3 Galaxy photometry

3.1 Data reduction

Standard reduction procedures for CCD photometry were applied. Once raw images were bias subtracted and flat-field corrected, cosmic rays were removed. The dark current was found to be negligible for all the cameras. During each night at least 10 bias images were obtained; in all cases they were very stable, so for each run we combined all of them to get an averaged bias that we subtracted to each image. We also took at least eight dome-flats that we combined and corrected from illumination failure with a combined sky-flat of at least six images. Finally cosmic rays were removed using the CR_UTILS IRAF package that replaced the values of the affected pixels by an interpolation of the surrounding pixels in an annulus. Foreground stars near the objects were also masked using a similar procedure.

3.2 Flux calibration

Integrated photometry was performed using the APPHOT IRAF package, mainly the polyphot and phot tasks. Standard Landolt ([1992]) stars observed during each night under different airmasses were used for calibration. They were measured with different apertures using the phot task. The curve of growth of each star was built following the algorithm found in Stetson ([1990]). A least-square method was used to get the following transformation equations:

$$B-2.5\cdot \log(F_{B})=C+K_{B}\cdot X+ K_{B-r}\cdot (B-r)$$ (1)

where B is the Johnson B apparent magnitude, F_B is the flux in counts ${\rm s}^{-1}$, C is the instrumental constant, K_B the extinction, X the airmass, and K_B-r the colour constant referred to the Johnson B-Gunn r colour (we already had Gunn r magnitudes of the galaxies).

Whereas our sample of galaxies was observed in the Gunn r filter, photometric star data from Landolt ([1992]) refer to the Cousins system. Therefore, we have corrected the colours included in the Bouguer fit with an averaged $r-R_{\rm C}=0.37$ (Fukugita et al. [1995]).

The errors of the galaxy magnitudes due to the Bouguer fit were calculated for each object with the covariance matrix of the least-square fit according to the expression:

$$\Delta m_{\rm Bouguer} = t_{1\%}\cdot \sigma_{\rm lsf}\cdot \sqrt{X^{\dagger}\cdot A^{-1}\cdot X}$$ (2)

where $t_{1\%}$ is the value of the t distribution with $N_{\rm stars}-4$ degrees of freedom, and ${\sigma}_{\rm lsf}$ is an unbiased estimation of the standard deviation of the least-square fit. The variance-covariance matrix of the least-square fit, A, the column and line matrixes X and $X^{\dagger}$ for each object are defined as:

$$A=\left[\begin{array}{ccc} N & {\displaystyle \sum_{i=1}^{N}... ...\displaystyle\sum_{i=1}^{N} (B-r)_{i}^{2}} \end{array} \right]$$ (3)

$$X=\left(\begin{array}{c} 1 \\ X \\ B-r \end{array} \right) \h... ...er}=\left(\begin{array}{ccc} 1 & X & B-r \end{array} \right).$$ (4)

The transformation equations for each night are listed in Table 2.
 

Table 2: Instrument features and photometric transformations for each night

Telescope	Date	CCD	RN	Gain	Scale	C	KB	KB-r
			(e-)	(e-/ADU)	( $\hbox{$^{\prime\prime}$ }$/pix)
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)
JKT	Nov. 27, 1997	TEK#4	4.10	1.63	0.30	23.00 $\pm$ 0.03	-0.22 $\pm$ 0.02	0.03 $\pm$ 0.01
JKT	Dec. 01, 1997	TEK#4	4.10	1.63	0.30	23.01 $\pm$ 0.07	-0.24 $\pm$ 0.05	0.02 $\pm$ 0.01
JKT	Dec. 02, 1997	TEK#4	4.10	1.63	0.30	22.78 $\pm$ 0.08	-0.12 $\pm$ 0.06	0.01 $\pm$ 0.02
1.52 m	Jun. 18, 1998	TEK1024	6.38	6.55	0.40	21.45 $\pm$ 0.03	-0.33 $\pm$ 0.02	0.09 $\pm$ 0.01
1.52 m	Jun. 19, 1998	TEK1024	6.38	6.55	0.40	21.40 $\pm$ 0.06	-0.27 $\pm$ 0.04	0.09 $\pm$ 0.01
1.23 m	Oct. 28, 1998	TEK7c_12	5.52	0.80	0.50	22.28 $\pm$ 0.02	-0.21 $\pm$ 0.01	0.08 $\pm$ 0.01
1.52 m	Jun. 10, 1999	TEK1024	6.38	6.55	0.40	21.80 $\pm$ 0.14	-0.36 $\pm$ 0.10	0.10 $\pm$ 0.03
1.23 m	Jun. 16, 1999	LORAL#11	8.50	1.70	0.31	22.95 $\pm$ 0.06	-0.27 $\pm$ 0.04	0.04 $\pm$ 0.01
1.23 m	Jun. 17, 1999	SITe#18	5.20	2.60	0.50	22.03 $\pm$ 0.03	-0.19 $\pm$ 0.02	0.05 $\pm$ 0.01
1.23 m	Jun. 19, 1999	TEK#13	5.10	0.60	0.50	22.81 $\pm$ 0.04	-0.25 $\pm$ 0.03	0.09 $\pm$ 0.01
1.23 m	Jun. 20, 1999	TEK#13	5.10	0.60	0.50	22.84 $\pm$ 0.05	-0.25 $\pm$ 0.03	0.07 $\pm$ 0.01
JKT	Jul. 12, 1999	TEK#5	4.82	1.53	0.30	23.09 $\pm$ 0.03	-0.50 $\pm$ 0.02	0.04 $\pm$ 0.01
JKT	Jul. 13, 1999	TEK#5	4.82	1.53	0.30	22.77 $\pm$ 0.05	-0.21 $\pm$ 0.04	0.03 $\pm$ 0.01
JKT	Jul. 15, 1999	TEK#5	4.82	1.53	0.30	22.81 $\pm$ 0.02	-0.24 $\pm$ 0.01	0.07 $\pm$ 0.01
JKT	Jul. 16, 1999	TEK#5	4.82	1.53	0.30	22.75 $\pm$ 0.03	-0.25 $\pm$ 0.03	0.07 $\pm$ 0.01
JKT	Jul. 17, 1999	TEK#5	4.82	1.53	0.30	22.75 $\pm$ 0.01	-0.20 $\pm$ 0.01	0.06 $\pm$ 0.01
JKT	Jul. 18, 1999	TEK#5	4.82	1.53	0.30	22.85 $\pm$ 0.05	-0.27 $\pm$ 0.04	0.06 $\pm$ 0.01

Table 2: (1) Telescope name. JKT stands for the Jacobus Kapteyn Telescope in La Palma (Spain); 1.52 m for the Spanish Telescope in Calar Alto, Almería (Spain); 1.23 m refers to the telescope at the German-Spanish Observatory in Calar Alto. (2) Date of the observation. (3) CCD detector used. (4) Readout noise of the CCD in electrons. (5) Gain of the CCD in electrons per ADU. (6) Scale of the chip in arcsec per pixel. (7) Instrumental constant of the photometric calibration for each night using Landolt ([1992]) stars. (8) Extinction in the Johnson B band. (9) Colour term of the Bouguer fit refered to the B-r colour (Johnson B and Gunn r).

