NGC 1275:修订间差异
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小 機器人 新增: hr:NGC 1275 |
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{{Infobox Galaxy |
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{{NGCInfoBox|NGCID=NGC 1275|發現者=德亞瑞司特|發現日期=1863年2月14日|其他編號=UGC 2669,MCG 7-7-63,ZWG 540.103|曆元=J2000.0|赤經=3時19分48.1秒 |
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| image = [[Image:NGC 1275 Hubble.jpg|280px|]] |
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|赤緯=41°30'41"|星座=英仙座|星體=星系|星等=11.7|表面亮度=13|藍等=12.7}} |
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| caption = [[哈柏太空望遠鏡]]的NGC 1275影像 |
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| credit = HST/[[NASA]]/[[ESA]]/[[STScI]]/[[AURA]]. |
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| name = [[New General Catalogue|NGC]] 1275 |
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| epoch = [[J2000]] |
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| type = cD;pec;NLRG<ref name="ned">{{cite web |
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| title=NASA/IPAC Extragalactic Database |
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| work=Results for NGC 3109 |
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| url=http://nedwww.ipac.caltech.edu/ |
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| accessdate=2006-11-19 }}</ref> |
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| ra = {{RA|03|19|48.1}}<ref name="ned" /> |
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| dec = {{DEC|+41|30|42}}<ref name="ned" /> |
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| dist_ly = 235 [[光年|Mly]] |
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| z = 5264 ± 11 公里/[[秒]]<ref name="ned" /> |
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| appmag_v = 12.6<ref name="ned" /> |
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| size_v = 2′.2 × 1′.7<ref name="ned" /> |
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| constellation name = [[英仙座]] |
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| notes = |
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| names = Perseus A,<ref name="ned" /> [[Principal Galaxies Catalogue|PGC]] 12429,<ref name="ned" /> [[Uppsala General Catalogue|UGC]] 2669<ref name="ned" /> |
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}} |
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''' NGC 1275 '''(也稱為英仙座 A)是1.5型的[[西佛星系]] <ref name="hoetal1997">{{citation |
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| last1 = Ho |
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| first1 = Luis C. |
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| last2 = Filippenko |
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| first2 = Alex V. |
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| last3 = Sargent |
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| first3 = Wallace L. W. |
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| title = A Search for "Dwarf" Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies |
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| year = 1997 |
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| date = October 1997 |
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| periodical = Astrophysical Journal Supplement |
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| volume = 112 |
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| pages = 315-390 |
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| URL = http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1997ApJS..112..315H |
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}}</ref>,位在[[英仙座]]的方向上,距離大約2億3500萬[[光年]]。NGC 1275對應於[[電波星系]][[NGC 1275|英仙座 A]],是位於巨大的[[英仙座星系團]]中心的星系。 |
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== 動力學 == |
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[[Image:Ngc1275a.jpg|250px|thumb|left|[[哈柏太空望遠鏡]](HST)的NGC 1275影像。創建者:HST/[[NASA]]/[[ESA]]。]] |
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{{commons|Category:NGC 1275|NGC 1275}} |
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NGC 1275包含2個星系,在[[英仙座星系團]]中央的[[CD 星系]],和躺在前方以3,000公里/秒朝向主體高度移動,並且相信應該與[[英仙座星系團]]合併的"高速系統"(HVS)<ref>Minkowski R., 1957, in IAU Symp 4, Radio astronomy, p107 |
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</ref>。HVS與[[CD 星系]]的距離至少有20萬光年,因此不受它的影響<ref>Gillmon K., Sanders J.S., Fabian A.C., [http://adsabs.harvard.edu/abs/2004MNRAS.348..159G An X-ray absorption analysis of the high-velocity system in NGC 1275], 2004, [[MNRAS]], 348, 159</ref>。星系團中心的星系包含散發出纖維狀[[譜線]]的大質量網路<ref>Lynds R., [http://adsabs.harvard.edu/abs/1970ApJ...159L.151L Improved Photographs of the NGC1275 Phenomenon], 1970, ApJ, 159, L151 |
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</ref>,看起來似乎會延遲相對論性[[電漿]]引發的氣泡在中心的[[活躍星系核]]中的生成<ref>Hatch N.A., Crawford C.S., Johnstone R.M., Fabian A.C.: [http://ukads.nottingham.ac.uk/abs/2006MNRAS.367..433H On the origin and excitation of the extended nebula surrounding NGC1275], 2006, [[MNRAS]], 367, 433</ref>。由氣體組成長的氣體絲成螺旋狀的延伸至星系之外,進入數百萬度高溫,充滿了星系團輻射出X射線的氣體。在一條典型螺旋細絲上的氣體包含的質量百萬倍於我們的太陽,但寬度只有200光年,並且可以筆直的延伸達20,000光年<ref>[http://newswise.com/articles/view/543637/ Hubble Sees Magnetic Monster in Erupting Galaxy] Newswise, Retrieved on [[August 21]], [[2008]].</ref>。 |
