Abstract
Abstract NGC 7067 is a young open cluster located in the direction between the first and the second Galactic quadrants and close to the Perseus spiral arm. This makes it useful for studies of the nature of the Milky Way spiral arms. Strömgren photometry taken with the Wide Field Camera at the Isaac Newton Telescope allowed us to compute individual physical parameters for the observed stars and hence to derive the cluster's physical parameters. Spectra from the 1.93-m telescope at the Observatoire de Haute-Provence helped to check and improve the results. We obtained photometry for 1233 stars, individual physical parameters for 515 and spectra for 9 of them. The 139 selected cluster members lead to a cluster distance of 4.4 ± 0.4 kpc, with an age below log10(t(yr)) = 7.3 and a present mass of 1260 ± 160 M⊙. The morphology of the data reveals that the centre of the cluster is at (α, δ) = (21: 24: 13.69, +48: 00: 39.2) J2000, with a radius of 6.1 arcmin. Strömgren and spectroscopic data allowed us to improve the previous parameters available for the cluster in the literature.
Highlights
Open clusters are a good framework to study stellar and Galactic evolution
The analysis of the Stromgren data, together with the nine available spectra, allowed us to compute the physical parameters for the cluster NGC 7067. 139 likely member stars were selected from the photometric diagrams
From a main-sequence fitting to the cluster data, we obtained a distance of 4.4 ± 0.4 kpc, while using the mean of individual star distances, we obtained 4.0 ± 0.8 kpc
Summary
Open clusters are a good framework to study stellar and Galactic evolution. The assumption that all the stars belonging to a cluster were born at the same time provides us a snapshot of the stellar evolutionary process for different stellar masses, which is key to analyse stellar evolution. Afterwards, Becker (1965) tried to improve the distance determination to the cluster, adding the two colour–colour magnitude diagram information of ∼60 stars using photographic plates, and obtained 4500 pc. Hoag & Applequist (1965) used calibrations that provide absolute magnitudes from Hγ equivalent widths for only three early-type stars in NGC 7067 obtaining a distance of 2290 pc. The uvbyβ Stromgren CCD photometry (Stromgren 1966) provides more accurate information than the usual Johnson UBV photometry since the bands are narrower This system is the most adequate for the study of early-type stars since it has been purposely designed to provide accurate measurements of their intrinsic properties.
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