3.3 Galaxy integrated photometry

Many galaxies were found to be very irregular in shape, being very difficult to apply the standard circular apertures. We decided to measure fluxes using the IRAF task polyphot. This task allowed us to build polygons around the galaxies including the whole object and minimizing the area of sky also included. At least two polygons were used in three different positions (securing a minimum of six measures) to avoid errors due to the specific shape of the polygon. The sky was determined as an average of at least 8 measures with a circular aperture around the object.

The errors were calculated as follows. Each flux measurement included an error due to Poisson noise, the uncertainty in the sky determination, and the readout noise of the CCD. This error, in magnitude representation, is described by the expression:

$$\Delta m_{i} = 1.0857\cdot\frac{\sqrt{\frac{F}{G} + {\rm Ar... ...c{{\rm Area}^{2}\cdot\sigma_{\rm sky}^{2}}{N_{\rm sky}}}} {F}$$ (5)

where F is the flux in counts s^-1, G is the CCD gain in counts ${\rm e}^{-1}$, Area is the area in pixels enclosed by the polygon, $\sigma_{\rm sky}$ is the standard deviation of the sky measure and $N_{\rm sky}$ is the number of pixels of the sky measure. The first term of the sum inside the square root is the Poisson noise (square root of the number of electrons counted), the second term refers to the uncertainty in the determination of the sky level, and the third is related to the effects of flatfield errors in the sky determination. Several polygon measures were taken to assure a good magnitude determination. The final associated error was chosen to be the greatest among all the associated to each polygon and the standard deviation of all the polygon measures:

$$\Delta m_{\rm Flux} \: = \: \max(\Delta m_{i}).$$ (6)

Finally the Bouguer line errors were also taken in consideration, yielding a final expression for the magnitude error:

$$\Delta m_{B} =\sqrt{(\Delta m_{\rm Bouguer})^{2} + (\Delta m_{\rm Flux})^{2} }.$$ (7)

Apparent total B magnitudes, as measured with this method, are listed in Table 3. We have also calculated the B magnitudes inside the 24 mag arcsec^-2 isophote (B₂₄), and the total magnitudes using the Kron ([1980]) radius defined as:

$$r_k=\frac{\displaystyle \sum_{i} r_i\cdot F_i}{\displaystyle \sum_{i} F_i}$$ (8)

where i runs from the center to the aperture which has an isophotal level corresponding to the standard deviation of the sky. A second set of total magnitudes were measured within an aperture of radius $2\cdot r_k$ applying this method. In average, Kron magnitudes were 0.02$^{\rm m}$ fainter than the polygonal ones; the absolute differences ranged from 0.00 to 0.47 magnitudes. The highest differences were always due to the presence of field stars inside the Kron aperture or flux contamination from nearby objects, which have been previously deleted interactively using the CR_UTILS IRAF package.

The apparent magnitudes were converted into absolute magnitudes using the redshifts listed in Table 1. The standard galactic extinction correction was applied using the Burstein & Heiles ([1982]) maps. Because the Balmer decrements are also available for most of the objects (Gallego et al. [1996]), we provide these values in Table 1 to allow the correction from total extinction (Galactic and internal) through the B-V colour excess.

3.4 Effective radii and colours

The effective radius (defined as the radius that contains half of the total light) in the B images was measured in two different ways. First, an equivalent half light radius in arcsec was calculated as the geometric mean of the major and minor semi-axes of the elliptical isophote containing half of the galaxy flux (i.e., $B_{\rm T}+0.75$ magnitudes); this half-light radius $r_{1/2}(\hbox{$^{\prime\prime}$ })$ is tabulated in Col. (5) of Table 3. We also measured the flux of the galaxy inside circular apertures and selected the one containing half of the light. These radii were transformed into effective radius in kpc ($R_{\rm e}$, Col. (4) of Table 3) with the formula:

$$R_{\rm e}{\rm (kpc)}=58.1\cdot r_{\rm e}(\hbox{$^{\prime\prime}$ }) \cdot \frac{[(1+z) (1+z)^{0.5}]} {(1+z)^2}\cdot$$ (9)

B-r colours have also been calculated. We first aligned the Johnson B images with the original Gunn r images from Vitores et al. ([1996a]). Permitted modifications were rotation, scaling and shift. We measured the aperture colour inside the 24 mag arcsec^-2 Johnson B isophote. Then we also obtained the colour inside the isophote of radius the effective radius (as measured in the B band). Again, the Galactic extinction correction was performed using the Burstein & Heiles ([1982]) maps. Conversion constants are 3.98 in B and 2.51 in r; both values were interpolated from Fitzpatrick ([1999]).

In Table 3 we summarize all these results: apparent total and B₂₄ magnitudes in Cols. (2) and (3); effective radius in kpc and arcsec in Cols. (4) and (5) respectively; absolute B magnitudes corrected from Galactic extinction in Col. (6) and effective and isophote 24 mag arcsec^-2 B-r colours in Cols. (7) and (8). Colour information is only available for those galaxies with Gunn r magnitude measured by Vitores et al. ([1996a]).

 

