| Arp Madore 2 |
The CMD shows a well-traced TO and RGB with a short main sequence and a prominent RC at G=17. ASteCA gives ~11 kpc, 4.1 Gyr, and [Fe/H]=−0.33. Ortolani 1995 reports 12.4 kpc and [Fe/H]~−0.3 (no specific age); Lee 1997 finds 8.87 kpc, 5 Gyr, and [Fe/H]=−0.51; CG20 gives 11.7 kpc and 3.0 Gyr. ASteCA distance is a good match for CG20 and falls within the range of the prior studies. The metallicity agrees with the sub-solar values reported by Ortolani et al. and Lee. |
| Berkeley 102 |
A controversial object: Maciejewski 2008 concluded it is a chance alignment of unrelated stars. However, the CMD shows a scattered main sequence with the TO at G=18.5 and a well-defined giant branch, leading us to classify it as a genuine open cluster. The four catalogs span wildly different distances (2.6–10.5 kpc) and ages (0.6–4 Gyr). ASteCA gives 7.4 kpc and 4.9 Gyr. The age is close to CG20 (3.9 Gyr) but the distance is ~3 kpc smaller, placing the cluster below 9 kpc. |
| Berkeley 25 |
The CMD shows a clear giant branch and several stars above the TO that are BSS candidates. The RDP yields a radius of ~5’, the largest in the sample. Carraro 2005 used a much smaller 0.8’ radius and obtained 3.0 Gyr and 11.3 kpc; Carraro 2007 gives 5 Gyr and 13.2 kpc. ASteCA estimates 7.4 kpc and 5.2 Gyr, placing the cluster considerably closer than the Carraro et al. values and most databases (>11 kpc). CG20 gives a similar distance of 6.8 kpc but a much younger age of 2.5 Gyr. The underestimated cluster region likely explains the discrepancies with Carraro et al. |
| Berkeley 26 |
The cluster appears as a weak overdensity against the background field. The RDP gives a radius near 2’, but the TO is diffuse due to scatter and BSS candidates, and the giant branch is even less prominent. ASteCA sets the TO at G=18.5, resulting in a distance of 4.6 kpc and an age of 8.6 Gyr. Piatti 2010 reports 4.3 kpc and 4 Gyr — the distances are close, but the age difference is substantial, likely because ASteCA sets the TO almost half a magnitude fainter due to a large binary fraction (~70%). WEBDA and MWSC give 4.3 and 2.7 kpc; MWSC assigns a very young age of ~0.5 Gyr. The OC02 distance of 12.5 kpc appears to be a database recording error. |
| Berkeley 29 |
Tosi 2004 found this to be potentially the most distant cluster in the Galaxy, with an age of 3.5 Gyr and a distance of 11.2–14.4 kpc. The CMD shows a visible TO between 18<G<19, followed by sub-giant and giant branches with a RC at G~16.5. ASteCA finds a distance of 14.4 kpc and an age of 3.7 Gyr, in good agreement with Tosi et al. Frinchaboy 2006 gives 13.4 kpc and 4 Gyr; CG20 gives 12.6 kpc and 3 Gyr, both slightly smaller. Berkeley 29 is the second most distant cluster heliocentrically (after vdBH 176), but the most distant by galactocentric distance (~22 kpc), surpassing Saurer 1. |
| Berkeley 56 |
Always classified as an old open cluster; one of the most populated in the sample and the second most massive (~53000 M_sun). Janes 1994 gives 5.7 kpc and 5.67 Gyr; Carraro 2006 finds 12.1 kpc and 4 Gyr; Janes 2011 gives 15.2 kpc and 6 Gyr. OC02 and WEBDA adopt the Carraro values; MWSC gives 13.2 kpc and 2.5 Gyr; CG20 gives 9.5 kpc and 3 Gyr. There is a substantial spread across all studies. ASteCA gives 11.1 kpc and 5.2 Gyr, within the full range of published values. |
| Berkeley 73 |
The CMD shows a main sequence and a well-defined TO followed by a giant branch that is somewhat redder than expected. Some stars above the TO are BSS candidates; no clear RC. ASteCA estimates a distance of 5.5 kpc and an age of 4 Gyr, which is closer and older than any of the four databases or prior studies (Ortolani 2005: 2.3 Gyr/6.5 kpc; Carraro 2005 and 2007: 1.5 Gyr/9.7–11.5 kpc). The closest match is Dias 2021 (5.8 kpc, 2.2 Gyr). This places the cluster well inside the 9 kpc limit. |
| Berkeley 75 |
