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| name = Whirlpool Galaxy | name = Whirlpool Galaxy
| image = File:Messier51 sRGB.jpg | image = File:Messier51 sRGB.jpg
| caption = Whirlpool Galaxy (M51a), as taken by ], the smaller object in the upper right is ] (M51b)<br />(]/]) | caption = Whirlpool Galaxy (M51a), as taken by the ], the smaller object in the upper right is ] (M51b)<br />(]/])
| epoch = ] | epoch = ]
| constellation name = ]<ref name="sinnott1988"> | constellation name = ]<ref name="sinnott1988">
{{cite book {{cite book
| first=J. L. E. |last=Dreyer |editor-first=R. W. |editor-last=Sinnott | first=J. L. E. |last=Dreyer | authorlink = John Louis Emil Dreyer |editor-first=R. W. |editor-last=Sinnott
| title=The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters | title=The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters
| date=1988 | date=1988
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| access-date=2006-12-06 |df=mdy-all | access-date=2006-12-06 |df=mdy-all
}}</ref> }}</ref>
| size = {{cvt|23.58|kpc|ly|sigfig=3|lk=on}}<br />(diameter; ])<ref name="ned" /><ref name=RC3>{{cite book | bibcode=1991rc3..book.....D | year=1991 | title=Third Reference Catalogue of Bright Galaxies | last1=De Vaucouleurs | first1=Gerard | last2=De Vaucouleurs | first2=Antoinette | last3=Corwin | first3=Herold G. | last4=Buta | first4=Ronald J. | last5=Paturel | first5=Georges | last6=Fouque | first6=Pascal }}</ref> | size = {{cvt|23.58|kpc|ly|sigfig=3|lk=on}}<br />(diameter; ])<ref name="ned" /><ref name=RC3>{{cite book | bibcode=1991rc3..book.....D | year=1991 | title=Third Reference Catalogue of Bright Galaxies | last1=De Vaucouleurs | first1=Gerard | last2=De Vaucouleurs | authorlink = Gérard de Vaucouleurs | first2=Antoinette | authorlink2 = Antoinette de Vaucouleurs | last3=Corwin | first3=Herold G. | last4=Buta | first4=Ronald J. | last5=Paturel | first5=Georges | last6=Fouque | first6=Pascal }}</ref>
| size_v = {{val|11.2|x|6.9|ul=arcminute}}<ref name="ned"/> | size_v = {{val|11.2|x|6.9|ul=arcminute}}<ref name="ned"/>
| notes = Interacting with ]<ref name="arp1966"/> | notes = Interacting with ]<ref name="arp1966"/>
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}}</ref><ref name="elmegreenelmegreen1987"> }}</ref><ref name="elmegreenelmegreen1987">
{{cite journal {{cite journal
| first=H. |last=Arp | first=H. |last=Arp | authorlink = Halton Arp
| date=1966 | date=1966
| title=Atlas of Peculiar Galaxies | title=Atlas of Peculiar Galaxies
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==Discovery== ==Discovery==
] in 1845]] ] in 1845]]

⚫ What later became known as the Whirlpool Galaxy was discovered on October 13, 1773, by ] while hunting for objects that could confuse comet hunters, and was designated in ] as M51.<ref>
<ref>
{{cite book {{cite book
|first=Charles |last=Messier |first=Charles |last=Messier
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}}</ref> ], employing a {{Convert|72|in|m|adj=on}} ] at ], Ireland, found that the Whirlpool possessed a ], the first "nebula" to be known to have one.<ref>Rosse revealed the spiral structure of Whirlpool galaxy (M51) at the 1845 meeting of the British Association for the Advancement of Science. Rosse's illustration of M51 was reproduced in J.P. Nichol's book of 1846. }}</ref> ], employing a {{Convert|72|in|m|adj=on}} ] at ], Ireland, found that the Whirlpool possessed a ], the first "nebula" to be known to have one.<ref>Rosse revealed the spiral structure of Whirlpool galaxy (M51) at the 1845 meeting of the British Association for the Advancement of Science. Rosse's illustration of M51 was reproduced in J.P. Nichol's book of 1846.
* {{cite journal |last1=Rosse |first1=Earl of |title=On the nebula 25 Herschel, or 61 of Messier's catalogue |journal=Report of the Fifteenth Meeting of the British Association for the Advancement of Science; Held at Cambridge in June 1845 § Notices and Abstracts of Miscellaneous Communications to the Sections |series=Report of the ... Meeting of the British Association for the Advancement of Science (1833) |date=1846 |page=4 |url=https://babel.hathitrust.org/cgi/pt?id=njp.32101049356890&view=1up&seq=402 }} * {{cite journal |last1=Rosse |first1=Earl of |title=On the nebula 25 Herschel, or 61 of Messier's catalogue |journal=Report of the Fifteenth Meeting of the British Association for the Advancement of Science; Held at Cambridge in June 1845 § Notices and Abstracts of Miscellaneous Communications to the Sections |series=Report of the ... Meeting of the British Association for the Advancement of Science (1833) |date=1846 |page=4 |url=https://babel.hathitrust.org/cgi/pt?id=njp.32101049356890&view=1up&seq=402 }}
* {{cite book |last1=Nichol |first1=John Pringle |title=Thoughts on Some Important Points Relating to the System of the World |date=1846 |publisher=William Tait |location=Edinburgh, Scotland |page=23 |url=https://babel.hathitrust.org/cgi/pt?id=uc2.ark:/13960/t9k360k8b&view=1up&seq=65 }} Rosse's illustration of the Whirlpool galaxy appears on the plate that immediately precedes p. 23.</ref> These "]e" were not recognized as galaxies until ] was able to observe ]s in some of these spiral nebulae, which provided evidence that they were so far away that they must be entirely separate galaxies.<ref> * {{cite book |last1=Nichol |first1=John Pringle | authorlink = John Pringle Nichol |title=Thoughts on Some Important Points Relating to the System of the World |date=1846 |publisher=William Tait |location=Edinburgh, Scotland |page=23 |url=https://babel.hathitrust.org/cgi/pt?id=uc2.ark:/13960/t9k360k8b&view=1up&seq=65 }} Rosse's illustration of the Whirlpool galaxy appears on the plate that immediately precedes p. 23.</ref> These "]e" were not recognized as galaxies until ] was able to observe ]s in some of these spiral nebulae, which provided evidence that they were so far away that they must be entirely separate galaxies.
⚫ The Whirlpool Galaxy was discovered on October 13, 1773, by ] while searching for objects that might confuse comet hunters. It was later cataloged as M51 in ] list of astronomical objects.<ref>
{{cite journal {{cite journal
|last1=Hubble |first1=E. P. |last1=Hubble |first1=E. P.
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==Visual appearance== ==Visual appearance==
] ]

