Catalogue of open cluster data ------------------------------- 1983-05-09 A computer readable catalogue of open cluster data (3rd edition,1983) by Gosta Lynga, Lund Observatory, Box 1107, S-222 04 Lund, Sweden distributed by the Stellar Data Centre, Observatoire de Strasbourg 11 rue de l'Universite, F-67 000 Strasbourg, France File 1. Introduction and description: The following files are recorded on the tape: file 1. Introduction and description (this file); record length = 88. file 2. Catalogue in print-out format; record length = 140. file 3. References; record lenght = 88. file 4. Alias list; record length = 48. file 5. Clusters in order of galactic longitude; record length = 58 file 6. Catalogue for computer use; record length = 2672. The aim of this catalogue is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters these values have been selected from references, which are listed. In particular,for the 1983 edition I have added new information based on inspection of the Palomar, ESO and SERC surveys. For each cluster that could be identified on the available charts I have estimated the dia- meter, made a new classification in Trumpler's system and given an estimate of the number of member stars. The inspection has also been the basis for statements in the alias list that certain clusters are dubious. Those clusters that are dubious both according to my inspec- tion and according to the CSCA catalogue, have been removed from the catalogue but they still appear in the alias listing. The definitions of the data values are in most cases unambiguous. However, the following points should be clarified. Cluster diameter. In the literature some quite convincing cases have been made for the existence of large coronas around open clusters. This may be a general phenomenon, although for most clusters only the diameter of the cluster nucleus is known. For reasons of homogeneity, this is used even when the existence of a cluster corona is likely. For most clusters two diameters are given. My own estimates from survey prints (top line) should form a reasonably homogeneous sample. The second line contains the most reliable, often the only, value available in the literature. Interstellar extinction. Even when interstellar extinction is known to vary across a cluster I have chosen to quote the average value of A(V). The references given provide more details. If the reference gives only colour excess, I have derived the extinction using the relations A(V)=3.1 E(B-V) and A(V)=4.28 E(b-y) for the UBV and uvby systems. Extinc- tion and (B-V)turn-off values are given according to Janes and Adler (1.07). When that compilation includes multiple references, Dr. K. Janes has made the selection. Integrated properties. The total V magnitude and the integrated B-V colour have been calculated by Mr. B. Skiff, Flagstaff, Arizona, using available photometric data. The number of observed stars used is some- times different from my own estimate of membership from survey charts. Reasons for such difference can be inclusion of non-members or limited resolution on the survey charts. Cluster age. When a cluster shows star formation during an extended period, I have given the beginning of that period, i.e. the highest age. In my selection of age data I have preferred results based on isochrone evaluations. Nevertheless, most of the catalogue values for ages are from colour magnitude morphology. Metallicity. As far as possible metallicity values refer to [Fe/H] data such as can be derived from spectral analysis or from uvby photometry. Radial velocities. The data for cluster radial velocities have been collected by Dr. S. Wramdemark of Lund Observatory. They represent weighted mean values for member star velocities as published up to 1980. The weighting procedure takes into account the number of stars in the cluster for which radial velocity had been measured, the accuracy (Wilson class) for each stellar radial velocity and the calculated imprecision in the mean radial velocity for the cluster. Five weight classes are iden- tified by w= 1, 2, 3, 4 and 5 in order of increasing precision. File 2. Catalogue in print-out format: Each page contains eight columns, one for each cluster. The clusters are arranged according to right ascension for 1950.0. The following information is given in the different lines: 1.Cluster notation according to the system accepted by the Inter- national Astronomical Union in Montreal 1979 2-3.Traditional sequence name and number 4.OCL number (1.1) and number in file 6 of present catalogue 5-8.Equatorial coordinates at 1950.0 and precession values for ten years 9-10.Galactic coordinates as calculated 11.Angular diameter as estimated from sky survey prints 12.Angular diameter as selected from references quoted in section 2. 