Table 3: Photometry results in the B and r bandpass for the UCM survey

UCM name	$(m_{B})_{\rm T}$	(mB)24	$R_{\rm e}$(kpc)	$r_{1/2}(\hbox{$^{\prime\prime}$ })$	MB	$(B-r)_{\rm ef}$	(B-r)24
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
0000+2140	14.50 $\pm$ 0.04	14.82 $\pm$ 0.06	4.9	7.6	-21.41 $\pm$ 0.05	-	-
0003+2200	17.64 $\pm$ 0.05	17.81 $\pm$ 0.10	2.1	5.3	-18.16 $\pm$ 0.07	1.37$\pm$ 0.11	1.37 $\pm$ 0.14
0003+2215	16.63 $\pm$ 0.05	16.98 $\pm$ 0.08	4.5	9.6	-19.15 $\pm$ 0.06	-	-
0003+1955	14.09 $\pm$ 0.04	14.12 $\pm$ 0.07	0.8	1.0	-22.14 $\pm$ 0.06	-	-
0005+1802	16.32 $\pm$ 0.06	16.52 $\pm$ 0.08	2.1	3.8	-19.03 $\pm$ 0.08	-	-
0006+2332	14.92 $\pm$ 0.02	15.11 $\pm$ 0.05	4.1	8.5	-20.18 $\pm$ 0.05	-	-
0013+1942	17.11 $\pm$ 0.06	17.32 $\pm$ 0.08	2.0	2.7	-19.04 $\pm$ 0.07	-0.06 $\pm$ 0.06	0.52 $\pm$ 0.09
0014+1829	16.09 $\pm$ 0.10	16.31 $\pm$ 0.08	1.6	3.2	-19.21 $\pm$ 0.11	0.55 $\pm$ 0.12	0.58 $\pm$ 0.13
0014+1748	14.87 $\pm$ 0.03	15.21 $\pm$ 0.06	7.9	13.6	-20.41 $\pm$ 0.05	1.15 $\pm$ 0.10	1.06 $\pm$ 0.12
0015+2212	16.54 $\pm$ 0.04	16.83 $\pm$ 0.07	1.3	2.6	-18.97 $\pm$ 0.06	0.53 $\pm$ 0.33	0.84 $\pm$ 0.34
0017+1942	15.83 $\pm$ 0.04	15.97 $\pm$ 0.06	4.3	4.5	-20.39 $\pm$ 0.05	0.53 $\pm$ 0.11	0.52 $\pm$ 0.12
0017+2148	16.69 $\pm$ 0.05	17.07 $\pm$ 0.09	1.1	2.7	-18.74 $\pm$ 0.07	-	-
0018+2216	16.83 $\pm$ 0.01	16.91 $\pm$ 0.03	1.1	2.2	-18.34 $\pm$ 0.05	0.56 $\pm$ 0.03	0.79 $\pm$ 0.05
0018+2218	15.80 $\pm$ 0.03	16.24 $\pm$ 0.04	6.2	13.1	-19.95 $\pm$ 0.05		-
0019+2201	16.47 $\pm$ 0.03	16.87 $\pm$ 0.05	2.5	4.5	-18.97 $\pm$ 0.05	1.11 $\pm$ 0.33	1.08 $\pm$ 0.34
0022+2049	15.62 $\pm$ 0.02	15.76 $\pm$ 0.06	2.3	4.1	-19.73 $\pm$ 0.05	1.16 $\pm$ 0.10	1.16 $\pm$ 0.11
0023+1908	16.78 $\pm$ 0.04	16.89 $\pm$ 0.18	1.5	2.2	-19.23 $\pm$ 0.05	-	-
0034+2119	15.80 $\pm$ 0.04	16.09 $\pm$ 0.08	5.3	5.5	-20.66 $\pm$ 0.06	-	-
0037+2226	14.57 $\pm$ 0.02	14.71 $\pm$ 0.07	4.9	9.8	-20.95 $\pm$ 0.05	-	-
0038+2259	16.15 $\pm$ 0.04	16.32 $\pm$ 0.06	7.5	5.5	-21.14 $\pm$ 0.05	1.28 $\pm$ 0.10	1.25 $\pm$ 0.11
0039+0054	14.91 $\pm$ 0.09	15.29 $\pm$ 0.08	6.7	15.6	-20.40 $\pm$ 0.10	-	-
0040+0257	16.84 $\pm$ 0.05	17.02 $\pm$ 0.13	2.3	2.1	-19.95 $\pm$ 0.06	-0.25 $\pm$ 0.03	0.10 $\pm$ 0.13
0040+2312	15.59 $\pm$ 0.03	15.96 $\pm$ 0.05	6.8	7.6	-20.38 $\pm$ 0.05	-	-
0040+0220	17.07 $\pm$ 0.02	17.21 $\pm$ 0.07	1.0	2.0	-18.04 $\pm$ 0.05	0.44 $\pm$ 0.10	0.67 $\pm$ 0.12
0040-0023	13.64 $\pm$ 0.02	13.87 $\pm$ 0.03	5.8	14.9	-21.04 $\pm$ 0.06	-	-
0041+0134	14.31 $\pm$ 0.02	14.63 $\pm$ 0.05	9.9	21.0	-20.76 $\pm$ 0.05	-	-
0043+0245	17.24 $\pm$ 0.09	17.36 $\pm$ 0.14	1.0	2.0	-18.03 $\pm$ 0.10	-	-
0043-0159	13.05 $\pm$ 0.01	13.09 $\pm$ 0.07	8.1	17.1	-21.94 $\pm$ 0.05	-	-
0044+2246	15.97 $\pm$ 0.02	16.26 $\pm$ 0.06	5.7	7.3	-20.04 $\pm$ 0.05	1.20 $\pm$ 0.15	1.08 $\pm$ 0.16
0045+2206	14.97 $\pm$ 0.03	15.08 $\pm$ 0.06	1.9	3.9	-20.53 $\pm$ 0.05	-	-
0047+2051	16.86 $\pm$ 0.02	16.91 $\pm$ 0.08	4.0	2.9	-20.94 $\pm$ 0.04	0.60 $\pm$ 0.10	0.77 $\pm$ 0.12
0047-0213	15.53 $\pm$ 0.03	15.71 $\pm$ 0.09	1.4	3.8	-19.32 $\pm$ 0.06	0.49 $\pm$ 0.03	0.67 $\pm$ 0.10
0047+2413	15.72 $\pm$ 0.03	15.96 $\pm$ 0.09	7.3	6.7	-20.99 $\pm$ 0.05	1.07 $\pm$ 0.05	1.02 $\pm$ 0.10
