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Observations

The 53 observed galaxies suspected to have a ``transition'' spectrum are listed in Table [*] with the various names under which they are known, and in Table [*] with the published line intensity ratios $\lambda$5007/H$\beta$, $\lambda$6300/H$\alpha$ and $\lambda$6583/H$\alpha$. Table [*] gives their optical positions measured on the Digitized Sky Survey[*] (Véron-Cetty & Véron 1996).


 
Table:   B1950 optical positions of the observed objects measured on the Digitized Sky Survey. The r.m.s. error is 06 in each coordinate; `` * '' indicates objects with larger errors due to their location near one edge of the Schmidt plate (Véron-Cetty & Véron 1996). References for finding charts: (1) Andreasian & Alloin (1994), (2) Arp (1966), (3) Bowen et al. (1994), (4) Carballo et al. (1992), (5) de Grijp et al. (1987), (6) Delgado & Perez (1996), (7) Duc et al. (1997), (8) Kazarian (1979), (9) Keel (1996), (10) Markarian & Lipovetski (1971), (11) Markarian & Lipovetski (1973), (12) Markarian & Lipovetski (1974), (13) Markarian et al. (1979a), (14) Markarian et al. (1979b), (15) Markarian & Stepanian (1983), (16) Mazzarella & Boroson (1993), (17) Olsen (1970), (18) Pesch & Sanduleak (1983), (19) Rubin et al. (1975), (20) Sandage & Bedke (1994), (21) Takase & Miyauchi-Isobe (1986), (22) Takase & Miyauchi-Isobe (1990), (23) Vogel et al. (1993), (24) Wyndham (1966).
Name $\alpha$ $\delta\; \; \; \; \; \; \;$ Ref. mag. Name $\alpha$ $\delta\; \; \; \; \; \; \;$ Ref. mag.
Mark 938 00 08 33.41 $\/-\,$12 23 06.6 (16) 13.5 IRAS 12474+4345S 12 47 25.08 $\;$ 43 45 16.6 (5) 15.4
Mark 957 00 39 09.65 $\;$ 40 04 51.6 (3) 15.1 UGC 8621 13 35 28.44 $\;$ 39 24 30.8 - 14.2
IRAS 01346-0924 01 34 37.53 $\/-\,$09 24 12.9 (5) 15.8 Mark 266SW 13 36 14.50 $\;$ 48 31 47.4 (16) 13.4
Mark 1066 02 56 49.91 $\;$ 36 37 21.1 (16) 14.0 Mark 266NE 13 36 14.99 $\;$ 48 31 53.5 (16) 13.4
IRAS 03355+0104 03 35 35.77 $\;$ 01 04 34.0 (23) 14.5 Mark 1361 13 44 36.53 $\;$ 11 21 20.1 (14) 15.3
IRAS 04210+0400 04 21 02.69 $\;$ 04 01 08.2 (5) 16.3 Mark 461 13 45 04.29 $\;$ 34 23 51.9 (9) 14.6
IRAS 04507+0358 04 50 47.50 $\;$ 03 58 48.9 (5) 15.0 4C 26.42 13 46 33.84 $\;$ 26 50 26.3 (17) 15.2
VII Zw 73 06 25 37.78 $\;$ 63 42 42.9 (5) 14.8 I Zw 81 14 06 20.29 $\;$ 49 05 56.1 - 16.5
Mark 622 08 04 21.03 $\;$ 39 08 57.4 (12) 14.1 Mark 477 14 39 02.52 $\;$ 53 43 03.3 (9) 15.0
3C 198.0 08 19 52.43 $\;$ 06 06 45.7 (24) 17.3 Mark 848S 15 16 19.40 $\;$ 42 55 35.9 (16) 15.0
KUG 0825+248 08 25 29.98 $\;$ 24 48 31.9 (21) 16.0 IRAS 15184+0834 15 18 27.10 $\;$ 08 34 33.9 (5) 13.9
IRAS 09111-1007E 09 11 13.06 $\/-\,$10 06 54.6 (7) 16.1 NGC 5953 15 32 13.23 $\;$ 15 21 35.9 (6) 13.1
Zw 238.066 09 27 45.68 $\;$ 49 18 00.4 - 16.5 Kaz 49 15 56 26.70 $\;$ 63 59 00.8 (8) 15.3
UGC 5101 09 32 04.95 $\;$ 61 34 36.5 (9) 15.5 IRAS 16129-0753 16 12 58.38 $\/-\,$07 53 07.2 (4) -
NGC 2989 09 43 03.79 $\/-\,$18 08 35.1 (20) 14.5 IRAS 16382-0613 16 38 11.57 $\/-\,$06 13 07.6 (4) 14.7
CG 49 09 58 07.76 $\;$ 31 26 44.7 (18) 16.0 Mark 700 17 01 21.49 $\;$ 31 31 37.8 (9) 15.5
NGC 3185 10 14 53.07 $\;$ 21 56 18.8 (20) 12.3 MCG 03.45.003* 17 33 25.27 $\;$ 20 49 37.6 (5) 13.4
Arp 107A 10 49 29.66 $\;$ 30 19 25.1 (2) 14.6 PGC 61548 18 10 07.06 $\;$ 21 52 15.9 - 14.2
NGC 3504 11 00 28.55 $\;$ 28 14 31.6 (20) 12.9 Kaz 214 18 46 15.77 $\;$ 72 07 42.9 (5) 15.5
IRAS 11058-1131 11 05 49.65 $\/-\,$11 31 56.8 (5) 14.9 NGC 6764 19 07 01.23 $\;$ 50 51 08.5 (19) 13.2
NGC 3642 11 19 25.03 $\;$ 59 20 54.9 (20) 14.1 IRAS 22114-1109 22 11 26.01 $\/-\,$11 09 21.1 - -
Mark 1291 11 21 00.13 $\/-\,$08 23 01.5 (13) 15.5 Mark 308 22 39 30.53 $\;$ 20 00 00.1 (10) 14.6
IRAS 11285+8240A 11 28 41.22 $\;$ 82 40 16.0 - 15.6 KUG 2239+200A 22 39 33.13 $\;$ 20 00 38.4 (22) 15.5
Mark 739W* 11 33 52.49 $\;$ 21 52 22.2 (16) 14.0 Mark 522 22 57 50.44 $\;$ 16 06 50.7 (11) 17.0
SBS 1136+594 11 36 24.27 $\;$ 59 28 31.4 (15) 16.0 Mark 313 22 59 32.07 $\;$ 15 41 44.3 (10) 14.0
NGC 3994* 11 55 02.44 $\;$ 32 33 21.1 (20) 12.9 Zw 453.062 23 02 28.55 $\;$ 19 16 55.2 - 15.1
NGC 4102 12 03 51.33 $\;$ 52 59 21.2 (20) 12.6 IC 5298 23 13 33.13 $\;$ 25 17 01.9 (1) 14.9