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細絲的存在引發一個問題,因為它們的溫度比星系團周圍的雲氣低,它們是如何或許維持了一億年之?它們為何不會變暖?消散或是塌縮成為恆星<ref name="nature20080821">{{ cite journal | url=http://www.nature.com/nature/journal/v454/n7207/abs/nature07169.html | title=Magnetic support of the optical emission line filaments in NGC 1275 | author=A. C. Fabian, et al. | journal=[[Nature (journal)|Nature]] | volume=454 | pages=968-970 | date=[[2008-08-21]] }}</ref><ref name="nytimes20080821">{{cite news | url=http://www.nytimes.com/2008/08/26/science/space/26galaxy.html | title=Hubble Images Solve Galactic Filament Mystery | first=Kenneth | last=Chang | publisher=[[The New York Times]] | date=2008-08-21 }}</ref>?一個可能是有著微弱的磁場(大約地球磁場強度的萬分之一)施加了足夠的力量使[[離子]]在螺線上聚集<ref name="nature20080821"/><ref name="nytimes20080821"/>。 |
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{{-}} |
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== 外部鏈結 == |
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* {{WikiSky}} |
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* [http://apod.gsfc.nasa.gov/apod/ap030505.html NASA image & description] |
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* [http://antwrp.gsfc.nasa.gov/apod/ap050725.html Another NASA image, showing unusual gas filaments] |
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* Fabian, A.C., et al. [http://arxiv.org/abs/astro-ph/0306036 A deep Chandra observation of the Perseus cluster: shocks and ripples]. Monthly Notices of the Royal Astronomical Society. Vol. 344 (2003): L43 (arXiv:astro-ph/0306036v2). |
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* Fabian, A.C. [http://www.nature.com/nature/journal/v454/n7207/abs/nature07169.html Nature 454, 968-970] |
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== 參考資料 == |
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{{Reflist}} |
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{{Sky|03|19|48.1|+|41|30|42|235000000}} |
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[[Category:特殊星系]] |
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[[Category:交互作用星系]] |
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[[Category:西佛星系]] |
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[[Category:星爆星系]] |
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[[Category:電波星系]] |
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[[Category:英仙座]] |
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[[Category:NGC天體|1275]] |
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[[Category:UGC天體|02669]] |
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[[Category:PGC天體|12429]] |
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[[Category:3C天體|84]] |
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[[Category:英仙座星系團]] |
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{{galaxy-stub}} |
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'''NGC 1275'''(英仙座A)是[[英仙座]]中一個少見的[[星系]]。 |
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{{NGCReference|1275}} |
{{NGCReference|1275}} |
2009年3月31日 (二) 13:03的版本
NGC 1275 | |
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哈柏太空望遠鏡的NGC 1275影像 | |
观测资料(J2000 曆元) | |
星座 | 英仙座 |
赤经 | 03h 19m 48.1s[1] |
赤纬 | +41° 30′ 42″[1] |
紅移 | 5264 ± 11 公里/秒[1] |
距离 | 235 Mly |
视星等 (V) | 12.6[1] |
特征 | |
类型 | cD;pec;NLRG[1] |
角直徑 (V) | 2′.2 × 1′.7[1] |
其他名称 | |
Perseus A,[1] PGC 12429,[1] UGC 2669[1] | |
NGC 1275 (也稱為英仙座 A)是1.5型的西佛星系 [2],位在英仙座的方向上,距離大約2億3500萬光年。NGC 1275對應於電波星系英仙座 A,是位於巨大的英仙座星系團中心的星系。
動力學
NGC 1275包含2個星系,在英仙座星系團中央的CD 星系,和躺在前方以3,000公里/秒朝向主體高度移動,並且相信應該與英仙座星系團合併的"高速系統"(HVS)[3]。HVS與CD 星系的距離至少有20萬光年,因此不受它的影響[4]。星系團中心的星系包含散發出纖維狀譜線的大質量網路[5],看起來似乎會延遲相對論性電漿引發的氣泡在中心的活躍星系核中的生成[6]。由氣體組成長的氣體絲成螺旋狀的延伸至星系之外,進入數百萬度高溫,充滿了星系團輻射出X射線的氣體。在一條典型螺旋細絲上的氣體包含的質量百萬倍於我們的太陽,但寬度只有200光年,並且可以筆直的延伸達20,000光年[7]。
細絲的存在引發一個問題,因為它們的溫度比星系團周圍的雲氣低,它們是如何或許維持了一億年之?它們為何不會變暖?消散或是塌縮成為恆星[8][9]?一個可能是有著微弱的磁場(大約地球磁場強度的萬分之一)施加了足夠的力量使離子在螺線上聚集[8][9]。
外部鏈結
- WikiSky上关于NGC 1275的内容:DSS2, SDSS, GALEX, IRAS, 氢α, X射线, 天文照片, 天图, 文章和图片
- NASA image & description
- Another NASA image, showing unusual gas filaments
- Fabian, A.C., et al. A deep Chandra observation of the Perseus cluster: shocks and ripples. Monthly Notices of the Royal Astronomical Society. Vol. 344 (2003): L43 (arXiv:astro-ph/0306036v2).
- Fabian, A.C. Nature 454, 968-970
參考資料
- ^ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 NASA/IPAC Extragalactic Database. Results for NGC 3109. [2006-11-19].
- ^ Ho, Luis C.; Filippenko, Alex V.; Sargent, Wallace L. W., A Search for "Dwarf" Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies, Astrophysical Journal Supplement 112, October 1997, 112: 315–390
- ^ Minkowski R., 1957, in IAU Symp 4, Radio astronomy, p107
- ^ Gillmon K., Sanders J.S., Fabian A.C., An X-ray absorption analysis of the high-velocity system in NGC 1275, 2004, MNRAS, 348, 159
- ^ Lynds R., Improved Photographs of the NGC1275 Phenomenon, 1970, ApJ, 159, L151
- ^ Hatch N.A., Crawford C.S., Johnstone R.M., Fabian A.C.: On the origin and excitation of the extended nebula surrounding NGC1275, 2006, MNRAS, 367, 433
- ^ Hubble Sees Magnetic Monster in Erupting Galaxy Newswise, Retrieved on August 21, 2008.
- ^ 8.0 8.1 A. C. Fabian; et al. Magnetic support of the optical emission line filaments in NGC 1275. Nature. 2008-08-21, 454: 968–970.
- ^ 9.0 9.1 Chang, Kenneth. Hubble Images Solve Galactic Filament Mystery. The New York Times. 2008-08-21.
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