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{{Infobox Galaxy
{{Infobox galaxy
| name = [[Messier object|Messier]] 74
| name = [[w:Messier object|Messier]] 74
| image = [[Image:NGC 628.jpg|350px]]
| image = [[file:Messier 74 by HST.jpg|350px]]
|caption = Messier 74. Credit: NASA/ESA/GMOS/HST.
|caption = Messier 74. Credit: NASA/HST.
| epoch = [[J2000]]
| epoch = [[w:J2000]]
| constellation name = [[Pisces (constellation)|Pisces]]<ref name="sinnott1988">{{cite book
| constellation name = [[w:Pisces (constellation)|Pisces]]<ref name="sinnott1988">{{cite book
| author=R. W. Sinnott, editor
| author=R. W. Sinnott, editor
| title= The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer
| title= The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer
Line 13: Line 13:
| ra = {{RA|01|36|41.8}}<ref name="ned" />
| ra = {{RA|01|36|41.8}}<ref name="ned" />
| dec = {{DEC|+15|47|01}}<ref name="ned" />
| dec = {{DEC|+15|47|01}}<ref name="ned" />
| dist_ly = 30 ± 6 [[light-year|Mly]]<ref name="hendryetal2005" />
| dist_ly = 30 ± 6 [[w:light-year|Mly]]<ref name="hendryetal2005" />
| z = 657 [[kilometer|km]]/[[second|s]]<ref name="ned" />
| z = 657 [[w:kilometer|km]]/[[w:second|s]]<ref name="ned" />
| appmag_v = 10.0<ref name="ned" />
| appmag_v = 10.0<ref name="ned" />
| size_v = 10&prime;.5 &times; 9&prime;.5<ref name="ned" />
| size_v = 10&prime;.5 &times; 9&prime;.5<ref name="ned" />
| names = [[New General Catalogue|NGC]] 628, [[Uppsala General Catalogue|UGC]] 1149, [[Principal Galaxies Catalogue|PGC]] 5974<ref name="ned" />
| names = [[w:New General Catalogue|NGC]] 628, [[w:Uppsala General Catalogue|UGC]] 1149, [[w:Principal Galaxies Catalogue|PGC]] 5974<ref name="ned" />
}}
}}


'''Messier 74''' (also known as NGC 628) is a face-on [[spiral galaxy]] in the [[constellation]] [[Pisces (constellation)|Pisces]]. The galaxy contains two clearly-defined [[spiral arm]]s and is therefore used as an archetypal example of a [[Grand Design Spiral Galaxy]].<ref name="carnegieatlas">{{cite book
'''Messier 74''' (also known as NGC 628) is a face-on [[w:spiral galaxy]] in the [[w:constellation]] [[w:Pisces (constellation)|Pisces]]. The galaxy contains two clearly-defined [[w:spiral arm]]s and is therefore used as an archetypal example of a [[w:Grand Design Spiral Galaxy]].<ref name="carnegieatlas">{{cite book
| author=A. Sandage, J. Bedke
| author=A. Sandage, J. Bedke
| year=1994
| year=1994
Line 27: Line 27:
| publisher=Carnegie Institution of Washington
| publisher=Carnegie Institution of Washington
| location=Washington, D.C.
| location=Washington, D.C.
| isbn=0-87279-667-1 }}</ref> The galaxy's low surface brightness makes it the most difficult [[Messier Catalogue|Messier object]] for amateur astronomers to observe.<ref name="omeara1998">{{cite book
| isbn=0-87279-667-1 }}</ref> The galaxy's low surface brightness makes it the most difficult [[w:Messier Catalogue|Messier object]] for amateur astronomers to observe.<ref name="omeara1998">{{cite book
| author=S. J. O'Meara
| author=S. J. O'Meara
| year=1998
| year=1998
Line 41: Line 41:
| publisher=Cambridge University Press
| publisher=Cambridge University Press
| location=Cambridge
| location=Cambridge
| isbn=0-521-37079-5 }}</ref> However, the relatively large angular size of the galaxy and the galaxy's face-on orientation make it an ideal object for professional astronomers who want to study [[spiral arm]] structure and [[Density wave theory|spiral density wave]]s.
| isbn=0-521-37079-5 }}</ref> However, the relatively large angular size of the galaxy and the galaxy's face-on orientation make it an ideal object for professional astronomers who want to study [[w:spiral arm]] structure and [[w:Density wave theory|spiral density wave]]s.


