3. Notes on individual objects

4C 12.05 (Gower et al. 1967) = PKS 0035+121 (Shimmins et al. 1975) has been tentatively identified by Wills & Wills (1976) and Jauncey et al. (1978) with a 16.5-17.0 mag object, the position of which is in good agreement with the accurate radio position measured by Condon et al. (1977); but they have shown that the optical spectrum, although inconclusive, was probably that of a star. However, Wills & Wills have remarked that there appears to be a small, fainter, south-preceeding blue object, visible on the Palomar Sky Survey prints, blended with the image of the star. A V image, obtained on August 10, 1996 with EFOSC at the 3.6 m ESO telescope in La Silla shows that, indeed, the object is double, with a separation of 2.8 arcsec. The spectrograph slit was aligned on the two objects (); a 10 min exposure spectrum shows the north-following object to be a star, while the south-preceeding object is a QSO at z=1.395 (Fig. 1 (click here)). The magnitude of the QSO, as measured on the spectrum is about 0.55 mag weaker than the star in B, and 0.87 mag in V. The emission line fluxes are 570 and 360 for and , respectively.

  
Figure 1: Low dispersion spectra (resolution ) of four objects observed with the 3.6 m ESO telescope. The fluxes are in units of

 

Name z FWHM FHWM Spectral type

Mark 1147 0.0364 14 (780) 2.18 2.3 11 (635) 0.24 11.4 HII

Mark 971 0.0823 15 280 0.41 5.6 - - - - HII

Mark 998 0.0761 - - - - 22 (580) 0.23 10.3 HII

Q 0155+0220 0.0651 -1 325 0.71 8.4 - - - - HII

Mark 596 0.0388 -16 (960) >5.0 <0.6 45 (720) 1.14 2.2 S2

KUV 03079-0101 0.0807 -15 (860) >10.0 <0.4 - - - - S1.0

-29 3360 - 3.1 -28 2570 - 12.2

CBS 74 0.0920 143 (945) 15.6 1.9 -10 260 0.89 27.8 S1.2

1485 14500 - 2.3 1092 12200 - 10.4

HS 0843+2533 0.0507 - - - - 90 475 1.6 2.5 S1

- - - - -70 4850 - 7.3

Mark 391 0.0133 9 210 1.21 9.9 45 225 0.55 36.7 HII

KUG 0929+324 0.0158 - - - - -6 150 0.10 17.6 HII

CG 49 0.0438 - - - - 15 300 0.79 17.4 S2

UM 446 0.0061 - - - - 9 160 0.04 79.8 HII

US 2896 0.0594 - - - - -3 185 0.43 S1

- - - - -120 2100 - 12.3

Mark 646 0.0536 - - - - 0 280 0.46 62.8 S1

- - - - -16 2350 - 8.0

2E 1219+0447 0.0947 - - - - 3 225 0.54 5.5 S1

- - - - 222 8440 - 1.6

KUV 13000+2908 0.0223 - - - - 3 185 <0.1 7.0 HII

Q 1356-067 0.0746 - - - - 6 280 0.16 HII

Mark 469 0.0689 -9 295 1.38 19.4 18 260 0.18 HII

Mark 816 0.0887 -19 240 0.63 10.5 - - - - HII

Mark 833 0.0395 - - - - -8 225 0.30 25.7 HII

Mark 483 0.0481 - - - - -5 225 0.12 48.3 HII

KUV 15519+2144 0.0392 - - - - -9 185 0.11 HII

Q 1619+3752 0.0331 -3 240 2.56 20.4 - - - - HII

EXO 1622.0+2611 0.0394 - - - - 15 225 0.40 93.0 S1

- - - - 12 1770 - 33.0

Q 1624+4628 0.0301 - - - - 6 195 0.40 HII

Q 1638+4634 0.0581 10 (720) 0.86 1.8 36 (625) 0.40 10.3 HII

Kaz 110 0.0527 -5 225 2.83 22.9 9 170 0.09 23.1 HII

RN 73 0.0491 18 310 7.4 5.4 -16 185 0.37 16.3 S1.9

- - - - -34 1590 - 3.1

Q 2233+0123 0.0566 - - - - 15 290 0.60 8.5 S1

- - - - 1080 5500 - 21.3

Q 2257+0221 0.0466 3 495 16.7 1.9 - - - - S2

NGC 7678 0.0116 12 270 0.25 9.5 45 250 0.52 HII

E 2344+184 0.1365 24 425 > 6.0 < 0.5 - - - - S2

UM 11 0.0390 -8 310 0.46 3.8 21 290 0.56 80.2 HII

Table 4: Fitting profile analysis results (see text). Column 2 gives the redshift used to deredshift the spectra, while Cols. 3 and 7 give the velocity of the lines as measured on the dereshifted spectra. Columns 6 and 10 give the peak intensity of the and lines respectively (in units of ). The FWHM are observed values, not corrected for the instrumental profile; values in parenthesis are from low dispersion spectra and are unresolved

 

