Investigating variable stars in the open cluster NGC 1912 and its surrounding field

Li, Chunyan; Esamdin, Ali; Song, Fengfei; Zeng, Xiangyun; Chen, Li; Niu, Hubiao; Bai, Jianying; Liu, Junhui

doi:10.1088/1674-4527/21/3/068

Cited by 3 publications

(2 citation statements)

References 41 publications

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“…The metallicity of this cluster is not well determined, given that spectroscopic analyses of small samples of cluster stars have provided a range of [Fe/H] determinations between ∼ −0.07 and MNRAS 523, 5148-5154 (2023) ∼ −0.38, and E ( B − V ) estimates range between ∼ 0.25 and ∼ 0.35 mag (see e.g. Subramaniam & Sagar 1999 ;Dias et al 2002 ;Majaess, Turner & Lane 2007 ;Frinchaboy et al 2013 ;Carrera R. et al 2019 ;Donor et al 2020 ;Zhong et al 2020 ;Li et al 2021 ).…”

Section: T H E Gaia C O L O U R -M Ag N I T U D E D I Ag R a Mmentioning

confidence: 99%

The broadening of the main sequence in the open cluster M38

Griggio

Salaris

Bedin

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Our recent multi-band photometric study of the colour width of the lower main sequence of the open cluster M37 has revealed the presence of a sizeable initial chemical composition spread in the cluster. If initial chemical composition spreads are common amongst open clusters, this would have major implications for cluster formation models and the foundation of the chemical tagging technique. Here we present a study of the unevolved main sequence of the open cluster M38, employing Gaia DR3 photometry and astrometry, together with newly acquired Sloan photometry. We have analysed the distribution of the cluster’s lower main sequence stars with a differential colour-colour diagram made of combinations of Gaia and Sloan magnitudes, like in the study of M37. We employed synthetic stellar populations to reproduce the observed trend of M38 stars in this diagram, and found that the observed colour spreads can be explained simply by the combined effect of differential reddening across the face of the cluster and the presence of unresolved binaries. There is no need to include in the synthetic sample a spread of initial chemical composition as instead necessary to explain the main sequence of M37. Further photometric investigations like ours, as well as accurate differential spectroscopic analyses on large samples of open clusters, are necessary to understand whether chemical abundance spreads are common among the open cluster population.

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Section: T H E Gaia C O L O U R -M Ag N I T U D E D I Ag R a Mmentioning

confidence: 99%

The broadening of the main sequence in the open cluster M38

Griggio

Salaris

Bedin

et al. 2023

Monthly Notices of the Royal Astronomical Society

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“…For crowded star fields, it performs median filtering on the distribution to suppress possible local overestimations due to bright stars (Bertin & Arnouts 1996). Based on the IRAF and SExtractor, a pipeline is built, for data processing, to obtain the instrumental magnitudes that are used widely for NOWT time-domain surveys (Song et al 2016;Ma et al 2018;Li et al 2021).…”

Section: Observations and Data Reductionsmentioning

confidence: 99%

Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region

Wang

Zhang

Zeng

et al. 2022

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We have investigated the variable stars in the field surrounding NGC 2355 based on the time-series photometric observation data. More than 3000 CCD frames were obtained in the V band spread over 13 nights with the Nanshan One-meter Wide-field Telescope. We have detected 88 variable stars, containing 72 new variable stars and 16 known variable stars. By analyzing these light curves, we classified the variable stars as follows: 26 eclipsing binaries, 52 pulsating stars, four rotating variables, and six unclear type-variable stars for which their periods are much longer than the time baseline chosen. Employing Gaia DR2 parallax, kinematics, and photometry, the cluster memberships of these variable stars were also analyzed for NGC 2355. In addition to the 11 variable members reported by Cantat-Gaudin et al. (2018), we identify four more variable member candidates located at the outer region of NGC 2355 and showed homogeneity in space positions and kinematic properties with the cluster members. The main physical parameters of NGC 2355 estimated from the two-color and color–magnitude diagrams are log(age/yr) = 8.9, E(B − V) = 0.24 mag, and [Fe/H] = −0.07 dex.

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Period–Luminosity–Metallicity–Color Relations of Late-type Contact Binaries in the Big Data Era

Song,

Tian

2024

ApJ

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Binary stars ubiquitous throughout the Universe are important. Contact binaries (CBs) possessing period–luminosity (PL) relations could be adopted as distance tracers. The PL relations of CBs are influenced by metallicity abundance and color index, which are connected to both the radius and luminosity of stars. Here we propose fine relations of the period–luminosity–metallicity–color (PLZC) from the ultraviolet to infrared bands based on current surveys. The accuracy of the distance estimation is 6% and 8%, respectively, depending on the PLZC relations of the CBs in the infrared and optical bands of the collected data. PLZC models are still more accurate than PLC models in determining intrinsic luminosity, notwithstanding their limited improvement. Meanwhile, these relations based on synthetic photometry are also calibrated. On the basis of the synthetic photometry, a 6% accuracy of distance is estimated. The measured or synthetic data of PLZC or PLC relations in infrared bands comes first in the list of suggestions for distance estimations and is followed by the measured data of optical bands.

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Investigating variable stars in the open cluster NGC 1912 and its surrounding field

Cited by 3 publications

References 41 publications

The broadening of the main sequence in the open cluster M38

The broadening of the main sequence in the open cluster M38

Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region

Period–Luminosity–Metallicity–Color Relations of Late-type Contact Binaries in the Big Data Era

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