Candidate WR galaxies resulting from some of the searches discussed in Sect. 2 or found loosely in the literature are listed in Table 3. The reader is referred to the original papers for the justification of the possible presence of WR stars.
R.A. | Decl. | Morphology | mb | Vrad | Reference | ||
Name | [1950] | [1950] | [mag] | [km s-1] | |||
Fairall 4 | 00 12 49.2 | -57 31 22 | (R)SA(r)b | 15.1 | 9796 | P99 | |
Tol 0030-388 | 00 30 38.3 | -38 50 29 | 13800 | MMO91 | |||
Fairall 0007 | 00 42 06.0 | -60 07 00 | MMO91 | ||||
UM 080 | 00 57 46.8 | +04 23 46 | 17.8 | 4797 | P99 | ||
EQ 0102-310 | 01 02 | -31.0 | MMO91 | ||||
Tol 0127-397 | 01 27 02.4 | -39 46 03 | 4797 | P99 | |||
UM 354 | 01 37 11.1 | +01 10 57 | 9294 | P99 | |||
UM 377 | 01 52 18.8 | +01 02 28 | 8694 | P99 | |||
UM 396 | 02 04 51.0 | +02 42 41 | 6296 | P99 | |||
NGC 848 | 02 07 50.4 | -10 33 25 | (R')SB(s)ab | 13.6 | 4001 | GIT98 | |
NGC 1068 | 02 40 07.0 | -00 13 32 | (R)SA(rs)b | 9.6 | 1136 | ED86 | |
CAM 0357-3915 | 03 57 22.1 | -39 14 51 | HII | 22545 | P99 | ||
Tol 0440-381 | 04 40 23.3 | -38 06 41 | 12300 | MMO91,P99 | |||
Tol 0513-393 | 05 13 39.7 | -39 20 59 | 15000 | P99 | |||
Tol 0538-416 | 05 38 32.9 | -41 38 37 | HII | 13491 | P99 | ||
Tol 0559-393 | 05 59 04.9 | -39 19 08 | Irr | 15.0 | 24915 | MMO91,P99 | |
Tol 0620-386 | 06 30 08.3 | -38 39 11 | 20100 | P99 | |||
Tol 0645-376 | 06 45 07.0 | -37 40 02 | 7795 | MMO91 | |||
NPM1G+16.0158 | 08 41 01.4 | +16 10 38 | 18.3 | P99 | |||
ESO 566-8 | 09 42 39.2 | -19 28 55 | S pec | 16.3 | 9761 | C96 | |
Mrk 709 | 09 46 33.2 | +17 06 44 | BCD | 17.0 | 1197 | P99 | |
Tol 1021-289 | 10 21 22.0 | -28 58 30 | Interacting | 16.9 | 17658 | P99 | |
Tol 1025-285 | 10 25 06.2 | -28 32 13 | N | 16.2 | 8694 | P99 | |
Abell 1068 | 10 37 51.3 | +40 12 51 | cD | 16.0 | 41580 | A95 | |
Tol 1032-283 | 10 32 18.4 | -28 19 52 | E4: | 14.4 | 3190 | KS86 | |
Mrk 1301 | 11 33 10.9 | +35 36 43 | S0/a | 14.5 | 1603 | RC93 | |
UM 456 | 11 48 02.5 | -00 17 21 | Pec | 15.9 | 1757 | P99 | |
Pox 52 | 12 00 22.9 | -20 39 21 | 17.2 | KSB87 | |||
UM 482 | 12 09 29.4 | -00 19 43 | Sm | 16.2 | 10544 | P99 | |
UM 483 | 12 09 41.0 | +00 21 01 | 16.7 | 2099 | P99 | ||
M100 | 12 20 22.9 | +16 05 58 | SAB(s)bc | 7.4 | 1571 | WO98 | |
NGC 4509 | 12 30 38.9 | +32 22 02 | Sab pec? | 14.1 | 937 | RC93 | |
Tol 1258-363 | 12 58 19.0 | -36 19 54 | 4887 | P99 | |||
UM 594 | 13 35 32.7 | +00 16 26 | HII? | 15.8 | 6653 | P99 | |
NGC 5257 (W) | 13 37 19.7 | +01 05 33 | SAB(s)b pec | 12.9 | 6798 | MMO91 | |
NGC 5291 | 13 44 33.3 | -30 09 31 | E pec: | 15.1 | 4386 | DM98 | |
Tol 1345-419 | 13 45 14.2 | -41 55 23 | Sy2 | 17.0 | 11572 | P99 | |
UM 618 | 13 50 03.1 | +00 16 07 | 18.4 | 4197 | P99 | ||
Abell 1835 | 13 58 30.0 | +03 06 00 | cD | 19.3 | 75690 | A95 | |
EQ 1409-120 | 14 09 | +01 20 | MMO91 | ||||
Cam 1409+1200 | 14 09 14.3 | +11 59 33 | 16800 | P99 | |||
NGC 6090 | 16 10 24.0 | +52 35 04 | Sd pec | 14.5 | 8822 | RC93 | |
Tol 2006-393 | 20 06 39.7 | -39 22 32 | 9294 | P99 | |||
Tol 2138-405 | 21 38 14.8 | -40 32 35 | 16800 | P99 | |||
Tol 2146-391 | 21 46 45.0 | -39 08 10 | 8994 | MMO91,P99 | |||
Tol 2259-398 | 22 59 34.0 | -39 49 42 | Compact | 15.6 | 8858 | MMO91,P99 | |
UM 159 | 23 19 31.9 | +01 12 24 | HII | 8694 | P99 | ||
UM 160 W | 23 21 46.0 | -00 23 30 | 2400 | P99 | |||
KEY TO REFERENCES. -- A95 Allen 1995, C91 Conti 1991, DM98 Duc & Mirabel 1998 DRM93 Drissen et al. 1993, ED86 Evans & Dopita 1986, GIT98 Guseva et al. 1998, KS86 Kunth & Schild 1986, KSB87 Kunth et al. 1987, MMO91 Masegosa et al. 1991, P99 Pindao et al. 1999, RC93 Robledo-Rella & Conti 1993, VC92 Vacca & Conti 1992, WO98 Wozniak et al. 1998 |
