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Coordinates: Sky map 14h 03m 12.6s, +54° 20′ 57″
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| editor=R. W. Sinnott
| editor=R. W. Sinnott
| 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
| year=1988
| date=1988
| publisher=Sky Publishing Corporation / Cambridge University Press
| publisher=Sky Publishing Corporation / Cambridge University Press
| isbn=0-933346-51-4
| isbn=0-933346-51-4
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| journal=[[Astrophysical Journal Supplement]]
| journal=[[Astrophysical Journal Supplement]]
| volume=173
| volume=173
|issue=2 |pages=185–255 | year=2007
|issue=2 |pages=185–255 | date=2007
| arxiv=astro-ph/0606440
| arxiv=astro-ph/0606440
| doi=10.1086/516636
| doi=10.1086/516636
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== Structure and composition ==
== Structure and composition ==
[[File:NASA-SpiralGalaxyM101-20140505.jpg|thumb|right|Combined infrared, visible, and x-ray images of M101 showing that both young and old stars are evenly distributed along the tightly-wound spiral arms.]]
[[File:NASA-SpiralGalaxyM101-20140505.jpg|thumb|right|Combined infrared, visible, and x-ray images of M101 showing that both young and old stars are evenly distributed along the tightly-wound spiral arms.]]
M101 is a relatively large galaxy compared to the [[Milky Way]]. With a diameter of 170,000 light-years it is seventy percent larger than the Milky Way. It has a disk mass on the order of 100 billion solar masses, along with a small central bulge of about 3 billion solar masses.<ref name="M101 mass">{{cite journal |author=Comte, G., Monnet, G., & Rosado, M. |year=1979 |title=An optical study of the galaxy M 101 - Derivation of a mass model from the kinematic of the gas |journal=Astronomy and Astrophysics |volume=72 |pages=73–81 |bibcode=1979A&A....72...73C |last2=Monnet |last3=Rosado }}</ref>
M101 is a relatively large galaxy compared to the [[Milky Way]]. With a diameter of 170,000 light-years it is seventy percent larger than the Milky Way. It has a disk mass on the order of 100 billion solar masses, along with a small central bulge of about 3 billion solar masses.<ref name="M101 mass">{{cite journal |author=Comte, G., Monnet, G., & Rosado, M. |date=1979 |title=An optical study of the galaxy M 101 - Derivation of a mass model from the kinematic of the gas |journal=Astronomy and Astrophysics |volume=72 |pages=73–81 |bibcode=1979A&A....72...73C |last2=Monnet |last3=Rosado }}</ref>


