View source for Astronomy:NGC 3114

{{short description|Open cluster in the constellation Carina}}
{{Infobox open cluster
| image   = [[File:NGC 3114 Eguivar-crop.jpg|300 px]]
| caption = Open cluster NGC 3114 in Carina
| name = [[Astronomy:New General Catalogue|NGC]] 3114
| type = open cluster
| epoch = [[Astronomy:J2000|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
  | access-date=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 = [[Astronomy:Carina (constellation)|Carina]]
| radius_ly = 
| absmag_v = 
| notes = 
| names = [[Astronomy:Collinder catalogue|Cr]] 215
}}
'''NGC 3114''' is a sparse [[Astronomy:Open cluster|open cluster]] which is projected onto the outskirts of the [[Astronomy: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 [[Astronomy:Milky Way#Composition and structure|disc of the Milky Way]], it is very difficult 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 [[Astronomy:UBV photometric system|UBV photometry]]  for 171 of its stars and photoelectric UBV photometry of 52 stars.  They estimated the [[Astronomy:Star cluster|cluster]] to be 910 [[Astronomy:Parsec|parsec]]s from the [[Astronomy:Sun|Sun]], its mean [[Astronomy:Extinction|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 [[Astronomy:Photometry|photometry]] data for 122 stars, revising the cluster [[Astronomy:Extinction|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 [[Engineering: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 [[Astronomy:Star#Chemical composition|chemical abundance]], finding that NGC 3114 has basically the same metal richness as the Sun, for which <math>[Fe/H] = -0.04\pm0.04</math><ref name="CarraroPatat" /> (Fe - [[Chemistry:Iron|Iron]], H - [[Chemistry:Hydrogen|Hydrogen]]).

==Gallery==
<gallery>
NGC 3114.jpg|NGC 3114 from a 5 inches reflector
</gallery>

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

==References==
{{Reflist}}

==External links==


{{Stellar system}}

[[Category:Open clusters]]
[[Category:Carina (constellation)]]
[[Category:NGC objects|3114]]

{{Sourceattribution|NGC 3114}}