查看“︁NGC 6166”︁的源代码

{{Sky|16|28|38.276|+|39|33|04.97}}

{{Infobox galaxy
| name = NGC 6166
| image = [[File:Monster Galaxies Lose Their Appetite With Age 03.jpg|250px]]
| caption = 星系NGC 6166
| epoch = [[J2000]]
| type = cD2 pec.
| mass =  
| stars =  
| ra = {{RA|16|28|38.276}}
| dec = {{DEC|+39|33|04.97}}
| dist_ly = 490 [[光年|Mly]] <br /> (142 [[秒差距|mpc]]) 
| z = z = −0.030354 <br /> (負負符號<br />表示'''[[藍移]]''')
| h_radial_v = −9100 km/s
| appmag_v = 12.78 <ref>{{Cite web |url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=NGC%20%206166 |title=存档副本 |accessdate=2014-08-30 |archive-date=2015-06-18 |archive-url=https://web.archive.org/web/20150618172530/http://simbad.u-strasbg.fr/simbad/sim-id?Ident=NGC%20%206166 |dead-url=no }}</ref>
 | size_v = 1.9’ x 1.4’
| constellation name = [[武仙座]]
| absmag_v = −24.1
| names = '''UGC''' 10409 '''CGCG''' 2205.6+3107 0504 '''MCG''' +07 -34-060 058 265 338
}}
 
'''NGC 6166'''是[[阿貝爾2199]]星系團中的一個[[橢圓星系]]，位於[[武仙座]]，距離地球4億9千萬年。在這個星系團中主要的星系是在[[X射線]]排放上，已知最明亮的星系之一<ref>{{cite journal |last=Bridges |first=T.J. |last2=Cater |first2=D |date=April 26, 1996 |title=B-R Colors of Globular Clusters in NGC 6166 (A2199) |journal=The Astrophysical Journal |volume= |page=1 |arxiv=astro-ph/9604159v1 |accessdate=February 3, 2013 |url=http://arxiv.org/pdf/astro-ph/9604159v1.pdf |bibcode=1996MNRAS.281.1290B |archive-date=2017-07-29 |archive-url=https://web.archive.org/web/20170729051430/https://arxiv.org/pdf/astro-ph/9604159v1.pdf |dead-url=no }}</ref>。

== 敘述 ==
NGC 6166是質量特別大的[[cD星系]]，並且是這一類型星系的好例子，在它的內部還有幾個小星系<ref>{{Cite web |url=http://ned.ipac.caltech.edu/cgi-bin/nph-datasearch?search_type=Note_id&objid=57565&objname=NGC%206166&img_stamp=YES&hconst=73.0&omegam=0.27&omegav=0.73&corr_z=1&of=table |title=Notes for object NGC 6166 (NED) |accessdate=2014-08-30 |archive-date=2019-02-17 |archive-url=https://web.archive.org/web/20190217083900/http://ned.ipac.caltech.edu/cgi-bin/nph-datasearch?search_type=Note_id&objid=57565&objname=NGC |dead-url=no }}</ref>。

它被懷疑是經過大量的星系碰撞造成的，並且擁有為數眾多的[[球狀星團]]（數量在6,200至22,000之間）<ref>{{cite journal |last=Bridges |first=T.J. |last2=Cater |first2=D |date=April 26, 1996 |title=B-R Colors of Globular Clusters in NGC 6166 (A2199) |journal=The Astrophysical Journal |volume= |page=3 |arxiv=astro-ph/9604159v1 |accessdate=February 3, 2013 |url=http://arxiv.org/pdf/astro-ph/9604159v1.pdf |bibcode=1996MNRAS.281.1290B |archive-date=2017-07-29 |archive-url=https://web.archive.org/web/20170729051430/https://arxiv.org/pdf/astro-ph/9604159v1.pdf |dead-url=no }}</ref> 環繞星系核心.<ref>http://adsabs.harvard.edu/full/1990ApJ...355..410P</ref>。

這個星系中心藏有超大質量[[黑洞]]，估計有著十億<math>\begin{smallmatrix}M_\odot\end{smallmatrix}</math><ref name="Di Matteo L19">{{cite journal |last=Di Matteo |first=Tiziana |last2=Johnstone |first2=Roderick M |date=March 8, 2001 |title=Accretion onto Nearby Supermassive Black Holes: Chandra Constraints on the Dominant Cluster Galaxy NGC 6166 |journal=The Astrophysical Journal |volume=550 |page=L19 |arxiv=astro-ph/0012194 |id= |accessdate= |url=http://iopscience.iop.org/1538-4357/550/1/L19/fulltext/ |bibcode=2001ApJ...550L..19D |doi=10.1086/319489 |archive-date=2020-02-20 |archive-url=https://web.archive.org/web/20200220093211/https://iopscience.iop.org/article/10.1086/319489 |dead-url=no }}</ref>。

NGC 6166也是眾所周知的[[活躍星系核]]，被歸類為FRI[[無線電波源|源]]，有對稱的兩個秒差距尺度無線電噴流和無線電瓣，並且引起體氣體進入造成[[冷卻流]]，每年會累積200太陽質量的氣體<ref name="Di Matteo L19"/>。

曾有人指出NGC 6166的中心可能會有一些[[恆星光譜|O-型恆星]] <ref name="Fisher1995">{{cite journal
    | author=Fisher, David; Illingworth, Garth; Franx, Marijn
    | title=Kinematics of 13 brightest cluster galaxies
    | journal=The Astrophysical Journal Letters
    | year=1995
    | volume=438
    | number=2
    | pages=539–562
    | bibcode=1995ApJ...438..539F
    | doi=10.1086/175100}}</ref>。

== 相關條目 ==
*[[阿貝爾2199]]
*[[星系列表]]

== 參考資料 ==
{{reflist}}

[[Category:阿貝爾天體|2199]]
[[Category:活躍星系]]
[[Category:武仙座NGC天體|6166]]
[[Category:電波星系]]