==History==
==History==
⚫
M74 was discovered by [[w:Pierre Méchain]] in [[w:1780]]. Méchain then communicated his discovery to [[w:Charles Messier]], who listed the galaxy in his [[w:Messier Catalogue|catalog]].<ref name="jones1991" />

⚫
M74 was discovered by [[Pierre Méchain]] in [[1780]]. Méchain then communicated his discovery to [[Charles Messier]], who listed the galaxy in his [[Messier Catalogue|catalog]].<ref name="jones1991" />


==Supernovae==
==Supernovae==
⚫
Two [[w:supernovae]] have been identified in M74:<ref name="ned">{{cite web
<!-- Image with unknown copyright status removed: [[Image:NGC 678.jpg|thumb|left| SN 2003gd|{{deletable image-caption|1=Thursday, 17 April 2008}}]] -->

⚫
Two [[supernovae]] have been identified in M74:<ref name="ned">{{cite web
| title=NASA/IPAC Extragalactic Database
| title=NASA/IPAC Extragalactic Database
| work=Results for NGC 628
| work=Results for NGC 628
| url=http://nedwww.ipac.caltech.edu/
| url=http://nedwww.ipac.caltech.edu/
| accessdate=2006-08-12
| accessdate=2006-08-12
| accessdate=2006-08-12}}</ref> [[SN 2002ap]]<ref name="iauc7810">{{cite journal
| accessdate=2006-08-12}}</ref> [[w:SN 2002ap]]<ref name="iauc7810">{{cite journal
| author=S. Nakano, R. Kushida, Y. Kushida, W. Li
| author=S. Nakano, R. Kushida, Y. Kushida, W. Li
| title=Supernova 2002ap in M74
| title=Supernova 2002ap in M74
Line 61: Line 58:
| year=2002
| year=2002
| volume=7810
| volume=7810
| url=http://adsabs.harvard.edu/abs/2002IAUC.7810....1N}}</ref> and [[SN 2003gd]].<ref name="iauc8150">{{cite journal
| url=http://adsabs.harvard.edu/abs/2002IAUC.7810....1N}}</ref> and [[w:SN 2003gd]].<ref name="iauc8150">{{cite journal
| author=R. Evans, R. H. McNaught
| author=R. Evans, R. H. McNaught
| title=Supernova 2003gd in M74
| title=Supernova 2003gd in M74
Line 69: Line 66:
| url=http://adsabs.harvard.edu/abs/2003IAUC.8150....2E}}</ref>
| url=http://adsabs.harvard.edu/abs/2003IAUC.8150....2E}}</ref>