13.Linear diameter in parsecs (calculated) 14.Distance value selected from references quoted in section 3. 15.Interstellar extinction, A(V) 16-22.The number of members that belong to particular star types. These data have been collected by Dr. A. Feinstein and are referenced in section 12. The following star types have been noted: Ap stars Am stars Marginal Ap stars Marginal Am stars WR stars Of stars Be stars Shell stars Be+Shell stars He weak stars He rich stars Cepheids Planetary nebulae Carbon stars Long period variables Delta Scu stars Beta Cep stars R Cor Bor stars Ba II stars U Gem stars 23-25.References for the peculiar star data as quoted in section 12 26.Sky survey used for examination of cluster 27.Number of the sky survey chart 28.Coordinates for the centre of the chart 29.X/Y coordinates for the cluster on the chart 30.Trumpler class with the following notation: Concentration I Detached, strong concentration II Detached, slight concentration III Detached, no concentration IV Not detached Range of brightness 1 Most stars of nearly the same brightness 2 Medium range in brightness 3 Bright and faint stars in the cluster Richness vp Very poor p Poor m Medium r Rich vr Very rich 31.Membership number as estimated from sky survey print 32.Total magnitude of cluster from reference (1.10) 36.Reddening of cluster as quoted in (1.7) 38-39.Earliest spectral class for a cluster member, (1.3) and (1.5) 40.Earliest spectral class for a cluster member as deduced from the colour of the star (1.5) 41.Magnitude of the brightest cluster member (1.3) 42.Logarithm of cluster age from references quoted in section 4 43.Logarithm of metallicity relative to the sun. Quotations from references in section 5 44.Logarithm of cluster mass (1.4) 45.Radial velocity (1.8) with weight estimate 46.Comments, mainly on whether a cluster has been considered dubious by reference 1.01 or 1.09. If considered dubious by both these references, the cluster has been removed from the catalogue File 3. References: References have been divided into the following sections: - 1. General - 2. Angular diameters - 3. Distances - 4. Ages - 5. Metallicities - 11. Comments on dubiousness - 12. Peculiar members - 13. Photometry (compilation according to Janes and Adler) Other sections will be added in future editions of the catalogue. Note that the same paper may well be referenced under several different headings. File 4. Alias list: The alias listing is arranged in right ascension. Cluster names and OCL numbers are given as well as alternative names than have been used. Comments are also given as to identity of clusters in relation to other neighbouring clusters. Comments from NGC catalogue are in- cluded for NGC clusters. File 5. Clusters in order of galactic longitude: After the catalogue and the reference sections there is a table in which clusters are listed in order of increasing galactic longitude. Information given is galactic longitude and latitude, OCL number, IAU number and traditional notation. File 6. Catalogue for computer use: This file is the most comprehensive one being directly derived from the Lund disc at the time of submitting the present version to the CDS. The information for each cluster is stored in 222 columns written with the format (8X,222F12.5). The record length is thus 2672 bytes. The record for one cluster contains (default value =-1000 in all places): The CDS identification of the file, '7041F83 ' followed by : 1 Sequence code 2 Number inside sequence 3 RA, 2000.0, hours 4 RA, 2000.0, minutes 5 Dec, 2000.0, degrees 6 Dec, 2000.0, minutes 7 RA, 1950.0, hours 8 RA, 1950.0, minutes 9 Dec, 1950.0, degrees 10 Dec, 1950.0, minutes 11 Precession, 10 years, RA, minutes of time 12 Precession, 10 years, Dec, minutes of arc 13 Galactic longitude, degrees 14 Galactic latitude, degrees 15 Block number on Lund disc 16 OCL number (1,1) 21 Angular diameter, min of arc 22 Reference for entry 21 (2.01 etc) 23 Distance, pc 24 Reference for entry 23 (3.01 etc) 25 Log age, years 26 Reference for entry 25 (4.01 etc) 27 Metallicity, log [Fe/H] - log [Fe/H] for sun 28 Reference for entry 27 (5.01 etc) 29 Interstellar extinction, A(V) 30 Reference for entry 29 (1.02, 1.03 or 1.05) 31-38 Various other parameter with references (Lynga,in preparation) 39 Indication=1 if cluster has been considered doubtful =2 if cluster has been considered globular 40 Reference for entry 39 (11.01 etc) 51-70 Numbers of peculiar stars (Feinstein) 51 Ap stars 52 Am stars 53 Marginal Ap stars 54 Marginal Am stars 55 WR stars 56 Of stars 57 Be stars 58 Shell stars 59 Be+Shell stars 60 He weak stars 61 He rich stars 62 Cepheids 63 Planetary nebulae 64 Carbon stars 65 Long period variable stars 66 Delta Scuti stars 67 Beta Cephei stars 