0047+2414	15.21 $\pm$ 0.03	15.28 $\pm$ 0.07	5.1	4.9	-21.50 $\pm$ 0.05	-	-
0049-0006	18.24 $\pm$ 0.13	18.77 $\pm$ 0.13	1.9	1.7	-18.60 $\pm$ 0.14	0.01 $\pm$ 0.17$^\dagger$	-
0049+0017	16.97 $\pm$ 0.02	17.38 $\pm$ 0.07	1.4	3.7	-17.71 $\pm$ 0.06	-0.33 $\pm$ 0.04	0.16 $\pm$ 0.08
0049-0045	15.21 $\pm$ 0.01	15.39 $\pm$ 0.05	0.7	5.7	-17.23 $\pm$ 0.14	-	-
0050+0005	16.26 $\pm$ 0.02	16.46 $\pm$ 0.06	2.9	3.0	-20.40 $\pm$ 0.04	0.44 $\pm$ 0.05	0.50 $\pm$ 0.07
0050+2114	15.53 $\pm$ 0.06	-	-	-	-20.41 $\pm$ 0.07	0.83 $\pm$ 0.33$^\dagger$	-
0051+2430	15.19 $\pm$ 0.04	15.34 $\pm$ 0.05	3.8	8.5	-19.99 $\pm$ 0.07	-	-
0054-0133	15.74 $\pm$ 0.05	16.09 $\pm$ 0.11	7.2	5.7	-21.87 $\pm$ 0.06	-	-
0054+2337	15.19 $\pm$ 0.02	15.50 $\pm$ 0.05	3.8	8.7	-19.94 $\pm$ 0.06	-	-
0056+0044	16.60 $\pm$ 0.05	17.32 $\pm$ 0.11	3.7	10.7	-18.67 $\pm$ 0.07	0.28 $\pm$ 0.08	0.26 $\pm$ 0.11
0056+0043	16.56 $\pm$ 0.03	16.64 $\pm$ 0.08	1.3	2.3	-18.78 $\pm$ 0.05	0.26 $\pm$ 0.03	0.42 $\pm$ 0.09
0119+2156	16.59 $\pm$ 0.05	16.82 $\pm$ 0.09	9.6	5.3	-21.32 $\pm$ 0.06	1.26 $\pm$ 0.05	1.13 $\pm$ 0.10
0121+2137	15.81 $\pm$ 0.09	15.98 $\pm$ 0.23	8.5	9.8	-20.93 $\pm$ 0.10	0.51 $\pm$ 0.04	0.40 $\pm$ 0.23
0129+2109	15.11 $\pm$ 0.03	15.22 $\pm$ 0.07	8.3	10.1	-21.66 $\pm$ 0.05	-	-
0134+2257	15.89 $\pm$ 0.05	16.26 $\pm$ 0.07	6.9	7.3	-21.14 $\pm$ 0.06	-	-
0135+2242	16.79 $\pm$ 0.04	17.21 $\pm$ 0.10	2.4	3.0	-20.33 $\pm$ 0.05	0.67 $\pm$ 0.04	0.74 $\pm$ 0.11
0138+2216	17.58 $\pm$ 0.02	17.82 $\pm$ 0.06	3.9	2.3	-20.62 $\pm$ 0.04	-	-
0141+2220	16.26 $\pm$ 0.04	16.36 $\pm$ 0.09	1.7	3.0	-19.18 $\pm$ 0.06	0.39 $\pm$ 0.09	0.37 $\pm$ 0.13
0142+2137	15.39 $\pm$ 0.05	15.66 $\pm$ 0.07	9.4	9.9	-21.59 $\pm$ 0.06	1.20 $\pm$ 0.10	1.11 $\pm$ 0.12
0144+2519	15.64 $\pm$ 0.03	15.89 $\pm$ 0.09	9.6	10.7	-21.79 $\pm$ 0.05	0.77 $\pm$ 0.10	0.67 $\pm$ 0.13
0147+2309	16.72 $\pm$ 0.05	16.94 $\pm$ 0.08	1.9	3.4	-18.91 $\pm$ 0.07	0.75 $\pm$ 0.10	0.79 $\pm$ 0.13
0148+2124	16.88 $\pm$ 0.06	17.28 $\pm$ 0.10	1.2	3.2	-18.40 $\pm$ 0.08	0.39 $\pm$ 0.11	0.62 $\pm$ 0.14
0150+2032	16.66 $\pm$ 0.05	16.99 $\pm$ 0.12	6.3	8.7	-19.98 $\pm$ 0.07	0.60 $\pm$ 0.15	0.58 $\pm$ 0.16
0156+2410	15.16 $\pm$ 0.03	15.33 $\pm$ 0.09	2.1	5.3	-19.75 $\pm$ 0.06	0.48 $\pm$ 0.03	0.53 $\pm$ 0.10
0157+2413	15.03 $\pm$ 0.04	15.16 $\pm$ 0.06	5.4	8.7	-20.44 $\pm$ 0.06	1.20 $\pm$ 0.04	1.14 $\pm$ 0.07
0157+2102	14.87 $\pm$ 0.02	14.95 $\pm$ 0.07	1.6	4.4	-19.40 $\pm$ 0.07	0.24 $\pm$ 0.03	0.33 $\pm$ 0.08
0159+2354	17.19 $\pm$ 0.07	17.41 $\pm$ 0.16	1.1	2.4	-18.20 $\pm$ 0.09	1.00 $\pm$ 0.13$^\dagger$	-
0159+2326	15.87 $\pm$ 0.02	16.01 $\pm$ 0.05	2.5	4.9	-19.56 $\pm$ 0.05	0.99 $\pm$ 0.03	1.02 $\pm$ 0.06
1246+2727	15.88 $\pm$ 0.02	15.94 $\pm$ 0.09	3.5	5.6	-19.55 $\pm$ 0.05	-	-
1247+2701	16.63 $\pm$ 0.05	16.77 $\pm$ 0.06	2.3	3.4	-19.11 $\pm$ 0.07	0.49 $\pm$ 0.04	0.55 $\pm$ 0.07
1248+2912	14.87 $\pm$ 0.02	15.18 $\pm$ 0.06	5.8	10.5	-20.75 $\pm$ 0.05	-	-
1253+2756	15.81 $\pm$ 0.04	15.98 $\pm$ 0.06	1.5	3.2	-19.20 $\pm$ 0.06	0.67 $\pm$ 0.10	0.68 $\pm$ 0.10
1254+2741	16.70 $\pm$ 0.07	17.20 $\pm$ 0.10	2.4	5.0	-18.40 $\pm$ 0.08	1.10 $\pm$ 0.07	1.05 $\pm$ 0.10