Mark 1147 is an emission line galaxy (Markarian et al. 1980); it has been erroneously classified as a Seyfert 1 by Véron-Cetty & Véron (1985). Our low dispersion spectrum (Fig. 2 (click here)) shows that it is a HII region, with and ; this is in agreement with Markarian et al. (1980), who have noticed that is weak compared to .

  
Figure 2: Low dispersion spectra (resolution ), in the rest frame, of three objects observed with the 1.93 m OHP telescope. The fluxes are in units of

Mark 971 = KUG 0101+353 (Takase & Miyauchi-Isobe 1991b). Markarian et al. (1984) suggested that it could have an active nucleus; this, however, was not confirmed neither by Denisyuk & Lipovetski (1984) nor by Lipovetski et al. (1989). Our spectrum (Fig. 6 (click here)) shows narrow emission lines ( FWHM) with together with an line in absorption; this object is, therefore, a HII region.

Mark 998. According to Markarian et al. (1984), this galaxy could have an active nucleus; Denisyuk & Lipovetski (1984) and Lipovetski et al. (1989) were not able to confirm this. Our low dispersion spectrum (Fig. 2 (click here)) shows . It follows that this object is most probably a HII region.

Q 0155+0220 is an emission line galaxy according to Schneider et al. (1994). Our spectrum (Fig. 6 (click here)) shows it to be a HII region with narrow () and emission lines, and .

Mark 596. This object, having may have an active nucleus (Markarian et al. 1984). It is indeed a Seyfert 2 galaxy as our spectrum (Fig. 2 (click here)) shows that and .

(Noguchi et al. 1980) is an emission line galaxy according to Chaffee et al. (1991). Our spectrum (Fig. 3 (click here)) shows broad Balmer lines () and narrow lines. The ratio of the total flux to the flux is R=10; this object is therefore a Seyfert 1.0 galaxy (Winkler 1992).

  
Figure 3: Same as in Fig. 2 (click here) for three additional objects

CBS 74 is a Seyfert galaxy according to Wagner et al. (1988). It was not detected at 4850 MHz by Gregory & Condon (1991) () and is therefore a radioquiet object. Our spectra (Figs. 3 (click here), 9 (click here)) show that it is a Seyfert 1.2 galaxy with a very broad component () and R=3.6. Such broad lines are common in radioloud quasars and broad line radiogalaxies (Miley & Miller 1979; Wills & Browne 1986; Brotherton et al. 1994; Eracleous & Halpern 1994), but they are rare in Seyfert galaxies although a few cases are known, such as 2E 0450-1816 (Eracleous & Halpern 1994) and Arp 102B (Chen & Halpern 1989). Indeed, powerful radiogalaxies and radioloud quasars with extended radio morphologies tend to have the broadest Balmer lines, while AGNs with compact radiostructure and radioquiet objects have narrower Balmer lines (Miley & Miller 1979; Steiner 1981; Wills & Browne 1986).

HS 0843+2533. The ROSAT X-ray source RX J08469+2522 was identified by Bade et al. (1995) with a 16.8 mag AGN called HS 0843+2533, which exhibits a broad emission line (). Our spectrum (Fig. 9 (click here)) shows, indeed, a strong, broad emission line (); this object is therefore a Seyfert 1 galaxy.

Mark 391 = NGC 2691 is a S0a galaxy (Huchra 1977). For Arakelian et al. (1972), it weakly shows the characteristics of the Seyfert nuclei, with a broad emission line (). On this basis, Véron-Cetty & Véron (1985) classified it as a Seyfert 1. Shuder & Osterbrock (1981), however, concluded from their own spectroscopic observations that it is not a Seyfert. Our spectra (Fig. 4 (click here)) show Balmer lines in absorption together with narrow () emission lines with and , proving that it is a HII region.