Deep in the constellation ], M51 is often found by finding the easternmost star of the ], ], and going 3.5° southwest. Its declination is, rounded, +47°, making it ] (never setting) for observers above the ];{{efn|47 out of 90 degrees north of the ]. Thus its light emits as far south, to a good minimal cumulation of 15° above the horizon, once a day, on the ].}} it reaches a high altitude throughout this hemisphere making it an accessible object from the early hours in November through to the end of May, after which observation is more coincidental in modest latitudes with the risen sun (due to the Sun approaching to and receding from its ], specifically figuring in ], just to the north). Deep in the constellation ], M51 is often found by finding the easternmost star of the ], ], and going 3.5° southwest. Its declination is, rounded, +47°, making it ] (never setting) for observers above the ];{{efn|47 out of 90 degrees north of the ]. Thus its light emits as far south, to a good minimal cumulation of 15° above the horizon, once a day, on the ].}} it reaches a high altitude throughout this hemisphere making it an accessible object from the early hours in November through to the end of May, after which observation is more coincidental in modest latitudes with the risen sun (due to the Sun approaching to and receding from its ], specifically figuring in ], just to the north).


M51 is visible through ] under dark sky conditions, and it can be resolved in detail with modern amateur telescopes.<ref name="apod"/> When seen through a 100&nbsp;mm telescope the basic outlines of M51 (limited to 5×6') and its companion are visible. Under dark skies, and with a moderate eyepiece through a 150&nbsp;mm telescope, M51's intrinsic spiral structure can be detected. With larger (>300&nbsp;mm) instruments under dark sky conditions, the various spiral bands are apparent with ]s visible, and M51 can be seen to be attached to ]. M51 is visible through ] under dark sky conditions, and it can be resolved in detail with modern amateur telescopes.<ref name="apod"/> When seen through a 100&nbsp;mm telescope the basic outlines of M51 (limited to 5×6') and its companion are visible. Under dark skies, and with a moderate eyepiece through a 150&nbsp;mm telescope, M51's intrinsic spiral structure can be detected. With larger (>300&nbsp;mm) instruments under dark sky conditions, the various spiral bands are apparent with ]s visible, and M51 can be seen to be attached to ].


As is usual for galaxies, the true extent of its structure can only be gathered from inspecting photographs; long exposures reveal a large nebula extending beyond the visible circular appearance. In 1984, thanks to the high-speed detector—the so-called image-photon-counting- IPCS—system—developed jointly by the CNRS Laboratoire d'Astronomie Spatiald (L.A.S.- CNRS) and the Observatoire de Haute Provence (O.H.P.) along with the particularly nice seeing offered by the Canada-France-Hawaii-Telescope (C.F.H.T.) 3.60m Cassegrain focus at Mauna Kea summit in Hawaii, Hua et al. detected the double component of the very nucleus of the Whirlpool galaxy.<ref>{{Cite journal |last=Hua |title=Unknown |display-authors=etal |journal=Astrophysical Letters and Communications |date=1987 |volume=25 |number=<!--poss 3--> |oclc=60627567 |pages=187-204 }}</ref>{{Full citation needed|date=October 2021}} As is usual for galaxies, the true extent of its structure can only be gathered from inspecting photographs; long exposures reveal a large nebula extending beyond the visible circular appearance. In 1984, thanks to the high-speed detector—the so-called image-photon-counting-system (IPCS)—developed jointly by the CNRS Laboratoire d'Astronomie Spatiald (L.A.S.-CNRS) and the Observatoire de Haute Provence (O.H.P.) along with the particularly nice visibility offered by the Canada-France-Hawaii-Telescope (C.F.H.T.) 3.60m Cassegrain focus on the summit of Mauna Kea in Hawaii, Hua et al. detected the double component of the very nucleus of the Whirlpool Galaxy.<ref>{{Cite journal |last1=Hua |display-authors=etal |date=1987 |title= |journal=Astrophysical Letters & Communications |volume=25 |number=<!--poss 3--> |issn=0888-6512 |oclc=60627567 |pages=187–204 }}</ref>{{Full citation needed|date=October 2021}}

⚫ In January 2005 the ] constructed a 11,477&nbsp;×&nbsp;7,965-pixel composite image (shown in the infobox above) of M51 using Hubble's ]. The image highlights the galaxy's spiral arms, and shows detail into some of the structures inside the arms.<ref>{{Cite web |title=Hubble Celebrates 15th Anniversary with Spectacular New Images |url=https://hubblesite.org/contents/news-releases/2005/news-2005-12.html |department=News Center |publisher=] |date=April 25, 2005 |access-date=13 October 2024}}</ref>


⚫ ]
⚫ In January 2005 the ] constructed a 11,477&nbsp;×&nbsp;7,965-pixel composite image (shown in the infobox above) of M51 using Hubble's ]. The image highlights the galaxy's spiral arms, and shows detail into some of the structures inside the arms.<ref>{{cite web | date=April 25, 2005 | url=http://hubblesite.org/newscenter/newsdesk/archive/releases/2005/12/image/a | title=Out of This Whirl: The Whirlpool Galaxy (M51) and Companion Galaxy | work=News Center | publisher=] | access-date=August 7, 2006 }}</ref>
⚫ ]


