Tautological consequence

2013-12-15T15:24:11Z

80.101.154.204: improved formatting in the Example section

{{cluster
| image =
| caption=An
| name = [[New General Catalogue|NGC]] 3114
| type = open cluster
| epoch = [[J2000]]
| ra = {{RA|10|02|42|}}<ref name="skymap">{{cite web
| title=News Sky Map
| work=NGC 3114
| url=http://www.news.sky-map.org/starview?object_type=4&object_id=713&object_name=NGC+3114&locale=FR
| accessdate=2012-01-04}}</ref>
| dec = {{DEC|-60|06|0}}<ref name="skymap" />
| dist_ly =
| appmag_v = + 4.2<ref name="skymap" />
| size_v =
| title=
| work=
| url=
| accessdate=
| constellation = [[Carina (constellation)|Carina]]
| radius_ly =
| absmag_v =
| notes =
| names =
}}
'''NGC 3114''' is a sparse [[open cluster]] which is projected onto the outskirts of the [[Carina (constellation)|Carina]] complex.<ref name="CarraroPatat">G. Carraro, F. Patat, "Star clusters in the Carina complex: UBVRI photometry of NGC 3114, Colliner 228 and vdB-Hage 99*, A&A, '''Volume 379''', Number 1, November 2001, pp. 136-146</ref>

Because of the high number of field [[stars]] from the [[Milky_Way#Composition_and_structure|disc of the Milky Way]], it is very difficult [[Celestial body|object]] to study<ref name="CarraroPatat" /> as this contamination makes its size ambiguous.

==Studies of NGC 3114==
NGC 3114 has first been subject of studies in 1963, when Jankowitz and McCosh obtained photographic [[UBV photometric system|UBV photometry]] for 171 of its stars and photoelectric UBV photometry of 52 stars. They estimated the [[Star cluster|cluster]] to be 910 [[parsec]]s from the [[Sun]], its mean [[Extinction (astronomy)|visual extinction]] <math>E(B-V) = 0.27</math> and its age to range from <math>6\times 10^{7}</math> and <math>2\times 10^{8}</math> years.<ref name="CarraroPatat" />

In 1988, Schneider and Weiss obtained [[photometry (astronomy)|photometry]] data for 122 stars, revising the cluster [[Extinction (astronomy)|reddening]] to be <math>E(B-V) = 0.03</math>.<ref name="CarraroPatat" />

Three years later, Sagar and Sharpless made the largest data recording of the cluster to date, obtaining BV [[Charge-coupled device|CCD]] photometry of around 350 stars from seven 3.6'×5.4' regions. Because these regions were rather far from the cluster centre, a substantial contamination was expected. Nevertheless, by assuming the cluster reddening value obtained by Schneider and Weiss, they found the cluster to be <math>940 \pm 60</math> pc, which agreed with the measurements taken 28 years previously by Jankowitz and McCosh. They also found the age of the cluster to be <math>1-2 \times 10^{8}</math> years.<ref name="CarraroPatat" />

Finally, in 1989 Claria' et al. estimated the cluster [[Star#Chemical_composition|chemical abundance]], finding that NGC 3114 has basically the same [[metal (astronomy)|metal]] richness as the Sun, for which <math>[Fe/H] = -0.04\pm0.04</math><ref name="CarraroPatat" /> (Fe - [[Iron]], H - [[Hydrogen]]).

==See also==
* [[List of open clusters]]
* [[Open cluster family]]
* [[Open cluster remnant]]
* [[Star clusters]]
* [[Stellar associations]]

==References==
{{Reflist}}

{{Stellar system}}

[[Category:Open clusters]]

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Tautological consequence