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2. Observations

Most of the observations were carried out in 1995, 1996 and 1997 with the spectrograph CARELEC (Lemaıtre et al. 1989) attached to the Cassegrain focus of the Observatoire de Haute Provence (OHP) 1.93 m telescope. The spectrograph settings used during these runs are given in Table 1 (click here). The detector was a tex2html_wrap_inline1980 pixels, tex2html_wrap_inline1982 Tektronic CCD. The slit width was 2.1 arcsec, corresponding to a projected slit width on the detector of tex2html_wrap_inline1984, or 1.9 pixel. The resolution, as measured on the night sky emission lines, was 13.5 and 3.4 Å FWHM at low and high resolution, respectively. The spectra were flux calibrated using the standard stars given in Table 1 (click here), taken from Oke (1974), Stone (1977), Oke & Gunn (1983) or Massey et al. (1988).

Additional observations were made with EFOSC (Dekker et al. 1988) at the 3.6 m ESO telescope in La Silla during two runs in July 1995 and August 1996. The detector was the CCD ESO#26, similar to the one used at OHP. The dispersion was tex2html_wrap_inline1988; the slit width was 1.5 arcsec, corresponding to 2.2 pixels and resulting in a resolution of 15 Å. The wavelength range was tex2html_wrap_inline1990. The spectra were flux calibrated using the standard stars W 485A and GD 190 (Oke 1974).

 

Date Dispersion tex2html_wrap_inline1992 Range Standard
(tex2html_wrap_inline1994) () stars
21 - 23.03.95 66 6500 - 7400 BD 26tex2html_wrap_inline19982606
24 - 28.08.95 260 4500 - 8000 BD 25tex2html_wrap_inline19983941
BD 28tex2html_wrap_inline19984211
28 - 31.08.95 66 6700 - 7600 BD 25tex2html_wrap_inline19983941
BD 28tex2html_wrap_inline19984211
31.08 - 04.09.95 66 4860 - 5760 Feige 15
BD 28tex2html_wrap_inline19984211
10.05.96 66 6700 - 7600 GD 140
BD 26tex2html_wrap_inline19982606
13.05.96 66 4860 - 5760 Feige 98
Kopff 27
08.06.96 66 4860 - 5760 Feige 66
Kopff 27
09.06.96 66 6700 - 7600 Feige 66
BD 28tex2html_wrap_inline19984211
06 - 08.01.97 66 4720 - 5620 EG 247
08 - 11.01.97 66 6175 - 7075 EG 247
Table 1: Spectrograph settings and standard stars during OHP observations

 

 

Name Disp. Date Exp. time Name Disp. Date Exp. time
(min) (min)
4C 12.05 D 10.08.96 tex2html_wrap_inline2024 PKS 1420-27 D 25.07.95 tex2html_wrap_inline2024
Mark 1147 A 26.08.95 tex2html_wrap_inline2030 Mark 816 B 13.05.96 tex2html_wrap_inline2030
Mark 971 B 01.09.95 tex2html_wrap_inline2030 PKS 1437-153 D 27.07.95 tex2html_wrap_inline2024
Mark 998 A 26.08.95 tex2html_wrap_inline2030 Mark 833 C 22.03.95 tex2html_wrap_inline2030
Q 0155+0220 B 31.08.95 tex2html_wrap_inline2030 Mark 483 C 22.03.95 tex2html_wrap_inline2030
Mark 596 A 25.08.95 tex2html_wrap_inline2030 KUV 15519+2144 C 22.03.95 tex2html_wrap_inline2030
KUV 03079-0101 A 27.08.95 tex2html_wrap_inline2030 Q 1619+3752 B 01.09.95 tex2html_wrap_inline2030
CBS 74 A 30.04.95 tex2html_wrap_inline2064 EXO 1622.0+2611 C 22.03.95 tex2html_wrap_inline2030
C 22.03.95 tex2html_wrap_inline2030 Q 1624+4628 C 28.08.95 tex2html_wrap_inline2030
HS 0843+2533 C 10.01.97 tex2html_wrap_inline2030 Q 1638+4634 A 27.08.95 tex2html_wrap_inline2030
Mark 391 B 07.01.97 tex2html_wrap_inline2030 Kaz 110 B 23.06.96 tex2html_wrap_inline2030
C 10.01.97 tex2html_wrap_inline2030 C 22.06.96 tex2html_wrap_inline2030
KUG 0929+324 C 21.03.95 tex2html_wrap_inline2030 PKS 1903-80 D 28.07.95 tex2html_wrap_inline2024
CG 49 C 10.05.96 tex2html_wrap_inline2030 RN 73 B 31.08.95 tex2html_wrap_inline2030
UM 446 C 21.03.95 tex2html_wrap_inline2030 C 30.08.95 tex2html_wrap_inline2030
US 2896 C 22.03.95 tex2html_wrap_inline2030 Q 2233+0123 C 30.08.95 tex2html_wrap_inline2030
Mark 646 C 22.03.95 tex2html_wrap_inline2030 Q 2257+0221 B 02.09.95 tex2html_wrap_inline2030
2E 1219+0447 C 22.03.95 tex2html_wrap_inline2030 NGC 7678 B 02.09.95 20*
KUV 13000+2908 C 22.03.95 tex2html_wrap_inline2030 C 30.08.95 tex2html_wrap_inline2030
Q 1356-067 C 22.03.95 tex2html_wrap_inline2030 E 2344+184 B 01.09.95 tex2html_wrap_inline2030
Mark 469 B 08.06.96 tex2html_wrap_inline2030 UM 11 B 02.09.95 20*
C 09.06.96 tex2html_wrap_inline2030 C 29.08.95 tex2html_wrap_inline2030
Table 2: Journal of observations. A: OHP, tex2html_wrap_inline2014; B: OHP, tex2html_wrap_inline2016 blue; C: OHP, tex2html_wrap_inline2016 red; D: ESO, tex2html_wrap_inline1988. An " * '' after the exposure time indicates the presence of clouds during the exposure