 

Table 3: continued

UCM name	$(m_{B})_{\rm T}$	(mB)24	$R_{\rm e}$(kpc)	$r_{1/2}(\hbox{$^{\prime\prime}$ })$	MB	$(B-r)_{\rm ef}$	(B-r)24
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
1254+2802	16.81 $\pm$ 0.03	17.00 $\pm$ 0.06	2.9	3.7	-19.15 $\pm$ 0.05	0.90 $\pm$ 0.05	0.98 $\pm$ 0.07
1255+2819	15.51 $\pm$ 0.07	16.08 $\pm$ 0.08	7.7	10.8	-20.64 $\pm$ 0.08	0.83 $\pm$ 0.14	0.77 $\pm$ 0.15
1255+3125	16.14 $\pm$ 0.08	16.41 $\pm$ 0.08	2.1	3.2	-19.86 $\pm$ 0.09	1.12 $\pm$ 0.09	1.14 $\pm$ 0.11
1255+2734	16.69 $\pm$ 0.02	16.96 $\pm$ 0.06	2.7	5.7	-19.08 $\pm$ 0.05	0.88 $\pm$ 0.20	0.85 $\pm$ 0.21
1256+2717	17.62 $\pm$ 0.07	18.13 $\pm$ 0.09	1.5	2.6	-18.48 $\pm$ 0.08	-	-
1256+2732	15.95 $\pm$ 0.06	16.18 $\pm$ 0.06	2.8	4.3	-19.82 $\pm$ 0.07	0.52 $\pm$ 0.08	0.53 $\pm$ 0.09
1256+2701	16.62 $\pm$ 0.05	16.88 $\pm$ 0.08	4.7	5.6	-19.25 $\pm$ 0.07	0.44 $\pm$ 0.09	0.39 $\pm$ 0.11
1256+2910	16.22 $\pm$ 0.05	16.22 $\pm$ 0.05	4.6	4.8	-19.96 $\pm$ 0.07	0.83 $\pm$ 0.04	0.86 $\pm$ 0.06
1256+2823	15.72 $\pm$ 0.12	16.04 $\pm$ 0.15	6.0	6.3	-20.68 $\pm$ 0.12	0.90 $\pm$ 0.15	0.80 $\pm$ 0.15
1256+2754	15.37 $\pm$ 0.05	15.44 $\pm$ 0.06	2.6	5.0	-19.74 $\pm$ 0.07	0.49 $\pm$ 0.21	0.50 $\pm$ 0.21
1256+2722	17.09 $\pm$ 0.05	17.28 $\pm$ 0.10	2.4	2.7	-19.11 $\pm$ 0.06	0.64 $\pm$ 0.10	0.80 $\pm$ 0.14
1257+2808	16.14 $\pm$ 0.02	16.34 $\pm$ 0.04	1.7	3.3	-19.10 $\pm$ 0.05	0.66 $\pm$ 0.06	0.71 $\pm$ 0.08
1258+2754	15.82 $\pm$ 0.04	16.03 $\pm$ 0.06	4.1	5.6	-20.13 $\pm$ 0.06	0.42 $\pm$ 0.08	0.38 $\pm$ 0.09
1259+2934	14.21 $\pm$ 0.04	-	-	-	-21.59 $\pm$ 0.06	0.03 $\pm$ 0.06$^\dagger$	-
1259+3011	16.21 $\pm$ 0.04	16.32 $\pm$ 0.07	1.9	2.3	-20.13 $\pm$ 0.05	0.72 $\pm$ 0.09	0.84 $\pm$ 0.11
1259+2755	15.37 $\pm$ 0.02	15.51 $\pm$ 0.05	3.2	4.4	-20.42 $\pm$ 0.05	0.84 $\pm$ 0.12	0.95 $\pm$ 0.13
1300+2907	17.07 $\pm$ 0.04	17.37 $\pm$ 0.12	1.4	2.7	-18.56 $\pm$ 0.06	0.03 $\pm$ 0.05	0.35 $\pm$ 0.13
1301+2904	15.45 $\pm$ 0.13	15.81 $\pm$ 0.14	5.8	8.0	-20.61 $\pm$ 0.13	0.48 $\pm$ 0.14	0.36 $\pm$ 0.15
1302+2853	16.22 $\pm$ 0.02	16.43 $\pm$ 0.04	2.7	4.3	-19.59 $\pm$ 0.05	0.48 $\pm$ 0.03	0.47 $\pm$ 0.05
1302+3032	16.56 $\pm$ 0.02	16.74 $\pm$ 0.05	2.3	2.7	-20.04 $\pm$ 0.04	-	-
1303+2908	16.78 $\pm$ 0.03	16.99 $\pm$ 0.12	3.5	4.6	-19.24 $\pm$ 0.05	0.38 $\pm$ 0.13	0.56 $\pm$ 0.14
1304+2808	15.84 $\pm$ 0.07	16.12 $\pm$ 0.10	4.2	8.8	-19.71 $\pm$ 0.08	1.12 $\pm$ 0.12	1.04 $\pm$ 0.13
1304+2830	18.57 $\pm$ 0.05	18.69 $\pm$ 0.05	0.8	1.3	-17.05 $\pm$ 0.07	-0.08 $\pm$ 0.03	0.41 $\pm$ 0.07
1304+2907	15.12 $\pm$ 0.07	15.38 $\pm$ 0.10	5.1	12.6	-19.82 $\pm$ 0.09	0.45 $\pm$ 0.07	0.48 $\pm$ 0.10
1304+2818	15.75 $\pm$ 0.01	15.91 $\pm$ 0.04	4.5	5.9	-20.13 $\pm$ 0.04	0.81 $\pm$ 0.10	0.81 $\pm$ 0.11
1306+2938	15.27 $\pm$ 0.02	15.47 $\pm$ 0.04	2.7	4.4	-20.27 $\pm$ 0.05	0.41 $\pm$ 0.07	0.49 $\pm$ 0.08
1306+3111	16.25 $\pm$ 0.04	16.40 $\pm$ 0.09	1.7	3.5	-18.79 $\pm$ 0.06	0.97 $\pm$ 0.12	0.91 $\pm$ 0.14
1307+2910	14.04 $\pm$ 0.03	14.41 $\pm$ 0.05	9.2	17.5	-21.21 $\pm$ 0.06	1.07 $\pm$ 0.10	0.98 $\pm$ 0.11
1308+2958	15.25 $\pm$ 0.01	15.46 $\pm$ 0.03	6.8	10.3	-20.42 $\pm$ 0.04	0.88 $\pm$ 0.03	0.82 $\pm$ 0.05
1308+2950	14.83 $\pm$ 0.06	15.10 $\pm$ 0.06	10.2	13.8	-21.05 $\pm$ 0.07	1.17 $\pm$ 0.05	1.06 $\pm$ 0.07
1310+3027	16.51 $\pm$ 0.04	16.77 $\pm$ 0.06	2.6	3.7	-19.28 $\pm$ 0.06	0.90 $\pm$ 0.09	0.89 $\pm$ 0.11
1312+3040	15.49 $\pm$ 0.04	15.67 $\pm$ 0.07	2.8	4.6	-20.05 $\pm$ 0.06	0.96 $\pm$ 0.11	0.90 $\pm$ 0.12
1312+2954	16.10 $\pm$ 0.03	16.24 $\pm$ 0.06	4.4	5.6	-19.64 $\pm$ 0.05	0.90 $\pm$ 0.05	0.88 $\pm$ 0.07
1313+2938	16.68 $\pm$ 0.05	16.82 $\pm$ 0.13	1.6	1.7	-20.18 $\pm$ 0.06	0.06 $\pm$ 0.10	0.39 $\pm$ 0.16
