0039 This seems to be a newly discovered old open cluster just 4.6kpc from the 
0039  Galactic Centre. The sequence in the CMD and CCD suggest we see a number 
0039  of red giants, including redclump stars. There is no detectable main 
0039  sequence in the 2MASS data, hence the age of 1Gyr is an upper limit. 
0039  The cluster seems highly reddened with AK=1.22mag, but at a distance of 
0039  3.5kpc and a Galactic Longitude of just 10{deg} this is no surprise.
0050 The CMD and CCD sequence suggest that this is an about 5Gyr old open 
0050  cluster. There are not many red giant stars to determine the properties 
0050  accurately, however the isochrone fitseems to fit the top of the main 
0050  sequence the giants well. If confirmed, this object as well would be an 
0050  inner Galaxy old open cluster with only 5.6kpc distance to the Galactic 
0050  Centre.
0076 The fit to the high probability cluster members seems very uncertain and it
0076  is not clear if this object really rep-resents an old stellar cluster. In 
0076  particular the group of st ars with J-K=1.2mag and K=13.6mag seems not to 
0076  belong to the cluster sequence. We hence consider this object still as a 
0076  cluster candidate.
0119 This object was classified as not being a cluster by Bica et al. 
0119  (2008MNRAS.384.1733B). It is, however, possible to fit a 2.5Gyr 
0119  old isochrone to the CMD. In the CCD the high probability members which 
0119  should represent the upper end of the main sequence seem not to fit the 
0119  same isochrone. They are scattered towards much too large J-H values. But 
0119  this could simply be due to the fact that these stars are at the detection
0119  limit in all three bands, and in particular in the H-band, as similar 
0119  scattering is observed in some other objects. In any case we consider this
0119  object still as a cluster candidate.
0123 There seems to be a clear top of the main sequence visible in the CMD, but 
0123  only a small number of scattered giant stars. Hence the fit of an 0.5Gyr 
0123  old isochrone is uncertain.
0131 Similar to FSR 0123, there are only a few high probability membership red 
0131  giant and clump of stars probabl y co-incident with the top of the main 
0131  sequence. The scatter of the later in the CCD could be attributed to the 
0131  faint fluxes. Hence the determined cluster parameters are uncertain.
0134 This is a very nice example of a newly discovered old (0.8Gyr) cluster in 
0134  the FSR sample. There is a clearly visible top of the main sequence and 
0134  more than a dozen red giant in the cluster.
0141 (NGC 6802, Collinder 400) In this case the isochrone with the literature 
0141  parameters does not seem to fit the cluster main sequence and red giants. 
0141  Our fit with a distance of 2.7kpc and 0.5Gyrs seems to represent the 
0141  cluster much better.  
0155 (Teutsch 7) The isochrone with the literature parameters seems not to fit 
0155  the data at all. Instead the cluster is 3.8kpc away and has an age of 
0155  about 0.6Gyrs.
0156 (BDS 2003 158) The cluster has been identified by Bica et al. (2003, 
0156  Cat. J/A+A/404/223) but no parameters are determined. We find that this 
0156  object can be well fit by an isochrone with 0.4Gyrs age and a distance of 
0156  7.5kpc, rendering this one of the most distant open clusters in our sample
0167 There are only very few red giant stars that might be part of the cluster. 
0167  Hence the parameters are uncertain.
0170 There are no main sequence stars visible in the 2MASS data. However, a 
0170  clump of red giant stars as well as a RGB are visible. The age of 1Gyr is 
0170  hence a lower limit and the distance uncertain.
0177 (Kronberger 52) There are a number of main se-quence and giant stars 
0177  visible in the CMD and CCD to properly determine the cluster parameter of 
0177  this object. It is best fit by a 0.8Gyr old cluster at a distance of 
0177  3.6kpc.
0184 There seems to be a red clump of stars, as well as some sub-giants in the 
0184  CMD. No main sequence stars are detected. Hence, the determined cluster 
0184  parameters are uncertain. The strange value required for CHK hints that 
0184  this object might not be a real cluster.
0191 (Berkeley 49) This is another example where the literature parameters do 
0191  not fit the 2MASS data at all. Using the small number of red giants we 
0191  find that 0.2Gyr old and 3.4kpc distant cluster fits the data best.
0202 (NGC 6819, Melotte 223) Despite the nice fit, a rather large value for CHK 
0202  is required to fit the CCD.