==Properties== ==Properties==
The Whirlpool Galaxy lies at a distance of about 23<ref name=ned /> to 31 million light-years from Earth.<ref>{{Cite web |url= https://www.nasa.gov/feature/goddard/2017/messier-51-the-whirlpool-galaxy |title= Hubble's Messier Catalogue – Messier 51 (The Whirlpool Galaxy) |date=2017-10-17 |publisher=NASA |language=en |access-date=2021-09-06|df=mdy-all}}</ref> Based on the 1991 measurement by the Third Reference Catalogue of Bright Galaxies using the ] at the B-band, the Whirlpool Galaxy has a diameter of {{convert|23.58|kpc|ly|sigfig=3|abbr=off|lk=on}}.<ref name="ned" /><ref name=RC3 /> Overall the galaxy is about 88% the size of the ].<ref name=Average>{{cite arXiv |eprint=astro-ph/9704216 |title=The Milky Way is just an average spiral | date=22 April 1997|last1=Goodwin |first1=S. P. |last2=Gribbin |first2=J. |last3=Hendry |first3=M. A. }}</ref><ref name="Goodwin">{{cite journal |last1=Goodwin |first1=S. P. |last2=Gribbin |first2=J. |last3=Hendry |first3=M. A. |date=August 1998 |title=The relative size of the Milky Way |bibcode=1998Obs...118..201G |journal=The Observatory |volume=118 |pages=201–208 }}</ref><ref name=Castro>{{cite journal |arxiv=astro-ph/0205553|doi=10.1051/0004-6361:20020895 |title=Warps and correlations with intrinsic parameters of galaxies in the visible and radio |year=2002 |last1=Castro-Rodríguez |first1=N. |last2=López-Corredoira |first2=M. |last3=Sánchez-Saavedra |first3=M. L. |last4=Battaner |first4=E. |journal=Astronomy & Astrophysics |volume=391 |issue=2 |pages=519–530 |bibcode=2002A&A...391..519C |s2cid=17813024 }}</ref> Its ] is estimated to be 160 billion solar masses,<ref>{{Cite web |url=http://herschel.cf.ac.uk/results/whirlpool-galaxy |title=Whirlpool Galaxy |date=2009-06-19 |website=Herschel Space Observatory |publisher=Cardiff University |language=en |access-date=2018-10-11 |df=mdy-all |archive-date=2019-01-10 |archive-url=https://web.archive.org/web/20190110061926/http://herschel.cf.ac.uk/results/whirlpool-galaxy |url-status=dead }}</ref> or around 10.3% of the mass of Milky Way Galaxy. The Whirlpool Galaxy lies at a distance of 23<ref name=ned /> to 31 million light-years from Earth.<ref>{{Cite web |url= https://www.nasa.gov/feature/goddard/2017/messier-51-the-whirlpool-galaxy |title= Hubble's Messier Catalogue – Messier 51 (The Whirlpool Galaxy) |date=2017-10-17 |publisher=NASA |language=en |access-date=2021-09-06|df=mdy-all}}</ref> Based on the 1991 measurement by the Third Reference Catalogue of Bright Galaxies using the ] at the B-band, the Whirlpool Galaxy has a diameter of {{convert|23.58|kpc|ly|sigfig=3|abbr=off|lk=on}}.<ref name="ned" /><ref name=RC3 /> Overall the galaxy is about 88% the size of the ].<ref name=Average>{{cite arXiv |eprint=astro-ph/9704216 |title=The Milky Way is just an average spiral | date=22 April 1997|last1=Goodwin |first1=S. P. |last2=Gribbin |first2=J. | authorlink2 = John Gribbin |last3=Hendry |first3=M. A. }}</ref><ref name="Goodwin">{{cite journal |last1=Goodwin |first1=S. P. |last2=Gribbin |first2=J. |last3=Hendry |first3=M. A. |date=August 1998 |title=The relative size of the Milky Way |bibcode=1998Obs...118..201G |journal=The Observatory |volume=118 |pages=201–208 }}</ref><ref name=Castro>{{cite journal |arxiv=astro-ph/0205553|doi=10.1051/0004-6361:20020895 |title=Warps and correlations with intrinsic parameters of galaxies in the visible and radio |year=2002 |last1=Castro-Rodríguez |first1=N. |last2=López-Corredoira |first2=M. |last3=Sánchez-Saavedra |first3=M. L. |last4=Battaner |first4=E. |journal=Astronomy & Astrophysics |volume=391 |issue=2 |pages=519–530 |bibcode=2002A&A...391..519C |s2cid=17813024 }}</ref> Its ] is estimated to be 160 billion solar masses,<ref>{{Cite web |url=http://herschel.cf.ac.uk/results/whirlpool-galaxy |title=Whirlpool Galaxy |date=2009-06-19 |website=Herschel Space Observatory |publisher=Cardiff University |language=en |access-date=2018-10-11 |df=mdy-all |archive-date=2019-01-10 |archive-url=https://web.archive.org/web/20190110061926/http://herschel.cf.ac.uk/results/whirlpool-galaxy |url-status=dead }}</ref> or around 10.3% of the mass of Milky Way Galaxy.


] ]


A ], once thought to be surrounded by a ring of dust, but now believed to be partially occluded by dust instead, exists at the heart of the spiral. A pair of ]s extend from the active galactic nucleus.<ref>{{cite web | date=June 8, 1992 | url=http://hubblesite.org/newscenter/newsdesk/archive/releases/1992/17/text/ | title=NASA's Hubble Space Telescope Resolves a Dark "x" Across the Nucleus of M51 | work=News Center | publisher=HubbleSite | access-date=August 7, 2006 }}</ref> A ], once thought to be surrounded by a ring of dust, but now believed to be partially occluded by dust instead, exists at the heart of the spiral. A pair of ]s extend from the active galactic nucleus.<ref>{{cite web | date=June 8, 1992 | url=http://hubblesite.org/newscenter/newsdesk/archive/releases/1992/17/text/ | title=NASA's Hubble Space Telescope Resolves a Dark "x" Across the Nucleus of M51 | work=News Center | publisher=HubbleSite | access-date=August 7, 2006 }}</ref>


===Spiral structure=== ===Spiral structure===
The Whirlpool Galaxy has two, very prominent spiral arms that wind clockwise. One arm deviates from a constant angle significantly. <ref name="structure">{{cite journal |last1=Honig |first1=Z.N. |last2=Reid |first2=M.J. |title=Characteristics of Spiral Arms in Late-type Galaxies |journal=The Astrophysical Journal |date=February 2015 |volume=800 |issue=1 |pages=5387–5394 |doi=10.1088/0004-637X/800/1/53 |pmid=53 |arxiv=1412.1012 |bibcode=2015ApJ...800...53H |s2cid=118666575 |url=https://ui.adsabs.harvard.edu/abs/2015ApJ...800...53H/abstract |access-date=November 10, 2022}}</ref> The Whirlpool Galaxy has two, very prominent spiral arms that wind clockwise. One arm deviates from a constant angle significantly. <ref name="structure">{{cite journal |last1=Honig |first1=Z.N. |last2=Reid |first2=M.J. |title=Characteristics of Spiral Arms in Late-type Galaxies |journal=The Astrophysical Journal |date=February 2015 |volume=800 |issue=1 |pages=5387–5394 |doi=10.1088/0004-637X/800/1/53 |pmid=53 |arxiv=1412.1012 |bibcode=2015ApJ...800...53H |s2cid=118666575 |url=https://ui.adsabs.harvard.edu/abs/2015ApJ...800...53H/abstract |access-date=November 10, 2022}}</ref> The pronounced spiral structure of the Whirlpool Galaxy is believed to be the result of the close interaction between it and its companion galaxy ], which may have passed through the main disk of M51 about 500 to 600 million years ago. In this proposed scenario, NGC 5195 came from behind M51 through the disk towards the observer and made another disk crossing as recently as 50 to 100 million years ago until it is where we observe it to be now, slightly behind M51.<ref name="Salo & Laurikainen">
The pronounced spiral structure of the Whirlpool Galaxy is believed to be the result of the close interaction between it and its companion galaxy ], which may have passed through the main disk of M51 about 500 to 600 million years ago. In this proposed scenario, NGC 5195 came from behind M51 through the disk towards the observer and made another disk crossing as recently as 50 to 100 million years ago until it is where we observe it to be now, slightly behind M51.<ref name="Salo & Laurikainen">
{{cite journal {{cite journal
| last1=Salo |first1=Heikki |last2=Laurikainen |first2=Eija | last1=Salo |first1=Heikki |last2=Laurikainen |first2=Eija
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| doi=10.1023/A:1017002909665 | doi=10.1023/A:1017002909665
|s2cid=189838328 }}</ref> |s2cid=189838328 }}</ref>

