研究目的
To analyze the observed polarization in a sample of 30 Type 1 active galactic nuclei (AGNs) and use the observed polarization in the broad lines for determination of the central black hole (BH) masses and characteristics (the inclination and emissivity) of the broad-line region (BLR).
研究成果
The spectropolarimetric observations of 30 Type 1 AGNs revealed that equatorial scattering is the dominant polarization mechanism in the sample. This allows for the determination of central black hole masses and characteristics of the broad-line region using the observed polarization in the broad lines. The method provides accurate BH masses that correlate well with stellar velocity dispersion, suggesting its utility for calibration purposes. The BLR in the sample has an averaged inclination of 35?±9? and a flatter emissivity than expected for a classical accretion disc.
研究不足
The accuracy of the observations is limited by the variation of the depolarization in the Earth atmosphere. The method assumes equatorial scattering as the dominant polarization mechanism and Keplerian-like motion of the broad-line emitting gas.
1：Experimental Design and Method Selection:
The observations were performed with the 6 m telescope of SAO RAS using the modified SCORPIO-2 spectropolarimeter. A double Wollaston prism was used as a polarization analyser. The spectral resolution was 8–11 ?, and two gratings, VPHG940 and VPHG1026, were used for spectral coverage.
2：Sample Selection and Data Sources:
A sample of 30 Type 1 AGNs was observed. The observations were corrected for system sensitivity function and extinction, and flux calibration was performed using spectrophotometric standards.
3：List of Experimental Equipment and Materials:
The 6 m telescope of SAO RAS, modified SCORPIO-2 spectropolarimeter, double Wollaston prism, and spectral gratings VPHG940 and VPHG
4：Experimental Procedures and Operational Workflow:
10 Observations for each object were performed in a series of exposures with the integration aperture of 2 × 10 arcsec. Polarization standards and zero-polarization stars were observed before or after the object exposure. The method of observations and data reduction was described in detail by Afanasiev & Amirkhanyan (2012).
5：2). Data Analysis Methods:
5. Data Analysis Methods: The degree of linear polarization and polarization angle were obtained using relations involving the Stokes parameters. The accuracy of the observations was limited by the variation of the depolarization in the Earth atmosphere.
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