A 10 min I image (FWHM = 18) and a 30 m B image (FWHM = 19) were obtained with EFOSC at the 3.6m telescope on August 10 and 11, 1996 and three 15 min I images (FWHM = 13) with the NTT on May 2, 1992. These images show the object to be associated with a large luminous galaxy in a crowded field with many galaxies and stars (fig. ). One of these is seemingly situated within the galaxy.
To establish its nature we have obtained on Aug 11, 1996 two 5 min
spectra through the EFOSC B300 and R300 grims which yielded a useful spectral
range of 3740-9280 Åwith a FWHM of 15 Åfor the night sky lines.
The 15 slit was oriented in PA = 19, so as to obtain the
spectrum of the nucleus, object 1 at 48 NE and object 2 at 69 NE
(fig. ).
The nucleus shows a continuum typical for a gE galaxy with probably
Mg I b and Na I D in
absorption and with a set of emission lines typical for a Seyfert 2 galaxy with
[N II]6583/ H=2.1, [O I]6300/H=
0.4 and [OIII]5007/H=5.5, measured on the spectrum after
subtraction of a template gE galaxy spectrum (fig. ). For H/H
we measured an uncertain value of 5.5 and for [OII]3727/H3. The FWHM of the lines near H is 23 Å or, upon correction for
instrumental broadening of 15Å, about 700 km s-1 in the rest frame. We
obtained z = 0.2230 0.0001, very close to z = 0.2227 found by White et
al. (1988).
Object 1 also has a continuum compatible with a gE, with H, Mg I b and Na I D in absorption and H weakly in emission. The rather noisy spectrum yielded a redshift z = 0.2252 0.0004. This corresponds to a relative velocity of 540100 km s-1 in the rest frame. It may well be, therefore, that object 1 is a galaxy being captured by PKS 1353-341, though it could also be an independent galaxy in the surrounding cluster. As we shall discuss later the velocity derived for PKS 1353-341 from emission lines may not necessarily represent the systemic velocity and the velocity difference might well be smaller.
Object 2 turns out to have a blue continuum with Mg I b in absorption and
emission lines corresponding to a low excitation H II region (6583/H=0.6; 6300/H< 0.04 and 5007/H= 0.6); the
emission lines are unresolved at our resolution. The redshift z
= 0.21570.0001 which corresponds to a velocity of
1800 km s-1, in the rest frame of PKS 1353-341, probably indicating the
presence of a substantial cluster of gala- xies.
Elliptical isophotes with b/a=0.7 and major axis in PA=40 were fitted to the I and B images of PKS 1353-341, excluding the part influenced by object 1. To obtain the surface brightness in V we have corrected for the (1 + z)4 factor, the k-term and for galactic absorption (table ) and we have assumed q0=0 and V0-I0=1.15 and B0-V0= 0.95, the standard values for gE. The resulting surface brightness distribution is shown in fig. , where also some of Schombert's (1987) standard curves for gE are indicated. PKS 1353-341 appears to have a slightly flatter profile than a typical gE for r less than 40 kpc (r1/4=2.5). Further from the center the distribution flattens, indicative of a cD galaxy. Between 3 and 10 from the center where the photometry is most reliable we obtain B-I=3.01 about the value expected for a standard gE at this redshift.
Upon subtracting an r1/4 model and a PSF centered on the nucleus from the observed NTT image one clearly sees the extended nature of the object 1 which may be traced to approximately 5 (30 kpc) from its center. The integrated magnitude of object 1 within a 22 kpc radius is I18.6with B-I roughly 3.0 corresponding, with the normal colour of a gE, to M21.4, probably a minimum estimate for its total luminosity. Such a galaxy certainly could perturb an object like PKS 1353-341. The more distant object 2 has B=20.40 and I=18.42 corresponding to a late type galaxy.
Beyond 10 from the center the light distribution flattens and a cD envelope begins to dominate. The integrated magnitudes of the whole system to 120 (780 kpc) from the center are I=13.62, and B=16.57 from the 10 min and B=16.49 from the 30 min exposures. As a result of the great extent of the envelope it is possible that our sky level is still contaminated by light from the galaxy. A larger CCD would be needed to determine the integrated magnitudes and their uncertainty with confidence. Our measured magnitudes give M=-27.5 and M=-25.6 which would correspond to M=-26.4 or to log(L/L)= 12.5. Hence PKS 1353-341 is a very luminous galaxy indeed. In the list of 26 cD galaxies by Schombert (1988) there are only two that are still more luminous.