------------------------------------------------------------------------------------------------------ Revised Dolidze-Cluster-List (MK, AUG 2006) ------------------------------------------------------------------------------------------------------ tentative types: AST .. asterism DUB .. dubious cluster candidate OC? .. possible cluster OC .. likely cluster ASS .. association PAS .. part of association list-column: D .. included in DAML 2.6 Drem .. included in DAML 2.6_removed - .. not included in DAML Name RA 2000 DEC 2000 Type diam list notes ---------------------------------------------------------------------------------------------------- Dolidze 52 18 23.9 -16 39 00 6.0 x 3.0 The only one I could not identify (MK) Dolidze 34? 18 41 54 -04 16 37 DUB 4.0 - Dolidze 53 19 46 23 +24 39 05 ASS? 12.8 - Dolidze 49 06 47 04 -00 00 25 OC? 2.2 - Dolidze 34? 18 42 01 -04 33 05 DUB 1.8 - Dolidze 50 16 05 40 -20 30 25 AST 12.0 - Dolidze 54 21 01 06 +41 21 50 AST 9.6 - Dolidze 18? 05 23 21 +33 30 29 (OC ) 14.3 - part of cluster NGC 1893 ? Dolidze 55 21 09 46 +40 35 20 AST 4.7 - Dolidze 12? 00 36 29 +60 20 45 AST? 20.2 - Dolidze 20? 05 27 49 +33 47 36 DUB 10.5 - Dolidze 20? 05 30 05 +33 26 44 AST 12.9 - Dolidze 56 22 04 11 +59 51 47 AST 7.2 - Dolidze 51 18 10 24 -17 44 29 AST 7.1 - Dolidze 44 20 29 41 +41 42 17 AST 14.9 D Dolidze 19 05 23 37 +08 11 21 AST 21.7 D Dolidze 21 05 27 03 +06 54 18 AST 12.7 D Dolidze 23? 06 42 55 +00 02 46 DUB? 12.7 D Dolidze 15 05 06 35 +34 51 24 DUB 16.5 D Dolidze 26 07 30 00 +11 57 59 AST 21.0 D Dolidze 38 20 06 13 +41 11 13 AST 12.3 D Dolidze 9 20 25 31 +41 54 38 AST 5.6 D Dolidze 32 18 41 05 -04 04 51 OC 9.8 D Dolidze 10 20 25 19 +40 06 26 AST 18.8 D Dolidze 28 18 25 29 -14 39 21 OC? 11.6 D Dolidze 5? 20 20 10 +39 19 50 DUB 7.5 D Dolidze 2 20 10 54 +41 11 33 AST 10.4 D Dolidze 1? 20 09 38 +36 30 21 OC? 7.9 D Dolidze 16 05 14 44 +32 41 19 OC? 19.8 D Dolidze 35 19 25 16 +11 39 50 AST 9.5 D Dolidze 1? 20 08 04 +36 39 41 OC? 6.8 D Dolidze 36 20 02 33 +42 04 09 AST 12.5 D Dolidze 24 06 44 41 +01 41 05 OC 18.8 D Dolidze 33 18 41 18 -04 21 37 DUB? 8.9 D Dolidze 25 06 45 16 +00 13 23 OC? 26.0 D Dolidze 14 04 06 43 +27 32 34 DUB? 18.0 D Dolidze 6 20 20 32 +41 21 24 DUB? 7.8 D Dolidze 11 20 26 27 +41 24 59 AST 8.0 D Dolidze 8 20 24 23 +42 16 52 OC 7.3 D Dolidze 3 20 15 29 +36 51 47 OC 14.9 D Dolidze 39 20 16 01 +37 53 15 OC? 15.5 D Dolidze 4 20 17 56 +36 42 19 DUB 8.7 D Dolidze 42 20 19 30 +38 09 04 OC? 10.0 D Dolidze 41 20 18 54 +37 46 23 AST 10.8 D asterism, superimposed on cluster Berkeley 85 ! Dolidze 40 20 17 56 +37 55 59 OC? 16.6 D cluster Feibelman 1 is included in northern part Dolidze 45 21 10 46 +37 34 28 OC? 16.2 D Dolidze 5? 20 20 15 +39 22 10 DUB 7.3 D Dolidze 18? 05 24 02 +33 23 14 DUB? 9.5 D Dolidze 37 20 02 51 +37 42 44 AST 9.3 D Dolidze 13 00 49 42 +64 07 35 DUB 16.0 D Dolidze 47 20 41 55 +36 34 37 OC? 11.0 D Dolidze 27 16 36 28 -08 56 58 AST 28.1 D Dolidze 23? 06 42 44 -00 18 33 DUB 11.4 D Dolidze 22 06 23 21 +04 35 57 DUB 19.4 D Dolidze 31 18 36 35 -06 43 19 OC? 14.2 Drem Dolidze 12? 00 40 31 +60 53 26 AST 15.2 Drem Dolidze 30 18 33 26 -05 57 53 DUB? 13.9 Drem Dolidze 29 18 32 05 -06 23 59 AST 14.0 Drem Dolidze 43 20 20 47 +39 48 02 PAS 21.9 Drem Dolidze 17 05 22 16 +07 06 20 AST 13.2 Drem Dolidze 46 23 22 21 +56 22 19 AST? 11.7 Drem ---------------------------------------------------------------------------------------------------- Thanks to Dave Riddle's recent input on some Simeis nebulosities, I was able to finish my Dolidze cluster project which kept me busy for several months. Results see below ! Matthias ********************************************************************* In the following table, precise data on position and size of every stellar aggregate Madona Dolidze (MD) has discovered (or, to be more precise: may have discovered) are given. Whenever possible, I used the original data from the discovery papers to identify the clustering; this was necessary as the notes provided by MD for individual are much more extensive (though still sparse) than those in later catalogues of open clusters, as e.g. [5]. Many, many thanks in that respect to D. Lorenz from the University Vienna who finally located these obscure publications! In some cases, an unambiguous identification of the object was not possible, either due to poor positional data or, because the aggregate at the position did not match the description of MD. These cases are commented in detail in the notes section following the table. This section deals also with objects that have been incorrectly identified in the past due to positional errors, typos in the original papers, etc.. Anyway, here's the list. If anybody is interested in further details on objects and the data given in the table below, please send me a note. ID RA 2000.0 DE 2000.0 size notes (**: see text below) Dolidze 1 20 08 03.5 +36 39 41 6.8' ** 20 09 38.3 +36 30 21 7.9' ** Dolidze 2 20 10 53.5 +41 11 33 10.4' ** Dolidze 3 20 15 28.8 +36 51 47 14.9' Dolidze 4 20 17 56.4 +36 42 19 8.7' Dolidze 5 20 20 15.0 +39 22 10 7.3' ** 20 20 09.9 +39 19 50 7.5' ** Dolidze 6 20 20 32.2 +41 21 24 7.8' Dolidze 7 = Berkeley 87 Dolidze 8 20 24 23.0 +42 16 52 7.3' Dolidze 9 20 25 30.8 +41 54 38 5.6' asterism Dolidze 10 20 25 19.2 +40 06 26 18.8' ** Dolidze 11 20 26 26.5 +41 24 59 8.0' Dolidze 12 00 40 30.5 +60 53 26 15.2' ** 00 36 29.4 +60 20 45 20.2' ** Dolidze 13 00 49 42.4 +64 07 35 16.0' Dolidze 14 04 06 42.9 +27 32 34 18.0' Dolidze 15 05 06 34.6 +34 51 24 16.5' ** Dolidze 16 05 14 43.8 +32 41 19 19.8' Dolidze 17 05 22 15.7 +07 06 20 13.2' asterism Dolidze 18 05 23 20.9 +33 30 29 14.3' ** 05 24 01.9 +33 23 14 9.5' Dolidze 19 05 23 36.8 +08 11 21 21.7' asterism Dolidze 20 05 27 49.2 +33 47 36 10.5' ** 05 30 05.0 +33 26 44 12.9' ** Dolidze 21 05 27 02.7 +06 54 18 12.7' asterism Dolidze 22 06 23 20.7 +04 35 57 19.4' Dolidze 23 06 42 54.5 +00 02 46 12.7' ** 06 42 43.7 -00 18 33 11.4' ** Dolidze 24 06 44 41.1 +01 41 05 18.8' Dolidze 25 06 45 15.5 +00 13 23 26.0' Dolidze 26 07 30 00.3 +11 57 59 21.0' asterism Dolidze 27 16 36 28.4 -08 56 58 28.1' asterism Dolidze 28 18 25 28.7 -14 39 21 11.6' Dolidze 29 18 32 04.7 -06 23 59 14.0' ** Dolidze 30 18 33 25.6 -05 57 53 13.9' ** Dolidze 31 18 36 35.3 -06 43 19 14.2' ** Dolidze 32 18 41 05.4 -04 04 51 9.8' ** Dolidze 33 18 41 18.0 -04 21 37 8.9' ** Dolidze 34 18 42 01.4 -04 33 05 1.8' ** 18 41 54.0 -04 16 37 4.0' ** Dolidze 35 19 25 15.7 +11 39 50 9.5' asterism Dolidze 36 20 02 33.2 +42 04 09 12.5' asterism Dolidze 37 20 02 51.1 +37 42 44 9.3' asterism Dolidze 38 20 06 12.5 +41 11 13 12.3' asterism; dense knot of stars at 20 06 05.5 +41 06 57 could be physical grouping Dolidze 39 20 16 01.3 +37 53 15 15.5' Dolidze 40 20 17 55.9 +37 55 59 16.6' Dolidze 41 20 18 54.1 +37 46 23 10.8' asterism Dolidze 42 20 19 29.7 +38 09 04 10.0' Dolidze 43 20 20 47.0 +39 48 02 21.9' Dolidze 44 20 29 41.2 +41 42 17 14.9' asterism Dolidze 45 21 10 45.6 +37 34 28 16.2' ** Dolidze 46 23 22 20.7 +56 22 19 11.7' ** Dolidze 47 20 41 55.4 +36 34 37 11.0' ****************************************************************** Extended notes: Dolidze 1: correctly identifying this group is very difficult: the given coordinates are significantly off and there are no further informations given ( except from the size of 6' ). In fact, there are two groups in the vicinity of the given position that match the description of MD: The first candidate is at 20 08 03.5 +36 39 41 and appears as an inconspicuous grouping around HD 227835 and HD 191379 ( diam. ~7' ). Although