===Tidal features=== ===Tidal features===
As a result of the Whirpool Galaxy's interaction with NGC 5195, a variety of tidal features have been created. The largest of these features is the so-called Northwest plume, which extends out to {{convert|43|kpc|ly|sigfig=3|abbr=off|lk=on}} from the galaxy's center. This plume is uniform in color and likely originated from the Whirpool Galaxy itself due to having diffuse gas. Adjacent to it are two other plumes that have a slightly bluer color, referred to as the Western plumes due to their location.<ref name=watkinsM51/> As a result of the Whirpool Galaxy's interaction with NGC 5195, a variety of tidal features have been created. The largest of these features is the so-called Northwest plume, which extends out to {{convert|43|kpc|ly|sigfig=3|abbr=off|lk=on}} from the galaxy's center. This plume is uniform in color and likely originated from the Whirpool Galaxy itself due to having diffuse gas. Adjacent to it are two other plumes that have a slightly bluer color, referred to as the Western plumes due to their location.<ref name=watkinsM51/>



In 2015, a study discovered two new tidal features caused by the interaction between the Whirlpool Galaxy and NGC 5195, the "Northeast plume" and the "South plume". The study remarks that a simulation that takes into account only one passage of NGC 5195 into the Whirpool Galaxy will fail to produce an analogue to the Northeast tail.<ref name="watkinsM51">{{cite journal |last1=Watkins |first1=Aaron E. |last2=Mihos |first2=J. Christopher |last3=Harding |first3=Paul |title=Deep Imaging of M51: a New View of the Whirlpool's Extended Tidal Debris |journal=The Astrophysical Journal |date=February 2015 |volume=800 |issue=1 |pages=7 |doi=10.1088/2041-8205/800/1/L3 |arxiv=1501.04599 |bibcode=2015ApJ...800L...3W |s2cid=118603790 |url=https://ui.adsabs.harvard.edu/abs/2015ApJ...800L...3W/abstract |access-date=November 18, 2022}}</ref> In contrast, the multiple-passage simulations made by Salo and Laurikainen et.al reproduce the northeast plume. <ref name="Salo & Laurikainen" /><ref name="watkinsM51"/> In 2015, a study discovered two new tidal features caused by the interaction between the Whirlpool Galaxy and NGC 5195, the "Northeast plume" and the "South plume". The study remarks that a simulation that takes into account only one passage of NGC 5195 into the Whirpool Galaxy will fail to produce an analogue to the Northeast tail.<ref name="watkinsM51">{{cite journal |last1=Watkins |first1=Aaron E. |last2=Mihos |first2=J. Christopher |last3=Harding |first3=Paul |title=Deep Imaging of M51: a New View of the Whirlpool's Extended Tidal Debris |journal=The Astrophysical Journal |date=February 2015 |volume=800 |issue=1 |pages=7 |doi=10.1088/2041-8205/800/1/L3 |arxiv=1501.04599 |bibcode=2015ApJ...800L...3W |s2cid=118603790 |url=https://ui.adsabs.harvard.edu/abs/2015ApJ...800L...3W/abstract |access-date=November 18, 2022}}</ref> In contrast, the multiple-passage simulations made by Salo and Laurikainen et.al reproduce the northeast plume. <ref name="Salo & Laurikainen" /><ref name="watkinsM51"/>


===Star formation=== ===Star formation===
⚫ The central region of M51 appears to be undergoing a period of enhanced star formation. The present efficiency of star formation, defined as the ratio of mass of new stars to the mass of star-forming gas, is only ~1%, quite comparable to the global value for the Milky Way and other galaxies. It is estimated that the current high rate of star formation can last no more than another 100 million years or so.<ref name="Thronson & Greenhouse">
The central region of M51 appears to be undergoing a period of enhanced star formation.
⚫ The present efficiency of star formation, defined as the ratio of mass of new stars to the mass of star-forming gas, is only ~1%, quite comparable to the global value for the Milky Way and other galaxies. It is estimated that the current high rate of star formation can last no more than another 100 million years or so.<ref name="Thronson & Greenhouse">
{{cite journal {{cite journal
| last1=Thronson |first1=Harley A. |last2=Greenhouse |first2=Matthew A. | last1=Thronson |first1=Harley A. |last2=Greenhouse |first2=Matthew A.
Line 131: Line 133:
Three ]e have been observed in the Whirlpool Galaxy:<ref>{{cite web | url=http://www.cbat.eps.harvard.edu/lists/Supernovae.html | title=List of Supernovae | publisher=Central Bureau for Astronomical Telegrams | access-date=February 27, 2016}}</ref> Three ]e have been observed in the Whirlpool Galaxy:<ref>{{cite web | url=http://www.cbat.eps.harvard.edu/lists/Supernovae.html | title=List of Supernovae | publisher=Central Bureau for Astronomical Telegrams | access-date=February 27, 2016}}</ref>


In 1994, ] was observed in the Whirlpool Galaxy. It was classified as ], indicating that its progenitor star was very massive and had already shed much of its mass, and its brightness peaked at ] 12.91.<ref>{{cite journal | title = The properties of the 'standard' Type Ic supernova 1994I from spectral models | display-authors = 4 | author = Sauer, D. N. | author2 = Mazzali, P. A. | author3 = Deng, J. | author4 = Valenti, S. | author5 = Nomoto, K. | author6 = Filippenko, A. V. | journal = ] | volume = 369 | issue = 4 | pages = 1939–1948 | date = 2006 | doi = 10.1111/j.1365-2966.2006.10438.x | bibcode = 2006MNRAS.369.1939S|arxiv = astro-ph/0604293 | s2cid = 119510845 }}</ref> In 1994, ] was observed in the Whirlpool Galaxy. It was classified as ], indicating that its progenitor star was very massive and had already shed much of its mass, and its brightness peaked at ] 12.91.<ref>{{cite journal | title = The properties of the 'standard' Type Ic supernova 1994I from spectral models | display-authors = 4 | author = Sauer, D. N. | author2 = Mazzali, P. A. | author3 = Deng, J. | author4 = Valenti, S. | author5 = Nomoto, K. | author6 = Filippenko, A. V. | journal = ] | volume = 369 | issue = 4 | pages = 1939–1948 | date = 2006 | doi = 10.1111/j.1365-2966.2006.10438.x | doi-access = free | bibcode = 2006MNRAS.369.1939S|arxiv = astro-ph/0604293 | s2cid = 119510845 }}</ref>