M101 is noted for its high population of [[H II region]]s, many of which are very large and bright. H II regions usually accompany the enormous clouds of high density molecular hydrogen gas contracting under their own gravitational force where [[Star formation|stars form]]. H II regions are ionized by large numbers of extremely bright and hot young stars; those in M101 are capable of creating hot [[superbubble]]s.<ref>{{cite journal |url=http://iopscience.iop.org/0004-637X/554/1/202/ |title=ROSAT X-Ray Observations of the Spiral Galaxy M81 |journal=The Astrophysical Journal |volume=554 |issue=1 |author=Immler, Stefan and Wang, Q. Daniel |year=2001 |page=202 |doi=10.1086/321335 |accessdate=12 May 2014|arxiv = astro-ph/0102021 |bibcode = 2001ApJ...554..202I }}</ref> In a 1990 study, 1264 H II regions were cataloged in the galaxy.<ref>{{cite journal |bibcode=1990ApJS...73..661H |title=The H II regions of M101. I - an atlas of 1264 emission regions |author=Hodge, Paul W. et al |date=August 1990 |journal=Astrophysical Journal Supplement Series |volume=73 |pages=661–670 |doi=10.1086/191483 |last2=Gurwell |first2=Mark |last3=Goldader |first3=Jeffrey D. |last4=Kennicutt |first4=Robert C., Jr. }}</ref> Three are prominent enough to receive [[New General Catalogue]] numbers - NGC 5461, NGC 5462, and NGC 5471.<ref>{{Cite journal|arxiv=astro-ph/9903334|last1= Giannakopoulou-Creighton|first1= J.|title= Star formation in the giant HII regions of M101|journal= The Astrophysical Journal|volume= 522|pages= 238|last2= Fich|first2= M.|last3= Wilson|first3= C. D.|year= 1999|doi= 10.1086/307619|bibcode = 1999ApJ...522..238G }}</ref>
M101 is noted for its high population of [[H II region]]s, many of which are very large and bright. H II regions usually accompany the enormous clouds of high density molecular hydrogen gas contracting under their own gravitational force where [[Star formation|stars form]]. H II regions are ionized by large numbers of extremely bright and hot young stars; those in M101 are capable of creating hot [[superbubble]]s.<ref>{{cite journal |url=http://iopscience.iop.org/0004-637X/554/1/202/ |title=ROSAT X-Ray Observations of the Spiral Galaxy M81 |journal=The Astrophysical Journal |volume=554 |issue=1 |author=Immler, Stefan and Wang, Q. Daniel |date=2001 |page=202 |doi=10.1086/321335 |accessdate=12 May 2014|arxiv = astro-ph/0102021 |bibcode = 2001ApJ...554..202I }}</ref> In a 1990 study, 1264 H II regions were cataloged in the galaxy.<ref>{{cite journal |bibcode=1990ApJS...73..661H |title=The H II regions of M101. I - an atlas of 1264 emission regions |author=Hodge, Paul W. et al. |date=August 1990 |journal=Astrophysical Journal Supplement Series |volume=73 |pages=661–670 |doi=10.1086/191483 |last2=Gurwell |first2=Mark |last3=Goldader |first3=Jeffrey D. |last4=Kennicutt |first4=Robert C., Jr. }}</ref> Three are prominent enough to receive [[New General Catalogue]] numbers - NGC 5461, NGC 5462, and NGC 5471.<ref>{{Cite journal|arxiv=astro-ph/9903334|last1= Giannakopoulou-Creighton|first1= J.|title= Star formation in the giant HII regions of M101|journal= The Astrophysical Journal|volume= 522|pages= 238|last2= Fich|first2= M.|last3= Wilson|first3= C. D.|date= 1999|doi= 10.1086/307619|bibcode = 1999ApJ...522..238G }}</ref>


M101 is asymmetrical due to the tidal forces from interactions with its companion galaxies. These gravitational interactions compress [[Interstellar medium|interstellar hydrogen gas]], which then triggers strong [[star formation]] activity in M101's spiral arms that can be detected in ultraviolet images.<ref>{{cite journal |url=http://iopscience.iop.org/0004-637X/481/1/169 |title=Ultraviolet Signatures of Tidal Interaction in the Giant Spiral Galaxy M101 |author=Waller, William H. et al |journal=The Astrophysical Journal |volume=481 |issue=1 |page=169 |date=20 May 1997 |doi=10.1086/304057 |accessdate=12 May 2014|last2=Bohlin |first2=Ralph C. |last3=Cornett |first3=Robert H. |last4=Fanelli |first4=Michael N. |last5=Freedman |first5=Wendy L. |last6=Hill |first6=Jesse K. |last7=Madore |first7=Barry F. |last8=Neff |first8=Susan G. |last9=Offenberg |first9=Joel D. |last10=O'Connell |first10=Robert W. |last11=Roberts |first11=Morton S. |last12=Smith |first12=Andrew M. |last13=Stecher |first13=Theodore P. |arxiv = astro-ph/9612165 |bibcode = 1997ApJ...481..169W }}</ref>
M101 is asymmetrical due to the tidal forces from interactions with its companion galaxies. These gravitational interactions compress [[Interstellar medium|interstellar hydrogen gas]], which then triggers strong [[star formation]] activity in M101's spiral arms that can be detected in ultraviolet images.<ref>{{cite journal |url=http://iopscience.iop.org/0004-637X/481/1/169 |title=Ultraviolet Signatures of Tidal Interaction in the Giant Spiral Galaxy M101 |author=Waller, William H. et al. |journal=The Astrophysical Journal |volume=481 |issue=1 |page=169 |date=20 May 1997 |doi=10.1086/304057 |accessdate=12 May 2014|last2=Bohlin |first2=Ralph C. |last3=Cornett |first3=Robert H. |last4=Fanelli |first4=Michael N. |last5=Freedman |first5=Wendy L. |last6=Hill |first6=Jesse K. |last7=Madore |first7=Barry F. |last8=Neff |first8=Susan G. |last9=Offenberg |first9=Joel D. |last10=O'Connell |first10=Robert W. |last11=Roberts |first11=Morton S. |last12=Smith |first12=Andrew M. |last13=Stecher |first13=Theodore P. |arxiv = astro-ph/9612165 |bibcode = 1997ApJ...481..169W }}</ref>


