Chandra surveys, which cover a flux range significantly fainter than ours, will be considered later, in the discussion of the $\log N-\log S$(Sect. 7.2).

The best available comparison could be with the sample of candidate normal galaxies found by Zimmermann et al. (2001) in the ROSAT All Sky Survey (RASS) and with the normal galaxies found in the Einstein Extended Medium Sensitivity Survey (EMSS; Gioia et al. 1990), both X-ray selected. An effective optically selected sample for comparison is the Einstein galaxy sample (Fabbiano et al. 1992; Shapley et al. 2001; Eskridge et al. 1995).

Zimmermann et al. (2001) made a correlation study of the RASS Bright Source Catalogue (Voges et al. 1999) with the Catalogue of Principal Galaxies (Paturel et al. 1989), from which they selected a sample of 198 candidate galaxies, i.e. X-ray sources whose optical counterpart was not designated as AGN in the literature. These selection criteria are similar to ours, and the Catalogue of Principal Galaxies is a preliminary version of the current LEDA database, so the two samples can be easily compared; however most of their sources have fluxes above 10-12 erg cm-2 s-1 (computed in the 0.1 - 2.4 keV band, assuming a power law spectrum with photon index $\Gamma = 2.3$).

  \begin{figure}
\par\includegraphics[width=8.6cm,clip]{1520fig5.ps}
\end{figure} Figure 5: The integral $\log N-\log S$ distribution for the complete serendipitous subsample (asterisks). The solid line represents the -1.1 slope and the dashed line the Euclidean -1.5 slope.

The EMSS was obtained from analysis of 1453 images of the imaging proportional counter (IPC) on board the Einstein Observatory. The survey covers an area of 778 deg2 at |b| > 20$^\circ $ with limiting sensitivity ranging from $\sim$ $5 \times 10^{-14}$ to $\sim$ $3 \times
10^{-12}$ erg cm-2 s-1 ( 0.3 - 3.5 keV band). 835 serendipitous sources were detected at or above the 4$\sigma$ level (see Gioia et al. 1990; Stocke et al. 1991). Among these, 17 were identified as normal galaxies.

The Einstein sample is the catalogue of normal galaxies observed by the Einstein satellite, compiled by Fabbiano et al. (1992) and reanalyzed by Eskridge et al. (1995, for early-type galaxies) and by Shapley et al. (2001, for spiral galaxies); we no longer distinguish the two samples here since early and late type galaxies are mixed in the BMW-HRI sample. We consider here only detections in the Einstein sample; the exclusion of upper limits should not affect the results, since their distribution is consistent with that of detections (see Fig. 5 in Shapley et al. 2001).

  \begin{figure}
\par\includegraphics[width=8.6cm,clip]{1520fig6.ps}
\end{figure} Figure 6: B flux versus X-ray flux for our total sample (solid triangles), for the Einstein sample (empty circles), for the Zimmermann et al. (2001) sample galaxies (asterisks), and for the EMSS galaxies (empty pentagons). Solid lines correspond to log  $(F_{\rm X}/F_B)= 0$, -2, -4, as indicated; the horizontal dashed line is the mB = 15.5 limit. Only detections in the Einstein sample and only objects with $F_{0.1 - 2} > 2 \times 10^{-12}$ erg cm-2 s-1 and log  $L_{\rm X} < 42.7 $in the Zimmermann et al. (2001) sample are plotted (see text).

In Fig. 6 we plot the distribution of $F_{\rm X}$ and FB values from all samples considered. For consistency with the values in Table 1, all fluxes are converted to the 0.1 - 2 keV energy band, using a thermal bremsstrahlung spectrum with temperature kT = 5 keV and $N_{\rm H} = 3 \times 10^{20}$ cm-2.

Figure 6 clearly indicates that galaxies belonging to different samples populate different regions in the plot. Our sample (solid triangles) has an X-ray flux range between 10-14 and 10-11 erg cm-2 s-1 and log ( $F_{\rm X}/F_B$) between -4 and 0 (see also Fig. 3). The bulk of Einstein galaxies (empty circles) is typically at higher average fluxes and at lower values of log ( $F_{\rm X}/F_B)$ (between -4 and -2) compared to our distribution and to the X-ray selected samples in general. This sample is the largest; it is effectively optically selected and reasonably clean of contamination from AGN (Shapley et al. 2001). However, since it is not complete, it might not provide true distribution of the X-ray-to-optical ratios.

The second largest sample is derived from Zimmermann et al. (2001), with an additional flux limit $F_{\rm X} > 2 \times 10^{-12}$ erg cm-2 s-1 (for completeness, see discussion below) and an upper limit in luminosity at $\log L_{\rm X} = 42.7$ erg s-1, the highest luminosity in our complete sample, comparable to their limit to exclude potential AGNs from the sample. The distribution of candidate galaxies in Zimmermann et al. (2001) (asterisks) is significantly different from that of the Einstein sample and extends at $\log~(F_{\rm X}/F_B) > 0$. The $F_{\rm X}/F_B$ distribution for EMSS galaxies (empty pentagons) is at intermediate values and more consistent with that of our sample.

Also plotted in Fig. 6 is the optical flux limit applied to our sample, mB = 15.5. It is evident that excluding galaxies fainter than this for the $\log N-\log S$ calculation has an effect that increases as flux decreases. We attepted to quantify it in order to correct the curve for lost objects. Unfortunately we could not properly estimate the correction because none of the galaxy samples available allows us to derive the true distribution of X-ray-to-optical ratios of normal galaxies. The EMSS should represent the true $F_{\rm X}/$FB distribution, but given the small number of galaxies (17, of which only 15 have B-magnitude), statistical errors are large. The difference in distribution of ratios between the two larger samples in Fig. 6 suggests that they might be affected by opposite biases; the Zimmermann et al. (2001) sample is likely to contain unclassified AGNs, while the Einstein sample could lose objects at the highest X-ray-to-optical ratios. If we use the three samples to estimate how many galaxies are lost as a function of X-ray flux, we find that corrections to the $\log N-\log S$ are small and the recomputed curve is consistent with the Euclidean slope in the observed flux range.

We also tried to estimate the correction by considering optically fainter galaxies. At mB = 16, LEDA is about 90% complete (see Fig. 7 in Paturel et al. 1997). If we include galaxies down to this flux limit, we only add 4 objects to our serendipitous sample, distributed over the whole range of X-ray fluxes; therefore, their inclusion influences only slightly the normalization, not the slope of the distribution.

We conclude that since the effects introduced by the optical limit are small, the $\log N-\log S$ we derive is consistent with the Euclidean slope.

