A precursive study of the time-domain survey of the Galactic Anti-center using the Nanshan 1-meter telescope with variable stars detected

Ma, Shuguo; Esamdin, Ali; Ma, Lihua; Niu, Hubiao; Fu, Jian-Ning; Liu, Jinzhong; Yang, Tianyu; Song, Fengfei; Pu, Guang-Xin

doi:10.1007/s10509-018-3289-y

Cited by 9 publications

(6 citation statements)

References 25 publications

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“…The telescope was equipped with a standard Johnson multicolor filter system (i.e., U B V R I filters) (e.g., Cousins 1976) and an E2V CCD 203-82 (blue) camera mounted on the primary focus of the telescope. The CCD camera, which has 4K×4K pixels and a 1.3°×1.3°field of view, operated at a temperature of about −120 °C cooling with liquid nitrogen (Song et al 2016;Ma et al 2018).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Pulsations of the SX Phe Star BL Camelopardalis

Zong

Esamdin

et al. 2019

PASP

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We carried out photometric observations of the SX Phe star BL Cam in 2014, 2017 and 2018 using Nanshan 1-m telescope. In addition to the dominated frequency of 25.5790(3) cd −1 and its two harmonics, an independent frequency of 25.247 (2) cd −1 , which is a nonradial mode frequency, was detected from the data in 2014. A total of 123 new times of light maxima were determined from our light curves in the three years, which, together with that published in the literature, were used to analyze the O−C diagram. The change rate of the main period was derived as (1/P)(dP/dt) = -2.39 (8)×10 −8 yr −1 , which is lower than that published in previous literature. A periodical change with a period of 14.01 (9) yr was found in the residuals of the O−C curve fitting. If it was caused by the light-time effect, BL Cam should be a binary system. The mass of the companion was restricted as low as that of a brown dwarf. No evidence of the triple system suggested by previous authors was shown in our analysis.

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Section: Observations and Data Reductionmentioning

confidence: 99%

Pulsations of the SX Phe Star BL Camelopardalis

Zong

Esamdin

et al. 2019

PASP

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“…In 2017 January, ten days of photometric observations were conducted by using the Nanshan One-meter Wide-field Telescope (NOWT; Song et al 2016;Ma et al 2018;Bai et al 2020) located at the Nanshan station of Xinjiang Astronomical Observatory (XAO), CAS. An E2V CCD203-82 (blue) chip CCD camera with 4096 × 4136 pixels was mounted at the prime focus of the telescope, providing a field of view (FOV) of 1.3 × 1.3 deg 2 .…”

Section: Observations and Data Reductionsmentioning

confidence: 99%

Variable Star Detection in the Field of Open Cluster NGC 188

Song,

Niu,

Esamdin

et al. 2023

Res. Astron. Astrophys.

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This work presents the charge-coupled device (CCD) photometric survey of the old open cluster NGC 188. Time-series V-band photometric observations were conducted for ten nights in January 2017 using the Nanshan One-meter Wide-field Telescope (NOWT) to search for variable stars in the field of the cluster field. A total of 25 variable stars, including one new variable star, were detected in the target field. Among the detected variables, 16 are cluster member stars, and the others are identified as field stars. The periods, radial velocities, effective temperatures, and classifications of the detected variables are discussed in this work. Most of the stars’ effective temperatures are between 4200 K and 6600 K, indicating theirspectral types are G or K. The newly discovered variable is probably a W UMa system. In this study, a known cluster variable star (V21 = V0769 Cep) is classified as an EA-type variable star based on the presence of an 0.5 magnitude eclipse in its light curve.

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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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A precursive study of the time-domain survey of the Galactic Anti-center using the Nanshan 1-meter telescope with variable stars detected

Cited by 9 publications

References 25 publications

Pulsations of the SX Phe Star BL Camelopardalis

Pulsations of the SX Phe Star BL Camelopardalis

Variable Star Detection in the Field of Open Cluster NGC 188

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

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