imported>InternetArchiveBot：Add 1 book for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot

2025-10-18T02:07:04Z

Add 1 book for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot

新页面

{{Infobox Galaxy
| name = [[梅西耶天體|梅西耶]] 74
| image = [[File:PESSTO Snaps Supernova in Messier 74.jpg|250px]]
|caption =美麗的螺旋星系，M74
| epoch = [[J2000]]
| constellation name = [[雙魚座]]<ref name="sinnott1988">
{{cite book
| editor=R. W. Sinnott
| title= The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer
| url=https://archive.org/details/ngc20000complete0000drey
| date=1988
| publisher=[[Sky Publishing Corporation]] / [[Cambridge University Press]]
| isbn=0-933346-51-4
}}</ref>
| type = SA(s)c<ref name="ned" />
| ra = {{RA|01|36|41.8}}<ref name="ned" />
| dec = {{DEC|+15|47|01}}<ref name="ned" />
| dist_ly = 30 ± 6 [[光年|Mly]]<ref name="hendryetal2005" />
| z = 657 [[公里|km]]/[[秒|s]]<ref name="ned" />
| stars = 1000億（1×10<sup>11</sup>）
| appmag_v = 10.0<ref name="ned" />
| size_v = 10′.5 × 9′.5<ref name="ned" />
| names = [[NGC天體|NGC]] 628, [[Uppsala General Catalogue|UGC]] 1149, [[Principal Galaxies Catalogue|PGC]] 5974<ref name="ned" />
|size = 95,000光年(直徑)<ref>{{Cite web |url=http://messier.seds.org/m/m074.html |title=存档副本 |accessdate=2016-02-24 |archive-date=2015-02-27 |archive-url=https://web.archive.org/web/20150227083245/http://messier.seds.org/m/m074.html |dead-url=no }}</ref>}}

'''M74''' （也稱為'''NGC 628'''）位於[[星座]][[雙魚座]]內，是一個正面朝向地球的[[螺旋星系]]，與地球的距離為3200萬光年<ref name="APOD">{{cite web|title=Astronomy Picture of the Day, M74: The Perfect Spiral|url=http://apod.nasa.gov/apod/ap110406.html|publisher=NASA|accessdate=2011-04-07|date=2011-04-06|archive-date=2013-06-25|archive-url=https://www.webcitation.org/6HdFqoOm4?url=http://apod.nasa.gov/apod/ap110406.html|dead-url=no}}</ref>。這個星系有兩條明顯的[[螺旋臂]]，因此被作為[[宏觀螺旋星系]]的典型範例<ref name="carnegieatlas">
{{cite book
| author=A. Sandage | author2=J. Bedke
| date=1994
| title=Carnegie Atlas of Galaxies
| publisher=[[Carnegie Institution of Washington]]
| isbn=0-87279-667-1
}}</ref>。這個星系的低表面亮度，使它成為業餘天文學家最難觀測的[[梅西耶天體]]之一<ref name="omeara1998">
{{cite book
| author=S. J. O'Meara
| date=1998
| title=The Messier Objects
| publisher=[[Cambridge University Press]]
| isbn=0-521-55332-6
}}</ref><ref name="jones1991">
{{cite book
| author=K. G. Jones
| date=1991 | edition= 2nd
| title=Messier's Nebulae and Star Clusters
| publisher=[[Cambridge University Press]]
| location=Cambridge
| isbn=0-521-37079-5
}}</ref>。然而，相對較大的視角大小和以正面朝向地球，使它成為專業天文學家研究[[螺旋臂]]和[[密度波|螺旋臂密度波]]的理想天體。估計M74擁有1,000億顆恆星<ref name="APOD"/>。

== 歷史 ==
M74是[[皮埃爾·梅香]]在1780年發現的。然後梅香將他的發現通知[[查爾斯·梅西耶|梅西耶]]，後者並將這個星系列入[[梅西耶天體]] <ref name="jones1991" />