   
7.2 Comparison with the literature: log N - log S


  \begin{figure}
\par\includegraphics[width=8.5cm,clip]{1520fig7.ps}
\end{figure} Figure 7: Comparison of the $\log N-\log S$ distribution obtained from the present sample (asterisks) with several other relations for normal galaxies from the literature. The dashed line represents the Euclidean relationship of Fig. 5 extrapolated to the full flux range considered. Symbols refer to: EMSS galaxies (empty circles); candidate galaxies in Zimmermann et al. (2001; solid squares); normal galaxies (crosses), including LLAGN (solid circles, Georgakakis et al. 2004a), and stacking analysis (solid triangles, Georgakakis et al. 2003) found in the XMM-Newton/2dF survey; XMM-Newton/Sloan DSS normal galaxies from Georgakakis et al. (2004b; empty squares); Chandra Deep Fields results from Hornschemeier et al. (2003; empty triangles); optimistic or pessimistic curves given by Bauer et al. (2004) (upper/lower dotted line); Bayesian sample of Norman et al. (2004) reported by Ranalli et al. (2004; dot - dashed line). Open stars and horned-shaped box indicate the detections and fluctuation analysis predictions of Miyaji & Griffiths (2002).

Figure 7 shows the comparison between the $\log N-\log S$ derived above with several available from the literature. All fluxes are recomputed in the 0.5 - 2 keV range that we use. We find excellent agreement with other samples that cover similar or brighter flux ranges than the present sample.

The candidate galaxies (Zimmermann et al. 2001) appear to connect smoothly with the Euclidean extrapolation of the BMW-HRI $\log N-\log S$ above 10-12 erg cm-2 s-1. We interpret the flattening observed in the Zimmermann et al. (2001) data at lower fluxes as a result of their selection criteria. In fact, they indicate a $\ge$90% completeness for count rates $\ge$0.1 count s-1, which converts to a flux of $F_{0.5-2} \sim 7 \times 10^{-13}$ erg cm-2 s-1.

Although small, the EMSS is a truly complete sample, since it is serendipitously X-ray selected and $\sim$$96\%$ identified (Gioia et al. 1990; Stocke et al. 1991; Maccacaro et al. 1994). The EMSS appears to be Euclidean and almost coincident with our curve for fluxes above 10-13 erg cm-2 s-1.

We also extended the comparison to include samples at fainter fluxes. Georgakakis et al. (2004a) compute the $\log N-\log S$ of sources in the XMM-Newton/2dF survey, obtained with the EPIC instrument on board the XMM-Newton satellite. This survey covers an area of about 2.5 deg2 to the flux limit $\sim$10-14 erg cm-2 s-1 in the 0.5 -8 keV band (or $F_{0.5 {-} 2} \sim 5 \times 10^{-15}$ erg cm-2 s-1). They find two "normal'' galaxies in their sample, which implies a density of <1 source at $F_{\rm X} \sim
10^{-14}$ erg cm-2 s-1, lower than what we find.

However, the sample of Georgakakis et al. (2004a) contains three additional galaxies (at $z \leq 0.1$ with $L_{0.5 {-} 8} \sim 10^{42}$ erg s-1) that the authors do not consider because they might contain Low Luminosity AGNs (LLAGNs, see their Fig. 2). Since we cannot exclude that our sample also contains a few LLAGNs (see above and Sect. 6), we should consider these objects for better comparison with our sample. With inclusion of these objects the $\log N-\log S$ matches ours better.

Also shown in Fig. 7 are the constraints from the stacking analysis results of Georgakakis et al. (2003) at fainter fluxes, computed from optically selected galaxies at a mean redshift of $z \sim 0.1$. The point derived from the total sample considered is in excellent agreement with our $\log N-\log S$.

Recently Georgakakis et al. (2004b) have presented a pilot sample of normal galaxies serendipitously detected in XMM-Newton public observations. They find 11 "normal'' galaxy candidates with luminosities below 1042 erg s-1 over an area of $\sim$4.5 deg2. They find that the ${\rm log} N-{\rm log} S$ derived from this sample (plotted in Fig. 7) is again almost Euclidean in slope, although at a smaller normalization than ours.

We also plot the results from deeper surveys, using data from Hornschemeier et al. (2003), Norman et al. (2004) as reported by Ranalli et al. (2004), and Bauer et al. (2004) derived from the Chandra Deep Fields. All these relations fall close to, though generally below, the extrapolation from our sample. Different authors derive different slopes for their samples, but they are all consistent with the Euclidean one.

The lower normalizations found in these latter samples could be explained in part by the combined effects of a) more stringent criteria to minimize contamination from the AGNs, even though of low luminosity, and b) different relative occurrence of the galaxy types (spiral/starburst vs early types).

As already discussed, some residual contamination from low luminosity AGNs could be present in the sample we considered, since we have little information on the optical spectra and could only reject known AGNs. We note, however, that Zimmermann et al. (2001) apply the same criterium adopted by Georgakakis et al. (2004a), namely an X-ray to optical luminosity ratio smaller than 10-2, and that the EMSS sample, which is well studied optically, should not be contaminated by AGNs. We nevertheless considered discarding sources in our sample that have a log (F0.5-2/FB) < -2. We have 7 objects that violate this limit, mostly at the high flux end. The resulting $\log N-\log S$ relation is slightly steeper, but consistent with that presented in Fig. 5, and would not significantly lower the normalization of the "Euclidean'' curve plotted. However the location of the points from Georgakakis et al. (2004a) that consider/discard possible contamination from LLAGNs gives an idea of the possible uncertainties involved.

The effect of different relative contributions from the early/late types is more complicated to assess. The lowest flux points (Hornschemeier et al. 2003) are derived from late type galaxies, so they could underrepresent the total population. However, Bauer et al. (2004) suggest that the early type galaxies follow a flatter distribution; in any case their ${\rm log} N-\log S$ is always below those from starburst/quiescent galaxies (see their Fig. 9), so their contribution could in fact be negligeable at the fainter fluxes. In the range covered by Georgakakis et al. (2004b), there is only one early type galaxy (but the sample is very small), while our sample has a sizeable fraction of early types (1/3 among the objects with a morphological classification); and the percentage increases to $\sim$50% in the "candidate normal galaxies'' of Zimmermann et al. (2001), for which there is moreover no apparent significant different in the two slopes. The stacking analysis results from Georgakakis et al. (2003), derived separately for E/S0 and Sa-Scd, bracket the extrapolation of the Euclidean $\log N-\log S$ obtained from brighter samples, with Sa-Scd in better agreement with the samples at low fluxes. Since the emission from early and late type galaxies is due to significantly different processes (Kim et al. 1992; Shapley et al. 2001; Fabbiano et al. 1992; Fabbiano 1989; Eskridge et al. 1995), a different evolution is not out of the question. Assessment of the local ${\rm log} N-\log S$ separately for each morphological type would be a step toward better understanding of the properties of galaxies as a class, and would provide stronger constraints for the investigation of normal galaxies at higher redshifts, which is beyond the scope of the present work. For now, we simply notice how remarkable it is that, in spite of the different selection criteria and instruments used to define all the samples considered, the surface density of normal galaxies is consistent with a single Euclidean distribution for about 6 decades in flux (from $\sim$10-11 to $\sim$ $
3 \times 10^{-17}$ erg cm-2 s-1).