68 R Cor Bor stars 69 Ba II stars 70 U Geminorum stars 71-75 References for entries 51-70 (12.01 etc) 76-90 Part of Dixon's catalogue of non-stellar objects (1.02): 76 POSS chart type (SO/O/E=1/2/3) 77 POSS chart number 78-80 POSS chart RA,Dec 81-82 Position on POSS chart, mm 83 Max angular diam, min of arc 84 Mag brightest star 85-87 Trumpler classification 85 Concentration class 86 Range class 87 Richness class 88 Nebulosity (n/u/e=1/2/3) 89 Indication=1 if cluster is in ref (1.02) 90 Indication=1 if cluster has POSS data in ref (1.02) 91-100 Part of Strasbourg-Bochum file (1.03): 91 Selected angular diam, min of arc 92 Distance, pc 93 Mag,brightest star 94 Spectral class code 96 Total mag 98 Colour excess 100 Indication=1 if cluster is in ref (1.03) 101-108 Some derived quantities: 101 X coordinate, positive towards l = 90 102 Y coordinate, positive towards l = 180 103 Z coordinate, positive towards b = 90 104 Absolute magnitude for brightest star in cluster 105 Absolute total magnitude of cluster 106 Linear diameter, parsec 107 Average density, solar masses/(parsec)^3 108 Projection of distance from galactic centre 109 Projection of distance on galactic plane 110-116 Parameters assuming R(0)=7000 pc 110 Distance 111 Linear diameter 112 Galactocentric distance 113 X coordinate 114 Y coordinate 115 Z coordinate 116 Projection of distance on galactic plane 118-120 Data received from B. Skiff (1.10) 118 Total magnitude 119 Integrated B-V 120 Number of stars considered 121-145 Data received from K. Janes: 121 Janes-Adler star number 122 Janes-Adler class 123 Janes-Adler references 124-135 Other Janes-Adler data 140 Janes-Adler maximum class 141 Janes-Adler richness class 142 Janes-Adler E(B-V) 143 Janes-Adler ref for E(B-V) 144 Janes-Adler (B-V)turn-off 145 Janes-Adler ref for (B-V)to 151-157 Merge of positions 76-82 and 169-175 151 Survey chart type (SO/O/E/J/I/SR=1/2/3/4/5/6/7) 152 Chart number 153-155 Chart RA,Dec 156 Distance X from left edge of chart, mm 157 Distance Y from bottom edge of chart, mm 161 =1 if cluster dubious according to reference 11.01 162 =1 if cluster dubious according to reference 11.02 163-177 Results of 1982 examination (1.09) 163 Trumpler concentration class (Lynga, 1982) 164 Trumpler range class (Lynga, 1982) 165 Trumpler richness class (Lynga, 1982) 166 Nebulosity (Lynga,1982) 167 Number of member stars (Lynga, 1982) 168 Angular diameter (Lynga, 1982) 169 Survey chart type (SO/O/E/J/R/I/SR=1/2/3/4/5/6/7) 170 Chart number 171-173 Chart RA,Dec 174 Distance X from left edge of chart, mm 175 Distance Y from bottom edge of chart, mm 176 Indication = 1 if cluster was classified in ref (1.09) 177 Indication = 1 if cluster is on ESO/SERC survey 178 Weights for r.v. 182 Radial velocity (1.08), km/s 183 Weight class for radial velocity 184- 188 References for radial velocities 201-208 Buscombe compilation (1.04): 201 Radial velocity, km/s 202 Distance, pc 203 E(B-V), mag 204 Integrated app. mag.(pg), mag 205 Integrated abs. mag.(B), mag 206 Diameter, pc 207 Age, log t, years 208 Mass, log m, solar masses 209 Indication=1 if cluster is in ref(1.04) 210-217 Basel data (1.05): 210 Photometric system for following data 211 Colour type of bluest star 212 Interstellar extinction, mag 213 Distance, pc 214 Spectral type of hottest star 215 Colour type of bluest star 216 Cluster diameter, pc 217 Type of observation 218 Indication=1 if cluster is in ref (1.05) 220-221 vanden Bergh-Hagen data(1.06): 220 Diameter, min of arc 221 Richness: 1=vp, 2=p, 3=m, 4=r, 5=vr 222 Indication=1 if cluster is in ref (1.06) Sequence codes: 1 NGC 2 IC 3 Berkeley 4 Czernik 5 Dolidze 6 Collinder 7 Upgren 8 Tombaugh 9 Ruprecht 10 King 11 Stock 13 Trumpler 14 Markarian 16 Haffner 17 Hogg 18 Sher 19 Feinstein 20 Harvard 21 Lynga 22 Westerlund 23 Basel 24 Blanco 25 Barkhatova 26 Biurakan 27 Melotte 28 Pismis 30 Trapezium 32 Pleiades 33 Graff 34 Iskudarian 35 Stephenson 36 Roslund 37 Hyades 41 vanden Bergh-Hagen 42 Bochum 43 Dolidze-Dzimselejsvili 45 Antalova 46 Moffat 47 Havlen-Moffat 48 Frolov 50 vandenBergh 51 Mayer 52 Latysev 53 Sigma Ori 54 Graham 55 Aveni-Hunter 56 Loden 57 Grasdalen 58 Waterloo 59 Auner 60 CV Mon 61 Schuster 62 Danks 63 Muzzio Acknowledgements: As in previous editions Dr. A. Feinstein has selected the data on peculiar cluster members. The data on total magnitudes were prepared by Mr. B. Skiff, Flagstaff, Arizona. Dr. K. Janes has provided data on E(B-V) and (B-V)turn-off. During the preparation I had the continuous help of Mr. J. van den Born. Mr. T. Wiklind helped with the input of various data values. Dr. S. Wramdemark has submitted his large compilation on radial velocity data. I am grateful to all these and many more who have discussed the catalogue with me. Lund, May 1983 Gosta Lynga