has dimension has unit 単位を持つ has value 値を持つ magnitude magnitude m Reverse logarithmic measure of the brightness of an object. The magnitude scale was originally created by Hipparchos of Nicea (160-127 BCE) and was measured by comparing the brightness between stars. Initially this was done inaccurately by eye but is currently done by using photoelectric photometers or even more recently by CCDs. Hipparchos divided the stars into six magnitude (brightness classes), the brightest stars being assigned to the first class and the faintest to the sixth class. By about the middle 1800s it became apparent that the traditional magnitude scale is close to a logarithmic scale with base 2.5. This is due to the fact that the response of the eye is nearly logarithmic. N.R. Pogson formalised the magnitude scale to closely match the traditional (visual) scale. It is now defined as: m₁ - m₂ = - 2.5 log (f₁ / f₂) where m₁ - m₂ is the magnitude difference between two objects, and f₁ and f₂ are the luminous fluxes of the two objects. The magnitude of Vega (α Lyrae, HD 172167) is defined to be 0 in all wavelengths and passbands, although in practice this can only be an approximation. The zero point is now defined using multiple standard stars from the north polar sequence (non-variable stars within 2 degrees of the north celestial pole) or secondary standard stars from other parts of the sky. Please note that the scale is inverted, objects of magnitude 1 have a higher luminous flux than objects of magnitude 5. Stars of magnitude 6 are just visible to the naked eye under good observing conditions. The units of magnitude, also called magnitude, are usually not indicated except when indicating small magnitude differences when milli- or micromagnitudes are used. magnitude unit quantity 量 dimensionOne magnitude magnitude micromagnitude micromagnitude millimagnitude millimagnitude one