In 2001, the x-ray source P98, located in M101, was identified as an [[ultra-luminous X-ray source]] - a source more powerful than any single star but less powerful than a whole galaxy - using the [[Chandra X-ray Observatory]]. It received the designation M101 ULX-1. In 2005, [[Hubble Space Telescope|Hubble]] and [[XMM-Newton]] observations showed the presence of an optical counterpart, strongly indicating that M101 ULX-1 is an [[x-ray binary]].<ref>{{cite journal |url=http://iopscience.iop.org/1538-4357/620/1/L31/fulltext/19014.text.html |title=The Optical Counterpart of M101 ULX-1 |journal=The Astrophysical Journal |volume=620 |issue=1 |pages=L31–L34 |author=Kuntz, K.D. et al |doi=10.1086/428571|bibcode=2005ApJ...620L..31K |date=10 February 2005 |accessdate=12 May 2014}}</ref> Further observations showed that the system deviated from expected models - the black hole is just 20 to 30 [[solar mass]]es, and consumes material (including captured stellar wind) at a higher rate than theory suggests.<ref>{{Cite journal|arxiv=1312.0337|last1=Liu|first1=Jifeng|title=Puzzling accretion onto a black hole in the ultraluminous X-ray source
In 2001, the x-ray source P98, located in M101, was identified as an [[ultra-luminous X-ray source]] - a source more powerful than any single star but less powerful than a whole galaxy - using the [[Chandra X-ray Observatory]]. It received the designation M101 ULX-1. In 2005, [[Hubble Space Telescope|Hubble]] and [[XMM-Newton]] observations showed the presence of an optical counterpart, strongly indicating that M101 ULX-1 is an [[x-ray binary]].<ref>{{cite journal |url=http://iopscience.iop.org/1538-4357/620/1/L31/fulltext/19014.text.html |title=The Optical Counterpart of M101 ULX-1 |journal=The Astrophysical Journal |volume=620 |issue=1 |pages=L31–L34 |author=Kuntz, K.D. et al. |doi=10.1086/428571|bibcode=2005ApJ...620L..31K |date=10 February 2005 |accessdate=12 May 2014}}</ref> Further observations showed that the system deviated from expected models - the black hole is just 20 to 30 [[solar mass]]es, and consumes material (including captured stellar wind) at a higher rate than theory suggests.<ref>{{Cite journal|arxiv=1312.0337|last1=Liu|first1=Jifeng|title=Puzzling accretion onto a black hole in the ultraluminous X-ray source
M101 ULX-1|journal=Nature|volume=503|issue=7477|pages=500|last2= Bregman|first2=Joel N.|last3=Bai|first3=Yu|last4=Justham|first4=Stephen|last5=Crowther|first5=Paul|year=2013|doi=10.1038/nature12762|bibcode = 2013Natur.503..500L }}</ref>
M101 ULX-1|journal=Nature|volume=503|issue=7477|pages=500|last2= Bregman|first2=Joel N.|last3=Bai|first3=Yu|last4=Justham|first4=Stephen|last5=Crowther|first5=Paul|date=2013|doi=10.1038/nature12762|bibcode = 2013Natur.503..500L }}</ref>