SN 2002ap has attracted considerable attention because it is one of the few Type Ic supernovae (or [[hypernova]]e) observed within 10 [[parsec|Mpc]] in recent years.<ref name="mazzalietal2002">{{cite journal
SN 2002ap has attracted considerable attention because it is one of the few Type Ic supernovae (or [[w:hypernova]]e) observed within 10 [[w:parsec|Mpc]] in recent years.<ref name="mazzalietal2002">{{cite journal
| author=P. A. Mazzali, J. Deng, K. Maeda, K. Nomoto, H. Umeda, K. hatano, K. Iwamoto, Y. Yoshii, Y. Kobayashi, T. Minezaki, M. Doi, K. Enya, H. Tomita, S. J. Smartt, K. Kinugasa, H. Kawakita, K. Ayani, T. Kawabata, H. Yamaoka, Y. L. Qiu, K. Motohara, C. L. Gerardy, R. Fesen, K. S. Kawabata, M. Iye, N. Kashikawa, G. Kosugi, Y. Ohyama, M. Takada-Hidai, G. Zhao, R. Chornock, A. V. Filippenko, S. Benetti, M. Turatto
| author=P. A. Mazzali, J. Deng, K. Maeda, K. Nomoto, H. Umeda, K. hatano, K. Iwamoto, Y. Yoshii, Y. Kobayashi, T. Minezaki, M. Doi, K. Enya, H. Tomita, S. J. Smartt, K. Kinugasa, H. Kawakita, K. Ayani, T. Kawabata, H. Yamaoka, Y. L. Qiu, K. Motohara, C. L. Gerardy, R. Fesen, K. S. Kawabata, M. Iye, N. Kashikawa, G. Kosugi, Y. Ohyama, M. Takada-Hidai, G. Zhao, R. Chornock, A. V. Filippenko, S. Benetti, M. Turatto
| title=The Type Ic Hypernova SN 2002ap
| title=The Type Ic Hypernova SN 2002ap
Line 93: Line 90:
| pages=L73–L77
| pages=L73–L77
| url=http://adsabs.harvard.edu/abs/2002MNRAS.332L..73G | doi=10.1046/j.1365-8711.2002.05535.x
| url=http://adsabs.harvard.edu/abs/2002MNRAS.332L..73G | doi=10.1046/j.1365-8711.2002.05535.x
}}</ref> This supernovae has been used to test theories on the origins of similar Type Ic supernovae at higher distances<ref name="smarttetal2002" /> and theories on the connection between supernovae and [[gamma ray burst]]s.<ref name="galyametal2002" />
}}</ref> This supernovae has been used to test theories on the origins of similar Type Ic supernovae at higher distances<ref name="smarttetal2002" /> and theories on the connection between supernovae and [[w:gamma ray burst]]s.<ref name="galyametal2002" />


SN 2003gd is a Type II-P supernova.<ref name="vandyketal2003">{{cite journal
SN 2003gd is a Type II-P supernova.<ref name="vandyketal2003">{{cite journal
Line 103: Line 100:
| pages=1289–1295
| pages=1289–1295
| url=http://adsabs.harvard.edu/abs/2003PASP..115.1289V
| url=http://adsabs.harvard.edu/abs/2003PASP..115.1289V
| doi=10.1086/378308}}</ref> Type II supernovae have known luminosities, so they can be used to accurately measure distances. The distance measured to M74 using SN 2003gd is 9.6 ± 2.8 [[parsec|Mpc]], or 31 ± 9 million [[light-year|ly]].<ref name="hendryetal2005">{{cite journal
| doi=10.1086/378308}}</ref> Type II supernovae have known luminosities, so they can be used to accurately measure distances. The distance measured to M74 using SN 2003gd is 9.6 ± 2.8 [[w:parsec|Mpc]], or 31 ± 9 million [[w:light-year|ly]].<ref name="hendryetal2005">{{cite journal
| author=M. A. Hendry, S. J. Smartt, J. R. Maund, A. Pastorello, L. Zampieri, S. Benetti, M. Turatto, E. Cappellaro, W. P. S. Meikle, R. Kotak, M. J. Irwin, P. G. Jonker, L. Vermaas, R. F. Peletier, H. van Woerden, K. M. Exter, D. L. Pollacco, S. Leon, S. Verley, C. R. Benn, G. Pignata
| author=M. A. Hendry, S. J. Smartt, J. R. Maund, A. Pastorello, L. Zampieri, S. Benetti, M. Turatto, E. Cappellaro, W. P. S. Meikle, R. Kotak, M. J. Irwin, P. G. Jonker, L. Vermaas, R. F. Peletier, H. van Woerden, K. M. Exter, D. L. Pollacco, S. Leon, S. Verley, C. R. Benn, G. Pignata
| title=A study of the Type II-P supernova 2003gd in M74
| title=A study of the Type II-P supernova 2003gd in M74
Line 111: Line 108:
| pages=906–926
| pages=906–926
| url=http://adsabs.harvard.edu/abs/2005MNRAS.359..906H | doi=10.1111/j.1365-2966.2005.08928.x
| url=http://adsabs.harvard.edu/abs/2005MNRAS.359..906H | doi=10.1111/j.1365-2966.2005.08928.x
}}</ref> For comparison, distances measured using the brightest supergiants are 7.7 ± 1.7 [[parsec|Mpc]] and 9.6 ± 2.2 [[parsec|Mpc]].<ref name="hendryetal2005" /> Ben E. K. Sugerman found a "light echo" - a reflection of supernova explosion that appeared after the explosion itself - associated with SN 2003gd.<ref name="sugerman2005">{{cite journal
}}</ref> For comparison, distances measured using the brightest supergiants are 7.7 ± 1.7 [[w:parsec|Mpc]] and 9.6 ± 2.2 [[w:parsec|Mpc]].<ref name="hendryetal2005" /> Ben E. K. Sugerman found a "light echo" - a reflection of supernova explosion that appeared after the explosion itself - associated with SN 2003gd.<ref name="sugerman2005">{{cite journal
| author=B. E. K. Sugerman
| author=B. E. K. Sugerman
| title=Discovery of a Light Echo from SN 2003gd
| title=Discovery of a Light Echo from SN 2003gd
Line 130: Line 127:


