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δ Doradus (often Latinised to Delta Doradus, abbreviated to δ Dor or delta Dor) is a star in the southern constellation of Dorado. Based upon an annual parallax shift of 21.80 mas as seen from Earth, it is located around 150 light years from the Sun. The star is visible to the naked eye with an apparent visual magnitude of +4.34. [2]
Pi 1 Doradus, Latinized from π 1 Doradus, is a solitary star [15] located in the southern constellation Dorado near the southwestern border with Mensa.It is faintly visible to the naked eye as an orange-hued point of light with an apparent magnitude of 5.54. [2]
This is the list of notable stars in the constellation Dorado, sorted by decreasing brightness. Name B G. Var HD HIP RA Dec vis. mag. abs. mag. Dist. Sp. class Notes ...
AB Doradus is a pre-main-sequence quadruple [5] star system in the constellation Dorado. The primary is a flare star that shows periodic increases in activity. A visual band light curve for AB Doradus. The main plot shows the long-term variability, and the inset shows the periodic variability (as of Oct/Nov 1989).
Dorado (US: / d ə ˈ r eɪ d oʊ /, also UK: /-ˈ r ɑː d oʊ /) is a constellation in the Southern Sky. It was named in the late 16th century and is now one of the 88 modern constellations . Its name refers to the mahi-mahi ( Coryphaena hippurus ), which is known as dorado ("golden") in Spanish , although it has also been depicted as a ...
Johann Bode included the Tarantula in his 1801 Uranographia star atlas and listed it in the accompanying Allgemeine Beschreibung und Nachweisung der Gestirne catalog as number 30 in the constellation "Xiphias or Dorado". Instead of being given a stellar magnitude, it was noted to be nebulous.
Gamma Doradus, Latinized from γ Doradus, is the third-brightest star in the southern constellation of Dorado. [11] It is faintly visible to the naked eye with an apparent visual magnitude of approximately 4.25, and is a variable star, the prototype of the class of Gamma Doradus variables. [3]
The NGC 1566 Group of Dorado contains H I with M HI = 3.5 × 10 10 M ⊙ of which 40% alone comes from the NGC 1566 galaxy. [5] More than half of its members are outside its virial radius of 580 kpc which suggests this group is a young non-virialized group. The 2005 Kilborn et al. set of confirmed NGC 1566 Group members (within the Dorado Group ...