== Companion galaxies ==
== Companion galaxies ==
M101 has five prominent companion galaxies: [[NGC 5204]], [[NGC 5474]], [[NGC 5477]], [[NGC 5585]], and [[Holmberg IV]].<ref name="carnegieatlas" >{{cite book | author=A. Sandage, J. Bedke| year=1994| title=Carnegie Atlas of Galaxies| publisher=[[Carnegie Institution of Washington]]| isbn=0-87279-667-1}}</ref> As stated above, the gravitational interaction between M101 and its satellites may have triggered the formation of the grand design pattern in M101. M101 has also probably distorted the companion galaxy NGC 5474.<ref name="carnegieatlas"/> M101 and its companion galaxies comprise most or possibly all of the [[M101 Group]].<ref name="nbg">{{cite book
M101 has five prominent companion galaxies: [[NGC 5204]], [[NGC 5474]], [[NGC 5477]], [[NGC 5585]], and [[Holmberg IV]].<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> As stated above, the gravitational interaction between M101 and its satellites may have triggered the formation of the grand design pattern in M101. M101 has also probably distorted the companion galaxy NGC 5474.<ref name="carnegieatlas"/> M101 and its companion galaxies comprise most or possibly all of the [[M101 Group]].<ref name="nbg">{{cite book
| author=R. B. Tully
| author=R. B. Tully
| year=1988
| date=1988
| title=Nearby Galaxies Catalog
| title=Nearby Galaxies Catalog
| publisher=[[Cambridge University Press]]
| publisher=[[Cambridge University Press]]
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| last3=Chamaraux
| last3=Chamaraux
| last4=Paturel
| last4=Paturel
| year=1992
| date=1992
}}</ref><ref name="garcia1993">
}}</ref><ref name="garcia1993">
{{cite journal
{{cite journal
| author=A. Garcia
| author=A. Garcia
| year=1993
| date=1993
| title=General study of group membership. II – Determination of nearby groups
| title=General study of group membership. II – Determination of nearby groups
| journal=[[Astronomy and Astrophysics Supplement]]
| journal=[[Astronomy and Astrophysics Supplement]]
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}}</ref><ref name="giuricinetal2002">
}}</ref><ref name="giuricinetal2002">
{{cite journal
{{cite journal
| author=G. Giuricin, C. Marinoni, L. Ceriani, A. Pisani
| author=G. Giuricin |author2=C. Marinoni |author3=L. Ceriani |author4=A. Pisani
| year=2000
| date=2000
| title=Nearby Optical Galaxies: Selection of the Sample and Identification of Groups
| title=Nearby Optical Galaxies: Selection of the Sample and Identification of Groups
| journal=[[Astrophysical Journal]]
| journal=[[Astrophysical Journal]]
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==Supernova==
==Supernova==
[[File:Supernova in M101 2011-08-25.jpg|thumb|right|150px|Type Ia supernova [[SN 2011fe]]]]
[[File:Supernova in M101 2011-08-25.jpg|thumb|right|150px|Type Ia supernova [[SN 2011fe]]]]
On August 24, 2011, a [[Type Ia supernova]], [[SN 2011fe]], initially designated PTF 11kly, was discovered in M101. The supernova was [[Apparent magnitude|visual magnitude]] 17.2 at discovery and reached magnitude 9.9 at its peak.<ref>{{cite web |title=Young Type Ia Supernova PTF11kly in M101 |url=http://www.astronomerstelegram.org/?read=3581 |author=Nugent, Peter et al |publisher=The Astronomer's Telegram |date=24 August 2011 |accessdate=25 August 2011}}</ref><ref>{{cite web |title=Supernova Caught in the Act |url=http://www.nersc.gov/news-publications/science-news/2011/supernova-caught-in-the-act/ |author=Nugent, Peter et al |accessdate=7 September 2011}}</ref><ref>{{cite web |title=Supernova 2011fe in M101|author=Hartmut Frommert and Christine Kronberg |url=http://messier.seds.org/more/m101_sn2011fe.html |date=15 Sep 2011 |accessdate=17 Sep 2011}}</ref> This was the fourth supernova recorded in M101. The first, SN 1909A, was discovered by [[Max Wolf]] in January 1909 and reached magnitude 12.1. SN 1951H reached magnitude 17.5 in September 1951 and SN 1970G reached magnitude 11.5 in January 1970.<ref>Stoyan, Ronald Atlas of the Messier Objects, Cambridge University Press 2008 page 329</ref>
On August 24, 2011, a [[Type Ia supernova]], [[SN 2011fe]], initially designated PTF 11kly, was discovered in M101. The supernova was [[Apparent magnitude|visual magnitude]] 17.2 at discovery and reached magnitude 9.9 at its peak.<ref>{{cite web |title=Young Type Ia Supernova PTF11kly in M101 |url=http://www.astronomerstelegram.org/?read=3581 |author=Nugent, Peter et al. |publisher=The Astronomer's Telegram |date=24 August 2011 |accessdate=25 August 2011}}</ref><ref>{{cite web |title=Supernova Caught in the Act |url=http://www.nersc.gov/news-publications/science-news/2011/supernova-caught-in-the-act/ |author=Nugent, Peter et al. |accessdate=7 September 2011}}</ref><ref>{{cite web |title=Supernova 2011fe in M101|author=Hartmut Frommert and Christine Kronberg |url=http://messier.seds.org/more/m101_sn2011fe.html |date=15 Sep 2011 |accessdate=17 Sep 2011}}</ref> This was the fourth supernova recorded in M101. The first, SN 1909A, was discovered by [[Max Wolf]] in January 1909 and reached magnitude 12.1. SN 1951H reached magnitude 17.5 in September 1951 and SN 1970G reached magnitude 11.5 in January 1970.<ref>Stoyan, Ronald Atlas of the Messier Objects, Cambridge University Press 2008 page 329</ref>
{{-}}
{{-}}