In June 2005 the type II supernova ] was observed in the Whirlpool Galaxy, peaking at apparent magnitude 14.<ref>{{cite web | last=MacRobert | first=Alan M. | date=August 24, 2005 | url=http://skyandtelescope.com/news/article_1544_1.asp | title=Supernova in M51 | work=Sky Tonight | publisher=Sky and Telescope | access-date=August 7, 2006 }}</ref><ref>{{cite web | last=Bishop | first=David | url=http://www.supernovae.net/sn2005/sn2005cs.html | title=Supernova 2005cs in M51 | work=supernovae.net | access-date=August 7, 2006 | url-status=dead | archive-url=https://web.archive.org/web/20061003010723/http://www.supernovae.net/sn2005/sn2005cs.html | archive-date=October 3, 2006 }}</ref> In June 2005 the type II supernova ] was observed in the Whirlpool Galaxy, peaking at apparent magnitude 14.<ref>{{cite web | last=MacRobert | first=Alan M. | date=August 24, 2005 | url=http://skyandtelescope.com/news/article_1544_1.asp | title=Supernova in M51 | work=Sky Tonight | publisher=Sky and Telescope | access-date=August 7, 2006 }}</ref><ref>{{cite web | last=Bishop | first=David | url=http://www.supernovae.net/sn2005/sn2005cs.html | title=Supernova 2005cs in M51 | work=supernovae.net | access-date=August 7, 2006 | url-status=dead | archive-url=https://web.archive.org/web/20061003010723/http://www.supernovae.net/sn2005/sn2005cs.html | archive-date=October 3, 2006 }}</ref>
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]]] ]]]


On 22 January 2019, a ], designated ], was discovered in Messier 51. The transient was later identified as a ]. The progenitor star was detected in archival ] infrared images. No object could be seen at the position of the transient in archival ] images, indicating that the progenitor star was heavily obstructed by ]. 2019abn peaked at magnitude 17, reaching an ] of <math>M_{r}=-14.9</math>.<ref>{{Cite journal|arxiv=1904.07857|title=Discovery of an intermediate-luminosity red transient in M51 and its likely dust-obscured, infrared-variable progenitor|author1=Jacob E. Jencson|author2=Scott M. Adams|author3=Howard E. Bond|doi=10.3847/2041-8213/ab2c05|journal=The Astrophysical Journal Letters|volume=880|year=2019|issue=L20|pages = L20|bibcode = 2019ApJ...880L..20J|s2cid=119110002 |doi-access=free }}</ref> On 22 January 2019, a ], designated ], was discovered in Messier 51.<ref>{{cite web | website=Transient Name Server | title=AT{{nbsp}}2019abn| url=https://www.wis-tns.org/object/2019abn | publisher = ] | access-date=24 August 2024}}</ref> The transient was later identified as a ]. The progenitor star was detected in archival ] infrared images. No object could be seen at the position of the transient in archival ] images, indicating that the progenitor star was heavily obstructed by ]. 2019abn peaked at magnitude 17, reaching an ] of <math>M_{r}=-14.9</math>.<ref>{{Cite journal|arxiv=1904.07857|title=Discovery of an intermediate-luminosity red transient in M51 and its likely dust-obscured, infrared-variable progenitor|author1=Jacob E. Jencson|author2=Scott M. Adams|author3=Howard E. Bond|doi=10.3847/2041-8213/ab2c05|journal=The Astrophysical Journal Letters|volume=880|year=2019|issue=L20|pages = L20|bibcode = 2019ApJ...880L..20J|s2cid=119110002 |doi-access=free }}</ref>


===Planet candidate=== ===Planet candidate===
In September 2020, the detection by the ]<ref>{{Cite news|date=2021-10-25|title=Signs of first planet found outside our galaxy|language=en-GB|work=BBC News|url=https://www.bbc.com/news/science-environment-59044650 |archive-url=https://web.archive.org/web/20211025214850/https://www.bbc.com/news/science-environment-59044650# |archive-date=2021-10-25 |url-status=live}}</ref> of a ], named '''M51-ULS-1b''', orbiting the ] M51-ULS-1 in this galaxy was announced. If confirmed, it would be the first known instance of an ], a planet ''outside'' the ] Galaxy. The planet candidate was detected by ] of the ] (XRS), which consists of a stellar remnant (either a ] or a ]) and a massive star, likely a ] ]. The planet would be slightly smaller than ] and orbit at a distance of some tens of ]s.<ref name="NS-20200923">{{cite news |last=Crane |first=Leah |title=Astronomers may have found the first planet in another galaxy |url=https://www.newscientist.com/article/2255431-astronomers-may-have-found-the-first-planet-in-another-galaxy/ |date=23 September 2020 |work=] |access-date=25 September 2020 }}</ref><ref>{{Cite journal|last1=Di Stefano|first1=Rosanne|last2=Berndtsson|first2=Julia|last3=Urquhart|first3=Ryan|last4=Soria|first4=Roberto|last5=Kashyap|first5=Vinay L.|last6=Carmichael|first6=Theron W.|last7=Imara|first7=Nia|date=2021-10-25|title=A possible planet candidate in an external galaxy detected through X-ray transit|url=https://www.nature.com/articles/s41550-021-01495-w|journal=Nature Astronomy|volume=5 |issue=12 |pages=1297–1307 |language=en|arxiv=2009.08987|doi=10.1038/s41550-021-01495-w|bibcode=2021NatAs...5.1297D |s2cid=239892362 |issn=2397-3366}}</ref> In September 2020, the detection by the ]<ref>{{Cite news|date=2021-10-25|title=Signs of first planet found outside our galaxy|language=en-GB|work=BBC News|url=https://www.bbc.com/news/science-environment-59044650 |archive-url=https://web.archive.org/web/20211025214850/https://www.bbc.com/news/science-environment-59044650 |archive-date=2021-10-25 |url-status=live}}</ref> of a ], named '''M51-ULS-1b''', orbiting the ] M51-ULS-1 in this galaxy was announced. If confirmed, it would be the first known instance of an ], a planet ''outside'' the ] Galaxy. The planet candidate was detected by ] of the ] (XRS), which consists of a stellar remnant (either a ] or a ]) and a massive star, likely a ] ]. The planet would be slightly smaller than ] and orbit at a distance of some tens of ]s.<ref name="NS-20200923">{{cite news |last=Crane |first=Leah |title=Astronomers may have found the first planet in another galaxy |url=https://www.newscientist.com/article/2255431-astronomers-may-have-found-the-first-planet-in-another-galaxy/ |date=23 September 2020 |work=] |access-date=25 September 2020 }}</ref><ref>{{Cite journal|last1=Di Stefano|first1=Rosanne|last2=Berndtsson|first2=Julia|last3=Urquhart|first3=Ryan|last4=Soria|first4=Roberto|last5=Kashyap|first5=Vinay L.|last6=Carmichael|first6=Theron W.|last7=Imara|first7=Nia | authorlink7 = Nia Imara |date=2021-10-25|title=A possible planet candidate in an external galaxy detected through X-ray transit|url=https://www.nature.com/articles/s41550-021-01495-w|journal=Nature Astronomy|volume=5 |issue=12 |pages=1297–1307 |language=en|arxiv=2009.08987|doi=10.1038/s41550-021-01495-w|bibcode=2021NatAs...5.1297D |s2cid=239892362 |issn=2397-3366}}</ref>