==Galaxy group information==
==Galaxy group information==
⚫
M74 is the brightest member of the [[w:M74 Group]], a group of 5-7 galaxies that also includes the [[w:peculiar galaxy|peculiar]] [[w:spiral galaxy]] [[w:NGC 660]] and a few [[w:irregular galaxies]].<ref name="nbg">{{cite book

⚫
M74 is the brightest member of the [[M74 Group]], a group of 5-7 galaxies that also includes the [[peculiar galaxy|peculiar]] [[spiral galaxy]] [[NGC 660]] and a few [[irregular galaxies]].<ref name="nbg">{{cite book
| author=R. B. Tully
| author=R. B. Tully
| year=1988
| year=1988
Line 156: Line 152:


==Star formation==
==Star formation==

{|
{|
| [[Image:M74 3.6 5.8 8.0 microns spitzer.png|thumb|250px|M74 as observed with the [[Spitzer Space Telescope]] as part of the [[Spitzer Infrared Nearby Galaxy Survey]]. The blue colors represent the 3.6 micrometre emission from stars. The green and red colors represent the 5.8 and 8.0 micrometre emission from [[polycyclic aromatic hydrocarbon]]s and possibly dust.]]
| [[image:M74 3.6 5.8 8.0 microns spitzer.png|thumb|250px|M74 as observed with the [[w:Spitzer Space Telescope]] as part of the [[w:Spitzer Infrared Nearby Galaxy Survey]]. The blue colors represent the 3.6 micrometre emission from stars. The green and red colors represent the 5.8 and 8.0 micrometre emission from [[w:polycyclic aromatic hydrocarbon]]s and possibly dust.]]
|}
|}


==Suspected black hole==
==Suspected black hole==
In [[March 22]], [[2005]], it was announced <ref name="chandra2005">[http://chandra.harvard.edu/photo/2005/m74/index.html Chandra :: Photo Album :: M74 :: 22 Mar 05<!-- Bot generated title -->]</ref> that the [[Chandra X-ray Observatory]] had observed an [[ultraluminous X-ray source]] (ULX) in M74, radiating more X-ray power than a [[neutron star]] in periodic intervals of around two hours. It has an estimated mass of around 10,000 [[Sun]]s. This is an indicator of an [[intermediate-mass black hole]]. This would be a rather uncommon class of black holes, somewhere in between in size of stellar black holes and the massive black holes theorized to reside in the center of many galaxies. Because of this, they are believed to form not from single supernovae, but possibly from a number of lesser stellar black holes in a star cluster. The X-ray source is identified as CXOU J013651.1+154547.
In [[w:March 22]], [[w:2005]], it was announced <ref name="chandra2005">[http://chandra.harvard.edu/photo/2005/m74/index.html Chandra :: Photo Album :: M74 :: 22 Mar 05<!-- Bot generated title -->]</ref> that the [[w:Chandra X-ray Observatory]] had observed an [[w:ultraluminous X-ray source]] (ULX) in M74, radiating more X-ray power than a [[w:neutron star]] in periodic intervals of around two hours. It has an estimated mass of around 10,000 [[w:Sun]]s. This is an indicator of an [[w:intermediate-mass black hole]]. This would be a rather uncommon class of black holes, somewhere in between in size of stellar black holes and the massive black holes theorized to reside in the center of many galaxies. Because of this, they are believed to form not from single supernovae, but possibly from a number of lesser stellar black holes in a star cluster. The X-ray source is identified as CXOU J013651.1+154547.


