CCD UBVRI photometry of the open cluster Berkeley 8. (arXiv:1908.05479v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Cakmak_H/0/1/0/all/0/1">Hikmet Çakmak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Michel_R/0/1/0/all/0/1">Raul Michel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+KarataS_Y/0/1/0/all/0/1">Yüksel KarataŞ</a>
The poorly studied Berkeley 8 (Be8) open cluster is analysed from CCD UBVRI
photometric data taken with the 0.90 m telescope at the Sierra Nevada
Observatory. The Z = +0.008 PARSEC isochrone gave us a reddening of E(B-V) =
0.69 +- 0.03, a distance of 3410 +- 300 pc and an age of 2.8 +- 0.2 Gyr. Its
median Gaia DR2 distance, d = 3676 +- 810 pc is in good agreement with our
photometric distances, 3410 – 3620 pc within the uncertainties. The kinematic
parameters of five likely members of Be 8 with the circular orbits, ecc =
[0.23, 0.30] reflect the properties of the Galactic thin disc, which is also
consistent with what is expected of its metal content ([M/H] = -0.27). Be8 with
R > 9 kpc (co-rotation gap at 9 kpc) may have been originating from different
galactic radius or different star formation region.
The poorly studied Berkeley 8 (Be8) open cluster is analysed from CCD UBVRI
photometric data taken with the 0.90 m telescope at the Sierra Nevada
Observatory. The Z = +0.008 PARSEC isochrone gave us a reddening of E(B-V) =
0.69 +- 0.03, a distance of 3410 +- 300 pc and an age of 2.8 +- 0.2 Gyr. Its
median Gaia DR2 distance, d = 3676 +- 810 pc is in good agreement with our
photometric distances, 3410 – 3620 pc within the uncertainties. The kinematic
parameters of five likely members of Be 8 with the circular orbits, ecc =
[0.23, 0.30] reflect the properties of the Galactic thin disc, which is also
consistent with what is expected of its metal content ([M/H] = -0.27). Be8 with
R > 9 kpc (co-rotation gap at 9 kpc) may have been originating from different
galactic radius or different star formation region.
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