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== References ==
== References ==
{{reflist|2}}
{{reflist|30em}}


== External links ==
== External links ==

Revision as of 19:57, 23 January 2015

For other uses, see Pinwheel Galaxy (disambiguation).
Pinwheel Galaxy
Observation data (J2000 epoch)
ConstellationUrsa Major
Right ascension14h 03m 12.6s
Declination+54° 20′ 57″
Redshift0.000804
Heliocentric radial velocity241 ± 2 km/s
Distance20.9 ± 1.8 Mly (6.4 ± 0.5 Mpc)
Apparent magnitude (V)7.86
Characteristics
TypeSAB(rs)cd
Size~170,000ly in diameter[1]
Apparent size (V)28′.8 × 26′.9
Other designations
Messier 101, M101, NGC 5457, UGC 8981, PGC 50063, Arp 26
References: [2][3][4][5][6][7]

The Pinwheel Galaxy (also known as Messier 101, M101 or NGC 5457) is a face-on spiral galaxy distanced 21 million light-years (six megaparsecs)[3] away in the constellation Ursa Major, first discovered by Pierre Méchain on March 27, 1781, and communicated to Charles Messier who verified its position for inclusion in the Messier Catalogue as one of its final entries.

On February 28, 2006, NASA and the ESA released a very detailed image of the Pinwheel Galaxy, which was the largest and most detailed image of a galaxy by Hubble Space Telescope at the time.[8] The image was composed from 51 individual exposures, plus some extra ground-based photos.

On August 24, 2011, a Type Ia supernova, SN 2011fe, was discovered in M101.

Discovery

The Pinwheel Galaxy

Pierre Méchain, the discoverer of Messier 101, described it as a "nebula without star, very obscure and pretty large, 6' to 7' in diameter, between the left hand of Bootes and the tail of the great Bear. It is difficult to distinguish when one lits the [grating] wires."[9]

William Herschel noted in 1784 that "[M101] in my 7, 10, and 20-feet [focal length] reflectors shewed a mottled kind of nebulosity, which I shall call resolvable; so that I expect my present telescope will, perhaps, render the stars visible of which I suppose them to be composed."[9]

Lord Rosse observed M101 in his 72-inch diameter Newtonian reflector during the second half of the 19th century. He was the first to make extensive note of the spiral structure and made several sketches.[9]

To observe the spiral structure in modern instruments requires a fairly large instrument, very dark skies, and a low power eye piece.

Structure and composition

Combined infrared, visible, and x-ray images of M101 showing that both young and old stars are evenly distributed along the tightly-wound spiral arms.

M101 is a relatively large galaxy compared to the Milky Way. With a diameter of 170,000 light-years it is seventy percent larger than the Milky Way. It has a disk mass on the order of 100 billion solar masses, along with a small central bulge of about 3 billion solar masses.[10]

M101 is noted for its high population of H II regions, many of which are very large and bright. H II regions usually accompany the enormous clouds of high density molecular hydrogen gas contracting under their own gravitational force where stars form. H II regions are ionized by large numbers of extremely bright and hot young stars; those in M101 are capable of creating hot superbubbles.[11] In a 1990 study, 1264 H II regions were cataloged in the galaxy.[12] Three are prominent enough to receive New General Catalogue numbers - NGC 5461, NGC 5462, and NGC 5471.[13]

M101 is asymmetrical due to the tidal forces from interactions with its companion galaxies. These gravitational interactions compress interstellar hydrogen gas, which then triggers strong star formation activity in M101's spiral arms that can be detected in ultraviolet images.[14]