Most of the suspected WR galaxies come from the spectrophotometric catalogue of HII galaxies of Terlevich et al. (1991), following the analysis of Masegosa et al. (1991) or Pindao et al. (1999) which also includes new objects. As stated earlier, from Masegosa et al. (1991) we take the subset of objects included in their Table 1 but not in Table 2 as candidates. Although partly based on the same observations the analysis of Masegosa et al. (1991) and Pindao et al. (1999) do not always yield the same candidates. We have retained all objects classified as "candidate" by either one of these studies. New observations will be necessary to establish the definite presence or absence of WR features.
Few objects from Vacca & Conti (1992) have only an upper limit on broad HeII 4686. For most of them independent observations are now available. Otherwise these objects are retained as suspected WR galaxies.
In some studies of IUE spectra strong UV P-Cygni lines of N and C (N V 1240, C IV 1550) have been interpreted as signatures of WR stars in theses objects (e.g. Durret et al. 1985, Lamb et al. 1990). However, these lines are also strong in O stars and hence cannot be used as a clear diagnostic for WR stars (cf. Leitherer et al. 1995). Therefore, objects suspected on these grounds have not been included in Table 3.
In rare cases, WR stars have also been suspected on indirect grounds (e.g. M100: Wozniak et al. 1998).
Interestingly, a broad WR bump is suggested to be present in the optical spectrum of two distant central cluster galaxies with strong cooling flows (Abell 1068 and 1835, Allen 1995). The recent study of Contini et al. (1998), however, casts serious doubt about the reality of a broad feature in Abell 1835. If true, these objects with redshifts z ~ 0.14 and 0.25 respectively, represent the most distant objects known to date where WR stars have been detected from (rest-frame) optical spectra. High redshift galaxies (z ~ 3) may, however, also show WR signatures (see Sect. 7).
6.2. Emission line galaxies without HeII
Conti (1991, his Table 3) lists a sample of emission line galaxies which have properties similar to WR galaxies, and where a search for HeII 4686 emission (broad or narrow) has been made with negative results. For obvious reasons such a list is necessarily incomplete and the inclusion in such a list also strongly depends on the sensitivity (S/N, resolution etc.) of the data. We therefore renounce on such a compilation. However, few updates are appropriate on some objects from Table 3 of Conti (1991).
Mrk 1087 -- While Vacca & Conti (1992) provide only an upper limit on HeII 4686, a detection is provided in the recent spectra of Vaceli et al. (1997). No information on the width of this line is given. Retained as suspected WR galaxy.
Mrk 1094 -- We have retained the criteria of Kunth & Joubert (1985) and hence included this object in Table 1. No new observations published.
0833+652 = IRAS 08339+6517 -- From their spectrum Veilleux et al. conclude that no WR features are present in this galaxy (=0833+652 in Conti 1991).
Tol 2 = Tol 0957-278 -- Same comment as for Mrk 1094.
Tol 9 = Tol 1032-283 Although no broad HeII 4686 feature seems present in this object (Kunth & Schild 1986) we list in the category of suspected WR galaxies based on the possible detection of other broad features shortward of 5876 Å (Kunth & Schild 1986).
Other objects for which an upper limit on broad WR features is given or where a non-detection is signaled are found in publications issued from the systematic searches discussed in Sect. 2.