Spectroscopic observations were carried out during several observing runs in May, June and July 1996 and January, March, October and November 1997 with the spectrograph CARELEC (Lemaître et al. 1989) attached to the Cassegrain focus of the Observatoire de Haute-Provence (OHP) 1.93 m telescope. The detector was a 512 $\times$ 512 pixels, 27 $\times$ 27 $\mu$m Tektronic CCD. We used a 600 lmm-1 grating resulting in a dispersion of 66 Åmm-1; the spectral range was $\lambda\lambda$6700-7600 Å in the red (with a Schott GG 435 filter) and $\lambda\lambda$4860-5760 Å in the blue. In each case, the galaxy nucleus was centered on the slit.

Usually five columns of the CCD ($\sim$ 5) were extracted. The slit width was 21, corresponding to a projected slit width on the detector of 52 $\mu$m or 1.9 pixel. The slit position angle was not always the same for the blue and red spectra; as the aperture used is rectangular (21 $\times$ 5), this may introduce some inconsistencies when the line emitting regions are extended. The resolution, as measured on the night sky emission lines, was $\sim$ 3.4 Å FWHM. The spectra were flux calibrated using the standard stars given in Table [*], taken from Oke (1974), Stone (1977), Oke & Gunn (1983) and Massey et al. (1988). The journal of observations is given in Table [*].


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Next: Line profile fitting Up: Observations and data analysis Previous: Observations and data analysis

12/15/1998