In 2001, the x-ray source P98, located in M101, was identified as an ultra-luminous X-ray source - a source more powerful than any single star but less powerful than a whole galaxy - using the Chandra X-ray Observatory. It received the designation M101 ULX-1. In 2005, Hubble and XMM-Newton observations showed the presence of an optical counterpart, strongly indicating that M101 ULX-1 is an x-ray binary.[15] Further observations showed that the system deviated from expected models - the black hole is just 20 to 30 solar masses, and consumes material (including captured stellar wind) at a higher rate than theory suggests.[16]

Companion galaxies

M101 has five prominent companion galaxies: NGC 5204, NGC 5474, NGC 5477, NGC 5585, and Holmberg IV.[17] As stated above, the gravitational interaction between M101 and its satellites may have triggered the formation of the grand design pattern in M101. M101 has also probably distorted the companion galaxy NGC 5474.[17] M101 and its companion galaxies comprise most or possibly all of the M101 Group.[18][19][20][21]

Supernova

Type Ia supernova SN 2011fe

On August 24, 2011, a Type Ia supernova, SN 2011fe, initially designated PTF 11kly, was discovered in M101. The supernova was visual magnitude 17.2 at discovery and reached magnitude 9.9 at its peak.[22][23][24] This was the fourth supernova recorded in M101. The first, SN 1909A, was discovered by Max Wolf in January 1909 and reached magnitude 12.1. SN 1951H reached magnitude 17.5 in September 1951 and SN 1970G reached magnitude 11.5 in January 1970.[25]

See also

  • Messier 74 – a similar face-on spiral galaxy
  • Messier 83 – a similar face-on spiral galaxy that is sometimes called the Southern Pinwheel Galaxy
  • Messier 99 – a similar face-on spiral galaxy
  • Triangulum Galaxy – another galaxy sometimes called the Pinwheel Galaxy