== 超新星 ==
已經在M74發現三顆[[超新星]]<ref name="ned">{{cite web
| title=NASA/IPAC Extragalactic Database
| work=Results for NGC 628
| url=http://ned.ipac.caltech.edu/cgi-bin/objsearch?objname=messier+74&extend=no&hconst=73&omegam=0.27&omegav=0.73&corr_z=1&out_csys=Equatorial&out_equinox=J2000.0&obj_sort=RA+or+Longitude&of=pre_text&zv_breaker=30000.0&list_limit=5&img_stamp=YES
| accessdate=2006-08-12
| archive-date=2019-02-17
| archive-url=https://web.archive.org/web/20190217031838/http://ned.ipac.caltech.edu/cgi-bin/objsearch?objname=messier+74&extend=no&hconst=73&omegam=0.27&omegav=0.73&corr_z=1&out_csys=Equatorial&out_equinox=J2000.0&obj_sort=RA+or+Longitude&of=pre_text&zv_breaker=30000.0&list_limit=5&img_stamp=YES
| dead-url=no
}}</ref>：[[SN 2002ap]]<ref name="iauc7810">
{{cite journal
| last=Nakano | first=S.
| last2=Hirose | first2=Y.
| last3=Kushida | first3=R.
| last4=Kushida | first4=Y.
| last5=Li | first5=W.
| date=2002
| title=Supernova 2002ap in M74
| journal=IAU Circular
| volume=7810 | pages=1
| bibcode=2002IAUC.7810....1N
}}</ref>、[[SN 2003gd]]<ref name="iauc8150">
{{cite journal
| author=R. Evans
| author2=R. H. McNaught
| title=Supernova 2003gd in M74
| journal=[[IAU Circular]]
| date=2003
| volume=8150 | pages=2
| bibcode=2003IAUC.8150....2E
}}</ref>和[[SN 2013ej]]。

SN 2002ap是距離在10[[秒差距|百萬秒差距]]以內，又是近幾年相當少見的[[Ic型超新星]]（或是[[極超新星]]），因此吸引了相當大的注意<ref name="mazzalietal2002">
{{cite journal
| author=P. A. Mazzali
| author2=J. Deng
| author3=K. Maeda
| author4=K. Nomoto
| author5=H. Umeda
| author6=K. hatano
| author7=K. Iwamoto
| author8=Y. Yoshii
| author9=Y. Kobayashi
| author10=T. Minezaki
| author11=M. Doi
| author12=K. Enya
| author13=H. Tomita
| author14=S. J. Smartt
| author15=K. Kinugasa
| author16=H. Kawakita
| author17=K. Ayani
| author18=T. Kawabata
| author19=H. Yamaoka
| author20=Y. L. Qiu
| author21=K. Motohara
| author22=C. L. Gerardy
| author23=R. Fesen
| author24=K. S. Kawabata
| author25=M. Iye
| author26=N. Kashikawa
| author27=G. Kosugi
| author28=Y. Ohyama
| author29=M. Takada-Hidai
| author30=G. Zhao
| author31=R. Chornock
| author32=A. V. Filippenko
| author33=S. Benetti
| author34=M. Turatto
| displayauthors=6
| date=2002
| title=The Type Ic Hypernova SN 2002ap
| journal=[[Astrophysical Journal]]
| volume=572
| issue=1 | pages=L61–L65
| bibcode=2002ApJ...572L..61M
| doi=10.1086/341504
}}</ref><ref name="smarttetal2002">
{{cite journal
| author=S. J. Smartt
| author2=P. M. Vreeswijk
| author3=E. Ramirez-Ruiz
| author4=G. F. Gilmore
| author5=W. P. S. Meikle
| author6=A. M. N. Ferguson
| author7=J. H. Knapen
| displayauthors=6
| date=2002
| title=On the Progenitor of the Type Ic Supernova 2002ap
| journal=[[Astrophysical Journal]]
| volume=572
| issue=2 | pages=L147–L151
| bibcode=2002ApJ...572L.147S
| doi=10.1086/341747
|arxiv = astro-ph/0205241 }}</ref><ref name="galyametal2002">
{{cite journal
| author=A. Gal-Yam | author2=E. O. Ofek | author3=O. Shemmer
| date=2002
| title=Supernova 2002ap: The first month
| journal=[[Monthly Notices of the Royal Astronomical Society Letters]]
| volume=332
| issue=4 | pages=L73–L77
| bibcode=2002MNRAS.332L..73G
| doi=10.1046/j.1365-8711.2002.05535.x
|arxiv = astro-ph/0204008 }}</ref>。這顆超新星已經被用來測試距離更遙遠，類似Ic型超新星起源的理論<ref name="smarttetal2002" />，和超新星與[[伽瑪射線暴]]之間關連性的理論<ref name="galyametal2002" />。

