Table A3.

Coordinates, proper motions, parallax, and radial velocity (where known) of NGC 7772 members from the literature. Not a single pair of stars can be found with matching parameters. Between both sources the magnitudes of the stars extend from V = 11.08 to V = 18.00.

αδμα cos (δ)μδϖ|$v$|r
°°|$\mathrm{mas\, yr^{-1}}$||$\mathrm{mas\, yr^{-1}}$|mas|$\mathrm{km\, s^{-1}}$|
Membersa in Kharchenko et al. (2013)
357.991716.292017.13 ± 0.05–8.65 ± 0.021.39 ± 0.03
357.805416.11466.94 ± 0.34–2.56 ± 0.141.30 ± 0.16
357.500116.133112.52 ± 0.09–10.44 ± 0.042.77 ± 0.0422.7 ± 1.7b
358.258216.442418.28 ± 0.13–14.25 ± 0.061.03 ± 0.07
357.943416.249012.45 ± 0.05–7.38 ± 0.021.88 ± 0.03
357.928816.23527.30 ± 0.08–8.65 ± 0.040.52 ± 0.0422.1 ± 0.3b
357.905215.978611.59 ± 0.10–7.66 ± 0.041.05 ± 0.05
358.082816.281210.42 ± 0.30–6.91 ± 0.181.53 ± 0.15
357.942816.239812.50 ± 0.07–7.25 ± 0.041.95 ± 0.04–63.4 ± 0.1c
358.323316.057216.19 ± 0.09–9.59 ± 0.041.03 ± 0.05
Members in Carraro (2002)
357.942816.239812.50 ± 0.07–7.25 ± 0.041.95 ± 0.04–63.4 ± 0.1c
357.969016.18786.75 ± 0.16–38.26 ± 0.085.48 ± 0.09–20.1 ± 1.2b
357.912916.3036–16.76 ± 0.06–31.33 ± 0.032.04 ± 0.03
357.950616.25138.65 ± 0.06–10.52 ± 0.031.02 ± 0.03–69.9 ± 1.3b
357.943416.249012.45 ± 0.05–7.38 ± 0.021.88 ± 0.03
357.897716.2136–6.48 ± 0.05–18.50 ± 0.020.64 ± 0.03
357.950316.23330.52 ± 0.05–2.54 ± 0.032.34 ± 0.0318.8 ± 0.2c
357.991716.292017.13 ± 0.05–8.65 ± 0.021.39 ± 0.03
357.936716.245412.56 ± 0.055.86 ± 0.031.50 ± 0.03
357.953816.1833–4.48 ± 0.05–6.55 ± 0.031.59 ± 0.03–37.2 ± 0.1c
357.905616.30062.74 ± 0.080.49 ± 0.040.48 ± 0.04
αδμα cos (δ)μδϖ|$v$|r
°°|$\mathrm{mas\, yr^{-1}}$||$\mathrm{mas\, yr^{-1}}$|mas|$\mathrm{km\, s^{-1}}$|
Membersa in Kharchenko et al. (2013)
357.991716.292017.13 ± 0.05–8.65 ± 0.021.39 ± 0.03
357.805416.11466.94 ± 0.34–2.56 ± 0.141.30 ± 0.16
357.500116.133112.52 ± 0.09–10.44 ± 0.042.77 ± 0.0422.7 ± 1.7b
358.258216.442418.28 ± 0.13–14.25 ± 0.061.03 ± 0.07
357.943416.249012.45 ± 0.05–7.38 ± 0.021.88 ± 0.03
357.928816.23527.30 ± 0.08–8.65 ± 0.040.52 ± 0.0422.1 ± 0.3b
357.905215.978611.59 ± 0.10–7.66 ± 0.041.05 ± 0.05
358.082816.281210.42 ± 0.30–6.91 ± 0.181.53 ± 0.15
357.942816.239812.50 ± 0.07–7.25 ± 0.041.95 ± 0.04–63.4 ± 0.1c
358.323316.057216.19 ± 0.09–9.59 ± 0.041.03 ± 0.05
Members in Carraro (2002)
357.942816.239812.50 ± 0.07–7.25 ± 0.041.95 ± 0.04–63.4 ± 0.1c
357.969016.18786.75 ± 0.16–38.26 ± 0.085.48 ± 0.09–20.1 ± 1.2b
357.912916.3036–16.76 ± 0.06–31.33 ± 0.032.04 ± 0.03
357.950616.25138.65 ± 0.06–10.52 ± 0.031.02 ± 0.03–69.9 ± 1.3b
357.943416.249012.45 ± 0.05–7.38 ± 0.021.88 ± 0.03
357.897716.2136–6.48 ± 0.05–18.50 ± 0.020.64 ± 0.03
357.950316.23330.52 ± 0.05–2.54 ± 0.032.34 ± 0.0318.8 ± 0.2c
357.991716.292017.13 ± 0.05–8.65 ± 0.021.39 ± 0.03
357.936716.245412.56 ± 0.055.86 ± 0.031.50 ± 0.03
357.953816.1833–4.48 ± 0.05–6.55 ± 0.031.59 ± 0.03–37.2 ± 0.1c
357.905616.30062.74 ± 0.080.49 ± 0.040.48 ± 0.04

aOnly members with probability >0.8.

b|$v$|r from Gaia DR2.

c|$v$|r from GALAH.