1314+2827	16.14 $\pm$ 0.03	16.35 $\pm$ 0.06	1.9	2.8	-19.83 $\pm$ 0.05	0.07 $\pm$ 0.09	0.60 $\pm$ 0.11
1320+2727	17.41 $\pm$ 0.07	17.53 $\pm$ 0.09	1.3	1.9	-18.52 $\pm$ 0.08	-0.03 $\pm$ 0.05	0.39 $\pm$ 0.10
1324+2926	17.62 $\pm$ 0.08	18.02 $\pm$ 0.10	0.8	2.1	-17.46 $\pm$ 0.10	0.63 $\pm$ 0.11	0.89 $\pm$ 0.14
1324+2651	15.10 $\pm$ 0.06	15.20 $\pm$ 0.10	1.9	2.9	-20.79 $\pm$ 0.07	0.44 $\pm$ 0.05	0.61 $\pm$ 0.11
1331+2900	18.81 $\pm$ 0.12	19.12 $\pm$ 0.17	1.4	1.4	-17.87 $\pm$ 0.13	0.39 $\pm$ 0.11	0.50 $\pm$ 0.19
1428+2727	14.78 $\pm$ 0.02	14.91 $\pm$ 0.03	2.3	5.3	-19.98 $\pm$ 0.06	0.50 $\pm$ 0.11	0.44 $\pm$ 0.12
1429+2645	17.31 $\pm$ 0.09	17.83 $\pm$ 0.09	2.4	3.3	-19.17 $\pm$ 0.10	0.43 $\pm$ 0.08	0.64 $\pm$ 0.10
1430+2947	16.46 $\pm$ 0.06	16.91 $\pm$ 0.08	3.2	4.2	-19.76 $\pm$ 0.07	0.90 $\pm$ 0.09	0.79 $\pm$ 0.11
1431+2854	15.51 $\pm$ 0.06	15.64 $\pm$ 0.08	5.3	5.0	-20.85 $\pm$ 0.07	0.96 $\pm$ 0.13	0.81 $\pm$ 0.14
1431+2702	16.57 $\pm$ 0.07	17.12 $\pm$ 0.08	2.6	3.5	-20.28 $\pm$ 0.07	0.50 $\pm$ 0.07	0.55 $\pm$ 0.09
1431+2947	17.49 $\pm$ 0.07	18.23 $\pm$ 0.09	2.4	5.2	-18.12 $\pm$ 0.09	0.59 $\pm$ 0.10	0.55 $\pm$ 0.12
1431+2814	16.92 $\pm$ 0.03	17.05 $\pm$ 0.05	2.6	2.6	-19.51 $\pm$ 0.05	1.01 $\pm$ 0.05	1.04 $\pm$ 0.07
1432+2645	15.35 $\pm$ 0.02	15.66 $\pm$ 0.05	7.4	9.3	-21.04 $\pm$ 0.04	0.72 $\pm$ 0.07	0.74 $\pm$ 0.07
1440+2521S	16.80 $\pm$ 0.04	17.12 $\pm$ 0.04	3.3	3.7	-19.67 $\pm$ 0.05	0.74 $\pm$ 0.05	0.73 $\pm$ 0.06
1440+2511	16.37 $\pm$ 0.06	17.07 $\pm$ 0.08	6.4	8.7	-20.22 $\pm$ 0.07	0.95 $\pm$ 0.07	0.88 $\pm$ 0.09
1440+2521N	16.64 $\pm$ 0.03	16.84 $\pm$ 0.03	3.6	4.1	-19.83 $\pm$ 0.05	1.11 $\pm$ 0.05	0.97 $\pm$ 0.06
1442+2845	15.29 $\pm$ 0.02	15.49 $\pm$ 0.02	1.9	6.0	-18.81 $\pm$ 0.07	0.63 $\pm$ 0.02	0.66 $\pm$ 0.04
1443+2714	15.49 $\pm$ 0.10	15.80 $\pm$ 0.14	3.8	5.4	-20.79 $\pm$ 0.11	0.94 $\pm$ 0.15	0.78 $\pm$ 0.15
1443+2844	15.65 $\pm$ 0.02	15.73 $\pm$ 0.04	4.0	4.9	-20.51 $\pm$ 0.05	0.82 $\pm$ 0.08	0.74 $\pm$ 0.08
1443+2548	15.75 $\pm$ 0.03	15.80 $\pm$ 0.06	4.8	4.8	-20.99 $\pm$ 0.05	0.63 $\pm$ 0.04	0.57 $\pm$ 0.07
1444+2923	16.39 $\pm$ 0.03	17.13 $\pm$ 0.04	4.9	6.3	-19.76 $\pm$ 0.05	0.74 $\pm$ 0.09	0.69 $\pm$ 0.10
1452+2754	16.32 $\pm$ 0.04	16.46 $\pm$ 0.04	3.8	4.1	-20.32 $\pm$ 0.06	0.99 $\pm$ 0.10	0.89 $\pm$ 0.11
1506+1922	15.93 $\pm$ 0.03	16.23 $\pm$ 0.02	2.8	5.6	-19.60 $\pm$ 0.05	1.01 $\pm$ 0.03	1.00 $\pm$ 0.04
1513+2012	15.79 $\pm$ 0.09	15.96 $\pm$ 0.13	4.0	3.4	-21.09 $\pm$ 0.10	0.84 $\pm$ 0.15	0.79 $\pm$ 0.15
1537+2506N	15.13 $\pm$ 0.03	15.33 $\pm$ 0.03	4.8	6.6	-20.76 $\pm$ 0.05	0.90 $\pm$ 0.08	0.87 $\pm$ 0.09
1537+2506S	16.10 $\pm$ 0.05	16.32 $\pm$ 0.05	2.9	3.5	-19.79 $\pm$ 0.07	0.75 $\pm$ 0.09	0.67 $\pm$ 0.10
1557+1423	16.65 $\pm$ 0.09	16.83 $\pm$ 0.12	2.6	3.3	-19.55 $\pm$ 0.10	0.90 $\pm$ 0.14	0.87 $\pm$ 0.15
1612+1308	18.05 $\pm$ 0.05	18.11 $\pm$ 0.08	0.5	1.4	-16.27 $\pm$ 0.08	0.35 $\pm$ 0.12	0.37 $\pm$ 0.15
1646+2725	18.16 $\pm$ 0.03	18.54 $\pm$ 0.05	2.8	4.5	-18.61 $\pm$ 0.05	0.33 $\pm$ 0.20	0.27 $\pm$ 0.21
1647+2950	15.43 $\pm$ 0.03	15.56 $\pm$ 0.05	4.7	5.7	-20.91 $\pm$ 0.05	0.67 $\pm$ 0.11	0.66 $\pm$ 0.12
1647+2729	16.03 $\pm$ 0.06	16.06 $\pm$ 0.09	4.1	3.9	-20.91 $\pm$ 0.07	0.73 $\pm$ 0.10	0.68 $\pm$ 0.12
1647+2727	17.12 $\pm$ 0.04	16.15 $\pm$ 0.06	4.3	2.0	-19.83 $\pm$ 0.06	0.83 $\pm$ 0.09	0.74 $\pm$ 0.10
1648+2855	15.40 $\pm$ 0.02	15.58 $\pm$ 0.04	3.2	3.8	-21.13 $\pm$ 0.04	0.42 $\pm$ 0.07	0.48 $\pm$ 0.08
1653+2644	14.72 $\pm$ 0.03	15.01 $\pm$ 0.06	3.8	4.5	-22.37 $\pm$ 0.05	-	-
1654+2812	18.06 $\pm$ 0.11	18.60 $\pm$ 0.15	3.6	3.5	-18.84 $\pm$ 0.12	0.63 $\pm$ 0.08	0.63 $\pm$ 0.11