8 Conclusions

We present the results for an "almost serendipitous'' sample of 143 X-ray emitting normal galaxies selected from the cross-correlation of the BMW-HRI Catalogue and the LEDA database. Isointensity X-ray contours are overlayed onto the optical images for all galaxies and presented in an atlas in Fig. 2. The X-ray characteristics of the sample, listed in Table 1, are derived uniformly way and are used in comparison with other samples in the literature. We find that the general properties of the total sample are in good agreement with those already known for normal galaxies.

We also present a complete subsample of 32 truly serendipitous sources in the local universe (z < 0.07), for which we derive the $\log N-\log S$ distribution in the flux range between $\sim$1.1 and $ 110 \times 10^{-14}$ erg cm-2 s-1 in the 0.5 - 2 keV energy band. We find that this relation is consistent with the Euclidean distribution.

Moreover, we find good agreement between our $\log N-\log S$ and those derived from ROSAT PSPC and Einstein data at similar or brighter fluxes and from XMM-Newton and Chandra at fainter fluxes; the overall distribution appears to be consistent with a Euclidean slope for about 6 decades in flux, from $\sim$ $
3 \times 10^{-17}$ to 10-11 erg cm-2 s-1. The normalizations of different samples are consistent within a factor of $\sim$2.

Although with limited statistics, this work provides a first estimate of the number density of sources identified with normal galaxies in the nearby universe, in a flux range (both optical and X-ray) easily accessible for detailed follow up observations. This will allow us to provide a solid basis for studying and classifying objects found in deeper surveys.

While current efforts are mainly focused on probing the distant universe to determine the relevance of normal galaxies as a class at very faint fluxes, the success of these studies also depends on the constraints given by the bright flux end of the number counts, which has still not been studied well. This is particularly relevant at the lowest fluxes where number counts approach total source density (e.g. detections and fluctuation analysis results of Miyaji & Griffiths 2002, see Hornschemeier et al. 2002, and Fig. 7). The sample derived here will therefore be instrumental in studies of both the cosmological evolution of galaxies and the contribution of this class of sources to the X-ray background.

Acknowledgements
We thank Dr. R. Panzera for her invaluable help, in particular in the extraction of our sample from the BMW-HRI catalogue, and Dr. U. Zimmermann for useful discussion on their work and for providing us with the original data for their $\log N-\log S$ that we use in Fig. 7.
We acknowledge partial financial support from the Italian Space Agency (ASI).
This research made use of the Lyon-Meudon Extragalactic Database (LEDA), used the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and the SAOimage ds9 developed by the Smithsonian Astrophysical Observatory.
The compressed files of the "Palomar Observatory - Space Telescope Science Institute Digital Sky Survey'' of the northern sky, based on scans of the Second Palomar Sky Survey are copyright (c) 1993-2000 by the California Institute of Technology and are distributed by agreement. All Rights Reserved.

References

 

  
9 Online Material


 