0203 (Kronberger 73) There is only a small number of red giants that can be used
0203  to constrain the cluster parameters. We find that a 125Myr old and 
0203  distant (10.8kpc) cluster fits the data best. 
0208 (Berkeley 85) Using the six stars which are likely to be red giants we can 
0208  obtain a better fit than with the literature parameters. We find an age of
0208  125Myrs and a distance of 4.4kpc.
0214 (IC 1311): There only seem to be a handful of main sequence stars and in 
0214  general the isochrone with the literature parameters does not fit the 
0214  2MASS data. We find a better fit with an age of 0.5Gyr and a distance 
0214  of 8.7kpc.
0222 This newly identified cluster only stands out through a handful of red 
0222  clump stars and about the same number of stars at the top of the main 
0222  sequence. The remaining stars all have lower membership probabilities, 
0222  rendering the parame ters of the cluster uncertain.
0256 (Berkeley 54) What the literature parameter imply as the top of the main 
0256  sequence, actually seems to be a red clump of stars. There are no main 
0256  sequence stars visible in the 2MASS data. Using 4Gyrs as the age, we find 
0256  a distance of almost 7kpc.
0275 This newly identified cluster shows a dozen or so high probability members 
0275  which are red giants and the top of them main sequence. We determine an 
0275  age of 1Gyr and a distance of 3.6kpc.
0280 (Teutsch 156) We can identify a number of cluster red giants as well as the
0280  top of the main sequence and fit an isochrone with an age of 0.8Gyrs and 
0280  a distance of 4.4kpc.
0282 There are no or very few giants in the clusters. Hence the age and 
0282  distance determination is very uncertain.
0287 (Berkeley 91) The isochrone with the literature parameters fails to fit the
0287  data. We clearly can identify a clump of red giant stars, but there is no 
0287  main sequence. Hence the age of 0.4Gyrs is a lower limit and consequently 
0287  the distance is uncertain as well.
0294 (NGC 7031) There seem to be two possibilities to fit the CMD of this 
0294  cluster. Either using the literature parame-ters (140Myrs, 900pc) or a 
0294  much older distant cluster (0.5Gyrs, 7.1kpc). The latter fitting the high 
0294  probability members at JK=1.5mag as red clump stars. Non of the two fits 
0294  provides a satisfying result for all stars.
0304 This cluster contains a handful of red giant stars and one can identify the
0304  top of the main sequence. Those stars, however, show a large scatter in 
0304  the CCD. The best fit can be obtained with an age of 0.4Gyrs and a 
0304  distance of 6.8kpc.
0313 (Kronberger 81) This so far un-investigated clusters shows a very nice red 
0313  giant branch with at least 30 or 40 stars.  There is no main sequence 
0313  detected, hence the age of 1.6Gyrs is an upper limit and the distance of 
0313  6kpc is uncertain. Given the largenumber of giant stars, this object might
0313  well be a massive old and distant (10kpc to the Galactic Centre) cluster.
0327 (NGC 7128) This is a very young cluster in our sample of old clusters. This
0327  is caused by the fact that there are three high probability members which 
0327  could be red giants. However, no fit with an isochrone can be obtained 
0327  that includes these three stars.
0329 (Berkeley 92) There is no main sequence, but a number of red giant stars 
0329  detected for this cluster. It is best fit by a 1Gyr old isochrone at a 
0329  distance of 5.5kpc, where the age is a lower limit.
0333 The main sequence stars in this cluster only have a low membership 
0333  probability. But there are a sufficient number ofhigh probability member 
0333  red giants to determine an age of 1.2Gyrs and a distance of 5kpc.
0338 The high probability members of this newly identified cluster seem to 
0338  indicate an object with an age of 0.4Gyrs at a distance of 6kpc. The 
0338  scatter in the data points suggests larger than normal uncertainties for 
0338  the parameters.
0342 This is a well populated newly identified old cluster. A large part of the 
0342  main sequence as well as at least 10 red giant stars can be identified. 
0342  The cluster has an age of 1.2Gyrs and is at a distance of 2.6kpc.
0385 There is only a small number (three) of high probability members in this 
0385  cluster. Hence the parameters (age of 0.8Gyrs, distance of 1.7kpc) 
0385  are uncertain.
0386 The very small number of high probability members make the determination of
0386  the cluster parameter very un certain. We hence consider this object only 
0386  a cluster candidate.