A sparse cluster with fewer than 100 detected members. Carraro 2005 report a TO at V=17.5, a radius of 1’, an age of 3.5 Gyr, and a distance of 9.8 kpc. Our structural analysis gives a 2’ radius with the TO at G=17.7 mag. The giant branch is poorly populated but shows a two-star RC, and some stars above the sub-giant branch are likely binaries. ASteCA places Berkeley 75 at 8 kpc with an age of 5.5 Gyr. The distance is similar to CG20 (8.3 kpc), although CG20 assigns a much younger age of 1.7 Gyr. OC02 gives a closer age (4 Gyr) but a larger distance by ~1 kpc. |
| Berkeley 76 |
The CMD shows a diffuse TO at G=16.5 followed by a prominent giant branch. ASteCA gives a distance of 5.4 kpc and an age of 1.8 Gyr. Carraro 2013 found 12.6 kpc and 1.5 Gyr — the ages agree but the distance is very discrepant, attributable to Carraro et al. placing the TO 2 magnitudes fainter at V=18.5. OC02 and WEBDA reproduce the Carraro distance; CG20 gives a more reasonable 4.7 kpc. |
| Czernik 30 |
The CMD shows a robust main sequence and a well-defined giant branch, with the TO at approximately G=17.5. ASteCA gives a distance of 6.5 kpc and an age of 3.6 Gyr, in good agreement with Dias 2021 (5.9 kpc, 3 Gyr). Hayes 2015 found 9.12 kpc and 2.8 Gyr, and seven prior studies all give distances in the range 7.9–9.3 kpc, all of which appear to overestimate the distance. CG20, WEBDA, and MWSC are consistent with ASteCA at 6.2–6.8 kpc. The OC02 value of 9.1 kpc is rejected. A footnote notes that the distance modulus quoted in Table 7 of Hayes et al. is incorrect. |
| ESO 092 05 |
Ortolani 2008 used BVI photometry to estimate 6 Gyr and 11 kpc, and noted a strongly sub-solar metallicity of [Fe/H]~−0.7. ASteCA gives 12.7 kpc, 6 Gyr, and [Fe/H]~−0.12 — the age agrees well, the distance is somewhat larger, and the metallicity differs substantially. CG20 gives 12.4 kpc and 6 Gyr, in good agreement with ASteCA. The metallicity discrepancy with Ortolani et al. is likely due to their overestimation of the extinction (E_BV=0.17 vs. ASteCA’s 0.11, which is closer to the maximum Schlafly 2011 value for the region). |
| ESO 092 18 |
Kubiak 1991 estimated ~10 kpc and 8 Gyr; Carraro 1995 gives 8.1 kpc and 5 Gyr. The CMD shows a robust 2-magnitude main sequence with the TO at G=18.5, a well-defined RGB and RC, and BSS candidates in the range 15<G<17.5. ASteCA gives 11.2 kpc and 4.8 Gyr. The distance is consistent with CG20 (9.9 kpc), OC02 (10.6 kpc), and MWSC (9.5 kpc) within uncertainties. WEBDA lists 600 pc, almost certainly due to a wrong source reference; the correct Janes 1994 reference gives 6.3 kpc, still far from our estimate but much more plausible. |
| FSR 1212 |
A sparse cluster (<100 members) whose overdensity is clearly visible in coordinate space. The CMD shows a well-defined TO at G=17.5, a clear giant branch, and a well-established RC. A slight reddening along the giant branch is consistent with a binary fraction of ~50%. ASteCA gives an age of ~1.3 Gyr and a distance of 10.1 kpc, in good agreement with CG20 (1.4 Gyr, 9.6 kpc). MWSC places the cluster at only 1.8 kpc with an age of 0.4 Gyr, which appears entirely unreliable. |
| FSR 1419 |
A poorly studied cluster first reported in Froebrich 2007. The CMD shows a scattered TO at G~19, with BSS candidates and possible binaries near the top of the main sequence, and a grouping of stars at G~16.5 consistent with a RC. ASteCA gives an age of ~4 Gyr and a distance of 9.2 kpc. CG20 reports 11.1 kpc and 1.6 Gyr; MWSC gives 8.4 kpc and 0.2 Gyr. The ASteCA distance falls between these, while the age is substantially larger than both databases. |
| Kronberger 31 |
A compact, poorly studied cluster reported in Kronberger 2006 as a cluster candidate with RC, with E_BV=0.84 and a distance of 11.9 kpc using a 1.3’ radius. The CMD shows a short main sequence, TO at G=18.3, and a giant branch whose scatter is explained by field contamination, high color excess (ASteCA finds E_BV~1.3, ~0.5 mag above Kronberger’s value), and a large binary fraction (~80%). ASteCA gives 7.6 kpc and 1 Gyr, placing the cluster below the 9 kpc limit — in disagreement with Kronberger 2006 and MWSC (12.6 kpc). |
| Kronberger 39 |
