Table 2.

Parameters of the GCs analysed in this work. The values of iron abundances, reddening, and distance modulus are taken from the 2010 version of the Harris (1996) catalogue. The average GC proper motions are derived in this paper based on Gaia EDR3 motions. Cluster age, mass at the RGB tip, RGB mass-loss, mass-loss spread, and average HB mass are derived in this paper. Sources for [α/Fe]: (a) Sbordone et al. (2005), (b) Dias et al. (2015), (c) Monaco et al. (2018), (d) Cohen (2004), (e) Brown, Wallerstein & Zucker (1997), (f) Dotter et al. (2018, and references therein), (g) Pritzl, Venn & Irwin (2005), (h) Jahandar et al. (2017), (i) Koch & Côté (2019), and (l) from the indications in Kirby et al. (2008).

ID[Fe/H][α/Fe]E(BV) (mag)(m − M)V (mag)Age (Gyr)|$\rm \mathit{ M}^{Tip}/\mathit{ \mathrm{ M}}_\odot$||$\rm \mu /M_\odot$|δ/M|$\rm \bar{\mathit{ M}}^{HB}/M_\odot$|μα cosδ (mas yr−1)μδ (mas yr−1)
NGC 6426−2.150.4b0.3617.6813.50 ± 1.000.7820.096 ± 0.0290.008 ± 0.0020.693 ± 0.029−1.85 ± 0.02−2.98 ± 0.02
PALOMAR 12−0.850.0d, e0.0216.4610.00 ± 0.500.9090.226 ± 0.0350.003 ± 0.0010.683 ± 0.035−3.14 ± 0.04−3.33 ± 0.03
PALOMAR 15−2.070.4l0.4019.5113.25 ± 0.750.7830.126 ± 0.0300.005 ± 0.0020.657 ± 0.030−0.60 ± 0.19−1.24 ± 0.20
PYXIS−1.200.2l0.2118.6311.00 ± 0.750.8600.186 ± 0.0450.002 ± 0.0010.674 ± 0.0451.04 ± 0.050.18 ± 0.06
RUPRECHT 106−1.680.0e, f0.2017.2511.00 ± 0.500.8310.113 ± 0.0350.004 ± 0.0020.718 ± 0.035−1.24 ± 0.020.34 ± 0.02
TERZAN7−0.600.0a0.0717.019.00 ± 0.500.9540.276 ± 0.0450.006 ± 0.0020.678 ± 0.045−2.90 ± 0.02−1.66 ± 0.02
TERZAN8−2.160.4b0.1217.4713.50 ± 0.500.7820.110 ± 0.0220.005 ± 0.0020.672 ± 0.022−2.42 ± 0.02−1.59 ± 0.02
AM4−1.300.2l0.0517.6912.25 ± 0.750.829
E03−0.830.2c0.3015.4711.50 ± 1.000.899
PALOMAR 1−0.650.0h0.1515.709.50 ± 1.250.926
PALOMAR 13−1.880.4i0.0517.2311.00 ± 0.500.836
ID[Fe/H][α/Fe]E(BV) (mag)(m − M)V (mag)Age (Gyr)|$\rm \mathit{ M}^{Tip}/\mathit{ \mathrm{ M}}_\odot$||$\rm \mu /M_\odot$|δ/M|$\rm \bar{\mathit{ M}}^{HB}/M_\odot$|μα cosδ (mas yr−1)μδ (mas yr−1)
NGC 6426−2.150.4b0.3617.6813.50 ± 1.000.7820.096 ± 0.0290.008 ± 0.0020.693 ± 0.029−1.85 ± 0.02−2.98 ± 0.02
PALOMAR 12−0.850.0d, e0.0216.4610.00 ± 0.500.9090.226 ± 0.0350.003 ± 0.0010.683 ± 0.035−3.14 ± 0.04−3.33 ± 0.03
PALOMAR 15−2.070.4l0.4019.5113.25 ± 0.750.7830.126 ± 0.0300.005 ± 0.0020.657 ± 0.030−0.60 ± 0.19−1.24 ± 0.20
PYXIS−1.200.2l0.2118.6311.00 ± 0.750.8600.186 ± 0.0450.002 ± 0.0010.674 ± 0.0451.04 ± 0.050.18 ± 0.06
RUPRECHT 106−1.680.0e, f0.2017.2511.00 ± 0.500.8310.113 ± 0.0350.004 ± 0.0020.718 ± 0.035−1.24 ± 0.020.34 ± 0.02
TERZAN7−0.600.0a0.0717.019.00 ± 0.500.9540.276 ± 0.0450.006 ± 0.0020.678 ± 0.045−2.90 ± 0.02−1.66 ± 0.02
TERZAN8−2.160.4b0.1217.4713.50 ± 0.500.7820.110 ± 0.0220.005 ± 0.0020.672 ± 0.022−2.42 ± 0.02−1.59 ± 0.02
AM4−1.300.2l0.0517.6912.25 ± 0.750.829
E03−0.830.2c0.3015.4711.50 ± 1.000.899
PALOMAR 1−0.650.0h0.1515.709.50 ± 1.250.926
PALOMAR 13−1.880.4i0.0517.2311.00 ± 0.500.836
Table 2.