==Amateur astronomy observation information==
==Amateur astronomy observation information==
⚫
Messier 74 is located 1.5° east-northeast of [[w:Eta Piscium]].<ref name="jones1991" /><ref name="omeara1998" /> As stated above, the galaxy has the lowest surface brightness of all the Messier objects. It may be very difficult to see unless the sky is dark and clear,<ref name="jones1991" /> and it may be difficult to see in locations affected by [[w:light pollution]].<ref name="omeara1998" /> The galaxy may be best viewed under low magnification; when highly magnified, the diffuse emission becomes more extended and appears too faint to be seen by many people.<ref name="jones1991" /> Additionally, the galaxy may be more easily seen when using [[w:averted vision]] when the eyes are fully [[w:dark adaptation|dark adapted]].<ref name="jones1991" /><ref name="omeara1998" />

⚫
Messier 74 is located 1.5° east-northeast of [[Eta Piscium]].<ref name="jones1991" /><ref name="omeara1998" /> As stated above, the galaxy has the lowest surface brightness of all the Messier objects. It may be very difficult to see unless the sky is dark and clear,<ref name="jones1991" /> and it may be difficult to see in locations affected by [[light pollution]].<ref name="omeara1998" /> The galaxy may be best viewed under low magnification; when highly magnified, the diffuse emission becomes more extended and appears too faint to be seen by many people.<ref name="jones1991" /> Additionally, the galaxy may be more easily seen when using [[averted vision]] when the eyes are fully [[dark adaptation|dark adapted]].<ref name="jones1991" /><ref name="omeara1998" />

==See also==
{{commons|Messier 74}}
{{commons|Messier 74}}

* [[NGC 3184]] - ''a similar face-on spiral galaxy''
* [[Messier 101]] - ''a similar face-on spiral galaxy''
* [[Whirlpool Galaxy]] - ''a well-known face-on spiral galaxy''
* {{WikiSky}}

==External links==
==External links==
* [http://www.seds.org/messier/m/m074.html Spiral Galaxy M74 @ SEDS Messier pages]
* [http://www.seds.org/messier/m/m074.html Spiral Galaxy M74 @ SEDS Messier pages]


==References==
==References==

{{reflist}}
{{reflist}}


{{Messier objects}}
{{Messier Index}}
{{Sky|01|36|41.8|+|15|47|01|30000000}}
[[Category:Spiral galaxies|Messier 074]]
[[Category:Unbarred spiral galaxies|Messier 074]]
[[Category:M74 Group|Messier 074]]
[[Category:Pisces constellation|Messier 074]]
[[Category:Messier objects|074]]
[[Category:NGC objects|Messier 074]]
[[Category:UGC objects|01149]]
[[Category:PGC objects|05974]]

[[zh-min-nan:Messier 74]]
[[be:Аб'ект Месье M74]]
[[bg:M74]]
[[ca:Messier 74]]
[[cs:Messier 74]]
[[co:M74]]
[[de:Messier 74]]
[[es:Galaxia espiral M74]]
[[eo:M74]]
[[fa:مسیه ۷۴]]
[[fr:M74]]
[[ko:M74 (천체)]]
[[hr:Messier 74]]
[[it:M74 (astronomia)]]
[[lb:Messier 74]]
[[lt:Mesjė 74]]
[[hu:Messier 74]]
[[nl:Messier 74]]
[[ja:M74]]
[[nn:Messier 74]]
[[pl:Messier 74]]
[[pt:Messier 74]]
[[ro:Messier 74]]
[[ru:Спиральная галактика M74]]
[[sk:Galaxia M74]]
[[fi:Messier 74]]
[[sv:Messier 74]]
[[tr:NGC 628]]
[[uk:NGC 628]]
[[zh:M74]]

Latest revision as of 14:29, 15 July 2011

Messier 74
Messier 74. Credit: NASA/HST.
Observation data (w:J2000 epoch)
ConstellationPisces[1]
Right ascension01h 36m 41.8s[2]
Declination+15° 47′ 01″[2]
Redshift657 km/s[2]
Distance30 ± 6 Mly[3]
TypeSA(s)c[2]
Apparent dimensions (V)10′.5 × 9′.5[2]
Apparent magnitude (V)10.0[2]
Other designations
NGC 628, UGC 1149, PGC 5974[2]