==Companion== ==Companion==
{{main article|NGC 5195}} {{main article|NGC 5195}}

] (also known as Messier 51b or M51b) is a dwarf galaxy that is interacting with the Whirlpool Galaxy (also known as M51a or NGC 5194). Both galaxies are located approximately 25 million light-years away in the constellation Canes Venatici. Together, the two galaxies are one of the most widely studied interacting galaxy pairs. ] (also known as Messier 51b or M51b) is a dwarf galaxy that is interacting with the Whirlpool Galaxy (also known as M51a or NGC 5194). Both galaxies are located approximately 25 million light-years away in the constellation Canes Venatici. Together, the two galaxies are one of the most widely studied interacting galaxy pairs.


==Galaxy group information== ==Galaxy group information==
{{main article|M51 Group}} {{main article|M51 Group}}

The Whirlpool Galaxy is the brightest galaxy in the ], a small ] that also includes M63 (the ]), ], and ].<ref name="nbg"> The Whirlpool Galaxy is the brightest galaxy in the ], a small ] that also includes M63 (the ]), ], and ].<ref name="nbg">
{{cite book {{cite book
| first=R. B. |last=Tully | first=R. B. |last=Tully | authorlink = R. Brent Tully
| date=1988 | date=1988
| title=Nearby Galaxies Catalog | title=Nearby Galaxies Catalog
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| arxiv=astro-ph/0001140 |s2cid=9618325 }}</ref> This small group may actually be a subclump at the southeast end of a large, elongated group that includes the ] and the ], although most group identification methods and catalogs identify the three groups as separate entities.<ref name="ferrareseetal00"> | arxiv=astro-ph/0001140 |s2cid=9618325 }}</ref> This small group may actually be a subclump at the southeast end of a large, elongated group that includes the ] and the ], although most group identification methods and catalogs identify the three groups as separate entities.<ref name="ferrareseetal00">
{{cite journal {{cite journal
| first1=L. |last1=Ferrarese |first2=H. C. |display-authors=4 |last2=Ford |first3=J. |last3=Huchra |first4=R. C. |last4=Kennicutt Jr. |first5=J. R. |last5=Mould |first6=S. |last6=Sakai |first7=W. L. |last7=Freedman |first8=P. B. |last8=Stetson |first9=B. F. |last9=Madore |first10=B. K. |last10=Gibson |first11=J. A. |last11=Graham |first12=S. M. |last12=Hughes |first13=G. D. |last13=Illingworth |first14=D. D. |last14=Kelson |first15=L. |last15=Macri |first16=K. |last16=Sebo |first17=N. A. |last17=Silbermann | first1=L. |last1=Ferrarese |first2=H. C. |display-authors=4 |last2=Ford |first3=J. |last3=Huchra | authorlink3 = John Huchra |first4=R. C. |last4=Kennicutt Jr. | authorlink4 = Robert Kennicutt |first5=J. R. |last5=Mould |first6=S. |last6=Sakai |first7=W. L. |last7=Freedman |first8=P. B. |last8=Stetson |first9=B. F. |last9=Madore |first10=B. K. |last10=Gibson |first11=J. A. |last11=Graham |first12=S. M. |last12=Hughes |first13=G. D. |last13=Illingworth |first14=D. D. |last14=Kelson |first15=L. |last15=Macri |first16=K. |last16=Sebo |first17=N. A. |last17=Silbermann
| date=2000 | date=2000
| title=A Database of Cepheid Distance Moduli and Tip of the Red Giant Branch, Globular Cluster Luminosity Function, Planetary Nebula Luminosity Function, and Surface Brightness Fluctuation Data Useful for Distance Determinations | title=A Database of Cepheid Distance Moduli and Tip of the Red Giant Branch, Globular Cluster Luminosity Function, Planetary Nebula Luminosity Function, and Surface Brightness Fluctuation Data Useful for Distance Determinations
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==See also== ==See also==
⚫ {{Portal|Astronomy|Stars|Outer space}}
* ] – another grand-design spiral galaxy * ] – another grand-design spiral galaxy
⚫ * ]
* ] * ]
⚫ * ]

{{clear}}


==Notes== ==Notes==
{{notelist}} {{Notelist}}


==References== ==References==
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== External links == == External links ==
{{commons category|Whirlpool Galaxy}} {{Commons category|Whirlpool Galaxy}}
* *
* {{APOD|date=10 April 2001|title=M51: The Whirlpool Galaxy in Dust and Stars}} * {{APOD|date=10 April 2001|title=M51: The Whirlpool Galaxy in Dust and Stars}}
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* {{WikiSky|name=The Whirlpool Galaxy}} * {{WikiSky|name=The Whirlpool Galaxy}}


{{Sky|13|29|52.7|+|47|11|43|23400000}} {{Catalogs|M=51|NGC=5194|UGC=8493|PGC=47404|VV=403|Arp=85|GC=3572}} {{Sky|13|29|52.7|+|47|11|43|23400000}}
{{Catalogs|M=51|NGC=5194|UGC=8493|PGC=47404|VV=403|Arp=85|GC=3572}}
{{Messier objects}} {{Messier objects}}
{{Ngc55}} {{Ngc55}}
{{List of Seyfert galaxies}} {{List of Seyfert galaxies}}
{{Canes Venatici}} {{Canes Venatici}}

⚫ {{Portal bar|Astronomy|Stars|Outer space}}
{{DEFAULTSORT:Whirlpool Galaxy}} {{DEFAULTSORT:Whirlpool Galaxy}}
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Latest revision as of 02:58, 24 November 2024