0394 There is only a small number of probable main sequence stars at the 
0394  detection limit. The number of red giants allows us, however, to determine
0394  an age of 1.2Gyrs and a distance of 4.1kpc.
0412 (Pfleiderer 3) This so far uninvestigated cluster shows a large number of 
0412  red giants and the top of the main sequence is visible as well. The 
0412  cluster has an age of 1.2Gyrs and is at a distance of 6.1kpc.
0460 There are a number of red giant stars as well as the top of the main 
0460  sequence just above the detection limit. Hence, the uncertainties for the 
0460  parameters (1.2Gyrs, 6.1kpc) are lar ger than normal.
0478 (Juchert-Saloranta 1) This so far no investigated cluster shows about ten 
0478  red giants and main sequence stars. It can be fit with an isochrone age 
0478  of 0.8Gyrs and a distance of 5.1kpc.
0480 This is a newly identified cluster with a large number of red giants and 
0480  just a hint of main sequence stars at the detection limit. It represents 
0480  a 1.2Gyr old cluster at a distance of 5.8kpc.
0514 (Berkeley 61) This is another case where the literature parameters do not 
0514  fit the 2MASS data. We find that the CMD can be best fit with an 125Myr 
0514  old isochrone at a distance of 8kpc.
0548 (NGC 609) In this case the literature parameters do not fit the 2MASS data.
0548  We obtain a better fit using an age of 250Myrs and a distance of 4.2kpc. 
0563 (IC 166, Tombaugh 1) Here as well, we cannot bring the literature 
0563  parameters in agreement with the 2MASS data. Instead a good fit can be 
0563  obtained using an age of 1.4Gyrs and a distance of 5kpc.
0584 It has been suggested by Bica et al. (2007A&A...472..483B) that this object
0584  is a nearby, highly reddened globular cluster without, or with only a very
0584  small number of giant stars. The parameters for this object listed in 
0584  Table A1 are not a best fit, but rather the parameters for the solid 
0584  isochrone in Fig. C98. Given the fact that the four potentially reddened 
0584  giant stars are the least likely of thecluster members, the object could 
0584  well be an embedded younger cluster. Further investigation is certainly 
0584  needed to determine its nature reliably.
0648 (NGC 1245, Melotte 18) To fit this cluster we require a rather large value 
0648  for CHK.
0652 (IC 361) The literature parameters do not fit the 2MASS data. We obtain an 
0652  age of 1Gyr and a distance of 3.9kpc.
0667 This object contains only a small number of high probability members, which
0667  are, however, nicely represent an 0.8Gyr old cluster at a distance 
0667  of 750 pc.
0731 (Berkeley 18, King 22) Our decontamination suggests in this case that the 
0731  age of the cluster is smaller than the literature value, since there seems
0731  to be a number of sub-dwarfs visible in the CMD. Our fit uses an age 
0731  of 1.4Gyrs and a distance of 4.7kpc.
0790 This newly identified cluster lacks a clear detection of main sequence 
0790  stars, which are all near the detection limit. This introduces a larger 
0790  uncertainty into the determined parameters (2Gyrs, 6kpc).
0828 The literature values do not seem to fit the 2MASS data. We find an age 
0828  of 1.6Gyrs and a distance of 5.7kpc.
0877 (Basel 11b) The literature parameters seem to fit the main sequence of the 
0877  clusters. If we consider the three bright stars as cluster members than we
0877  can obtain a fit using an age of0.6Gyrs and a distance of 1.1kpc.
0879 (NGC 2266, Melotte 50) To fit this cluster we require a rather large value 
0879  for CHK.
0884 This object was classified as uncertain cluster by Bonatto & Bica 
0884  (2008A&A...485...81B, 2008A&A...491..767B). Given that we cannot fit the 
0884  CMD and CCD simultaneously with the same isochrone (the fit to the CMD 
0884  requires no extinction, while the fit to the CCD need an extinction), we 
0884  conclude that this object indeed might not be a real cluster.
0926 (Teutsch 58) This so far uninvestigated cluster shows a number of red giant
0926  stars as well as the top of the main sequence. We find it to be a 1.2Gyr 
0926  old cluster at a distance of 6kpc.
0963 The cluster shows only a small number of red giants, as a clear main 
0963  sequence. It can be fit by an isochrone with anage of 0.5Gyrs and a 
0963  distance of 2.5kpc.  