Parameters of the GCs analysed in this work. The values of iron abundances, reddening, and distance modulus are taken from the 2010 version of the Harris (1996) catalogue. The average GC proper motions are derived in this paper based on Gaia EDR3 motions. Cluster age, mass at the RGB tip, RGB mass-loss, mass-loss spread, and average HB mass are derived in this paper. Sources for [α/Fe]: (a) Sbordone et al. (2005), (b) Dias et al. (2015), (c) Monaco et al. (2018), (d) Cohen (2004), (e) Brown, Wallerstein & Zucker (1997), (f) Dotter et al. (2018, and references therein), (g) Pritzl, Venn & Irwin (2005), (h) Jahandar et al. (2017), (i) Koch & Côté (2019), and (l) from the indications in Kirby et al. (2008).

ID[Fe/H][α/Fe]E(BV) (mag)(m − M)V (mag)Age (Gyr)|$\rm \mathit{ M}^{Tip}/\mathit{ \mathrm{ M}}_\odot$||$\rm \mu /M_\odot$|δ/M|$\rm \bar{\mathit{ M}}^{HB}/M_\odot$|μα cosδ (mas yr−1)μδ (mas yr−1)
NGC 6426−2.150.4b0.3617.6813.50 ± 1.000.7820.096 ± 0.0290.008 ± 0.0020.693 ± 0.029−1.85 ± 0.02−2.98 ± 0.02
PALOMAR 12−0.850.0d, e0.0216.4610.00 ± 0.500.9090.226 ± 0.0350.003 ± 0.0010.683 ± 0.035−3.14 ± 0.04−3.33 ± 0.03
PALOMAR 15−2.070.4l0.4019.5113.25 ± 0.750.7830.126 ± 0.0300.005 ± 0.0020.657 ± 0.030−0.60 ± 0.19−1.24 ± 0.20
PYXIS−1.200.2l0.2118.6311.00 ± 0.750.8600.186 ± 0.0450.002 ± 0.0010.674 ± 0.0451.04 ± 0.050.18 ± 0.06
RUPRECHT 106−1.680.0e, f0.2017.2511.00 ± 0.500.8310.113 ± 0.0350.004 ± 0.0020.718 ± 0.035−1.24 ± 0.020.34 ± 0.02
TERZAN7−0.600.0a0.0717.019.00 ± 0.500.9540.276 ± 0.0450.006 ± 0.0020.678 ± 0.045−2.90 ± 0.02−1.66 ± 0.02
TERZAN8−2.160.4b0.1217.4713.50 ± 0.500.7820.110 ± 0.0220.005 ± 0.0020.672 ± 0.022−2.42 ± 0.02−1.59 ± 0.02
AM4−1.300.2l0.0517.6912.25 ± 0.750.829
E03−0.830.2c0.3015.4711.50 ± 1.000.899
PALOMAR 1−0.650.0h0.1515.709.50 ± 1.250.926
PALOMAR 13−1.880.4i0.0517.2311.00 ± 0.500.836
ID[Fe/H][α/Fe]E(BV) (mag)(m − M)V (mag)Age (Gyr)|$\rm \mathit{ M}^{Tip}/\mathit{ \mathrm{ M}}_\odot$||$\rm \mu /M_\odot$|δ/M|$\rm \bar{\mathit{ M}}^{HB}/M_\odot$|μα cosδ (mas yr−1)μδ (mas yr−1)
NGC 6426−2.150.4b0.3617.6813.50 ± 1.000.7820.096 ± 0.0290.008 ± 0.0020.693 ± 0.029−1.85 ± 0.02−2.98 ± 0.02
PALOMAR 12−0.850.0d, e0.0216.4610.00 ± 0.500.9090.226 ± 0.0350.003 ± 0.0010.683 ± 0.035−3.14 ± 0.04−3.33 ± 0.03
PALOMAR 15−2.070.4l0.4019.5113.25 ± 0.750.7830.126 ± 0.0300.005 ± 0.0020.657 ± 0.030−0.60 ± 0.19−1.24 ± 0.20
PYXIS−1.200.2l0.2118.6311.00 ± 0.750.8600.186 ± 0.0450.002 ± 0.0010.674 ± 0.0451.04 ± 0.050.18 ± 0.06
RUPRECHT 106−1.680.0e, f0.2017.2511.00 ± 0.500.8310.113 ± 0.0350.004 ± 0.0020.718 ± 0.035−1.24 ± 0.020.34 ± 0.02
TERZAN7−0.600.0a0.0717.019.00 ± 0.500.9540.276 ± 0.0450.006 ± 0.0020.678 ± 0.045−2.90 ± 0.02−1.66 ± 0.02
TERZAN8−2.160.4b0.1217.4713.50 ± 0.500.7820.110 ± 0.0220.005 ± 0.0020.672 ± 0.022−2.42 ± 0.02−1.59 ± 0.02
AM4−1.300.2l0.0517.6912.25 ± 0.750.829
E03−0.830.2c0.3015.4711.50 ± 1.000.899
PALOMAR 1−0.650.0h0.1515.709.50 ± 1.250.926
PALOMAR 13−1.880.4i0.0517.2311.00 ± 0.500.836
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