 

Table 3: continued

UCM name	$(m_{B})_{\rm T}$	(mB)24	$R_{\rm e}$(kpc)	$r_{1/2}(\hbox{$^{\prime\prime}$ })$	MB	$(B-r)_{\rm ef}$	(B-r)24
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
1655+2755	15.59 $\pm$ 0.09	15.88 $\pm$ 0.13	9.9	10.0	-21.30 $\pm$ 0.10	1.28$\pm$ 0.15	1.20 $\pm$ 0.15
1656+2744	16.84 $\pm$ 0.03	17.37 $\pm$ 0.23	1.7	3.0	-19.89 $\pm$ 0.04	0.74 $\pm$ 0.13	0.82 $\pm$ 0.26
1657+2901	17.12 $\pm$ 0.01	17.23 $\pm$ 0.04	2.2	2.3	-19.54 $\pm$ 0.04	0.73 $\pm$ 0.10	0.67 $\pm$ 0.11
1659+2928	15.73 $\pm$ 0.09	16.02 $\pm$ 0.12	4.9	4.4	-21.24 $\pm$ 0.10	0.76 $\pm$ 0.14	0.76 $\pm$ 0.14
1701+3131	15.27 $\pm$ 0.08	15.40 $\pm$ 0.11	4.2	4.2	-21.47 $\pm$ 0.08	0.99 $\pm$ 0.12	0.82 $\pm$ 0.13
2238+2308	14.86 $\pm$ 0.02	14.86 $\pm$ 0.05	5.4	5.6	-21.17 $\pm$ 0.05	0.81 $\pm$ 0.07	0.77 $\pm$ 0.08
2239+1959	14.82 $\pm$ 0.04	15.01 $\pm$ 0.05	3.0	4.4	-21.34 $\pm$ 0.05	0.78 $\pm$ 0.09	0.73 $\pm$ 0.10
2249+2149	15.96 $\pm$ 0.06	16.26 $\pm$ 0.06	7.9	5.9	-21.51 $\pm$ 0.07	1.27 $\pm$ 0.34	1.20 $\pm$ 0.35
2250+2427	15.39 $\pm$ 0.03	15.48 $\pm$ 0.06	3.0	2.6	-21.88 $\pm$ 0.04	0.32 $\pm$ 0.08	0.55 $\pm$ 0.10
2251+2352	16.36 $\pm$ 0.02	16.45 $\pm$ 0.05	1.8	2.4	-19.81 $\pm$ 0.04	0.50 $\pm$ 0.10	0.59 $\pm$ 0.11
2253+2219	16.12 $\pm$ 0.02	16.18 $\pm$ 0.08	1.9	3.7	-19.88 $\pm$ 0.05	0.61 $\pm$ 0.05	0.63 $\pm$ 0.09
2255+1930S	16.08 $\pm$ 0.02	16.16 $\pm$ 0.07	1.2	2.1	-19.54 $\pm$ 0.05	0.21 $\pm$ 0.21	0.56 $\pm$ 0.22
2255+1930N	15.76 $\pm$ 0.02	15.95 $\pm$ 0.05	2.2	3.8	-19.80 $\pm$ 0.05	1.02 $\pm$ 0.20	1.10 $\pm$ 0.21
2255+1926	16.74 $\pm$ 0.03	17.18 $\pm$ 0.06	3.2	5.5	-18.77 $\pm$ 0.06	0.55 $\pm$ 0.10	0.54 $\pm$ 0.11
2255+1654	16.62 $\pm$ 0.03	16.84 $\pm$ 0.06	6.8	10.2	-20.50 $\pm$ 0.04	1.20 $\pm$ 0.05	1.08 $\pm$ 0.08
2256+2001	15.62 $\pm$ 0.04	16.03 $\pm$ 0.04	8.2	12.2	-20.35 $\pm$ 0.06	1.11 $\pm$ 0.07	1.06 $\pm$ 0.08
2257+2438	16.04 $\pm$ 0.05	16.15 $\pm$ 0.10	1.3	1.4	-20.71 $\pm$ 0.06	-0.30 $\pm$ 0.10	0.14 $\pm$ 0.12
2257+1606	16.40 $\pm$ 0.07	16.57 $\pm$ 0.15	2.0	2.1	-20.38 $\pm$ 0.08	-	-
2258+1920	15.80 $\pm$ 0.05	15.99 $\pm$ 0.09	2.8	4.6	-19.95 $\pm$ 0.06	0.33 $\pm$ 0.10	0.41 $\pm$ 0.11
2300+2015	16.53 $\pm$ 0.04	16.87 $\pm$ 0.06	4.4	3.9	-20.27 $\pm$ 0.05	0.70 $\pm$ 0.11	0.80 $\pm$ 0.12
2302+2053W	17.97 $\pm$ 0.02	18.20 $\pm$ 0.08	1.6	1.7	-18.79 $\pm$ 0.04	0.53 $\pm$ 0.06	0.86 $\pm$ 0.10
2302+2053E	15.49 $\pm$ 0.02	15.85 $\pm$ 0.06	5.6	6.8	-21.28 $\pm$ 0.04	1.49 $\pm$ 0.05	1.37 $\pm$ 0.07
2303+1856	15.62 $\pm$ 0.03	15.86 $\pm$ 0.17	3.5	5.1	-20.64 $\pm$ 0.05	0.90 $\pm$ 0.11	0.85 $\pm$ 0.20
2303+1702	17.46 $\pm$ 0.05	17.76 $\pm$ 0.11	4.3	4.3	-19.86 $\pm$ 0.06	1.31 $\pm$ 0.12	1.27 $\pm$ 0.14
2304+1640	17.56 $\pm$ 0.02	17.89 $\pm$ 0.17	0.9	2.1	-17.81 $\pm$ 0.05	-0.18 $\pm$ 0.10	0.27 $\pm$ 0.19
2304+1621	16.69 $\pm$ 0.08	17.28 $\pm$ 0.14	2.9	4.0	-20.34 $\pm$ 0.08	1.22 $\pm$ 0.12$^\dagger$	-
2307+1947	16.62 $\pm$ 0.05	16.85 $\pm$ 0.06	2.9	3.7	-19.62 $\pm$ 0.06	1.01 $\pm$ 0.21	0.91 $\pm$ 0.21
2310+1800	16.76 $\pm$ 0.03	16.97 $\pm$ 0.05	3.7	3.6	-20.18 $\pm$ 0.05	0.78 $\pm$ 0.33	0.94 $\pm$ 0.33
2312+2204	17.13 $\pm$ 0.08	17.39 $\pm$ 0.10	2.1	2.6	-19.64 $\pm$ 0.08	-	-
2313+1841	16.59 $\pm$ 0.06	17.27 $\pm$ 0.12	3.1	8.8	-19.87 $\pm$ 0.07	0.87 $\pm$ 0.06	0.79 $\pm$ 0.13
2313+2517	14.91 $\pm$ 0.03	15.23 $\pm$ 0.04	5.7	6.4	-21.45 $\pm$ 0.05	-	-
2315+1923	17.22 $\pm$ 0.07	17.61 $\pm$ 0.16	2.2	2.6	-19.73 $\pm$ 0.08	0.39 $\pm$ 0.09	0.48 $\pm$ 0.18