SN 2003gd是IIp型超新星<ref name="vandyketal2003">
{{cite journal
| author=S. D. Van Dyk | author2=W. Li | author3=A. V. Filippenko
| date=2003
| title=On the Progenitor of the Type II-Plateau Supernova 2003gd in M74
| journal=[[Publications of the Astronomical Society of the Pacific]]
| volume=115
| issue=813 | pages=1289–1295
| bibcode=2003PASP..115.1289V
| doi=10.1086/378308
|arxiv = astro-ph/0307226 }}</ref>。II型超新星的[[亮度]]已經知道，所以它們可以用來精確的測量距離。使用SN 2003gd測得M74的距離是9.6 ± 2.8[[秒差距]]，或是31 ± 9 百萬[[光年]]<ref name="hendryetal2005">
{{cite journal
| author=M. A. Hendry
| author2=S. J. Smartt
| author3=J. R. Maund
| author4=A. Pastorello
| author5=L. Zampieri
| author6=S. Benetti
| author7=M. Turatto
| author8=E. Cappellaro
| author9=W. P. S. Meikle
| author10=R. Kotak
| author11=M. J. Irwin
| author12=P. G. Jonker
| author13=L. Vermaas
| author14=R. F. Peletier
| author15=H. van Woerden
| author16=K. M. Exter
| author17=D. L. Pollacco
| author18=S. Leon
| author19=S. Verley
| author20=C. R. Benn
| author21=G. Pignata
| displayauthors=6
| date=2005
| title=A study of the Type II-P supernova 2003gd in M74
| journal=[[Monthly Notices of the Royal Astronomical Society]]
| volume=359
| issue=3 | pages=906–926
| bibcode=2005MNRAS.359..906H
| doi=10.1111/j.1365-2966.2005.08928.x
|arxiv = astro-ph/0501341 }}</ref>。用最明亮的超巨星做為比較，測得的距離是7.7±1.7[[秒差距|Mpc]]和9.6±2.2[[秒差距|Mpc]] <ref name="hendryetal2005" />。Ben E. K. Sugerman發現與SN 2003gd相關聯的''回光'' —— 爆炸後出現本身的反射光<ref name="sugerman2005">
{{cite journal
| author=B. E. K. Sugerman
| date=2005
| title=Discovery of a Light Echo from SN 2003gd
| journal=[[Astrophysical Journal Letters]]
| volume=632
| issue=1 | pages=L17–L20
| bibcode=2005ApJ...632L..17S
| doi=10.1086/497578
|arxiv = astro-ph/0509009 }}</ref>。只有少數的超新星發現過這種反射光。這種反射似乎是來自超新星爆炸之前擴散出去，類似板狀雲的塵埃殼層，可以用來確認星際塵埃的成分<ref name="sugerman2005" /><ref name="vandyketal2006">
{{cite journal
| author=S. D. Van Dyk | author2=W. Li | author3=A. V. Filippenko
| date=2006
| title=The Light Echo around Supernova 2003gd in Messier 74
| journal=[[Publications of the Astronomical Society of the Pacific]]
| volume=118
| issue=841 | pages=351–357
| bibcode=2006PASP..118..351V
| doi=10.1086/500225
|arxiv = astro-ph/0508684 }}</ref>。

== 星系群的資訊 ==
M74是[[M74星系群]]中最亮的成員，這個群組有5-7個星系，包括[[特殊星系|特殊的]][[螺旋星系]][[NGC 660]]和幾個[[不規則星系]] <ref name="nbg">
{{cite book
| author=R. B. Tully
| date=1988
| title=Nearby Galaxies Catalog
| publisher=[[Cambridge University Press]]
| isbn=0-521-35299-1
}}</ref><ref name="garcia1993">
{{cite journal
| author=A. Garcia
| date=1993
| title=General study of group membership. II – Determination of nearby groups
| journal=[[Astronomy and Astrophysics Supplement]]
| volume=100 | pages=47–90
| bibcode=1993A&AS..100...47G
}}</ref><ref name="giuricinetal2002">
{{cite journal
| author=G. Giuricin | author2=C. Marinoni | author3=L. Ceriani | author4=A. Pisani
| date=2000
| title=Nearby Optical Galaxies: Selection of the Sample and Identification of Groups
| url=https://archive.org/details/sim_astrophysical-journal_2000-11-01_543_1/page/178 | journal=[[Astrophysical Journal]]
| volume=543
| issue=1 | pages=178–194
| bibcode=2000ApJ...543..178G
| doi=10.1086/317070
|arxiv = astro-ph/0001140 }}</ref>。由於用不同的方法識別組織的成員，有不同的結果，因此只有全都確定的才被納入群組<ref name="giuricinetal2002" />，所以群組確實的數量仍是未知數。