Galaxy in the constellation Canes Venatici "Galaxy M51" redirects here. For the smartphone, see Samsung Galaxy M51.
Whirlpool Galaxy
Whirlpool Galaxy (M51a), as taken by the European Space Agency, the smaller object in the upper right is NGC 5195 (M51b)
(NASA/ESA)
Observation data (J2000.0 epoch)
ConstellationCanes Venatici
Right ascension13 29 52.7
Declination+47° 11′ 43″
Redshift0.001534±0.000007
Distance7.22 ± 2.13 megaparsecs (23.5 ± 6.95 million light-years)


Apparent magnitude (V)8.4
Characteristics
TypeSA(s)bc pec
Size23.58 kpc (76,900 ly)
(diameter; 25.0 mag/arcsec B-band isophote)
Apparent size (V)11.2′ × 6.9′
Notable featuresInteracting with NGC 5195
Other designations
Question Mark Galaxy, Rosse's Galaxy, M51a, NGC 5194, UGC 8493, PGC 47404, VV 001a, VV 403, Arp 85, GC 3572

The Whirlpool Galaxy, also known as Messier 51a (M51a) or NGC 5194, is an interacting grand-design spiral galaxy with a Seyfert 2 active galactic nucleus. It lies in the constellation Canes Venatici, and was the first galaxy to be classified as a spiral galaxy. It is 7.22 megaparsecs (23.5 million light-years) away and 23.58 kiloparsecs (76,900 ly) in diameter.

The galaxy and its companion, NGC 5195, are easily observed by amateur astronomers, and the two galaxies may be seen with binoculars. The Whirlpool Galaxy has been extensively observed by professional astronomers, who study it and its pair with NGC 5195 to understand galaxy structure (particularly structure associated with the spiral arms) and galaxy interactions. Its pair with NGC 5195 is among the most famous and relatively close interacting systems, and thus is a favorite subject of galaxy interaction models.

Discovery

Sketch of M51 by Lord Rosse in 1845

William Parsons, 3rd Earl of Rosse, employing a 72-inch (1.8 m) reflecting telescope at Birr Castle, Ireland, found that the Whirlpool possessed a spiral structure, the first "nebula" to be known to have one. These "spiral nebulae" were not recognized as galaxies until Edwin Hubble was able to observe Cepheid variables in some of these spiral nebulae, which provided evidence that they were so far away that they must be entirely separate galaxies. The Whirlpool Galaxy was discovered on October 13, 1773, by Charles Messier while searching for objects that might confuse comet hunters. It was later cataloged as M51 in Messier's list of astronomical objects.

The advent of radio astronomy and subsequent radio images of M51 unequivocally demonstrated that the Whirlpool and its companion galaxy are indeed interacting. Sometimes the designation M51 is used to refer to the pair of galaxies, in which case the individual galaxies may be referred to as M51a (NGC 5194) and M51b (NGC 5195).

Visual appearance

The image of the Whirlpool Galaxy in visible light (left) and infrared light (right)

Deep in the constellation Canes Venatici, M51 is often found by finding the easternmost star of the Big Dipper, Alkaid, and going 3.5° southwest. Its declination is, rounded, +47°, making it circumpolar (never setting) for observers above the 43rd parallel north; it reaches a high altitude throughout this hemisphere making it an accessible object from the early hours in November through to the end of May, after which observation is more coincidental in modest latitudes with the risen sun (due to the Sun approaching to and receding from its right ascension, specifically figuring in Gemini, just to the north).

M51 is visible through binoculars under dark sky conditions, and it can be resolved in detail with modern amateur telescopes. When seen through a 100 mm telescope the basic outlines of M51 (limited to 5×6') and its companion are visible. Under dark skies, and with a moderate eyepiece through a 150 mm telescope, M51's intrinsic spiral structure can be detected. With larger (>300 mm) instruments under dark sky conditions, the various spiral bands are apparent with HII regions visible, and M51 can be seen to be attached to M51B.

As is usual for galaxies, the true extent of its structure can only be gathered from inspecting photographs; long exposures reveal a large nebula extending beyond the visible circular appearance. In 1984, thanks to the high-speed detector—the so-called image-photon-counting-system (IPCS)—developed jointly by the CNRS Laboratoire d'Astronomie Spatiald (L.A.S.-CNRS) and the Observatoire de Haute Provence (O.H.P.) along with the particularly nice visibility offered by the Canada-France-Hawaii-Telescope (C.F.H.T.) 3.60m Cassegrain focus on the summit of Mauna Kea in Hawaii, Hua et al. detected the double component of the very nucleus of the Whirlpool Galaxy.

In January 2005 the Hubble Heritage Project constructed a 11,477 × 7,965-pixel composite image (shown in the infobox above) of M51 using Hubble's ACS instrument. The image highlights the galaxy's spiral arms, and shows detail into some of the structures inside the arms.

Whirlpool Galaxy – Observed in Various Light
a) 0.4 and 0.7 μm; b) vis-blue/green and IR-red; c) 3.6, 4.5, and 8 μm; d) 24 μm

Properties

The Whirlpool Galaxy lies at a distance of 23 to 31 million light-years from Earth. Based on the 1991 measurement by the Third Reference Catalogue of Bright Galaxies using the D25 isophote at the B-band, the Whirlpool Galaxy has a diameter of 23.58 kiloparsecs (76,900 light-years). Overall the galaxy is about 88% the size of the Milky Way. Its mass is estimated to be 160 billion solar masses, or around 10.3% of the mass of Milky Way Galaxy.

A 1992 Hubble image showing a knot of dust encircling the black hole at the center of M51

A black hole, once thought to be surrounded by a ring of dust, but now believed to be partially occluded by dust instead, exists at the heart of the spiral. A pair of ionization cones extend from the active galactic nucleus.

Spiral structure

The Whirlpool Galaxy has two, very prominent spiral arms that wind clockwise. One arm deviates from a constant angle significantly. The pronounced spiral structure of the Whirlpool Galaxy is believed to be the result of the close interaction between it and its companion galaxy NGC 5195, which may have passed through the main disk of M51 about 500 to 600 million years ago. In this proposed scenario, NGC 5195 came from behind M51 through the disk towards the observer and made another disk crossing as recently as 50 to 100 million years ago until it is where we observe it to be now, slightly behind M51.

Tidal features

As a result of the Whirpool Galaxy's interaction with NGC 5195, a variety of tidal features have been created. The largest of these features is the so-called Northwest plume, which extends out to 43 kiloparsecs (140,000 light-years) from the galaxy's center. This plume is uniform in color and likely originated from the Whirpool Galaxy itself due to having diffuse gas. Adjacent to it are two other plumes that have a slightly bluer color, referred to as the Western plumes due to their location.

