New SX Phe variables in the globular cluster NGC 288★

Martinazzi, Elizandra; Costa, Jose Eduardo da Silveira; Pieres, A.; Bonatto, Charles Jose; Bica, E.

doi:10.1093/mnras/stu2472

Cited by 6 publications

(14 citation statements)

References 26 publications

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“…We obtained the updated values for NGC 288 with an age of 13.5 Gyr, metallicity of [Fe/H] = −1.39, and distance modulus of (m − M ) V = 14.75 mag. A value of interstellar reddening E(B − V ) = 0.02 mag was taken from Martinazzi et al (2015), and E(V − I) was adopted from the average E(V -I)/E(B -V ) ratio of 1.35 suggested by Kunder et al (2013).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…To analyze the binary light curve, the effective temperature of the hot primary star was fixed at 5 964 K, as derived from Flower's (1996) table by adopting the color index B − V = +0.60 of V10 obtained in this paper and E(B − V ) = +0.02 given by Martinazzi et al (2015). Because there is no previous light-curve solution of this binary system, we conducted an extensive q-search.…”

Section: Eclipsing Binary Starmentioning

confidence: 99%

“…b Comparison between our frequencies and the previous ones from Martinazzi et al (2015). The unit of frequency was converted from µHz to cycles day −1 .…”

Section: Eclipsing Binary Starmentioning

confidence: 99%

“…NGC 288 (R.A. J2000 = 00:52:45.24, DEC. J2000 = −26:34:57.4) belongs to Sculptor constellation and is close to the Southern Galactic Pole (l = 152.30, b = −89.38), where the interstellar reddening shows a low value of E(B − V ) = 0.02±0.01 (Martinazzi et al 2015). According to the Catalog of Parameters for Milky Way Globular Clusters by Harris (1996Harris ( , 2010 1 ), the metallicity and distance modulus of NGC 288 are [Fe/H] = -1.32 and (m−M ) V = 14.84, respectively.…”

Section: Introductionmentioning

confidence: 99%

“…According to the Catalog of Parameters for Milky Way Globular Clusters by Harris (1996Harris ( , 2010 1 ), the metallicity and distance modulus of NGC 288 are [Fe/H] = -1.32 and (m−M ) V = 14.84, respectively. Twelve variable stars -a semi-regular variable star (Oosterhoff 1943), two RR Lyr stars (Hollingsworth & Liller 1977;Kaluzny 1996), eight SX Phe stars (Kaluzny 1996;Kaluzny et al 1997;Martinazzi et al 2015), and an eclipsing binary star (Kaluzny et al 1997) -have been found so far in NGC 288. The location of each variable star in the FOV is shown in Figure 1.…”

Section: Introductionmentioning

confidence: 99%

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Time-Series Photometry of Variable Stars in the Globular Cluster NGC 288

Lee¹,

Koo²,

Hong³

et al. 2016

Journal of The Korean Astronomical Society

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We present the results of BV time-series photometry of the globular cluster NGC 288. Observations were carried out to search for variable stars using the Korea Microlensing Telescope Network (KMTNet) 1.6-m telescopes and a 4k pre-science CCD camera during a test observation from August to December, 2014. We found a new SX Phe star and confirmed twelve previously known variable stars in NGC 288. For the semi-regular variable star V1, we newly determined a period of 37.3 days from light curves spanning 137 days. The light-curve solution of the eclipsing binary V10 indicates that the system is probably a detached system. The pulsation properties of nine SX Phe stars were examined by applying multiple frequency analysis to their light curves. We derived a new Period-Luminosity (P -L) relation, M V = −2.476(±0.300) log P − 0.354(±0.385), from six SX Phe stars showing the fundamental mode. Additionally, the period ratios of three SX Phe stars that probably have a double-radial mode were investigated; P FO /P F = 0.779 for V5, P TO /P FO = 0.685 for V9, P SO /P FO = 0.811 for V11. This paper is the first contribution in a series assessing the detections and properties of variable stars in six southern globular clusters with the KMTNet system.

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Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Eclipsing Binary Starmentioning

confidence: 99%

“…b Comparison between our frequencies and the previous ones from Martinazzi et al (2015). The unit of frequency was converted from µHz to cycles day −1 .…”

Section: Eclipsing Binary Starmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Time-Series Photometry of Variable Stars in the Globular Cluster NGC 288

Lee¹,

Koo²,

Hong³

et al. 2016

Journal of The Korean Astronomical Society

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Accurate distances to Galactic globular clusters through a combination of Gaia EDR3, HST, and literature data

Baumgardt

Vasiliev

2021

Monthly Notices of the Royal Astronomical Society

252

112

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We have derived accurate distances to Galactic globular clusters by combining data from the Gaia Early Data Release 3 (EDR3) with distances based on Hubble Space telescope (HST) data and literature based distances. We determine distances either directly from the Gaia EDR3 parallaxes, or kinematically by combining line-of-sight velocity dispersion profiles with Gaia EDR3 and HST based proper motion velocity dispersion profiles. We furthermore calculate cluster distances from fitting nearby subdwarfs, whose absolute luminosities we determine from their Gaia EDR3 parallaxes, to globular cluster main-sequences. We finally use HST based stellar number counts to determine distances. We find good agreement in the average distances derived from the different methods down to a level of about 2 per cent. Combining all available data, we are able to derive distances to 162 Galactic globular clusters, with the distances to about 20 nearby globular clusters determined with an accuracy of 1 per cent or better. We finally discuss the implications of our distances for the value of the local Hubble constant.

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