 

The journal of observations is given in Table 2 (click here) and the list of the observed objects with relevant data, in Table 3 (click here). The spectra were analysed in terms of Gaussian components as described in Véron et al. (1997). Table 4 (click here) gives for each object the velocity, width and relative strength of each line, together with the adopted classification. Objects with broad Balmer lines were classified as Seyfert 1 galaxies, or QSOs whenever their absolute magnitude was brighter than MB = -23.0 (assuming tex2html_wrap_inline2150); Seyfert 2s and HII regions were distinguished on the basis of the value of the tex2html_wrap_inline2152 and tex2html_wrap_inline2154 line ratios (Veilleux & Osterbrock 1987). In some cases, the classification is based on a single line ratio, either tex2html_wrap_inline2156 or tex2html_wrap_inline2158. This is potentially dangerous; however we think that in most cases, there is no ambiguity, specially when tex2html_wrap_inline2160 (see Fig. 6a in Véron et al. 1997).

 

Name tex2html_wrap_inline2162 tex2html_wrap_inline2164 z mag old class. our class. Ref.
4C 12.05 00 35 41.98 12 11 03.6 - 17.5 ? Q (25)
Marktex2html_wrap_inline2172 00 45 57.94 10 03 56.9 0.036 15.7 S1 HII (18)
Marktex2html_wrap_inline2178 01 01 32.79 35 18 07.8 0.085 16.5 S? HII (16)
Marktex2html_wrap_inline2184 01 30 02.04 tex2html_wrap_inline2186 20 11.9 0.078 16.0 S? HII (17)
Q 0155+0220 01 55 47.90 02 20 26.3 0.066 16.7 ? HII (23)
Marktex2html_wrap_inline2196 02 40 12.67 07 23 09.5* 0.038 14.8 S? S2 (13)
KUV 03079-0101 03 07 54.83 tex2html_wrap_inline2204 01 10.3 0.080 16.3 ? S1.0 (7)
CBS 74 08 29 11.46 37 17 49.1 0.091 tex2html_wrap_inline2212 S S1.2 (21)
HS 0843+2533 08 43 56.47 25 33 14.7 0.050 16.8 S1 S1 -
Marktex2html_wrap_inline2220 08 51 32.38 39 43 45.5 0.013 14.1 S? HII (11)
KUG 0929+324 09 29 01.90 32 26 59.9* 0.005 17.5 ? HII (24)
CG 49 09 58 07.76 31 26 44.7 0.042 16.4 S2 S2 (20)
UM 446 11 39 12.06 tex2html_wrap_inline2204 37 27.1 0.005 17.3 ? HII (8)
US 2896 11 42 33.73 31 03 56.5 0.060 16.0 S1.5 S1 (22)
Marktex2html_wrap_inline2244 12 03 17.01 35 27 27.5 0.054 15.3 S S1 (14)
2E 1219+0447 12 19 04.62 04 47 04.3 0.094 16.8 ? S1 (3)
KUV 13000+2908 13 00 01.52 29 07 37.0 0.023 16.1 S2 HII (7)
Q 1356-067 13 56 44.90 tex2html_wrap_inline2264 07 43.8 0.072 16.2 S? HII -
Marktex2html_wrap_inline2268 14 16 12.98 34 35 46.0 0.069 16.0 ? HII (12)
PKS 1420-27 14 19 55.50 tex2html_wrap_inline2276 14 20.8 - tex2html_wrap_inline2280 Q? Q (2)