 
Table 4: The total sample.
BMW - HRI name X-ray coordinates Ext. LEDA name Other name Morph. d mB Count rate F0.1 - 2 log$L_{\rm X}$ Notes
  RA (2000) Dec (2000) ('')     type (Mpc)   (10-3 count s-1) (10-13 cgs) erg s-1  
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
BMW000523.9+161307 00 05 23.83 16 13 11.3 52 PGC 0000372     698   15.74 $\pm$ 2.49 7.40 $\pm$ 1.17 43.59 Cl
BMW002055.1+215208 00 20 55.43 21 51 52.2 p PGC 0001333 IC 1543 Sbc 112 14.54 7.63 $\pm$ 1.11 3.58 $\pm$ 0.52 41.71 c
BMW002055.2+215208                        
BMW002549.3-453227 00 25 49.26 -45 32 26.5 p PGC 0143535   Sab   16.57 18.64 $\pm$ 3.16 7.64 $\pm$ 1.30    
BMW002950.2-405630 00 29 50.99 -40 56 37.9 p PGC 0130966 DUKST 294-9 Sc 241 15.35 19.06 $\pm$ 2.31 7.81 $\pm$ 0.95 42.72 c
BMW003652.3-333310 00 36 52.82 -33 33 14.7 p PGC 0002204 ESO 350-IG38 S? 123 14.96 2.74 $\pm$ 0.43 1.12 $\pm$ 0.14 41.27 c
BMW003918.5+030220 00 39 18.47 03 02 14.8 p PGC 0002362 NGC 194 E 103 13.09 14.75 $\pm$ 1.94 6.49 $\pm$ 0.85 41.89 c; Gr
BMW003948.3+032219 00 39 48.77 03 22 21.0 p PGC 0002401 UM 57       6.15 $\pm$ 0.49 2.70 $\pm$ 0.22    
BMW004242.0+405154 00 42 42.48 40 51 52.6 60 PGC 0002555 NGC 221 (M 32) E 1.05 8.18 52.44 $\pm$ 1.06 26.75 $\pm$ 0.54 38.52 Gr
BMW010716.2+323117 01 07 16.20 32 31 16.6 p PGC 0003966 NGC 379 S0 110 13.48 1.37 $\pm$ 0.35 0.67 $\pm$ 0.17 40.98 Gr
BMW010717.4+322857 01 07 17.76 32 28 57.0 p PGC 0003969 NGC 380 E 88 13.24 4.19 $\pm$ 0.50 2.06 $\pm$ 0.24 41.26 Gr
BMW010717.8+322857                        
BMW010918.1+131013 01 09 18.63 13 10 11.4 60 PGC 0004117 UGC 716   356 14.78 3.77 $\pm$ 0.67 1.77 $\pm$ 0.32 42.41 c; Cl
BMW011314.7+153059 01 13 15.84 15 31 05.0 p PGC 0004392     276   1.60 $\pm$ 0.24 0.75 $\pm$ 0.12 41.78 Cl
BMW011315.3+153102                        
BMW011315.8+153059                        
BMW012038.2+294157 01 20 38.06 29 41 56.2 p PGC 0004848 IC 1672 Sb 142 13.28 7.83 $\pm$ 2.65 4.00 $\pm$ 1.35 41.96 c
BMW012038.8+294150                        
BMW012310.6+332738 01 23 11.33 33 27 29.5 50 PGC 0005060 NGC 499 E-S0 87 12.86 28.37 $\pm$ 1.51 13.90 $\pm$ 0.74 42.01 Gr
BMW012311.5+332741                        
BMW012558.8-012023 01 25 59.10 -01 20 22.8 18* PGC 0005323 NGC 545 E-S0 107 12.78 1.72 $\pm$ 0.28 0.81 $\pm$ 0.13 41.02 c; Cl
BMW012600.2-012040 01 26 00.44 -01 20 40.3 50* PGC 0005324 NGC 547 E 110 12.68 4.83 $\pm$ 0.69 2.27 $\pm$ 0.32 41.50 c; Cl
BMW012600.4-012039                        
BMW012600.7-012040                        
BMW012623.1+013921 01 26 23.24 01 39 17.7 p PGC 0144123 APMUKS(BJ)B012348.87+012346.1     17.13 9.92 $\pm$ 0.84 4.37 $\pm$ 0.37    
BMW014358.8+022053 01 43 58.82 02 20 52.5 40 PGC 0006367 UGC 1214 SO-a 103 14.49 15.22 $\pm$ 0.77 6.70 $\pm$ 0.34 41.90 c
BMW015641.6+330238 01 56 41.61 33 02 30.9 p PGC 0007289 NGC 736 E 87 12.72 1.17 $\pm$ 0.33 0.60 $\pm$ 0.17 40.71 c; Gr
BMW021853.5+423440 02 18 53.93 42 34 38.9 p PGC 0165335   E 110   0.48 $\pm$ 0.14 0.26 $\pm$ 0.08 40.53 Cl
BMW022537.8+365759 02 25 37.90 36 57 48.7 p PGC 0009215 UGC 1877 E 216 14.14 12.86 $\pm$ 1.02 6.30 $\pm$ 0.50 42.52 Cl
BMW022602.5-232136 02 26 02.54 -23 21 36.0 p PGC 0133905 DUKST479-024 Sc 337 15.59 2.79 $\pm$ 0.07 1.14 $\pm$ 0.03 42.15  
BMW023741.8+015827 02 37 41.49 01 58 27.5 p PGC 0009961 NGC 1004 E 130 13.70 5.19 $\pm$ 1.18 1.84 $\pm$ 0.52 41.58 Cl
BMW023819.3+020706 02 38 19.35 02 07 12.5 p PGC 0009997 NGC 1016 E 132 12.59 3.58 $\pm$ 1.16 1.58 $\pm$ 0.51 41.47 Cl
BMW024539.7-525748 02 45 39.70 -52 57 47.5 40 PGC 0010446 ESO-LV 1540110 S0   15.46 1.11 $\pm$ 0.40 0.48 $\pm$ 0.18   c
BMW031858.7+412808 03 18 58.42 41 28 08.3 p PGC 0012350 NGC 1270 E 98 13.40 1.61 $\pm$ 0.31 0.93 $\pm$ 0.18 40.99 Cl
BMW032244.0-370614 03 22 44.13 -37 06 12.2 p PGC 0012653 NGC 1317 SBa 25 11.58 3.27 $\pm$ 0.36 1.34 $\pm$ 0.15 40.00 Cl
BMW032244.1-370613                        
BMW033051.3-523034 03 30 51.46 -52 30 36.3 p PGC 0013046   E-S0 345 14.98 2.21 $\pm$ 0.89 0.87 $\pm$ 0.36 42.08 Cl
BMW033657.5-353015 03 36 57.51 -35 30 15.1 p PGC 0013344 NGC 1387 E-S0 25 11.69 6.76 $\pm$ 0.59 2.50 $\pm$ 0.22 40.26 Cl
BMW033728.0-243003 03 37 28.17 -24 30 05.8 p PGC 0013368 NGC 1385 SBc 26 10.87 6.20 $\pm$ 1.59 2.29 $\pm$ 0.59 40.26 c
BMW033828.6-352659 03 38 28.90 -35 27 02.1 500* PGC 0013418 NGC 1399 E 25 10.06 411.10 $\pm$ 22.67 152.10 $\pm$ 8.39 42.03 Cl
BMW033828.9-352659                        
BMW033830.0-352711                        
BMW033851.5-353536 03 38 51.92 -35 35 41.9 150* PGC 0013433 NGC 1404 E 25 10.62 111.00 $\pm$ 1.21 41.06 $\pm$ 0.45 41.46 Cl
BMW033851.6-353536                        
BMW033851.7-353536                        
BMW041205.3-325222 04 12 03.09 -32 52 28.9 $75 \times 150$ PGC 0014638 NGC 1532 SBb 20 9.69 5.16 $\pm$ 1.26 2.12 $\pm$ 0.52 40.00 Gr
BMW041544.5-553533 04 15 45.64 -55 35 33.2 60 PGC 0014757 NGC 1549 E 20 10.36 7.72 $\pm$ 0.78 3.17 $\pm$ 0.32 40.16 Gr