References

  1. ^ http://www.nasa.gov/multimedia/imagegallery/image_feature_2265.html#.VIX5BWf0DDE NASA/CXC/SAO; IR & UV: NASA/JPL-Caltech; Optical: NASA/STScI
  2. ^ "NASA/IPAC Extragalactic Database". Results for Messier 101. Retrieved 2006-12-06.
  3. ^ a b Shappee, Benjamin; Stanek, Kris (June 2011). "A New Cepheid Distance to the Giant Spiral M101 Based on Image Subtraction of Hubble Space Telescope/Advanced Camera for Surveys Observations". Astrophysical Journal. 733 (2): 124. arXiv:1012.3747. Bibcode:2011ApJ...733..124S. doi:10.1088/0004-637X/733/2/124.
  4. ^ R. W. Sinnott, ed. (1988). The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer. Sky Publishing Corporation / Cambridge University Press. ISBN 0-933346-51-4.
  5. ^ "Distance Results for Messier 101". NASA/IPAC Extragalactic Database. Retrieved 2010-05-01.
  6. ^ "SIMBAD-M101". SIMBAD Astronomical Database. Retrieved 2009-11-29.
  7. ^ Armando, Gil de Paz; Boissier; Madore; Seibert; Boselli; et al. (2007). "The GALEX Ultraviolet Atlas of Nearby Galaxies". Astrophysical Journal Supplement. 173 (2): 185–255. arXiv:astro-ph/0606440. Bibcode:2007ApJS..173..185G. doi:10.1086/516636. {{cite journal}}: Explicit use of et al. in: |author6= (help)
  8. ^ HubbleSite – NewsCenter – Hubble's Largest Galaxy Portrait Offers a New High-Definition View (02/28/2006) – Introduction
  9. ^ a b c SEDS Historical Notes
  10. ^ Comte, G., Monnet, G., & Rosado, M.; Monnet; Rosado (1979). "An optical study of the galaxy M 101 - Derivation of a mass model from the kinematic of the gas". Astronomy and Astrophysics. 72: 73–81. Bibcode:1979A&A....72...73C.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  11. ^ Immler, Stefan and Wang, Q. Daniel (2001). "ROSAT X-Ray Observations of the Spiral Galaxy M81". The Astrophysical Journal. 554 (1): 202. arXiv:astro-ph/0102021. Bibcode:2001ApJ...554..202I. doi:10.1086/321335. Retrieved 12 May 2014.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  12. ^ Hodge, Paul W.; Gurwell, Mark; Goldader, Jeffrey D.; Kennicutt, Robert C., Jr.; et al. (August 1990). "The H II regions of M101. I - an atlas of 1264 emission regions". Astrophysical Journal Supplement Series. 73: 661–670. Bibcode:1990ApJS...73..661H. doi:10.1086/191483. {{cite journal}}: Explicit use of et al. in: |author= (help)CS1 maint: multiple names: authors list (link)
  13. ^ Giannakopoulou-Creighton, J.; Fich, M.; Wilson, C. D. (1999). "Star formation in the giant HII regions of M101". The Astrophysical Journal. 522: 238. arXiv:astro-ph/9903334. Bibcode:1999ApJ...522..238G. doi:10.1086/307619.
  14. ^ Waller, William H.; Bohlin, Ralph C.; Cornett, Robert H.; Fanelli, Michael N.; Freedman, Wendy L.; Hill, Jesse K.; Madore, Barry F.; Neff, Susan G.; Offenberg, Joel D.; O'Connell, Robert W.; Roberts, Morton S.; Smith, Andrew M.; Stecher, Theodore P.; et al. (20 May 1997). "Ultraviolet Signatures of Tidal Interaction in the Giant Spiral Galaxy M101". The Astrophysical Journal. 481 (1): 169. arXiv:astro-ph/9612165. Bibcode:1997ApJ...481..169W. doi:10.1086/304057. Retrieved 12 May 2014. {{cite journal}}: Explicit use of et al. in: |author= (help)
  15. ^ Kuntz, K.D.; et al. (10 February 2005). "The Optical Counterpart of M101 ULX-1". The Astrophysical Journal. 620 (1): L31–L34. Bibcode:2005ApJ...620L..31K. doi:10.1086/428571. Retrieved 12 May 2014. {{cite journal}}: Explicit use of et al. in: |author= (help)
  16. ^ Liu, Jifeng; Bregman, Joel N.; Bai, Yu; Justham, Stephen; Crowther, Paul (2013). "Puzzling accretion onto a black hole in the ultraluminous X-ray source M101 ULX-1". Nature. 503 (7477): 500. arXiv:1312.0337. Bibcode:2013Natur.503..500L. doi:10.1038/nature12762. {{cite journal}}: line feed character in |title= at position 71 (help)
  17. ^ a b A. Sandage; J. Bedke (1994). Carnegie Atlas of Galaxies. Carnegie Institution of Washington. ISBN 0-87279-667-1.
  18. ^ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge University Press. ISBN 0-521-35299-1.
  19. ^ P. Fouque, E. Gourgoulhon, P. Chamaraux, G. Paturel; Gourgoulhon; Chamaraux; Paturel (1992). "Groups of galaxies within 80 Mpc. II – The catalogue of groups and group members". Astronomy and Astrophysics Supplement. 93 (2nd ed.): 211–233. Bibcode:1992A&AS...93..211F.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  20. ^ A. Garcia (1993). "General study of group membership. II – Determination of nearby groups". Astronomy and Astrophysics Supplement. 100: 47–90. Bibcode:1993A&AS..100...47G.
  21. ^ G. Giuricin; Marinoni; Ceriani; Pisani (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups". Astrophysical Journal. 543 (1): 178–194. arXiv:astro-ph/0001140. Bibcode:2000ApJ...543..178G. doi:10.1086/317070. {{cite journal}}: More than one of |author2= and |last2= specified (help); More than one of |author3= and |last3= specified (help); More than one of |author4= and |last4= specified (help)
  22. ^ Nugent, Peter; et al. (24 August 2011). "Young Type Ia Supernova PTF11kly in M101". The Astronomer's Telegram. Retrieved 25 August 2011. {{cite web}}: Explicit use of et al. in: |author= (help)
  23. ^ Nugent, Peter; et al. "Supernova Caught in the Act". Retrieved 7 September 2011. {{cite web}}: Explicit use of et al. in: |author= (help)
  24. ^ Hartmut Frommert and Christine Kronberg (15 Sep 2011). "Supernova 2011fe in M101". Retrieved 17 Sep 2011.
  25. ^ Stoyan, Ronald Atlas of the Messier Objects, Cambridge University Press 2008 page 329
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