研究目的
To conduct a multi photometric and astrometric study of open cluster FSR 814 (Koposov 36) using data from SDSS, 2MASS, PPMXL, and Gaia DR2 to estimate its astrophysical properties with high accuracy and compare with existing literature.
研究成果
The study provides high-accuracy astrophysical parameters for FSR 814, including diameter, age, distance, reddening, and mass functions, which are in good agreement with previous studies. The use of Gaia DR2 data offers improved astrometric precision. Future work could involve more advanced data or methods to reduce uncertainties.
研究不足
The study relies on data from external surveys, which may have inherent errors or limitations in coverage. Membership probability methods may be affected by field star contamination and inhomogeneous distributions. The accuracy is constrained by the precision of the astrometric and photometric data available.
1：Experimental Design and Method Selection:
The study uses photometric and astrometric data from multiple surveys (SDSS, 2MASS, PPMXL, Gaia DR2) to analyze the open cluster FSR 814. Methods include Gaussian fitting for cluster center determination, King's model for radial density profile, and membership probability calculations using statistical and proper motion-based techniques. Padova isochrones are applied for CMD fitting.
2：Methods include Gaussian fitting for cluster center determination, King's model for radial density profile, and membership probability calculations using statistical and proper motion-based techniques. Padova isochrones are applied for CMD fitting.
Sample Selection and Data Sources:
2. Sample Selection and Data Sources: Data extracted for stars within a 10 arcmin radius of FSR 814 coordinates (RA = 84.20417°, DEC = +31.21167°) from SDSS (griz bands), 2MASS (JHK bands), PPMXL (proper motions), and Gaia DR2 (G, GBP, GRP bands, parallax, proper motions). Sources include online databases and catalogs.
3：20417°, DEC = +21167°) from SDSS (griz bands), 2MASS (JHK bands), PPMXL (proper motions), and Gaia DR2 (G, GBP, GRP bands, parallax, proper motions). Sources include online databases and catalogs.
List of Experimental Equipment and Materials:
3. List of Experimental Equipment and Materials: No physical equipment; relies on data from astronomical surveys and software tools (e.g., PYTHON code for star counting).
4：Experimental Procedures and Operational Workflow:
Steps include data extraction, transformation of SDSS data to BVRI magnitudes, determination of cluster center via stellar density, radial density profile fitting, membership probability calculation using multiple methods, CMD construction and fitting with isochrones, and derivation of astrophysical parameters.
5：Data Analysis Methods:
Statistical analysis includes Poisson errors, Gaussian fitting, isochrone fitting, and power law fitting for mass function. Software tools like PYTHON are used for computations.
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