2316+2457	14.35 $\pm$ 0.03	14.51 $\pm$ 0.05	4.7	7.0	-22.03 $\pm$ 0.05	0.86 $\pm$ 0.09	0.77 $\pm$ 0.09
2316+2459	15.82 $\pm$ 0.04	16.24 $\pm$ 0.11	6.4	10.6	-20.53 $\pm$ 0.05	0.85 $\pm$ 0.08	0.83 $\pm$ 0.13
2316+2028	16.84 $\pm$ 0.04	17.08 $\pm$ 0.17	1.3	1.9	-19.33 $\pm$ 0.06	-0.38 $\pm$ 0.09	0.12 $\pm$ 0.20
2317+2356	13.86 $\pm$ 0.04	13.99 $\pm$ 0.11	8.8	9.8	-22.89 $\pm$ 0.05	0.75 $\pm$ 0.05	0.67 $\pm$ 0.12
2319+2234	16.50 $\pm$ 0.05	16.86 $\pm$ 0.13	3.2	3.2	-20.36 $\pm$ 0.06	-0.17 $\pm$ 0.08	0.12 $\pm$ 0.15
2319+2243	15.69 $\pm$ 0.05	16.05 $\pm$ 0.12	4.4	5.4	-20.83 $\pm$ 0.06	1.07 $\pm$ 0.07	1.02 $\pm$ 0.14
2320+2428	15.13 $\pm$ 0.06	15.80 $\pm$ 0.16	6.6	10.4	-21.51 $\pm$ 0.07	1.26 $\pm$ 0.07	1.21 $\pm$ 0.17
2321+2149	16.55 $\pm$ 0.05	16.74 $\pm$ 0.09	4.2	5.0	-20.36 $\pm$ 0.06	0.66 $\pm$ 0.10	0.66 $\pm$ 0.11
2321+2506	15.75 $\pm$ 0.05	15.86 $\pm$ 0.09	5.3	5.3	-20.86 $\pm$ 0.06	0.54 $\pm$ 0.10	0.51 $\pm$ 0.11
2322+2218	17.69 $\pm$ 0.02	17.89 $\pm$ 0.03	1.9	2.4	-18.32 $\pm$ 0.05	0.77 $\pm$ 0.33	0.95 $\pm$ 0.33
2324+2448	13.32 $\pm$ 0.07	13.62 $\pm$ 0.08	7.1	21.4	-21.20 $\pm$ 0.10	0.91 $\pm$ 0.10	0.81 $\pm$ 0.11
2325+2318	13.21 $\pm$ 0.01	13.37 $\pm$ 0.03	3.1	9.9	-21.25 $\pm$ 0.06	-	-
2325+2208	12.91 $\pm$ 0.04	13.00 $\pm$ 0.08	9.9	28.8	-21.67 $\pm$ 0.07	1.05 $\pm$ 0.11	0.98 $\pm$ 0.10
2326+2435	16.09 $\pm$ 0.04	16.54 $\pm$ 0.14	2.7	9.3	-19.17 $\pm$ 0.07	0.48 $\pm$ 0.08	0.44 $\pm$ 0.16
2327+2515N	15.83 $\pm$ 0.05	15.47 $\pm$ 0.06	2.9	2.3	-19.79 $\pm$ 0.07	0.34 $\pm$ 0.07	0.10 $\pm$ 0.09
2327+2515S	15.77 $\pm$ 0.05	15.64 $\pm$ 0.06	2.7	3.3	-19.85 $\pm$ 0.07	0.60 $\pm$ 0.07	0.46 $\pm$ 0.09
2329+2427	16.03 $\pm$ 0.08	16.39 $\pm$ 0.09	3.5	5.9	-19.52 $\pm$ 0.09	1.50 $\pm$ 0.10	1.45 $\pm$ 0.11
2329+2500	16.28 $\pm$ 0.04	16.47 $\pm$ 0.09	1.9	2.7	-20.16 $\pm$ 0.06	0.89 $\pm$ 0.12	0.99 $\pm$ 0.14
2329+2512	17.00 $\pm$ 0.07	17.43 $\pm$ 0.08	1.0	2.9	-17.63 $\pm$ 0.09	1.16 $\pm$ 0.32	1.15 $\pm$ 0.33
2331+2214	17.63 $\pm$ 0.07	17.99 $\pm$ 0.10	2.9	3.4	-19.11 $\pm$ 0.08	1.36 $\pm$ 0.08	1.34 $\pm$ 0.11
2333+2248	17.45 $\pm$ 0.06	17.79 $\pm$ 0.13	4.6	3.9	-19.60 $\pm$ 0.07	1.19 $\pm$ 0.16	1.09 $\pm$ 0.15
2333+2359	17.70 $\pm$ 0.06	18.01 $\pm$ 0.10	3.0	2.8	-19.08 $\pm$ 0.07	1.98 $\pm$ 0.13	1.91 $\pm$ 0.14
2348+2407	17.93 $\pm$ 0.08	18.25 $\pm$ 0.10	2.0	2.1	-18.88 $\pm$ 0.09	1.63 $\pm$ 0.10	1.64 $\pm$ 0.13
2351+2321	18.56 $\pm$ 0.08	18.80 $\pm$ 0.10	1.1	1.5	-17.69 $\pm$ 0.09	1.81 $\pm$ 0.17	2.06 $\pm$ 0.18

$^\dagger$ Total colour calculated from integrated magnitudes. No radial data are available due to low SNR in the images.

Table 3: (1) UCM name. (2) Total Johnson B magnitude calculated with several polygons. We have also measured the asymptotic magnitude at two Kron radius yielding an average difference with the polygon measure of 0.02 magnitudes. (3) Johnson B magnitude measured inside the 24 mag arcsec^-2 isophote. (4) Effective radius in kpc measured in circular apertures and converted to distance using a Hubble constant H₀=50 km s^-1 Mpc^-1 and a deceleration parameter q₀=0.5. (5) Equivalent half-light radius calculated with isophotal apertures. (6) Absolute magnitude corrected from Galactic extinction according to the maps of Galactic reddening of Burstein & Heiles ([1982]). (7) B-r colour measured inside the effective isophote. (8) B-r colour measured inside the 24 mag arcsec^-2 isophote.