BMW041545.1-553537                        
BMW041545.8-553533                        
BMW042900.6-533653 04 29 00.91 -53 36 45.0 p PGC 0015231 IC 2081 E-SO 255 14.62 3.39 $\pm$ 0.60 1.25 $\pm$ 0.22 41.98 Cl
BMW042900.7-533647                        
BMW043754.0-425852 04 37 55.01 -42 58 53.0 p PGC 0130376   E   15.53 12.38 $\pm$ 2.04 5.08 $\pm$ 0.84    
BMW044707.0-202847 04 47 06.29 -20 28 39.2 p PGC 0099957   E 430 15.41 6.05 $\pm$ 1.63 2.66 $\pm$ 0.72 42.75 Cl
BMW050138.5-041527 05 01 38.26 -04 15 33.5 p PGC 0016574 NGC 1741 Sm 81 14.56 3.60 $\pm$ 0.91 1.84 $\pm$ 0.46 41.15 c; Gr
BMW050943.5-083652 05 09 44.01 -08 36 51.9 p PGC 0147040   S0-a   17.00 0.89 $\pm$ 0.34 0.49 $\pm$ 0.19    
BMW053359.9-714524 05 34 00.41 -71 45 28.5 p PGC 0017451 ESO 56-G154   145 13.42 16.17 $\pm$ 1.94 8.90 $\pm$ 1.07 42.33 c
BMW062457.1+821914 06 24 57.12 82 19 13.8 p PGC 0018991 UGC 3435   86 14.19 3.17 $\pm$ 0.82 1.55 $\pm$ 0.40 41.10 c
BMW062545.7-042202 06 25 45.47 -04 22 04.4 p PGC 0075751 CGMW 1-0108 Sc     12.25 $\pm$ 0.66 11.39 $\pm$ 0.62    
BMW062545.8-042203                        
BMW071957.5-320041 07 19 58.78 -32 00 54.4 p PGC 0077028 CGMW 2-0778 Sbc   13.74 17.30 $\pm$ 3.91 10.03 $\pm$ 2.27    
BMW073217.8+854234 07 32 17.80 85 42 34.1 22.5 PGC 0021231 NGC 2300 E-S0 47 11.61 10.90 $\pm$ 0.43 5.56 $\pm$ 0.22 41.15 Gr
BMW073220.2+854230                        
BMW074914.6-055607 07 49 14.56 -05 56 11.3 p PGC 0078533 CGMW 1-1742 Sc     1.25 $\pm$ 0.26 0.72 $\pm$ 0.15    
BMW081023.2+421628 08 10 23.16 42 16 27.1 66 PGC 0022928 CGCG 207-40   379 15.90 22.15 $\pm$ 1.17 10.85 $\pm$ 0.57 43.25 Cl
BMW082133.8+470242 08 21 33.55 47 02 37.7 p PGC 0023450     775 17.61 1.27 $\pm$ 0.59 0.60 $\pm$ 0.28 42.61 Cl
BMW090825.4-093349 09 08 25.49 -09 33 41.9 p PGC 0025701     958 17.27 1.69 $\pm$ 0.26 0.82 $\pm$ 0.13 42.92 Cl
BMW090825.7-093336                        
BMW090851.5+110122 09 08 51.50 11 01 22.0 30 PGC 0025741     978 17.07 1.50 $\pm$ 0.31 0.66 $\pm$ 0.14 42.88 Cl
BMW090852.1+110138                        
BMW090943.9+071032 09 09 43.87 07 10 31.5 p PGC 0025825 NGC 2773 Sb 109 14.26 1.05 $\pm$ 0.32 0.50 $\pm$ 0.15 40.83 c
BMW091041.7+071223 09 10 41.86 07 12 27.0 p PGC 0025876 NGC 2777 Sab 26 14.45 1.67 $\pm$ 0.31 0.79 $\pm$ 0.15 39.79 Gr
BMW091826.3-122222 09 18 27.00 -12 22 26.9 75 PGC 0087445     315 15.68 9.97 $\pm$ 1.13 4.89 $\pm$ 0.56 42.74 Cl
BMW100108.4-192631 10 01 08.92 -19 26 26.8 p PGC 0028995 ESO 567-G003 Sab   14.30 10.91 $\pm$ 1.26 5.34 $\pm$ 0.61   c; Gr?
BMW100108.7-192621                        
BMW100114.9+554316 10 01 15.17 55 43 06.0 p PGC 0028990 MCG 9-17-9   31 15.20 1.10 $\pm$ 0.38 0.41 $\pm$ 0.14 39.64 c; Gr
BMW100115.1+554318                        
BMW100115.5+554308                        
BMW100158.3+554100 10 01 58.60 55 40 49.0 120 PGC 0029050 NGC 3079 SBcd 31 9.84 18.44 $\pm$ 1.18 6.82 $\pm$ 0.44 40.87 c; Gr
BMW100158.3+554060                        
BMW100158.4+554103                        
BMW100158.7+554051                        
BMW101010.1+541828 10 10 10.10 54 18 27.7 p PGC 0029594 CGCG 266-27   261 15.38 2.57 $\pm$ 1.27 0.95 $\pm$ 0.47 41.84  
BMW101825.0+215348 10 18 25.03 21 53 45.9 19 PGC 0030099 NGC 3193 E 35 11.72 1.21 $\pm$ 0.31 0.50 $\pm$ 0.13 39.84 Gr
BMW103633.4-271318 10 36 33.36 -27 13 17.4 106 PGC 0031453     215 14.71 9.12 $\pm$ 2.81 4.47 $\pm$ 1.38 42.42 Cl
BMW103719.0-271121 10 37 18.92 -27 11 24.8 25 PGC 0031540 NGC 3315 E-S0 75 13.84 1.39 $\pm$ 0.36 0.68 $\pm$ 0.18 40.65 Cl
BMW104827.8+123157 10 48 27.76 12 31 56.6 50 PGC 0032306 NGC 3389 Sc 34 11.63 3.23 $\pm$ 0.89 1.42 $\pm$ 0.39 40.26 Gr
BMW104925.3+324639 10 49 25.13 32 46 27.1 p PGC 0032390 IC 2604 SBm 50 14.18 2.45 $\pm$ 0.51 1.01 $\pm$ 0.21 40.45  
BMW110522.3+381421 11 05 23.18 38 14 13.2 p PGC 0033514 CGCG 213-27   170 15.92 9.06 $\pm$ 2.70 3.35 $\pm$ 1.00 42.05  
BMW113446.5+485718 11 34 46.51 48 57 17.6 p PGC 0035780 IC 711 E-SO 194 14.95 1.39 $\pm$ 0.41 0.57 $\pm$ 0.17 41.41 Cl
BMW113448.9+490440 11 34 49.51 49 04 39.6 p PGC 0035785 IC 712 E 201 13.67 1.48 $\pm$ 0.45 0.61 $\pm$ 0.18 41.44 Cl
BMW114223.6+101552 11 42 23.79 10 15 51.2 p PGC 0036348 NGC 3825 SBa 128 13.57 1.26 $\pm$ 0.33 0.55 $\pm$ 0.15 40.97 Gr
BMW114232.1+583706 11 42 32.04 58 37 05.8 p PGC 0036369 MCG +10-17-046     15.82 1.21 $\pm$ 0.32 0.45 $\pm$ 0.12    
BMW114430.3+305305 11 44 30.20 30 53 02.9 p PGC 0139685     458 16.51 4.29 $\pm$ 1.43 1.76 $\pm$ 0.59 42.65 Cl
BMW115535.8+232724 11 55 35.92 23 27 27.5 p PGC 0139725     815 17.55 3.24 $\pm$ 0.57 1.33 $\pm$ 0.23 42.99  
BMW120438.2+014717 12 04 38.50 01 47 10.5 p PGC 0038218 NGC 4077 S0 140 13.97 1.68 $\pm$ 0.64 0.69 $\pm$ 0.26 41.19 Gr
BMW120631.5-295119 12 06 31.46 -29 51 18.7 p PGC 0157406       14.62 0.52 $\pm$ 0.17 0.25 $\pm$ 0.08   c
BMW121049.5+392822 12 10 49.82 39 28 23.9 p PGC 0038773 NGC 4156 SBb 135 13.65 1.71 $\pm$ 0.13 0.70 $\pm$ 0.05 41.17 c