0972 (NGC 2429, Melotte 69, Collinder 154, Raab 56) Despite its large number of 
0972  member stars no literature value s for this cluster could be found. From 
0972  our isochrone fit we obtain an age of 2Gyrs and a distance of 2.3kpc. The 
0972  CCD cannot be fit properly by the same, extinction free isochrone as the 
0972  CMD.
0995 (NGC 2355, Melotte 63) To fit this cluster we require a rather large value 
0995  for CHK.
1113 There are only a handful of high probability members, which are difficult 
1113  to fit consistently with an isochrone in bot, the CMD and the CCD. Hence, 
1113  we consider this object just as a cluster candidate.
1119 (Czernik 28) Here the literature data does not seem to fit the 2MASS data 
1119  as good as it could. We find that a proper fit can only be obtained using 
1119  a sub-solar metallicity. Thenwe find an age of 1.4Gyrs and a distance 
1119  of 5.5kpc. This puts the cluster at a distance of almost 13kpc from the 
1119  Galactic Centre.
1121 (King 23) To fit this cluster we require a rather large value for CHK.
1138 (Berkeley 77) Both sets of parameters (ours and the literature) are unable 
1138  to fit the CCD simultaneously with the CMD.
1201 (NGC 2204, Melotte 44) The isochrone fit requires different parameters than
1201  the literature values. Furthermore, it only works with sub-solar 
1201  metallicities. We find an age of 2Gyrs and a distance of 4kpc, placing the
1201  cluster 11kpc from the Galactic Centre.
1214 (Berkeley 36): No main sequence visible, hence the age is an upper limit.
1222 (Melotte 71, Collinder 155) We find different cluster parameters than 
1222  listed in literature. The best fit is obtained with an age of 1.2Gyrs and 
1222  a distance of 2.3kpc.
1225 (NGC 2360, Melotte 64): To fit this cluster we require a rather large value
1225  for CHK. Furthermore, the parameters differ from the literature values. 
1225 We find an age of 1.2Gyrs and adistance of 900 pc.
1238 (NGC 2425) The isochrone fit works better witha sub-solar metallicity. The 
1238  cluster is 11.5kpc from the Galactic Centre, has an age of 1.4Gyrs and a 
1238  distance of 4.7kpc.
1241 (M 46, NGC 2437) To fit this cluster we require a rather large value     
1241  for CHK.
1244 (Ruprecht 26) The cluster parameters are highly uncertain as no reliable 
1244  fit to all high probability members can be made.
1250 (Haffner 2, Tombaugh 2) There is no main sequence detected, hence the age 
1250  of 1Gyr is a lower limit, and the distance of 8kpc is uncertain.
1256 (NGC 2539, Melotte 83) The isochrone fit works better with a sub-solar 
1256  metallicity. The cluster is 1Gyr old and hasa distance of 1kpc.
1266 (Teutsch 61) To fit this cluster we require a rather large value for CHK.
1267 (NGC 2432) The isochrone using the literature parameters does not fit 
1267  the 2MASS data. We find that the cluster has an age of 0.5Gyrs and a 
1267  distance of 2.1kpc.
1274 (NGC 2421) To fit this cluster we require a rather large value for CHK. The
1274  literature parameters do not fit the possible red giants in the cluster. 
1274  This can be done using an age of 0.6Gyrs and a distance of 1.8kpc.
1282 (NGC 2509, Melotte 81) To fit this cluster we require a rather large value 
1282  for C HK. We also obtain a much better fit than the literature parameters.
1282  We find an age of 1.2Gyrs an d adistance of 2.5kpc.
1296 (NGC 2243, Melotte 46) There is no main sequence detected, hence the age 
1296  of 4Gyrs is an upper limit and the distance of 4.5kpc uncertain.
1298 There is only a small number of high probability members (giants and main 
1298  sequence stars). Hence, the age of 1.4Gyrs and the distance of 3.2kpc 
1298  are uncertain.
1299 (Ruprecht 18) We find that there are a few probable cluster red giants 
1299  which are not fit by the literature para meters. We can include them into 
1299  the fit by using an age of 110Myrs and a distance of 2.3 Kpc.
1301 (M 93, NGC 2447, Collinder 160) We obtain abetter fit when using a 
1301  sub-solar metallicity.
1313 (Trumpler 9) There is one possible giant star, but if cannot be fit by 
1313  any isochrone.