sparse, several stars of the group have similar proper motion, so the possibility remains that it is real cluster. A better match, however, is the group situated at 20 09 38.3 +36 30 21; although already 1.5m away from the original position, it is much better defined than the prior one and contains some luminous early-type stars (ALS 10882, 10883(*) and 10884) that may have attracted MD (although she didn't note it as an O-type cluster in her paper). Again, several stars of the group have similar proper motion vectors so it may be a real one. * ... A note on ALS 10883: SIMBAD gives a spectral type of M2 for this star. This cannot be true, as both the B-V and the 2MASS J-Ks colour indices of this star suggest a much earlier spectral type (B-V = 0.33, J-Ks = 0.141). Dolidze 2: Likely the asterism of bright B and A type stars that surrounds IC 1311. The error in coordinates might have originated from the fact that the position of IC 1311 (which may have acted as reference) is significantly off in older catalogues (it is still in the DAML). Dolidze 5: Slight uncertainty concerning its identification; at the position given by MD, there is a group of 8 brighter stars and a fainter group that is partly superimposed on the southern edge. Both match the diameter of 7' given by MD very well. Which one she meant remains a mystery. Dolidze 10: Dolidze made probably an error of 1m in RA here when she determined the position of this specimen. The group itself is involved in the western part of the IC 1318 complex and - according to proper motion data - probably an asterism. Dolidze 12: In the discovery paper, this object is noted as a 18' diameter clustering that contains an emission-line star. Indeed, there is a clustering at this position that contains the emission line stars ALS 6291 and ALS 6297. However, the clustering itself (apparently an asterism) is - even for her standards - a very inconspicuous one, so it is unsure that this is the clustering she meant. As a possible alternative, it might be that MD made a mix-up regarding the identity of the included emission-line objects. Indeed, there is a conspicuous group around HD 3283 which contains the emission star CDS 58; this star, however, is not listed in any of her publications. so this interpretation is highly speculative. Dolidze 15: Nothing at the original position, but [3] notes the membership of the emission line star MWC 746 which is 2m E. Indeed, at this position one finds a loose grouping which is probably the one MD had in mind. Dolidze 18: This is another interesting case which deserves further attention. Dolidze notes here that the cluster is associated with IC 410 and contains one emission star. Indeed, about 5' N of the given position, a loose clustering is apparent that is involved in the outlying parts of the nebulosity. This group, however, does not contain an emission star. The possibility exists that Dolidze actually referred to the conspicuous clustering immediately NE of NGC 1893: This 14' measuring group (at 05 23 20.9 +33 30 29) contains the emission star GGA 333, which is listed in [3] as 05+020. Obviously, she must have observed that group. Dolidze 20: Very likely the clustering around HD 35681 that is about 1m W of the updated position of Dolidze. However, there remains the small possibility that Dolidze referred to the grouping at 05 30 05.0 +33 26 44 (12.9') that contains several nebulosities and the emission star GGA 341 (which has not been described by her, though). Dolidze 23: The identification of this object is slightly unsure, as MD does not provide any further information on this object. Almost on-spot at her position, there is a clustering that matches the diameter of Dolidze (12') well and is likely the object discovered by