BMW121049.5+392820                        
BMW121049.6+392823                        
BMW121633.3+072746 12 16 34.07 07 27 46.9 p PGC 0039328 NGC 4224 Sa 53 12.35 5.79 $\pm$ 1.06 2.37 $\pm$ 0.43 40.88 Cl
BMW121908.2+470531 12 19 08.40 47 05 20.5 p PGC 0039615 UGC 7356 Irr 7.5 15.35 1.87 $\pm$ 0.47 0.96 $\pm$ 0.17 38.65  
BMW122018.0+752214 12 20 17.39 75 22 16.6 40 PGC 0039791 NGC 4291 E 44 12.04 13.65 $\pm$ 1.37 6.01 $\pm$ 0.60 41.11  
BMW122503.5+125317 12 25 04.23 12 53 07.5 100 PGC 0040455 NGC 4374 (M 84) E 25 9.84 54.48 $\pm$ 2.77 23.97 $\pm$ 1.22 41.23 Cl
BMW122504.1+125308                        
BMW122504.3+125318                        
BMW122504.4+125316                        
BMW122504.4+125319                        
BMW122611.1+125642 12 26 11.68 12 56 45.2 $400 \times 200$ PGC 0040653 NGC 4406 (M 86) E 25 9.73 199.80 $\pm$ 7.89 87.91 $\pm$ 3.47 41.79 Cl
BMW122612.6+125628                        
BMW122716.2+085815 12 27 14.97 08 58 17.3 80 PGC 0094216     530 16.11 3.74 $\pm$ 1.03 1.53 $\pm$ 0.42 42.73 Cl
BMW123017.6+121936 12 30 17.59 12 19 35.7 30 PGC 0041297 NGC 4478 E 25 11.93 1.31 $\pm$ 0.30 0.68 $\pm$ 0.13 39.63 Cl
BMW123018.1+121926                        
BMW123018.1+121926                        
BMW123052.5+143307 12 30 52.51 14 33 06.7 40 PGC 0169455 VPC 774     18.18 7.98 $\pm$ 1.43 3.51 $\pm$ 0.63    
BMW123643.2+131515 12 36 43.14 13 15 19.0 p PGC 0042081 IC 3583 Irr 25 13.11 0.67 $\pm$ 0.32 0.30 $\pm$ 0.14 39.33 Cl
BMW124342.7+162340 12 43 42.68 16 23 38.0 p PGC 0042833 NGC 4651 Sc 25 10.81 1.30 $\pm$ 0.36 0.53 $\pm$ 0.15 39.55 c; Cl
BMW125232.8-153057 12 52 33.03 -15 31 02.2 p PGC 0043675 MCG -02-33-038 SO 87 14.39 3.19 $\pm 0.31 $ 1.50 $\pm$ 0.1 41.11 c; Gr
BMW125233.1-153102                        
BMW125302.3-152120 12 53 02.26 -15 21 19.7 p PGC 0043748 DRCG25-68 E-SO 266 15.55 0.54 $\pm$ 0.20 0.25 $\pm$ 0.09 41.38 Cl
BMW125318.1-153203 12 53 18.27 -15 32 03.4 30 PGC 0043777 DRCG25-39 E-SO 284 14.78 2.94 $\pm$ 0.34 1.38 $\pm$ 0.16 42.11 Cl
BMW125318.3-153203                        
BMW125749.0-171628 12 57 49.85 -17 16 25.3 50 PGC 0044369   E 296 14.77 13.80 $\pm$ 1.77 6.76 $\pm$ 0.87 42.84 Cl
BMW125750.2-171616                        
BMW130055.7+274740 13 00 55.99 27 47 29.8 p PGC 0044840 NGC 4911 SBbc 159 13.30 12.83 $\pm$ 1.03 4.74 $\pm$ 0.38 42.14 Cl
BMW130056.0+274737                        
BMW130056.2+274731                        
BMW130559.7+291647 13 05 59.46 29 16 46.8 p PGC 0045318 CGCG 160-136 E 159 15.08 4.42 $\pm$ 0.95 1.64 $\pm$ 0.35 41.66 c
BMW130803.0+292918 13 08 03.09 29 29 12.0 p PGC 0166974         2.61 $\pm$ 0.17 0.97 $\pm$ 0.06   Cl?
BMW130803.2+292910                        
BMW130803.3+292911                        
BMW130803.4+292903                        
BMW131324.5-325247 13 13 24.96 -32 52 44.7 p PGC 0158561       16.26 1.12 $\pm$ 0.41 0.55 $\pm$ 0.20    
BMW131413.5-425739 13 14 13.44 -42 57 38.8 60 PGC 0046023 NGC 5026 SBa 75 11.73 86.49 $\pm$ 3.71 47.57 $\pm$ 2.04 42.48 Cl?
BMW131912.4-123228 13 19 12.40 -12 32 28.1 20 PGC 0046432 NGC 5072 E-SO 136 14.23 2.09 $\pm$ 0.74 0.92 $\pm$ 0.33 41.27 c
BMW132040.2-434200 13 20 40.20 -43 42 00.3 p PGC 0046566 NGC 5082 S0 78 12.96 0.93 $\pm$ 0.50 0.51 $\pm$ 0.27 40.54 Gr
BMW132745.6-314751 13 27 45.41 -31 47 54.0 p PGC 0047177     265 14.53 3.74 $\pm$ 0.61 1.76 $\pm$ 0.29 42.15 Cl
BMW132759.6-272104 13 27 59.87 -27 21 29.6 p PGC 0047209 IC 4255 E 203 13.66 3.91 $\pm$ 1.11 1.92 $\pm$ 0.55 41.95 Cl
BMW132802.6-314519 13 28 02.56 -31 45 19.0 p PGC 0088857   E 258 15.01 3.37 $\pm$ 0.60 1.58 $\pm$ 0.28 42.08 Cl
BMW132958.2+471613 13 30 00.20 47 15 55.1 80 PGC 0047413 NGC 5195 (M 51b) SBpec 14 10.10 12.66 $\pm$ 0.77 5.19 $\pm$ 0.32 40.06 Gr
BMW132959.1+471555                        
BMW132959.8+471556                        
BMW133000.1+471558                        
BMW133006.4-014316 13 30 06.34 -01 43 06.8 45 PGC 0047432 NGC 5183 Sb 86 13.21 2.86 $\pm$ 0.98 1.17 $\pm$ 0.40 41.04 c
BMW133425.1+344127 13 34 24.86 34 41 26.9 60 PGC 0047822 NGC 5223 E 144 13.22 20.33 $\pm$ 1.70 7.52 $\pm$ 0.63 42.24 Cl
BMW134623.6-375810 13 46 23.36 -37 58 23.3 p PGC 0048817 ESO 325- G 016   228 14.67 11.43 $\pm$ 1.27 5.37 $\pm$ 0.60 42.48 Cl
BMW135321.7+402151 13 53 21.67 40 21 50.7 p PGC 0049347 NGC 5350 SBbc 57 11.87 1.38 $\pm$ 0.40 0.51 $\pm$ 0.15 40.26 Gr
BMW140715.2-270922 14 07 15.27 -27 09 27.7 30 PGC 0050373 ESO 510-G66 E-S0 146 13.97 9.04 $\pm$ 0.77 4.43 $\pm$ 0.38 42.03 Cl
BMW141319.7-030857 14 13 19.76 -03 08 58.0 p PGC 0050786 NGC 5507 SO 43 13.22 0.31 $\pm$ 0.09 0.14 $\pm$ 0.04 39.47  
BMW144104.0+532011 14 41 04.03 53 20 10.7 p PGC 0084264     629 17.53 5.88 $\pm$ 1.02 2.18 $\pm$ 0.38 42.99  
BMW151643.2+552432 15 16 42.26 55 24 22.2 p PGC 0054522 NGC 5908 Sb 66 12.20 0.53 $\pm$ 0.20 0.20 $\pm$ 0.07 39.92  