  
Figure 4: Blue and red high dispersion spectra (resolution ), in the rest frame, of three objects observed with the 1.93 m OHP telescope. The fluxes are in units of

  
Figure 5: Same as in Fig. 4 (click here) for three additional objects

KUG 0929+324 is a moderate excitation () emission line galaxy with an heliocentric radial velocity according to Augarde et al. (1994). Our spectrum (Fig. 7 (click here)) shows that it is a HII region with narrow emission lines () and . We found the radial velocity to be (Augarde 1995, private communication, gave ).

  
Figure 6: Blue high dispersion spectra (resolution ), in the rest frame, for six objects observed with the 1.93 m telescope. The fluxes are in units of

  
Figure 7: Red high dispersion spectra (resolution ), in the rest frame, for six objects observed with the 1.93 m telescope. The fluxes are in units of

CG 49. Salzer et al. (1995) published line intensity ratios for this object as follows: and . The line is too strong for a HII region and too weak for a Seyfert 2 galaxy. Our spectrum shows with the same low intensity, however it so happens that the redshifted wavelength of the line (6874 Å) falls precisely at the position of the atmospheric B band. When corrected for atmospheric absorption by dividing the observed spectrum by the spectrum of a standard star (Fig. 7 (click here)), we obtain , a normal value for a Seyfert 2 galaxy. The measured FWHM of the emission lines is , in agreement with the adopted classification.

UM 446 is a moderate excitation () emission line galaxy (Salzer et al. 1989). Our spectrum (Fig. 7 (click here)) shows narrow emission lines () with ; this object is therefore a HII region.

US 2896 (Huang & Usher 1984) = CS 109 (Sanduleak & Pesch 1984) is an emission line galaxy (Mitchell et al. 1984), and a Seyfert 1.5 galaxy according to Everett & Wagner (1995). This is confirmed by our spectrum (Fig. 7 (click here)) which shows a broad component (). A emission line is observed with .

Mark 646, PG 1203+35 (Green et al. 1986), CG 885 (Pesch & Sanduleak 1988) or KUG 1203+354 (Takase & Miyauchi-Isobe 1991a) is a Seyfert galaxy according to Green et al. (1986). Our spectrum (Fig. 7 (click here)) shows a broad component (); Mark 646 is therefore a Seyfert 1 galaxy. A emission line is observed with .

2E 1219+0447 is an emission line galaxy (Bothun et al. 1984; Margon et al. 1985). We classify it as a Seyfert 1 galaxy on the basis of a weak, broad () component (Fig. 9 (click here)).

KUV 13000+2908 (Noguchi et al. 1980), CG 963 (Sanduleak & Pesch 1990) or PB 3241 (Berger et al. 1991) is a Seyfert 2 galaxy according to Wegner & McMahan (1988). Our spectrum (Fig. 7 (click here)) shows narrow () emission lines with , so this object is a HII region.

is a QSO according to Goldschmidt et al. (1992). Our spectrum (Fig. 8 (click here)), however, shows narrow () emission lines with ; this object is therefore a HII region. A emission line is observed with .

  
Figure 8: Same as in Fig. 7 (click here) for six additional objects

Mark 469, CG 899 (Pesch & Sanduleak 1989) or KUG 1416+345 (Takase & Miyauchi-Isobe 1984) is a 16.1 mag, UV excess galaxy (Peterson et al. 1981). Our observations (Fig. 4 (click here)) show that it is a HII region, with and , the lines being narrow ().

. This radiosource was identified by Bolton & Ekers (1966) with an 18 mag QSO. The identification was later confirmed by accurate optical and radio position measurements (Hunstead 1971, 1972). Our spectrum (Fig. 1 (click here)) shows that it is indeed a QSO at z=0.985. The emission line fluxes are 83 and for and respectively.

Mark 816 = KUG 1431+529 (Takase & Miyauchi-Isobe 1985) is a 16.5 mag, possibly Seyfert, galaxy (Afanasev et al. 1979); however, (Afanasev et al. 1980). Our spectrum (Fig. 6 (click here)) shows narrow emission lines () with . This object is most probably a HII region.

is a flat spectrum radiosource identified by Condon et al. (1977) with a 19.0 mag starlike object. It has a featureless spectrum between 3800 and 7000 Å (Fig. 1 (click here)) and is most probably a BL Lac object.

