Kains, N, Bramich, DM, Ferro, AA, Jaimes, RF, Jorgensen, UG, Giridhar, S, Penny, MT, Alsubai, KA, Andersen, JM, Bozza, V, Browne, P, Burgdorf', M, Novati, SC, Damerdji, Y, Diehl, C, Dodds, P, Dominik, M, Elyiv, A, Fang, X-S, Giannini, E, Hardis, S, Harpsoe, K, Hinse, TC, Hornstrup, A, Hundertmark, M, Jessen-Hansen, J, Juncher, D, Kerins, E, Kjeldsen, H, Korhonen, H, Liebig, C, Lund, MN, Lundkvist, M, Mancini, L, Martin, R, Mathiasen, M, Rabus, M, Rahvar, S, Ricci, D, Sahu, K, Scarpetta, G, Skottfelt, J, Snodgrass, C, Southworth, J, Surdej, J, Tregloan-Reed, J, Vilela, C, Wertz, O, Williams, A and Consortium, M (2016) Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry (vol 555, pg A36, 2013). Astronomy & Astrophysics, 588.

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Abstract

Aims. We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M 30 (NGC 7099). We
used our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves to
derive values for the cluster’s parameters.
Methods. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster
parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. We also
derived an estimate for the age of the cluster by fitting theoretical isochrones to our colour-magnitude diagram (CMD).
Results. Out of 13 stars previously catalogued as variables, we find that only 4 are bona fide variables. We detect two new RR Lyrae variables,
and confirm two additional RR Lyrae candidates from the literature. We also detect four other new variables, including an eclipsing blue straggler
system, and an SX Phoenicis star. This amounts to a total number of confirmed variable stars in M 30 of 12. We perform Fourier decomposition of
the light curves of the RR Lyrae stars to derive cluster parameters using empirical relations. We find a cluster metallicity [Fe/H]ZW = −2.01±0.04,
or [Fe/H]UVES = −2.11 ± 0.06, and a distance of 8.32 ± 0.20 kpc (using RR0 variables), 8.10 kpc (using one RR1 variable), and 8.35 ± 0.42 kpc
(using our SX Phoenicis star detection in M 30). Fitting isochrones to the CMD, we estimate an age of 13.0 ± 1.0 Gyr for M 30.

Item Type: Article
Additional Information: © The Authors, EDP Sciences. The published version is available from http://dx.doi.org/10.1051/0004-6361/201321819e (This paper is also an erratum for Kains, N. et al., 2013. Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry. A&A, 555, p.A36. Available at: http://dx.doi.org/10.1051/0004-6361/201321819 published 25 June 2013
Uncontrolled Keywords: stars, variables, general stars, RR Lyrae, globular clusters, M 30 (NGC 7099), errata, addenda
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Related URLs:
Depositing User: Symplectic
Date Deposited: 14 Jun 2016 09:30
Last Modified: 10 Mar 2021 10:22
URI: https://eprints.keele.ac.uk/id/eprint/1845

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