In 2015, a study discovered two new tidal features caused by the interaction between the Whirlpool Galaxy and NGC 5195, the "Northeast plume" and the "South plume". The study remarks that a simulation that takes into account only one passage of NGC 5195 into the Whirpool Galaxy will fail to produce an analogue to the Northeast tail. In contrast, the multiple-passage simulations made by Salo and Laurikainen et.al reproduce the northeast plume.

Star formation

The central region of M51 appears to be undergoing a period of enhanced star formation. The present efficiency of star formation, defined as the ratio of mass of new stars to the mass of star-forming gas, is only ~1%, quite comparable to the global value for the Milky Way and other galaxies. It is estimated that the current high rate of star formation can last no more than another 100 million years or so. Similarly, the spiral arms are experiencing high levels of star formation, as well as the space along the arms.

Transient events

Three supernovae have been observed in the Whirlpool Galaxy:

In 1994, SN 1994I was observed in the Whirlpool Galaxy. It was classified as type Ic, indicating that its progenitor star was very massive and had already shed much of its mass, and its brightness peaked at apparent magnitude 12.91.

In June 2005 the type II supernova SN 2005cs was observed in the Whirlpool Galaxy, peaking at apparent magnitude 14.

On 31 May 2011 a type II supernova was detected in the Whirlpool Galaxy, peaking at magnitude 12.1. This supernova, designated SN 2011dh, showed a spectrum much bluer than average, with P Cygni profiles, which indicate rapidly expanding material, in its hydrogen-Balmer lines. The progenitor was probably a yellow supergiant and not a red or blue supergiant, which are thought to be the most common supernova progenitors.

Supernova impostor AT2019abn, imaged by the Hubble Space Telescope

On 22 January 2019, a supernova impostor, designated AT 2019abn, was discovered in Messier 51. The transient was later identified as a luminous red nova. The progenitor star was detected in archival Spitzer Space Telescope infrared images. No object could be seen at the position of the transient in archival Hubble images, indicating that the progenitor star was heavily obstructed by interstellar dust. 2019abn peaked at magnitude 17, reaching an intrinsic brightness of M r = − 14.9 {\displaystyle M_{r}=-14.9} .

Planet candidate

In September 2020, the detection by the Chandra X-ray Observatory of a candidate exoplanet, named M51-ULS-1b, orbiting the high-mass X-ray binary M51-ULS-1 in this galaxy was announced. If confirmed, it would be the first known instance of an extragalactic planet, a planet outside the Milky Way Galaxy. The planet candidate was detected by eclipses of the X-ray source (XRS), which consists of a stellar remnant (either a neutron star or a black hole) and a massive star, likely a B-type supergiant. The planet would be slightly smaller than Saturn and orbit at a distance of some tens of astronomical units.

Companion

Main article: NGC 5195

NGC 5195 (also known as Messier 51b or M51b) is a dwarf galaxy that is interacting with the Whirlpool Galaxy (also known as M51a or NGC 5194). Both galaxies are located approximately 25 million light-years away in the constellation Canes Venatici. Together, the two galaxies are one of the most widely studied interacting galaxy pairs.

Galaxy group information

Main article: M51 Group

The Whirlpool Galaxy is the brightest galaxy in the M51 Group, a small group of galaxies that also includes M63 (the Sunflower Galaxy), NGC 5023, and NGC 5229. This small group may actually be a subclump at the southeast end of a large, elongated group that includes the M101 Group and the NGC 5866 Group, although most group identification methods and catalogs identify the three groups as separate entities.

See also

Notes

  1. 47 out of 90 degrees north of the celestial equator. Thus its light emits as far south, to a good minimal cumulation of 15° above the horizon, once a day, on the 28th parallel south.

References

  1. Dreyer, J. L. E. (1988). Sinnott, R. W. (ed.). The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters. Sky Publishing Corporation/Cambridge University Press. ISBN 978-0-933346-51-2.
  2. ^ "NASA/IPAC Extragalactic Database". Results for NGC 5194. Retrieved December 6, 2006.
  3. "Messier 51 (The Whirlpool Galaxy)". 6 October 2017.
  4. "M51". SEDS.org.
  5. ^ De Vaucouleurs, Gerard; De Vaucouleurs, Antoinette; Corwin, Herold G.; Buta, Ronald J.; Paturel, Georges; Fouque, Pascal (1991). Third Reference Catalogue of Bright Galaxies. Bibcode:1991rc3..book.....D.
  6. ^ Elmegreen, D. M.; Elmegreen, B. G. (1987). "Arm classifications for spiral galaxies". Astrophysical Journal. 314: 3–9. Bibcode:1987ApJ...314....3E. doi:10.1086/165034.
  7. Arp, H. (1966). "Atlas of Peculiar Galaxies". Astrophysical Journal Supplement. 14: 1. Bibcode:1966ApJS...14....1A. doi:10.1086/190147.
  8. Matsushita, Satoki; Muller, Sebastien; Lim, Jeremy (9 April 2007). "Jet-disturbed molecular gas near the Seyfert 2 nucleus in M51". Astronomy & Astrophysics. 468 (A&A Letters Special Issue): L49–L52. arXiv:0704.0947. Bibcode:2007A&A...468L..49M. doi:10.1051/0004-6361:20067039. S2CID 15471799.
  9. "Whirlpool Galaxy: First Spiral Galaxy". Universe for Facts. Retrieved 2014-12-21.
  10. Garner, Rob (2017-10-06). "Messier 51 (The Whirlpool Galaxy)". NASA. Retrieved 2021-01-20.
  11. "M 51". Messier Objects 101.com. 2016-10-10. Archived from the original on 2016-10-28.
  12. ^ Nemiroff, R.; Bonnell, J., eds. (February 24, 2013). "M51: The Whirlpool Galaxy". Astronomy Picture of the Day. NASA. Retrieved October 11, 2018.
  13. Messier, Charles (1781). "Catalogue des Nébuleuses & des amas d'Étoiles". Connaissance des Temps . pp. 227–267 .
  14. Rosse revealed the spiral structure of Whirlpool galaxy (M51) at the 1845 meeting of the British Association for the Advancement of Science. Rosse's illustration of M51 was reproduced in J.P. Nichol's book of 1846.
  15. Hubble, E. P. (1929). "A spiral nebula as a stellar system, Messier 31". Astrophysical Journal. 69: 103–158. Bibcode:1929ApJ....69..103H. doi:10.1086/143167.
  16. Hua; et al. (1987). "". Astrophysical Letters & Communications. 25: 187–204. ISSN 0888-6512. OCLC 60627567.
  17. "Hubble Celebrates 15th Anniversary with Spectacular New Images". News Center. HubbleSite. April 25, 2005. Retrieved 13 October 2024.
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