her. However, there are several other, equally outstanding groupings in the field; one of them - 20' S of the original position - is listed in the table. Dolidze 29 - 34: Apparently, MD had difficulties to determine the coordinates of the objects she discovered in the northern part of the Scutum Star Cloud. Every position is significantly off, what explains the difficulties of former authors with identifying the correct star groups. The easiest one to identify is the cluster Dolidze 30. Nothing at the updated MD position, but the star HD 171149 about 0.5 minutes E is involved in a rather conspicuous, scattered grouping of stars which is likely the object MD observed. The updated position of Dolidze 30 helps with identifying nearby Dolidze 29: Again nothing at her position, but shifting the RA again 0.5 minutes towards E and using a declination that is 10' farther north (likely, a typo appeared in her position), one gets to the right star group. This grouping contains the carbon star Case 171, which was already known at the time of her observations and might have attracted her interest. The aggregate itself is rather loose and probably just a chance alignment of stars. Dolidze 31: At her position, nothing is visible; however she notes an association with the nebulosity Sh2-52 = Simeis 198, which is 2m in RA towards E. This nebulosity indeed contains a conspicuous clustering, with several stars are of spectral type B involved. A physical association of group and nebula is therefore likely. Dolidze 32: Again, nothing visible at the position given by MD. However, the Alter-Ruprecht catalogue states that the group contains a possible Cepheid. Together with MD's quote that the cluster holds 2 emission line stars, this points towards a conspicuous and likely real clustering 0.7m east which contains the Cepheid RR Sct and two emission stars. As in the case of Do 29 and Do 30, the corrected position of Dolidze 32 helps with finding a possible candidate for Dolidze 33: adding 0.7m of RA to MD's original position of that object, one finds a group - possibly a dust hole - which contains the ALS stars 9849 and 9853 and the M4 star RAFGL 2227. There is a little uncertainty with this identification as MD notes the presence of 2 emission-line stars which are not apparent in this grouping; however, the WR star V462 Sct that lies just 7.5' SW shows some emission lines in his spectrum (it had been classified as a PN previously) and may have contributed to her count. Dolidze 34: This object remains mysterious. The updated + corrected position of Dolidze points almost exactly towards an asterism of 4 stars; this identification seems to have been done already by Alter/Ruprecht [5], who listed Dolidze 34 at a position that is already shifted towards E in respect to the original one. Anyway, it is very doubtful that Dolidze had this grouping in mind because she lists it as containing 3(!) emission stars - which this clustering just does not contain. A possible explanation could be that MD simply made a typo in her positional data (her papers are notorious for containing numerous of them). Indeed, if one reverses the last two numbers of her declination ('42' --> '24') and updates this position, one gets almost on-spot to a grouping that is 0.6m E and 6' N of Dolidze 33; its diameter (4') also corresponds exactly to that quoted by her. However, this clustering does not contain any listed emission line stars so this identification is also doubtful. Another possibility could be that she observed Trumpler 35 but, for any reason, did not identify it as such; this scenario is purely speculative, however. Dolidze 45: Another interesting case. The updated original position (21 19.0 +37 37) points into nowhere; even if a 10m error in RA is assumed (21 