1330 (NGC 2489, vdB-Hagen 15) There are six possible cluster red giants which 
1330  are not fit at all when using the literature parameters. We find an age 
1330  of 0.6Gyrs and a distance of 1.3kpc.
1337 (Haffner 17, vdB-Hagen 12) The two probable cluster red giants are not fit 
1337  by the literature parameters. They are included if one uses an age 
1337  of 120Myrs and a distance of 3kpc.  
1354 (NGC 2567, vdB-Hagen 26) To fit this cluster we require a rather large 
1354  value for C HK.
1361 There are a handful of cluster red giants and a largenumber of main 
1361  sequence stars. The best fit can be obtained using an age of 1Gyr and a 
1361  distance of 1.5kpc.
1362 (NGC 2627, Collinder 188, Melotte 87, vdBHagen 38) To fit this cluster we 
1362  require a rather large value for CHK. Using an age of 1.4Gyrs and a 
1362  distance of 1.8kpc fits the data much better than the literature 
1362  parameters.
1385 (Pismis 3, vdB-Hagen 33) The literature parameters do not lead to a 
1385  satisfactory fit of the 2MASS data. Instead we use an age of 3Gyrs and a 
1385  distance of 2.1kpc.
1386 (Saurer 2) There is no detectable main sequence, hence the age of 1.4Gyrs 
1386  is an upper limit and the distance of 5kpc is uncertain.
1388 (Ruprecht 66, vdB-Hagen 41) This so far uninvestigated cluster shows a 
1388  number of red clump stars as well as many main sequence stars. We find an 
1388  age of 1.2Gyrs and a distance of 3.9kpc.
1396 (Collinder 147, Melotte 66) There is no main sequence detected, hence the 
1396  age of 3Gyrs is an upper limit and the distance of 5kpc uncertain.
1399 This cluster contains a handful of giant stars as well as a clear detection
1399  of the top of the main sequence. We find an age of 250Myrs and a 
1399  distance of 6.8kpc.
1404 (vdB-Hagen 55) This so far uninvestigated cluster has a number of red 
1404  giants and the top of the main sequence is detected as well. This enables 
1404  us to fit an isochrone with an age of1Gyr and a distance of 3.7kpc.
1408 (NGC 2818A, Melotte 96, vdB-Hagen 59) The isochrone using the the 
1408  literature parameter does not seem to fit the data. Instead we find an 
1408  age of 1.2Gyrs and a distance of 3.2kpc.
1409 (NGC 2671, vdB-Hagen 51) If we include the potential red giant into the 
1409  isochrone fit we find an age of 250Myrs and a distance of 1.5kpc, slightly
1409  different to the literature values.
1415 There is no main sequence, hence the determined age of 2.5Gyrs has to be 
1415  considered an upper limit, while the distance of 10kpc is uncertain. 
1415  If correct, this places the cluster 13.5kpc from the Galactic Centre.
1420 (Ruprecht 60, vdB-Hagen 31) This so far uninvestigated cluster shows a few 
1420  likely giant members as well as the top of the main sequence. We find an 
1420  age of 1Gyr and a distance of 3.9kpc.
1439 (NGC 2849, vdB-Hagen 61) To fit this cluster we require a rather large 
1439  value for C HK.
1458 (Pismis 12, vdB-Hagen 62) This cluster has no literature parameters but 
1458  shows a handful of red giants as well as the main sequence. We determine 
1458  an age of 1.2Gyrs and a distance of 2.1kpc.
1463 This newly identified cluster shows a number of red giants as well as the 
1463  top of the main sequence. We find an age of 1Gyr and a distance of 4.5kpc.
1480 (Pismis 15) The isochrone using the literature parameters does not seem to 
1480  fit the data properly. We find that an age of 1.2Gyrs and a distance 
1480  of 2.3kpc leads to a better fit.
1483 (vdB-Hagen 73) This cluster has no literature data but shows a number of 
1483  red clump stars as well as the top of the main sequence. 
1483  We find an age of 1Gyr and a distance of 5kpc.
1486 (vdB-Hagen 67) There seems to be only a few top of the main sequence stars 
1486  with reasonably high membership probabilities. Hence the determined age 
1486  of 0.4Gyrs and the distance of 7.6kpc are uncertain.
1494 (vdB-Hagen 72) This cluster without literature data can be fit using an age
1494  of 1Gyr and a distance of 3.2kpc.