Located in a region of high field star contamination. Kronberger 2006 used a 0.8’ radius and reported ~11.1 kpc with no age estimate, classifying it as a cluster candidate with RC. Monteiro 2020 later discarded it due to a poor isochrone fit. The least populated cluster in the sample (55 members). ASteCA identifies the TO at G~20 and the RC at G~17.5, giving 13 kpc and 2.8 Gyr — in reasonable agreement with Kronberger 2006. MWSC values of 1 Myr and 4.4 kpc are entirely inconsistent with the CMD features. |
| Saurer 1 |
First reported in Saurer 1994; analyzed by Carraro 2003 as Saurer A, who placed the TO at V=19 and estimated ~5 Gyr and 13.8 kpc. Our CMD also shows the TO at G=19, with a visible RGB and a handful of likely RC stars. ASteCA gives 12.4 kpc and 6.6 Gyr — the distance is in close agreement with Carraro 2003 given the uncertainties. Frinchaboy 2006 gives 13.1 kpc and 4.5 Gyr. Saurer 1 was previously thought to hold the record for largest galactocentric distance; this work finds Berkeley 29 to be ~2 kpc farther out. |
| Saurer 3 |
Also known as Saurer C; poorly studied. The CMD shows a dispersed sequence with the TO at G~19 and a clear RC at G=16.5. Members are scattered around the short main sequence, likely due to increasing Gaia photometric errors at G>19. ASteCA gives 6.1 kpc, 6.5 Gyr, and the largest binary fraction in the sample (~86%). Carraro 2003 used CCD VI photometry and reported 9.5 kpc and ~2 Gyr — both differ substantially from our values, likely because their CMD suffers from severe field star contamination spanning a broader but unreliable sequence. MWSC (7.1 kpc) is the closest catalog value. The cluster lies below 9 kpc, contradicting OC02 (~9.5 kpc, sourced from Carraro 2003). |
| Saurer 6 |
The CMD shows a wide and short main sequence with the TO at approximately G=18 mag. The giant branch is quite scattered although the RC is evident. The high star density in the region may explain the main sequence widening. Frinchaboy 2002 used CCD VI photometry and found 2 Gyr and 9.3 kpc. ASteCA gives 1.4 Gyr and 9.2 kpc, in close agreement. WEBDA and OC02 report the same distance as Frinchaboy; MWSC gives a smaller 7.3 kpc. |
| Tombaugh 2 |
A well-populated cluster with nearly 900 identified members. The CMD shows a wide main sequence, a prominent giant branch, and a clear RC; some stars above the TO are likely blue stragglers. ASteCA gives 8.7 kpc and 2.1 Gyr, close to Dias 2021 (9 kpc, 2.3 Gyr) and CG20 (9.3 kpc, 1.6 Gyr). OC02 and MWSC give distances below ~7 kpc; WEBDA gives over ~13 kpc. Frinchaboy 2008 proposed an abundance spread among members and adopted 7.9 kpc and 2.0 Gyr. Villanova 2010 places the cluster at 7.2 kpc. Kubiak 1992, studying variable stars, estimated 4 Gyr and 6.3 kpc. |
| VDBH 144 |
Also known as Andrew-Lindsay 1 and ESO 96-SC04; hosts the planetary nebula PHR 1315-6555. The CMD shows a densely populated main sequence with the TO at G=17.5 and a scattered RC at similar magnitude. Janes 1994 gives 7.6 kpc; Carraro 2005 used a small 0.6’ radius and obtained 16.9 kpc and 0.8 Gyr. Our RDP suggests a radius over 1.5’. ASteCA gives 10.1 kpc and ~1 Gyr. Majaess 2014 (10.0±0.4 kpc, 0.8±3 Gyr) and CG20 (9.6 kpc, 1.4 Gyr) are the closest matches. Fragkou 2019 gives ~12 kpc and 0.66 Gyr, consistent with OC02 and WEBDA. |
| VDBH 37 |
The CMD shows a main sequence extending for over 4 magnitudes with no clear RGB or RC. ASteCA gives 2.9 kpc and ~0.7 Gyr, close to Piatti 2010 (2.5 kpc, 0.7–1 Gyr). OC02 lists 11.22 kpc, which appears to be a recording error since the source is Piatti et al. Dias 2021 revised the distance to 3.4 kpc with an age of 0.3 Gyr. CG20 gives 4.0 kpc and a very young 0.17 Gyr, the largest discrepancy. |
| VDBH 4 |
Fewer than 70 confirmed members; the CMD shows a very weak but extended main sequence spanning almost 4 magnitudes. ASteCA estimates a distance of 8.1 kpc and an age of 1.3 Gyr, both with large uncertainties (16th–84th percentile range spans ~3 kpc). Carraro 2007 performed VI CCD photometry and reported 19.3 kpc and 0.2 Gyr — the distance lies outside ASteCA’s 2σ range and is likely inflated by severe field star contamination visible in their CMD. |
