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Method and filter for measuring the metallicity of fgk-type stars sage

A technology of stellar metals and optical filters, applied in color/spectral characteristic measurement, image enhancement, image analysis, etc., can solve the problems of multi-observation time, cost, insensitivity of spectral lines, etc., and achieve simple and easy installation and observation operation The effect that production, the measuring method are simple

Active Publication Date: 2020-01-10
NAT ASTRONOMICAL OBSERVATORIES CHINESE ACAD OF SCI
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Problems solved by technology

But for spectral observation, it takes a lot of observation time, and traditional photometry systems such as Johnson-CousinUBVRI and SDSS ugriz are not sensitive to spectral lines because of their wide bandwidth

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  • Method and filter for measuring the metallicity of fgk-type stars <sub>sage</sub>
  • Method and filter for measuring the metallicity of fgk-type stars <sub>sage</sub>
  • Method and filter for measuring the metallicity of fgk-type stars <sub>sage</sub>

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[0059] Specific embodiments of the present invention will be described in detail below in conjunction with specific drawings. It should be noted that the technical features or combinations of technical features described in the following embodiments should not be regarded as isolated, and they can be combined with each other to achieve better technical effects. In the drawings of the following embodiments, the same reference numerals appearing in each drawing represent the same features or components, which can be applied in different embodiments.

[0060] In the present invention, FGK-type stars are used as an example of the observation target, but this is not limiting, and includes any observation target composed of or dominated by FGK-type stars (such as star clusters, galaxies and other celestial bodies).

[0061] The embodiment of the present invention provides a v for measuring the metal abundance of FGK type stars SAGE filter, the filter v SAGE The central wavelength ...

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Abstract

The invention relates to the field of astronomical measurement, and provides a method for measuring FGK-type stellar metal abundance and a filter VSAGE. The filter has a center wavelength of 395 nanometer and a bandwidth of 29 namometer, can cover a CaII-H&K absorption line, accurately measure the absorption line, and effectively measure the stellar metal abundance. The measuring method comprisesthe following steps of: carrying out observation and data processing on a FGK-type star and a flow standard star to be measured; fitting an atmospheric extinction curve and carrying out a flow calibration on the star to be measured; fitting the '(VSAGE-g)-(g-i) Color-Metal Abundance Relationship [Fe / H]'; the stellar metal abundance to be measured is determined by a photometry method. The method has the advantages that the FGK-type star observation efficiency is high, the measurement method for the metal abundance is simple, the metal abundance of all the FGK-type stars in the observation fieldof view can be measured at one time, the speed is fast compared with the traditional method, and the method has no selection effect and is suitable for measurement and statistics of metal abundance of large sample stars.

Description

technical field [0001] The invention relates to the technical field of astronomical measurement, in particular to a method for measuring the metal abundance of FGK-type stars and an optical filter v SAGE . Background technique [0002] There are many methods for measuring the metal abundance of FGK stars. The traditional method is to use the observation of the spectrum to measure the intensity of the Fe line, and assume the local thermodynamic equilibrium LTE to calculate. It can also be based on some other spectral lines that are more sensitive to the metal abundance. Measurement, such as CaII H&K line (393.4 / 396.8nm), CaII triplet line (849.8 / 854.2 / 866.2nm) and other absorption lines. But for spectral observation, it takes a lot of observation time, and traditional photometry systems such as Johnson-CousinUBVRI and SDSS ugriz are not sensitive to spectral lines because of their wide bandwidth. Contents of the invention [0003] Purpose of the present invention is exact...

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Application Information

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Patent Type & Authority Patents(China)
IPC IPC(8): G01N21/31G06T5/50
CPCG01N21/31G06T5/50G06T2207/20221
Inventor 范舟
Owner NAT ASTRONOMICAL OBSERVATORIES CHINESE ACAD OF SCI
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