1520 (Ruprecht 85, vdB-Hagen 83) The isochronewith the literature data clearly 
1520  fails to fit the data. The potential cluster red giants have only a low 
1520  membership probability, hence the age of 0.4Gyrs and the distance 
1520  of 4kpc are uncertain.
1521 There are no main sequence stars detected, hence the age of 3Gyrs is an 
1521  upper limit and the distance of 4kpc is uncertain.
1523 (Schuster CL) This cluster without literature parameters shows a number of 
1523  high probability members (giants and main sequence stars). We find that 
1523  an age of 125Myrs and a distance of 7.5kpc fits the 2MASS data.
1528 (Teutsch 44) This so far uninvestigated cluster can be fit using an age 
1528  of 1.4Gyrs and a distance of 6.7kpc.
1529 (NGC 2808) To fit this cluster we require a ratherlarge value for C HK.
1534 (Bochum 8, vdB-Hagen 90) To fit this cluster we require a rather large 
1534  value for C HK. If we include the two potential giants into the fit we 
1534  obtain an age of 1.2Gyrs and a distance of 1kpc, very different from the 
1534  literature values.
1546 (NGC 3255, vdB-Hagen 96) There seem to be a number of cluster red giants 
1546  which are not at all fit by an isochrone using the literature parameters. 
1546  We find an age of 1Gyr and a distance of 3.7kpc instead.
1550 (Teutsch 105) This cluster without literature parameters can be fit using 
1550  an age of 1Gyr and a distance of 6.3kpc.
1559 (Teutsch 106) So far uninvestigated, this cluster shows a clear red clump 
1559  as well as the top of the main sequence.We find an age of 0.6Gyrs and 
1559  a distance of 6.9kpc.
1565 (Trumpler 19) We find a clear main sequence and a dozen giant stars in this
1565  so far uninvestigated cluster. We fit an isochrone with an age of 1.2Gyrs 
1565  and a distance of 3.1kpc.
1586 There are only a few possible cluster red giants, hence the parameters are 
1586  uncertain. We find an age of 0.8Gyrs and a distance of 2.4kpc.
1611 (NGC 4337, vdB-Hagen 129) The isochrone with the literature parameters 
1611  fails to fit the 2MASS data. We find that the clusters has an age 
1611  of 1.2Gyrs and a distance of 2.5kpc.
1624 (Trumpler 20, vdB-Hagen 137) Our fit using an age of 1.4Gyrs and a distance
1624  of 3.7kpc fits the data much better than using the literature parameters.
1632 (vdB-Hagen 140) This cluster without literature parameters shows a number 
1632  of red giants, but the top of the main sequence seems to be just below the
1632  detection limit. Thus, the age of 2.5Gyrs is a lower limit and the 
1632  distance of 5kpc is uncertain.
1637 (NGC 4815, vdB-Hagen 142) There are two potential cluster red giants which 
1637  could either be fit using the literature parameters or the values obtained
1637  by us: an age of 1Gyr and a distance of 2kpc.
1657 There seems to be a clump of red giant stars and a few brighter giants, but
1657  no indication of a main sequence, which could tentatively be fit using an 
1657  age of 1Gyr and a distance of 7kpc. However, the slope of the RGB cannot 
1657  be reproduced by any sensible value for the metallicity. We hence 
1657  consider this object only as a cluster candidate.
1670 (Loden 1101) This so far uninvestigated cluster shows a number of giant 
1670  stars as well as a main sequence. We fit an isochrone using an age 
1670  of 250Myrs and a distance of 2.5kpc.
1716 This potential globular cluster shows no main sequence, hence the age 
1716  of 2Gyrs is an upper limit and the distance of 7kpc uncertain.  
1724 (NGC 6208, Collinder 313, vdB-Hagen 198) The potential cluster red giants 
1724  detected in the 2MASS data can only befit if we use an age of 0.6Gyrs and 
1724  a distance of 3.2kpc.  
1726 (Lynga 9, vdB-Hagen 189) WEBDA states that this object actually my not be 
1726  a real cluster. However, one can obtain a very well fitting isochrone 
1726  using an age of 0.6Gyrs and a distance of 2.5kpc.
1750 This newly identified cluster shows a clear main sequence but only a 
1750  handful of probable giants, rendering the de-termined parameters 
1750  uncertain. We find that the age is 0.8Gyrs and the distance 2.4kpc.
1781 (vdB-Hagen 229, Dufay 1, HP 1) The reddening for this cluster seems to be 
1781  much smaller than what is given in the literature.