BMW160434.7+174315 16 04 34.65 17 43 21.9 300* PGC 0056962 NGC 6041 E-SO 209 13.90 183.30 $\pm$ 4.47 80.65 $\pm$ 1.97 43.60 Cl
BMW160435.9+174325                        
BMW160508.1+174528 16 05 07.32 17 45 27.4 p PGC 0057031 NGC 6045 SBc 204 13.58 1.12 $\pm$ 0.25 0.49 $\pm$ 0.11 41.37 Cl
BMW160508.2+174340 16 05 08.28 17 43 44.9 p PGC 0057033 NGC 6047 E 188 14.10 6.43 $\pm$ 0.52 2.83 $\pm$ 0.23 42.05 Cl
BMW160508.5+174344                        
BMW160533.6+173611 16 05 32.96 17 35 58.8 40 PGC 0057062 IC 1178 E-SO 204 14.74 2.57 $\pm$ 0.53 1.13 $\pm$ 0.24 41.71 Cl
BMW160534.4+323942 16 05 34.64 32 39 37.4 p PGC 0057078 CGCG 195-013 Sc   15.29 2.12 $\pm$ 0.44 0.87 $\pm$ 0.18   c
BMW160544.5+174303 16 05 44.49 17 43 02.4 p PGC 0057096 IC 1185 Sab 208 14.47 5.61 $\pm$ 0.51 2.47 $\pm$ 0.23 42.09 Cl
BMW161533.6-603948 16 15 32.22 -60 39 55.3 p PGC 0057637 ESO 137- G 007 E-SO 100 13.08 8.95 $\pm$ 1.48 8.33 $\pm$ 1.38 41.96 Cl
BMW161546.1-605509 16 15 46.04 -60 55 08.7 p PGC 0057649 ESO 137- G 008 E 77 12.28 6.43 $\pm$ 0.71 5.98 $\pm$ 0.66 41.60 Cl
BMW161720.2+345408 16 17 20.23 34 54 07.9 20 PGC 0057728 NGC 6107 E 184 14.26 4.32 $\pm$ 0.45 1.77 $\pm$ 0.18 41.84 c; Gr
BMW165944.0+323656 16 59 44.21 32 36 58.2 50 PGC 0059392     591 15.71 30.20 $\pm$ 3.62 12.38 $\pm$ 1.48 43.71 Cl
BMW171305.9+434202 17 13 05.49 43 42 02.2 p PGC 0059859 CGCG 225-70   330 15.75 4.68 $\pm$ 0.55 1.92 $\pm$ 0.22 42.37  
BMW171519.1+573932 17 15 18.99 57 39 33.5 p PGC 0059942 MCG 10-24-118   168 16.13 4.99 $\pm$ 0.72 2.20 $\pm$ 0.32 41.85  
BMW173356.4+433936 17 33 56.58 43 39 30.9 p PGC 0060505 CGCG 226-029     16.31 1.84 $\pm$ 0.49 0.81 $\pm$ 0.21    
BMW174336.7+330457 17 43 37.14 33 04 57.9 p PGC 0060757 CGCG 199-010     15.73 4.30 $\pm$ 0.85 2.02 $\pm$ 0.40    
BMW181055.5+500049 18 10 54.76 50 00 48.0 p PGC 0061505 MCG 08-33-027 E-S0 296 14.85 1.24 $\pm$ 0.41 0.58 $\pm$ 0.19 41.77 Cl?
BMW184359.5+453851 18 43 59.70 45 38 55.0 30 PGC 0165780     263 16.00 1.22 $\pm$ 0.42 0.62 $\pm$ 0.21 41.67  
BMW190012.7-362702 19 00 12.47 -36 27 04.6 p PGC 0209730 CGMW 4-4359       4.03 $\pm$ 0.98 2.22 $\pm$ 0.54    
BMW192131.5+435941 19 21 31.81 43 59 41.4 p PGC 0063122 CGCG 230-9 Sc 273 13.81 10.83 $\pm$ 1.75 5.96 $\pm$ 0.96 42.70 c; Cl
BMW201127.3-564408 20 11 27.57 -56 44 05.5 p PGC 0064228   E 324 15.74 8.58 $\pm$ 0.59 4.20 $\pm$ 0.29 42.70 Cl
BMW201214.3-563822 20 12 14.71 -56 38 16.4 p PGC 0095814       17.37 5.05 $\pm$ 0.50 2.48 $\pm$ 0.25   Cl?
BMW204843.3+251650 20 48 43.29 25 16 49.8 p PGC 0065435 MCG 04-49-003 E-S0 291 17.00 3.62 $\pm$ 0.46 2.10 $\pm$ 0.27 42.30 Cl
BMW210716.0-252807 21 07 16.01 -25 28 7.2 p PGC 0066136 NGC 7016 E 219 14.28 10.18 $\pm$ 1.04 4.99 $\pm$ 0.51 42.42 Cl
BMW210720.4-252917 21 07 20.05 -25 29 16.2 p PGC 0066137 NGC 7017 SO 222 14.24 4.18 $\pm$ 0.83 2.05 $\pm$ 0.41 42.07 Cl
BMW215209.2-194323 21 52 09.58 -19 43 22.7 20 PGC 0067523 ESO 600-G14 S0-a 581 15.36 2.12 $\pm$ 0.45 0.93 $\pm$ 0.20 42.54 C?
BMW215209.4-194318                        
BMW221818.1-593625 22 18 18.55 -59 36 23.4 p PGC 0068536 IC 5187 Sc   14.86 5.57 $\pm$ 1.08 2.28 $\pm$ 0.44   c
BMW223633.3+343010 22 36 32.97 34 30 09.2 p PGC 0069291     174 (16.60) 1.30 $\pm$ 0.36 0.72 $\pm$ 0.20 41.38  
BMW223718.9+342654 22 37 19.17 34 26 55.7 p PGC 0069338 NGC 7335 S0-a 126 13.90 1.10 $\pm$ 0.32 0.60 $\pm$ 0.18 41.03 c; Gr
BMW231221.4-435145 23 12 21.96 -43 51 53.2 p PGC 0070684 ESO 291-G006 E-S0   15.14 2.27 $\pm$ 0.73 0.93 $\pm$ 0.30   Cl?
BMW231546.1-590313 23 15 45.97 -59 03 11.3 p PGC 0070861 ESO 148-IG 002 Sm 268 14.76 1.80 $\pm$ 0.49 0.79 $\pm$ 0.21 41.81 c
BMW231713.2+184229 23 17 11.37 18 42 32.8 80 PGC 0070934 NGC 7578B E 241 14.21 43.44 $\pm$ 2.43 21.28 $\pm$ 1.19 43.14 Gr
BMW231756.7-421339 23 17 56.23 -42 13 32.5 p PGC 0131791   S0-a 336 15.63 0.53 $\pm$ 0.27 0.22 $\pm$ 0.11 41.41 Gr?
BMW231855.6-421406 23 18 55.60 -42 14 05.9 30 PGC 0071031 NGC 7590 Sbc 26 11.37 3.44 $\pm$ 0.58 1.41 $\pm$ 0.24 40.03 Gr
BMW231855.6-421359                        
BMW231921.5-415910 23 19 21.75 -41 59 02.9 p PGC 0095173   Sa   16.00 2.12 $\pm$ 0.65 0.87 $\pm$ 0.27   Gr?
BMW231921.5-415906                        
BMW232042.7+081305 23 20 42.72 08 13 05.1 p PGC 0071140 NGC 7626 E 69 11.92 5.55 $\pm$ 1.05 2.72 $\pm$ 0.51 41.16 Cl
BMW233842.8+271300 23 38 42.74 27 12 59.7 p PGC 0071994 CGCG 476-95 E 186 14.76 0.52 $\pm$ 0.25 0.25 $\pm$ 0.12 40.89 Cl
BMW234818.3+010623 23 48 18.80 01 06 24.0 p PGC 0196693     584 16.46 0.34 $\pm$ 0.20 0.16 $\pm$ 0.09 41.89  
BMW234823.7-280427 23 48 23.98 -28 04 24.3 p PGC 0072471 DUKST 471-012 SO 203 14.64 3.61 $\pm$ 0.87 1.48 $\pm$ 0.36 41.84 Cl
BMW234847.1-281217 23 48 46.73 -28 12 18.8 p PGC 0085790 DRCG54-31 SO   16.14 5.17 $\pm$ 1.22 2.12 $\pm$ 0.50   Cl?
BMW235415.0-100955 23 54 14.53 -10 09 52.0 55 PGC 0141285   Sbc 394 16.29 3.75 $\pm$ 0.62 1.65 $\pm$ 0.27 42.47 Cl
BMW235415.1-100950                        