Messier 74 (also known as NGC 628) is a face-on w:spiral galaxy in the w:constellation Pisces. The galaxy contains two clearly-defined w:spiral arms and is therefore used as an archetypal example of a w:Grand Design Spiral Galaxy.[4] The galaxy's low surface brightness makes it the most difficult Messier object for amateur astronomers to observe.[5][6] However, the relatively large angular size of the galaxy and the galaxy's face-on orientation make it an ideal object for professional astronomers who want to study w:spiral arm structure and spiral density waves.

History

M74 was discovered by w:Pierre Méchain in w:1780. Méchain then communicated his discovery to w:Charles Messier, who listed the galaxy in his catalog.[6]

Supernovae

Two w:supernovae have been identified in M74:[2] w:SN 2002ap[7] and w:SN 2003gd.[8]

SN 2002ap has attracted considerable attention because it is one of the few Type Ic supernovae (or w:hypernovae) observed within 10 Mpc in recent years.[9][10][11] This supernovae has been used to test theories on the origins of similar Type Ic supernovae at higher distances[10] and theories on the connection between supernovae and w:gamma ray bursts.[11]

SN 2003gd is a Type II-P supernova.[12] Type II supernovae have known luminosities, so they can be used to accurately measure distances. The distance measured to M74 using SN 2003gd is 9.6 ± 2.8 Mpc, or 31 ± 9 million ly.[3] For comparison, distances measured using the brightest supergiants are 7.7 ± 1.7 Mpc and 9.6 ± 2.2 Mpc.[3] Ben E. K. Sugerman found a "light echo" - a reflection of supernova explosion that appeared after the explosion itself - associated with SN 2003gd.[13] This is one of the few supernovae in which such a reflection has been found. This reflection appears to be from dust in a sheet-like cloud that lies in front of the supernova, and it can be used to determine the composition of the interstellar dust.[13][14]

Galaxy group information

M74 is the brightest member of the w:M74 Group, a group of 5-7 galaxies that also includes the peculiar w:spiral galaxy w:NGC 660 and a few w:irregular galaxies.[15][16][17] Although different group identification methods may consistently identify many of the same member galaxies in this group,[17] the exact group membership is still uncertain.

Star formation

M74 as observed with the w:Spitzer Space Telescope as part of the w:Spitzer Infrared Nearby Galaxy Survey. The blue colors represent the 3.6 micrometre emission from stars. The green and red colors represent the 5.8 and 8.0 micrometre emission from w:polycyclic aromatic hydrocarbons and possibly dust.

Suspected black hole

In w:March 22, w:2005, it was announced [18] that the w:Chandra X-ray Observatory had observed an w:ultraluminous X-ray source (ULX) in M74, radiating more X-ray power than a w:neutron star in periodic intervals of around two hours. It has an estimated mass of around 10,000 w:Suns. This is an indicator of an w:intermediate-mass black hole. This would be a rather uncommon class of black holes, somewhere in between in size of stellar black holes and the massive black holes theorized to reside in the center of many galaxies. Because of this, they are believed to form not from single supernovae, but possibly from a number of lesser stellar black holes in a star cluster. The X-ray source is identified as CXOU J013651.1+154547.

Amateur astronomy observation information

Messier 74 is located 1.5° east-northeast of w:Eta Piscium.[6][5] As stated above, the galaxy has the lowest surface brightness of all the Messier objects. It may be very difficult to see unless the sky is dark and clear,[6] and it may be difficult to see in locations affected by w:light pollution.[5] The galaxy may be best viewed under low magnification; when highly magnified, the diffuse emission becomes more extended and appears too faint to be seen by many people.[6] Additionally, the galaxy may be more easily seen when using w:averted vision when the eyes are fully dark adapted.[6][5]