09.0 instead of 21 19.0), there's nothing to find. What helps is MD's note that the cluster is involved in the nebulosity Simeis 258 = LBN 321 (**), a large arc of nebulosity that is roughly centered at 21 12 +38. Additionally, Alter/Ruprecht note in [5] the presence of a possible Cepheid. All this points towards a conspicuous grouping at 21 10 45.6 +37 34 28 which is situated on a brighter patch of the Simeis nebulosity and, contains the suspected variable star NSV 13580. (**) Actually, she identified it with Simeis 158 but D. Riddle pointed out to me that must be an error as S 158 is a nebulosity in Monoceros! Dolidze 46: The next Dolidze mystery. As so often, absolutely nothing can be found near the original position that would resemble a clustering according to her description (12' diameter, 1 emission-line star involved). Given the large numbers of typos in her paper, however, it may simply be that the position in [2] is simply not the one MD intended to quote. Indeed, if one reverses numbers for minutes in RA and assume an additional error in DE of -40', one gets exactly towards the emission-line star MWC 1081 = V813 Cas, which is involved in a scattered but rather distinct clustering. Anyway, this is not more than an intelligent guess, so it may be (as in several cases before) that I'm completely wrong with my assumption... ************************************************************************ Apart from the 47 known Dolidze clusters, I could locate in one of her publications [3] 11 other clusterings that seem to have been overlooked by any author who made a compilation of open clusters in the past (I wonder how many more such objects are hidden in obscure Russian circulars and Journals!). These objects were easier to identify as MD provided the x-y coordinates of the objects on the discovery plates (plus the coordinates of the plate centre!) which made it much easier to filter out any errors. Dolidze 47b = Basel 10 Dolidze 48 = NGC 1798 Dolidze 49 06 47 03.6 -00 00 25 2.2' a small clustering in Monoceros. May - or may not - be a real one. Dolidze 50 16 05 39.5 -20 30 25 12.0' a loose asterism in Scorpius. Nothing special Dolidze 51 18 10 24.2 -17 44 29 7.1' elongated grouping in Sagittarius. probably not a real cluster. Dolidze 52 18 23.9 -16 39 6'x3' [3] The only one I could not identify. Absolutely nothing to see at the position given in [3] Dolidze 53 19 46 23.4 +24 39 05 12.8' an interesting object; apparently a large association that contains several reflection nebulosities. Also involved: a tight group at 19 46 20 +24 36 36 that contains the IR cluster [BDB2003] 158 and may likely be a physical grouping Dolidze 54 21 01 06.4 +41 21 50 9.6' probable asterism with an emission line star included Dolidze 55 21 09 46.4 +40 35 20 4.7' The position given by MD cannot be correct, as this would put the object outside of the discovery plate. Obviously, there is a typo here in the RA; if this is corrected, one finds easily an asterism that matches her description. Dolidze 56 22 04 10.5 +59 51 47 7.2' asterism of 5 bright stars with an S star included. Nothing special Dolidze 57 = NGC 7510 Bibliography: [1] ... Dolidze, M. V., On the star cluster near gamma Cyg, Astron. Tsirk. 223, 11D (1961) [2] ... Dolidze, M. V., Some Data of the Nebulae and Star Clusters, Astron. Tsirk. 224, 18 (1961) [3] ... Dolidze, M. V., The Lists of S, C, MS Stars and Emission Objects Revealed in Red Light Observations, AbaOB 47, 3D (1975) [4] ... Dolidze, M.V., Ponomareva G.A., New emission stars in Cas. Sov. Astron., 9, 157 (1965) [5] ... Alter, G. et al., Catalogue of star clusters and associations, Budapest, Akademiai Kiado, 2nd ed. (1970) [6] ... Lynga, G., Catalogue of Open Cluster Data, Lund, Sweden: Lund Observatory (1987)