Mark 833 = CG 590 (Sanduleak & Pesch 1987) is an emission line galaxy (Markarian et al. 1985) which has been called a "narrow-line active galactic nucleus" by Veilleux & Osterbrock (1987), based on emission-line intensity ratios published by Shuder & Osterbrock (1981); it however happened that the object studied in this last paper is Mark 883 which is, in a few occasions mistakenly called Mark 833 (H. Falcke, private communication). The nature of the emission-line nebulosity in Mark 833 was therefore unknown. Our spectrum (Fig. 8 (click here)) shows narrow () emission lines with . This object is, therefore, a HII region.

Mark 483 = CG 741 (Sanduleak & Pesch 1987) is an emission line galaxy (Markarian et al. 1988; Izotov et al. 1993) with a strong UV excess (U-B =-0.45, Peterson et al. 1981). The emission-line ratios published by Markarian et al. () and Izotov et al. () suggested that it is a HII region. This is confirmed by our spectrum (Fig. 8 (click here)) which shows narrow emission lines () with .

KUV 15519+2144 is a Seyfert 2 galaxy according to Wagner & Swanson (1990). Our spectrum (Fig. 8 (click here)) shows it to be a HII region, with narrow () emission lines and . A emission line is observed with

Q 1619+3752, an emission line galaxy according to Schneider et al. (1994), is classified as a HII region, as it shows narrow emission lines () and (Fig. 6 (click here)).

EXO 1622.0+2611. An AGN for Giommi et al. (1991), this is a Seyfert 1 galaxy, as it presents a broad H component () (Fig. 8 (click here)).

Q 1624+4628. An emission line galaxy according to Schneider et al. (1994), it is a HII region, with narrow () emission lines and (Fig. 8 (click here)).

Q 1638+4634. An emission line galaxy according to Schneider et al. (1994), it is a HII region, with and (Fig. 3 (click here)).

Kaz 110. The emission-line gas in this object was shown to be ionized by hot stars (Kazarian & Tamazian 1993). Our spectra (Fig. 4 (click here)) confirm this result, the measured line ratios being: and .

. This flat spectrum radiosource (Quiniento & Cersosimo 1993) was identified with a 19.0 mag QSO by Anguita et al. (1979). The identification was confirmed by an accurate radioposition measurement (Russel et al. 1992). It is indeed a QSO at z=1.756 (Fig. 1 (click here)). The emission line fluxes are 57 and for and respectively.

RN 73 (Ryle & Neville 1962) = 8C 2037+880 (Rees 1990) was identified with a 17.5 mag emission line galaxy (Penston 1971). Our spectra (Fig. 5 (click here)) show a weak, broad () component, but no broad component: this object is a Seyfert 1.9 galaxy. However, the ratio is low for a Seyfert galaxy. Halliday (1977) published an accurate radiomap for this source; its position, as measured on this map (, ), is about 20 arcsec away from the position of the galaxy, suggesting that the radiostructure and the galaxy are not to be related.

Q 2233+0123. An emission line galaxy according to Schneider et al. (1994), it is a Seyfert 1, having a strong and broad () component (Fig. 9 (click here)). The profile of this line deviates significantly from a Gaussian, having a flat top.

  
Figure 9: Same as in Fig. 7 (click here) for four additional objects

Q 2257+0221 is an emission line galaxy according to Schneider et al. (1994). It is a Seyfert 2 having broad (), asymmetrical lines, that are much stronger than H () (Fig. 6 (click here)).

NGC 7678 = Kaz 336 (Kazarian & Kazarian 1980). Although classified as a Seyfert 2 galaxy by Kazarian (1993), this is a HII region with , and linewidth FWHM (Fig. 5 (click here)).

E 2344+184 is a spiral galaxy (Hutchings & Neff 1992). According to Margon et al. (1985), it is an emission line galaxy with a strong emission line. Our low signal-to-noise blue spectrum (Fig. 6 (click here)) shows a strong line (), so it is most probably a Seyfert 2 galaxy.

UM 11. Terlevich et al. (1991) gave line ratios: and , suggesting that this object is a Liner; our spectra (Fig. 5 (click here)) give and (with linewidth ) showing that it is a HII region instead.