Marktex2html_wrap_inline2282 14 31 40.78 52 59 26.8 0.089 16.5 S? HII (15)
PKS 1437-153 14 37 11.31 tex2html_wrap_inline2290 18 58.9 - tex2html_wrap_inline2294 Q? BL (4)
Marktex2html_wrap_inline2296 14 55 59.69 35 24 05.4 0.040 16.0 S? HII (15)
Marktex2html_wrap_inline2302 15 28 41.48 34 05 53.3 0.048 16.4 HII HII (12)
KUV 15519+2144 15 51 53.33 21 43 42.9 0.040 15.8 S2 HII (7)
Q 1619+3752 16 19 55.81 37 52 36.3 0.034 17.3 ? HII (23)
EXO 1622.0+2611 16 22 05.33 26 11 23.9 - 16.1 S? S1 -
Q 1624+4628 16 24 34.76 46 28 48.2 0.030 16.1 ? HII (23)
Q 1638+4634 16 38 50.52 46 34 38.8 0.059 16.4 ? HII (23)
Kaz 110 16 57 16.83 69 09 08.0 0.053 17.2 HII HII (5)
PKS 1903-80 19 03 56.16 tex2html_wrap_inline2344 14 59.8 - 19.0 Q? Q (1)
RN 73 20 36 08.47 88 02 05.4 0.047 17.5 ? S1.9 (19)
Q 2233+0123 22 33 08.78 01 24 00.2 0.058 16.6 ? S1 (23)
Q 2257+0221 22 57 00.37 02 21 29.8 0.048 16.7 ? S2 (23)
NGC 7678 23 25 57.91 22 08 44.7 0.012 15.3 S2 HII (6)
E 2344+184 23 44 53.30 18 28 10.8 0.138 15.9 ? S2 (10)
UM 11 23 50 45.22 03 26 22.3* 0.038 16.0 S HII (9)
Table 3: This table gives for each of the observed objects: the name (Col. 1), the B1950 optical position measured on the Digitized Sky Survey (Cols. 2 and 3), where the the rms error is 0.6 arcsec in each coordinate; " * '' indicates objects with larger errors because of their location near one edge of the Schmidt plate (Véron-Cetty & Véron 1996), the published redshift (Col. 4), the magnitude (Col. 5), the old spectral classification: S2: Seyfert 2, S1: Seyfert 1, HII: HII region, Q: Quasar, ?: unknown (Col. 6), and our classification (Col. 7). References for the finding charts (Col. 8): (1) Anguita et al. (1979), (2) Bolton & Ekers (1966), (3) Bowen et al. (1994), (4) Condon et al. (1977), (5) Kazarian (1979), (6) Kazarian & Kazarian (1980), (7) Kondo et al. (1984), (8) MacAlpine & Williams (1981), (9) MacAlpine et al. (1977), (10) Margon et al. (1985), (11) Markarian & Lipovetski (1971), (12) Markarian & Lipovetski (1972), (13) Markarian & Lipovetski (1973), (14) Markarian & Lipovetski (1974), (15) Markarian & Lipovetski (1976), (16) Markarian et al. (1977a), (17) Markarian et al. (1977b), (18) Markarian et al. (1979), (19) Penston (1971), (20) Pesch & Sanduleak (1983), (21) Pesch & Sanduleak (1986), (22) Sanduleak & Pesch (1984), (23) Schneider et al. (1994), (24) Takase & Miyauchi-Isobe (1985), (25) Wills & Wills (1976)

 


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