Abstract
Archival Vilnius CCD photometric observations are presented for the heavily reddened star cluster Melotte 105, resulting in colour-magnitude diagrams and spectral class estimates. There is considerable lack of agreement between studies for reddening, age and distance for this cluster explaining why the archival data are being made available by this paper. The derived reddening \(E(B-V)=0.34\pm 0.04\) mag and the distance \(V-M_{V}=12.9\pm 0.3\) mag are directly from the Vilnius photometry. The Gaia Data Release 2 (DR2) and Vilnius photometric data of the cluster were used to estimate the structural parameters of the cluster, probability of stellar membership in the cluster, the distance modulus and the cluster age. Lack of Y band observations prevented determination of metal abundance. The values of the colour excess and distance module are determined by two different methods (i.e., Q and Zero Age Main Sequence or ZAMS methods). A distance modulus of \(12.85\pm 0.07\) mag was derived by ZAMS fitting, in good agreement with the above estimate. ZAMS fitting indicates a reddening of \(0.403 \pm 0.02\) mag, within two sigma of the estimate above. The cluster’s metallicity and age are estimated to be 0.24 dex and \(240\pm 25\) Myr, respectively. The derived mass function is in good agreement with the Salpeter slope. The cluster space velocity components (U, V, W) were determined as (\(-3.90\pm 3.34\), \(-13.76\pm 5.69\), \(+3.45\pm 0.41\)) km/s. Perigalactic and apogalactic distances were obtained as \(R_{p}=6.85\) and \(R_{a}=7.44\) kpc respectively. The maximum vertical distance from the Galactic plane was calculated as \(Z_{\mathrm{max}}=84\) pc and the eccentricity of the orbit was determined as \(e=0.042\).
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Notes
\(\frac{A_U}{A_V} = 1.621\), \(\frac{A_P}{A_V} = 1.511\), \(\frac{A_X}{A_V} = 1.419\), \(\frac{A_Z}{A_V} = 1.082\), \(\frac{A_{VIL}}{A_V} = 1.004\) and \(A_{V} = 3.1 \times E(B-V)\).
See also, https://galpy.readthedocs.io/en/v1.5.0/.
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Acknowledgements
The first author, TB, is grateful for generous time allocations at Mount John University Observatory, the Vilnius Observatory for supplying the filter set, the New Zealand Lottery Board for financing the purchase of the set, the Acorn New Zealand for the loan of a R260 computer on which some of this work was performed and to the Foundation for Research, Science and Technology for partial funding of this project in conjunction with the VUW Internal Research Grant Committee. He also acknowledges partial support during this study by the inaugural R.H.T. Bates Postgraduate Scholarship. The authors would like to thank the anonymous referee for his/her helpful comments and advice which improved this paper. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement. IRAF was distributed by the National Optical Astronomy Observatories, which were operated by the Association of Universities for Research in Astronomy Inc., under contract with the National Science Foundation. It is with sadness the authors note the sudden death of Prof. Denis J. Sullivan (VUW) on Christmas day 2019. Prof. Sullivan was TB’s co-supervisor for his Ph.D. and instrumental in starting this project. The authors would like to express their condolences to his family.
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Banks, T., Yontan, T., Bilir, S. et al. Vilnius photometry and Gaia astrometry of Melotte 105. J Astrophys Astron 41, 6 (2020). https://doi.org/10.1007/s12036-020-9621-2
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DOI: https://doi.org/10.1007/s12036-020-9621-2