Table A3.

Coordinates, proper motions, parallax, and radial velocity (where known) of NGC 7772 members from the literature. Not a single pair of stars can be found with matching parameters. Between both sources the magnitudes of the stars extend from V = 11.08 to V = 18.00.

αδμα cos (δ)μδϖ|$v$|r
°°|$\mathrm{mas\, yr^{-1}}$||$\mathrm{mas\, yr^{-1}}$|mas|$\mathrm{km\, s^{-1}}$|
Membersa in Kharchenko et al. (2013)
357.991716.292017.13 ± 0.05–8.65 ± 0.021.39 ± 0.03
357.805416.11466.94 ± 0.34–2.56 ± 0.141.30 ± 0.16
357.500116.133112.52 ± 0.09–10.44 ± 0.042.77 ± 0.0422.7 ± 1.7b
358.258216.442418.28 ± 0.13–14.25 ± 0.061.03 ± 0.07
357.943416.249012.45 ± 0.05–7.38 ± 0.021.88 ± 0.03
357.928816.23527.30 ± 0.08–8.65 ± 0.040.52 ± 0.0422.1 ± 0.3b
357.905215.978611.59 ± 0.10–7.66 ± 0.041.05 ± 0.05
358.082816.281210.42 ± 0.30–6.91 ± 0.181.53 ± 0.15
357.942816.239812.50 ± 0.07–7.25 ± 0.041.95 ± 0.04–63.4 ± 0.1c
358.323316.057216.19 ± 0.09–9.59 ± 0.041.03 ± 0.05
Members in Carraro (2002)
357.942816.239812.50 ± 0.07–7.25 ± 0.041.95 ± 0.04–63.4 ± 0.1c
357.969016.18786.75 ± 0.16–38.26 ± 0.085.48 ± 0.09–20.1 ± 1.2b
357.912916.3036–16.76 ± 0.06–31.33 ± 0.032.04 ± 0.03
357.950616.25138.65 ± 0.06–10.52 ± 0.031.02 ± 0.03–69.9 ± 1.3b
357.943416.249012.45 ± 0.05–7.38 ± 0.021.88 ± 0.03
357.897716.2136–6.48 ± 0.05–18.50 ± 0.020.64 ± 0.03
357.950316.23330.52 ± 0.05–2.54 ± 0.032.34 ± 0.0318.8 ± 0.2c
357.991716.292017.13 ± 0.05–8.65 ± 0.021.39 ± 0.03
357.936716.245412.56 ± 0.055.86 ± 0.031.50 ± 0.03
357.953816.1833–4.48 ± 0.05–6.55 ± 0.031.59 ± 0.03–37.2 ± 0.1c
357.905616.30062.74 ± 0.080.49 ± 0.040.48 ± 0.04
αδμα cos (δ)μδϖ|$v$|r
°°|$\mathrm{mas\, yr^{-1}}$||$\mathrm{mas\, yr^{-1}}$|mas|$\mathrm{km\, s^{-1}}$|
Membersa in Kharchenko et al. (2013)
357.991716.292017.13 ± 0.05–8.65 ± 0.021.39 ± 0.03
357.805416.11466.94 ± 0.34–2.56 ± 0.141.30 ± 0.16
357.500116.133112.52 ± 0.09–10.44 ± 0.042.77 ± 0.0422.7 ± 1.7b
358.258216.442418.28 ± 0.13–14.25 ± 0.061.03 ± 0.07
357.943416.249012.45 ± 0.05–7.38 ± 0.021.88 ± 0.03
357.928816.23527.30 ± 0.08–8.65 ± 0.040.52 ± 0.0422.1 ± 0.3b
357.905215.978611.59 ± 0.10–7.66 ± 0.041.05 ± 0.05
358.082816.281210.42 ± 0.30–6.91 ± 0.181.53 ± 0.15
357.942816.239812.50 ± 0.07–7.25 ± 0.041.95 ± 0.04–63.4 ± 0.1c
358.323316.057216.19 ± 0.09–9.59 ± 0.041.03 ± 0.05
Members in Carraro (2002)
357.942816.239812.50 ± 0.07–7.25 ± 0.041.95 ± 0.04–63.4 ± 0.1c
357.969016.18786.75 ± 0.16–38.26 ± 0.085.48 ± 0.09–20.1 ± 1.2b
357.912916.3036–16.76 ± 0.06–31.33 ± 0.032.04 ± 0.03
357.950616.25138.65 ± 0.06–10.52 ± 0.031.02 ± 0.03–69.9 ± 1.3b
357.943416.249012.45 ± 0.05–7.38 ± 0.021.88 ± 0.03
357.897716.2136–6.48 ± 0.05–18.50 ± 0.020.64 ± 0.03
357.950316.23330.52 ± 0.05–2.54 ± 0.032.34 ± 0.0318.8 ± 0.2c
357.991716.292017.13 ± 0.05–8.65 ± 0.021.39 ± 0.03
357.936716.245412.56 ± 0.055.86 ± 0.031.50 ± 0.03
357.953816.1833–4.48 ± 0.05–6.55 ± 0.031.59 ± 0.03–37.2 ± 0.1c
357.905616.30062.74 ± 0.080.49 ± 0.040.48 ± 0.04

aOnly members with probability >0.8.

b|$v$|r from Gaia DR2.

c|$v$|r from GALAH.

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