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⊙ which can be divided into three main components: (i) a halo which is composed of an old population spherically distributed, (ii) a thin disk which is a flattened and young population of stars like the sun, and (iii) a more central and probably old population called the bulge.
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The Large and the Small Magellanic Clouds (LMC and SMC) are two satellites of the Milky Way at a distance of about 50 to 70 kpc visible from the southern hemisphere.
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The Hertzsprung-Russell diagram (HRD), first designed by E. Hertzsprung and H. N. Russell between 1905 and 1913, is an important tool in stellar astronomy. Luminosities of the stars are plotted on the y axis in units relative to the sun. Spectral types and/or T's are plotted on the x axis. The earliest HRD's were deduced from observations of bright and close-by stars. The stars were mainly found on the so-called MS running through the HRD from the low T-low L and low mass corner to the high T-high L and high mass corner. All these stars belong to the disk of the Milky Way and like the sun, they are burning H in their core. A few red stars are located in the low T-high L area of the HRD; this location implies a larger radius and that is why they are call red giant stars. Most of those stars will finally end up in the high T-low L part as white dwarfs. The other parts of the HDR are essentially empty of stars. The density of stars at a given location translates into a duration of the corresponding phase, the denser the stellar density the longer the stellar evolution phase. These HRD and their corresponding observational CMD are crucial in modern astronomy as most of the information available (age and chemical evolution) on globular clusters can be deduced from its shape. They bring to astronomers a global view of the stellar population studied.
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17
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1842394336
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The magnitude m = -2.5 log (L) + C with C being a constant.
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GCs can essentially be separated (astronomers say resolved) into individual for galactic GCs from regular ground-based observatories and within the Local Group from the HST and the few telescopes equipped with very high resolution devices.
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Due to the Doppler effect, a wavelength emitted at λ (emitted) is redshifted to the observed wavelength λ (observed) which is related to the former one by the relation λ (observed) = λ [emitted (1 + z)], with z being the redshift.
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