Wikimedia Commons has media related to: Messier 74

References

  1. ↑ R. W. Sinnott, editor (1988). The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer. Sky Publishing Corporation and Cambridge University Press. ISBN 0-933-34651-4. {{cite book}}: |author= has generic name (help)
  2. ↑ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 628. Retrieved 2006-08-12.
  3. ↑ a b c M. A. Hendry, S. J. Smartt, J. R. Maund, A. Pastorello, L. Zampieri, S. Benetti, M. Turatto, E. Cappellaro, W. P. S. Meikle, R. Kotak, M. J. Irwin, P. G. Jonker, L. Vermaas, R. F. Peletier, H. van Woerden, K. M. Exter, D. L. Pollacco, S. Leon, S. Verley, C. R. Benn, G. Pignata (2005). "A study of the Type II-P supernova 2003gd in M74". Monthly Notices of the Royal Astronomical Society. 359: 906–926. doi:10.1111/j.1365-2966.2005.08928.x.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  4. ↑ A. Sandage, J. Bedke (1994). Carnegie Atlas of Galaxies. Washington, D.C.: Carnegie Institution of Washington. ISBN 0-87279-667-1.
  5. ↑ a b c d S. J. O'Meara (1998). The Messier Objects. Cambridge: Cambridge University. ISBN 0-521-55332-6.
  6. ↑ a b c d e f K. G. Jones (1991). Messier's Nebulae and Star Clusters (2nd ed.). Cambridge: Cambridge University Press. ISBN 0-521-37079-5.
  7. ↑ S. Nakano, R. Kushida, Y. Kushida, W. Li (2002). "Supernova 2002ap in M74". IAU Circular. 7810.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  8. ↑ R. Evans, R. H. McNaught (2003). "Supernova 2003gd in M74". IAU Circular. 8150.
  9. ↑ P. A. Mazzali, J. Deng, K. Maeda, K. Nomoto, H. Umeda, K. hatano, K. Iwamoto, Y. Yoshii, Y. Kobayashi, T. Minezaki, M. Doi, K. Enya, H. Tomita, S. J. Smartt, K. Kinugasa, H. Kawakita, K. Ayani, T. Kawabata, H. Yamaoka, Y. L. Qiu, K. Motohara, C. L. Gerardy, R. Fesen, K. S. Kawabata, M. Iye, N. Kashikawa, G. Kosugi, Y. Ohyama, M. Takada-Hidai, G. Zhao, R. Chornock, A. V. Filippenko, S. Benetti, M. Turatto (2002). "The Type Ic Hypernova SN 2002ap". Astrophysical Journal. 572: L61–L65. doi:10.1086/341504.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  10. ↑ a b S. J. Smartt, P. M. Vreeswijk, E. Ramirez-Ruiz, G. F. Gilmore, W. P. S. Meikle, A. M. N. Ferguson, J. H. Knapen (2002). "On the Progenitor of the Type Ic Supernova 2002ap". Astrophysical Journal. 572: L147–L151. doi:10.1086/341747.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  11. ↑ a b A. Gal-Yam, E. O. Ofek, O. Shemmer (2002). "Supernova 2002ap: the first month". Monthly Notices of the Royal Astronomical Society. 332: L73–L77. doi:10.1046/j.1365-8711.2002.05535.x.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  12. ↑ S. D. Van Dyk, W. Li, A. V. Filippenko (2003). "On the Progenitor of the Type II-Plateau Supernova 2003gd in M74". Publications of the Astronomical Society of the Pacific. 115: 1289–1295. doi:10.1086/378308.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  13. ↑ a b B. E. K. Sugerman (2005). "Discovery of a Light Echo from SN 2003gd". Astrophysical Journal. 632: L17–L20. doi:10.1086/497578.
  14. ↑ S. D. Van Dyk, W. Li, A. V. Filippenko (2006). "The Light Echo around Supernova 2003gd in Messier 74". Publications of the Astronomical Society of the Pacific. 118: 351–357. doi:10.1086/500225.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  15. ↑ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge: Cambridge University Press. ISBN 0-521-35299-1.
  16. ↑ A. Garcia (1993). "General study of group membership. II - Determination of nearby groups". Astronomy and Astrophysics Supplement. 100: 47–90.
  17. ↑ a b G. Giuricin, C. Marinoni, L. Ceriani, A. Pisani (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups". Astrophysical Journal. 543: 178–194. doi:10.1086/317070.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  18. ↑ Chandra :: Photo Album :: M74 :: 22 Mar 05
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