   
Appendix A: Results of optical observations

The log of observations made at the Loiano Telescope in order to measure redshifts and magnitudes for some galaxies in our sample (see Sect. 5) is listed in Table A.1.

The seeing was about 2 $^{\prime \prime }$, so we used a long slit of width 2.5 $^{\prime \prime }$ for spectra. The spectral range was 3800 Å-8700 Å.

For photometry we used the B - V - R filters of Johnson-Kron-Cousin system. We made use of the Image Reduction and Analysis Facility (IRAF)[*] for spectroscopic and photometric data reduction.

We used all lines visible in the spectra to measure z, which is calculated from the average value. The redshifts obtained are reported in Table A.2. Only absorption lines, typical of early-type galaxies, and no sign of nuclear activity were detected in the galaxy spectra.

The atmosferic conditions were inadequate for photometric observations, however we list our raw estimate of magnitudes in Table A.3 and we use the value obtained for PGC 69291 in Table 1, where it is reported in brackets.

PGC 196693
After obtaining the spectrum, we discovered that NED lists the galaxy SDSS J234817.99+010617.0 at the same position and with the same redshift we obtained, although it does not give a PGC name. We therefore identify PGC 196693 as SDSS J234817.99+010617.0.

PGC 69291
The galaxy is identified as NGC 7325 by LEDA and as NGC 7327 by NED, with a note suggesting that it could be a star. Our observations show 2 objects, a star and a galaxy at $z = 0.0290 \pm 0.0009$ at the position of PGC 69291. Most of the optical flux is due to the star, as listed in Table A.3.

The uncertainty in the X-ray position (see also the map in Fig. 2) does not allow us to identify the X-ray source with either object. Unfortunately the bad quality of our optical does not allow us to use the X-ray-to-optical ratio (see for example Maccacaro et al. 1988) to discriminate between them, because it is consistent with both the star and the galaxy. We list the galaxy in the total sample but due to its faint estimated magnitude it is not included in the complete serendipitous sample.


 

 
Table A.1: Log of optical observations.
Name LEDA coordinates Spectroscopy Photometry
  RA (2000) Dec (2000) Exposure (s) Filter Exposure (s)
PGC 65435 20 48 43.09 25 16 53.0 2 $\times$ 1800 R 2 $\times$ 120
PGC 69291 22 36 33.58 34 30 04.5 2 $\times$ 1800 R 1 $\times$ 60
        R 3 $\times$ 40
        V 1 $\times$ 40
        V 3 $\times$ 80
        B 3 $\times$ 200
PGC 196693 23 48 18.07 01 06 17.3 1 $\times$ 1800    
Feige 110 23 19 58.40 -05 09 56.2 2 $\times$ 480 R 2 $\times$ 30
        V 2 $\times$ 30
        B 2 $\times$ 40



 

 
Table A.2: Average value of redshifts measured for the three galaxies observed.
Name Redshift
PGC 65435 0.0485 $\pm$ 0.0006
PGC 69291 0.0290 $\pm$ 0.0009
PGC 196693 0.093 $\pm$ 0.001



 

 
Table A.3: Estimated magnitudes for two of the three galaxies observed and for the star found near PGC 69291 resulting from our observations with the Loiano Telescope.
Name Magnitude
  B V R
PGC 65435     14.8
PGC 69291 galaxy 16.6 16.1 15.6
PGC 69291 star 13.0 12.5 12.2



  \begin{figure}
\mbox{
\psfig{figure=1520_213.eps,height=4.5cm,width=4.5cm,clip=}...
...g{figure=1520_224.eps,rheight=5cm,height=4.5cm,width=4.5cm,clip=} }
\end{figure} Figure 2: First page of the figure available in electronic form. It presents the X-ray contours from smoothed X-ray images superimposed onto optical images. Galaxies are generally at the center of the field. Smoothing is done with a Gaussian function of $\sigma = 5''$ for point-like sources and of $\sigma = 10''$ for extended sources.


  \begin{figure}
\mbox{
\psfig{figure=1520f21.eps,rheight=5cm,height=4.5cm,width=4...
...g{figure=1520f212.eps,rheight=5cm,height=4.5cm,width=4.5cm,clip=} }
\end{figure} Figure 2: X-ray contours from smoothed X-ray images superimposed onto optical images. Galaxies are generally at the center of the field. Smoothing is done with a Gaussian function of $\sigma = 5''$ for point-like sources and of $\sigma = 10''$ for extended sources.


  \begin{figure}
\par\mbox{
\psfig{figure=1520_225.eps,rheight=5cm,height=4.5cm,wi...
...g{figure=1520_236.eps,rheight=5cm,height=4.5cm,width=4.5cm,clip=} }
\end{figure} Figure 2: continued.


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\end{figure} Figure 2: continued.


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\end{figure} Figure 2: continued.


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\end{figure} Figure 2: continued.


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\end{figure} Figure 2: continued.


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\end{figure} Figure 2: continued.


  \begin{figure}
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\end{figure} Figure 2: continued.


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\end{figure} Figure 2: continued.


  \begin{figure}
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\end{figure} Figure 2: continued.


  \begin{figure}
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...g{figure=15202138.eps,rheight=5cm,height=4.5cm,width=4.5cm,clip=} }
\end{figure} Figure 2: continued.



Copyright ESO 2005