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Study of solar neighborhood open cluster NGC 6475 and 11 possible members B-type stars

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Abstract

In the present paper, we performed the optical, astrometric and spectroscopic studies for the open star cluster NGC 6475 using Gaia DR3 data. Using the radial density profile, we estimated the radius of the cluster to be equal to 1.44°. It is located at a distance of 279 ± 17 pc and has a service life of 224 ± 26 Myr. The mean proper motions in RA are 268.50 ± 0.80 mas yr−1 and in DEC, they are −34.83 ± 0.70 mas yr−1. Using spectroscopic radial velocity data of Gaia DR3, the median radial velocity is −14.47 ± 1.92 km s−1. We determined the physical parameters (Teff, log g and V sin i) for 11 possible members of the B-type stars in the open cluster NGC 6475, using the Barbier–Chalonge–Divan (BCD) spectrophotometry system. We also determined the projected rotational velocity of the stars by matching them with the theoretical LTE model and located our studied stars over the HR diagram. From the 11 studied B-type stars, we found six members from them.

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Acknowledgment

We would like to express our deep thanks to the anonymous referee, since his/her fruitful criticism of the version of this paper greatly helped us to improve the paper and the arguments, and we also gratefully appreciate his work, efforts and patience. This work has used data from the European Space Agency (ESA) mission Gaia processed by (https://www.cosmos.esa.int/web/gaia/data), i.e., the Gaia Data Processing & Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions; in particular, the institutions participating in the Gaia Multilateral Agreement. This study was made by using the UVES Paranal Observatory Project (POP). We would like to thank Dr M. Nouh, for his fruitful discussions and help.

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Authors and Affiliations

  1. Astronomy Department, National Research Institute of Astronomy and Geophysics (NRIAG), Helwan, Cairo, 11421, Egypt

    M. H. El-Depsey, Y. H. M. Hendy & Ahmed Shokry

  2. Department of Astronomy and Meteorology, Faculty of Science, Al-Azhar University, Cairo, Egypt

    Ahmed M. Abdelbar & M. M. Beheary

Authors
  1. M. H. El-Depsey
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  2. Y. H. M. Hendy
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  3. Ahmed Shokry
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  4. Ahmed M. Abdelbar
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  5. M. M. Beheary
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Corresponding author

Correspondence to M. H. El-Depsey.

Appendix: Notes on the individual objects

Appendix: Notes on the individual objects

In the following, we discussed about the previous results for studied B stars:

HD 162306 is a double-lined binary star; the star was classified as B8IV by Smoker et al. (2011), who reported a star as a non-member of the NGC 6475, which has been agreed with our investigation.

HD 162515 is the spectroscopic binary star (Ducati et al. 2011) and Morossi & Malagnini (1985) classified the star as B9 (III), whereas Silaj & Landstreet (2014) determined Teff of the system by 10,370 K by using the Geneva photometry system, our result of Teff \(=\) 10,075 is in a good agreement within error with their results, we investigated the star as a member in the NGC 6475 cluster.

HD 162576 is a double star, the star was classified as A0 by Abt (1975), while Catalano & Renson (1998) classified the star as B9, Silaj & Landstreet (2014) determined Teff of the system by 10,100 K by using the Geneva photometry system, Abt & Jewsbury (1969) determined Vrot < 40 km s−1, while Zorec & Royer (2012) determined V sin i as 17 km s−1, Folsom et al. (2007) determined Teff \(=\) 10,640 ± 270 and log g \(=\) 3.7 ± 0.1 and V sin i \(=\) 28 ± 3 km s−1, our determined value of Teff \(=\) 10,561 ± 18, log g \(=\,\)3.6 and V sin i \(=\) 30 km s−1 in a good agreement within error with that of Folsom et al. (2007). We investigated the star as a member in the NGC 6475 cluster.

HD162586 is a double star, Silaj & Landstreet (2014) determined Teff of the system by 12,707 K by using the Geneva photometry system, our result of Teff \(=\) 11,626 ± 8 in deference from their results of almost 1000 K, where this difference is due to the different method used in both the studies.

HD162631 is a single star, which is classified as A0III by Houk (1982).

HD162679 is a spectroscopic binary star (Pourbaix et al. 2004), Morossi & Malagnini (1985) classified the star as B9(V), Villanova et al. (2009) also classified the star as B9 (V) and determined Teff \(=\) 9962, log g \(=\) 3.49 and V sin i \(=\) 37 km s−1, while Silaj & Landstreet (2014) determined Teff of the system by 10,638 K. Our obtained Teff \(=\) 9698 ± 42, log g \(=\) 4.3 and V sin i \(=\) 30 km s−1 are in a very good agreement with that of Villanova et al. (2009). We investigated the star as a member in the NGC 6475 cluster.

HD162724 is an eclipsing binary star (Tokovinin 1997), the star was classified as B9 V by Mon (1968) and Silaj & Landstreet (2014) determined Teff of the system by 10,600 K by using the Geneva photometry system, our calculated Teff \(=\) 10,362 ± 56 is in a good agreement with their result.

HD162725 is an alpha2 CVn variable star (Silaj & Landstreet 2014), the star was classified as A0 p by Abt (1975), Glagolevskij (1994) determined Teff as 9800 and Folsom et al. 2007 determined the Teff \(=\) 9820 ± 400 and log g \(=\) 3.5 ± 0.2, while Silaj & Landstreet (2014) determined Teff of the system by 9600 K, our calculated Teff \(=\) 9777 ± 27 is within the range of their results. We investigated the star as a member in the NGC 6475 cluster.

HD162780 is a spectroscopic binary star (Pourbaix et al. 2004), the star was classified as A0 (IV) by Buscombe & Kennedy (1968) and Merezhin (1994) studied star as the spectroscopic binary system and determined Teff of the primary component as 10,300 and V sin i for the system as 295 km s−1, Silaj & Landstreet (2014) determined Teff of the system by 9902 K by using the Geneva photometry system, our calculated Teff \(=\) 9994 ± 25 is within the range of their results.

HD162781 is a normal single star, which was classified as A0IV by Buscombe & Kennedy (1968), Silaj & Landstreet (2014) determined Teff of the system by 9221 K by using the Geneva photometry system, our result of Teff \(=\) 1062 ± 95 in deference with their results almost 1000 K, where this difference is due to the different method used in both the studies, where our result could be more accurate due to depending on the modeling of the spectrum of star.

HD162817 is a normal B star with any appearance of peculiarities, the star was classified as B9.5/A0III by Buscombe & Kennedy (1968), while Hamdy et al. (1993) classified the star as B9.5, Hempel & Holweger (2003) determined Teff \(=\) 9190 and log g \(=\) 3.15 dex and V sin i \(=\) 76 ± 4 km s−1, Folsom et al. (2007) determined Teff \(=\) 9940 ± 360 and log g \(=\) 3.4 ± 0.1 and V sin i \(=\) 79 ± 3 km s−1, while Silaj & Landstreet (2014) determined Teff of the system by 9500 K by using the Geneva photometry system, our result of Teff \(=\) 9451 ± 21 is within the range of their results. We investigated the star as a member of the NGC 6475 cluster.

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El-Depsey, M.H., Hendy, Y.H.M., Shokry, A. et al. Study of solar neighborhood open cluster NGC 6475 and 11 possible members B-type stars. J Astrophys Astron 44, 65 (2023). https://doi.org/10.1007/s12036-023-09958-4

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