== 恆星形成 ==
[[File:M74 3.6 5.8 8.0 microns spitzer.png|thumb|left|250px|M74是[[史匹哲太空望遠鏡]]的[[史匹哲鄰近紅外星系調查]]的一部分。藍色是波長3.6微米的輻射。綠色和紅色分別代表可能來自[[多環芳香烴]]，也可能是塵埃的5.8和8.0微米的輻射。]]
{{-}}

== 疑似黑洞 ==
在2005年3月22日，[[錢德拉X射線天文台]]宣布<ref name="chandra2005">{{Cite web |url=http://chandra.harvard.edu/photo/2005/m74/index.html |title=Chandra :: Photo Album :: M74 :: 22 Mar 05 |accessdate=2016-02-25 |archive-date=2007-05-04 |archive-url=https://web.archive.org/web/20070504144127/http://chandra.harvard.edu/photo/2005/m74/index.html |dead-url=no }}</ref>在M74觀測到比[[中子星]]輻射更強的[[超亮X射線源]]（ULX，ultraluminous X-ray source），其週期約為2小時。估計它的質量是太陽的10,000倍，這是[[中等質量黑洞]]的一個指標。這是黑洞理論中的一種類型，其質量介於可能駐留在許多星系中心的超大質量黑洞和恆星黑洞之間。正因為這樣，它們被認為不是由單一的超新星形成，但有可能是少量的恆星黑洞聚集組成的星團。這個X射線源在被鑑定後，稱為CXOU J013651.1+154547。

== 業餘天文學觀測資訊 ==
M74位於[[雙魚座η]]東北東方1.5°<ref name="omeara1998" /><ref name="jones1991" />，是梅西耶天體中第二黯淡的（只有M91比他更暗淡）。除非天空夠黑暗以及晴朗，否則很難找到它<ref name="jones1991" />，所以在受到[[光汙染]]的地點很難看見它<ref name="omeara1998" />。這個天體比較適合使用低的放大倍率觀賞，在高倍率下會因為過度擴散，多數人會因為太微弱反而看不見<ref name="jones1991" />。此外，在完全[[適應 (眼)|適應]]黑暗的場所，使用[[側視|眼角餘光]]通常比較容易看見<ref name="omeara1998" /><ref name="jones1991" />。

== 相關條目 ==
{{commons|M74}}
* [[NGC 3184]]：一個相似的，以正面朝向的螺旋星系。
* [[風車星系|M101]]：一個相似的，以正面朝向的螺旋星系。
* [[渦狀星系]]：著名的以正面朝向的螺旋星系。

== 參考資料 ==
{{reflist}}

== 外部連結 ==
* {{WikiSky}}
* [http://messier.seds.org/m/m074.html Spiral Galaxy M74 @ SEDS Messier pages] {{Wayback|url=http://messier.seds.org/m/m074.html |date=20150227083245 }}
* {{cite web|last=Barrena|first=Rafael|title=M74 – Spiral Galaxy|url=http://www.deepskyvideos.com/videos/messier/M74.html|work=Deep Sky Videos|publisher=[[Brady Haran]]|author2=Crowther, Paul|accessdate=2016-02-25|archive-date=2020-07-02|archive-url=https://web.archive.org/web/20200702193658/http://www.deepskyvideos.com/videos/messier/M74.html|dead-url=no}}

{{梅西耶天體}}
{{Sky|01|36|41.8|+|15|47|01|30000000}}

[[Category:梅西耶天體|074]]
[[Category:螺旋星系|M074]]
[[Category:無棒螺旋星系|M074]]
[[Category:M74星系群|M074]]
[[Category:雙魚座|M074]]
[[Category:双鱼座NGC天体]]
[[Category:NGC天體|M074]]
[[Category:UGC天體|01149]]
[[Category:PGC天體|05974]]
[[Category:1780年發現的天體]]

M74 - 版本历史

imported>InternetArchiveBot：​Add 1 book for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot

imported>InternetArchiveBot：Add 1 book for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot