NGC 2362

From Vero - Wikipedia
Jump to navigation Jump to search

Template:Short description {{#invoke:Infobox|infobox}}Template:Template other{{#invoke:Check for unknown parameters|check|unknown=Template:Main other|preview=Page using Template:Infobox open cluster with unknown parameter "_VALUE_"|ignoreblank=y| age | alt | absmag_v | appmag_v | caption | constellation | credit | dec | dist_ly | dist_pc | epoch | galaxy | group | image | image_scale | mass_msol | name | names | notes | ra | radius_ly | size_v }}

NGC 2362, also known as Caldwell 64, is an open cluster of stars in the southern constellation of Canis Major. It was discovered by the Italian court astronomer Giovanni Batista Hodierna, who published his finding in 1654.<ref name=Dahm2008/> William Herschel called it a "beautiful cluster", while William Henry Smyth said it "has a beautiful appearance, the bright white star being surrounded by a rich gathering of minute companions, in a slightly elongated form, and nearly vertical position". In the past it has also been listed as a nebula, but in 1930 Robert J. Trumpler found no evidence of nebulosity.<ref name=OMeara2002/> The brightest member star system is Tau Canis Majoris, and therefore it is sometimes called the Tau Canis Majoris Cluster.

The cluster is located at a distance of approximately 1.48 kpc from the Sun,<ref name=Wu2009/> and appears associated with the giant nebula Sh2-310 that lies at the same distance,<ref name="VY"/> about one degree to the east. This giant H II region is being ionized by the brighter members of the NGC 2362 cluster.<ref name=Dahm2008/>

At 4–5 million years, NGC 2362 is a relatively young cluster<ref name=Currie2009/> but is devoid of star-forming gas and dust, indicating that the star formation process has come to a halt.<ref name=Dahm2008/> It is a massive open cluster, with more than 500 solar masses,<ref name=Currie2009/> an estimated 100-150 member stars, and an additional 500 forming a halo around the cluster. Of these cluster members, only around 35 show evidence of a debris disk.<ref name=Currie2009/> There is one slightly evolved O-type star, Tau Canis Majoris, and around 40 B-type stars still on the main sequence. Only one candidate classical Be star has been found, as of 2005.<ref name=Dahm2008/>

List of NGC 2362 members brighter than magnitude 10.0<ref name=members/>
Designation Right ascension Declination Spectral type Apparent magnitude
τ CMa Template:RA Template:Dec O9II 4.40
HD 57192 Template:RA Template:Dec B2V 6.81
CD−24°5180 Template:RA Template:Dec 8.21
TYC 6541-4237-1 Template:RA Template:Dec 8.38
CD−24°5175 Template:RA Template:Dec B2V 8.77
V422 CMa Template:RA Template:Dec B2IV/V 8.94
CD−24°5162 Template:RA Template:Dec 9.28
CD−24°5182 Template:RA Template:Dec B2V 9.31
NGC 2362 67 Template:RA Template:Dec 9.32
CD−24°2205 Template:RA Template:Dec B3V 9.54
CD−24°5189 Template:RA Template:Dec 9.56
CD−24°2207 Template:RA Template:Dec B2V 9.6
NGC 2362 39 Template:RA Template:Dec B2 9.78
CD−24°2250 Template:RA Template:Dec 9.80
CD−24°5170 Template:RA Template:Dec B5V 9.80
CD−24°5234 Template:RA Template:Dec 9.96
CD−25°4366 Template:RA Template:Dec 9.98

References

Template:Reflist

Template:Commonscat

Template:Sky Template:Catalogs Template:Caldwell catalogue Template:Ngc25 Template:Canis Major