研究目的
To determine the properties of the optical counterpart to the INTEGRAL source IGR J21343+4738 and study its long-term optical variability, confirming its nature as a Be/X-ray binary and deriving physical parameters such as spectral type, distance, and rotational velocity.
研究成果
The optical counterpart of IGR J21343+4738 is confirmed as a B1IVe shell star in a Be/X-ray binary system, located at approximately 8.5 kpc. The observed variability in Hα and other spectral lines is due to the formation and dissipation of a circumstellar disc, with fast V/R variations indicating a density perturbation. The system is viewed near edge-on, and the rotational velocity is estimated to be around 380 km/s. Future observations are needed to confirm the long-term cycle durations and further refine parameters.
研究不足
Observational gaps in the data may affect the precise determination of time scales for disc formation and dissipation. The study relies on optical observations, which may not capture all aspects of the X-ray binary system. The inclination angle and rotational velocity estimates have uncertainties due to model assumptions and instrumental effects.
1：Experimental Design and Method Selection:
The study involved long-term monitoring of IGR J21343+4738 using optical photometric and spectroscopic observations to analyze variability and derive astrophysical parameters. Methods included photometry in BVRI bands and spectroscopy covering 4000–7500 ?, with data reduction using standard procedures in IRAF and other packages.
2：Sample Selection and Data Sources:
The optical counterpart of the X-ray source IGR J21343+4738 was observed, with data collected from multiple telescopes over several years (2009-2013).
3：3).
List of Experimental Equipment and Materials:
3. List of Experimental Equipment and Materials: Telescopes used include the 1.3m Skinakas Observatory telescope, the 1.5m telescope at Fred Lawrence Whipple Observatory, and the 4.2m William Herschel Telescope. Equipment includes CCD cameras (e.g., ANDOR CCD, ISA SITe CCD), spectrographs (e.g., FAST-II spectrograph, ISIS spectrograph), and filters (Johnson/Bessel B, V, R, I filters).
4：3m Skinakas Observatory telescope, the 5m telescope at Fred Lawrence Whipple Observatory, and the 2m William Herschel Telescope. Equipment includes CCD cameras (e.g., ANDOR CCD, ISA SITe CCD), spectrographs (e.g., FAST-II spectrograph, ISIS spectrograph), and filters (Johnson/Bessel B, V, R, I filters).
Experimental Procedures and Operational Workflow:
4. Experimental Procedures and Operational Workflow: Observations were conducted through scheduled monitoring campaigns. Spectroscopic data were reduced with bias subtraction, flat-field correction, wavelength calibration using comparison lamps, and extraction of spectra. Photometric data were reduced with bias subtraction, flat-field correction, aperture photometry, and transformation to standard systems using Landolt standard stars.
5：Data Analysis Methods:
Data analysis included measuring equivalent widths, V/R ratios, radial velocities via cross-correlation with synthetic spectra, spectral classification using line ratios, and estimation of rotational velocities and distances based on photometric and spectroscopic parameters.
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