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{{short description|Spiral galaxy in the constellation Canes Venatici}} {{Short description|Spiral galaxy in the constellation Canes Venatici}}
{{Infobox Galaxy {{Infobox Galaxy
| name = Messier 63 | name = Messier 63
| image = M63 (NGC 5055).jpg | image = M63 (NGC 5055).jpg
⚫ | caption = Image taken by ], on 16 November 2001 at 450 and 814 nm<ref name=NASA/>
| image_size = 250px
| credit =
⚫ | caption = Image taken by ], on November 16, 2001 at 450 and 814 nm<ref name=NASA/>
| credit = ]
| epoch = ] | epoch = ]
| constellation name = ] | constellation name = ]
Line 14: Line 13:
| appmag_v = 9.3<ref name="ned" /> | appmag_v = 9.3<ref name="ned" />
| type = SAbc<ref name=Ann2015/> | type = SAbc<ref name=Ann2015/>
| size_v = 12&prime;.6 &times; 7&prime;.2<ref name="ned" /> | size_v = 12.6{{prime}} × 7.2{{prime}}<ref name="ned" />
| group_cluster = ] | group_cluster = ]
| names = ]63, ]&nbsp;5055, ]&nbsp;46153, ]&nbsp;8334<ref name="ned" /> | names = ]63, ]&nbsp;5055, ]&nbsp;46153, ]&nbsp;8334<ref name="ned" />
}} }}
⚫ ]


'''Messier 63''' or '''M63''', also known as '''NGC 5055''' or the seldom-used '''Sunflower Galaxy''',<ref name=Garfinkle1997/> is a ] in the northern ] of ] with approximately 400 billion stars.<ref>{{Cite web|title=Messier 63 - M63 - The Sunflower Galaxy (Spiral Galaxy) {{!}} freestarcharts.com|url=https://freestarcharts.com/messier-63|access-date=2020-06-23|website=freestarcharts.com}}</ref> M63 was first discovered by the French astronomer ], then later verified by his colleague ] on June 14, 1779.<ref name=Garfinkle1997/> The galaxy became listed as object 63 in the ]. In the mid-19th century, Anglo-Irish astronomer ] identified spiral structures within the galaxy, making this one of the first galaxies in which such structure was identified.<ref name=jonesbook1991/> '''Messier 63''' or '''M63''', also known as '''NGC 5055''' or the seldom-used '''Sunflower Galaxy''',<ref name=Garfinkle1997/> is a ] in the northern ] of ] with approximately 400 billion stars.<ref>{{Cite web|title=Messier 63 - M63 - The Sunflower Galaxy (Spiral Galaxy) {{!}} freestarcharts.com|url=https://freestarcharts.com/messier-63|access-date=2020-06-23|website=freestarcharts.com}}</ref> M63 was first discovered by the French astronomer ], then later verified by his colleague ] on 14 June 1779.<ref name=Garfinkle1997/> The galaxy became listed as object 63 in the ]. In the mid-19th century, Anglo-Irish astronomer ] identified spiral structures within the galaxy, making this one of the first galaxies in which such structure was identified.<ref name=jonesbook1991/>


The shape or morphology of this galaxy has a ] of SAbc,<ref name=Ann2015/> indicating a spiral form with no central ] (SA) and moderate to loosely wound ] (bc). There is a general lack of large-scale continuous spiral structure in visible light, so it is considered a '']''. However, when observed in the ], a symmetric, two-arm structure is seen. Each arm wraps 150° around the galaxy and extends out to {{convert|4000|pc|lk=on|order=flip|abbr=off}} from the nucleus.<ref name=Thornley1996/> The shape or morphology of this galaxy has a ] of SAbc,<ref name=Ann2015/> indicating a spiral form with no central ] (SA) and moderate to loosely wound ] (bc). There is a general lack of large-scale continuous spiral structure in visible light, so it is considered a '']''. However, when observed in the ], a symmetric, two-arm structure is seen. Each arm wraps 150° around the galaxy and extends out to {{convert|4000|pc|lk=on|order=flip|abbr=off}} from the nucleus.<ref name=Thornley1996/>


M63 is a weakly ] with a ] nucleus &ndash; short for 'low-ionization nuclear emission-line region'. This displays as an unresolved source at the galactic nucleus that is cloaked in a diffuse ]. The latter is extended along a ] of 110° relative to the ], and both ]s and hydrogen (]) emission can be observed coming from along nearly the same direction.<ref name=Masegosa2011/> The existence of a ] (SMBH) at the nucleus is uncertain; if it does exist, then the mass is estimated as {{Val|8.5e8|1.9|ul=solar mass}},<ref name=Graham2008/> or around 850&nbsp;million times the mass of the Sun. M63 is a weakly ] with a ] nucleus &ndash; short for 'low-ionization nuclear emission-line region'. This displays as an unresolved source at the galactic nucleus that is cloaked in a diffuse ]. The latter is extended along a ] of 110° relative to the ], and both ]s and hydrogen (]) emission can be observed coming from along nearly the same direction.<ref name=Masegosa2011/> The existence of a ] (SMBH) at the nucleus is uncertain; if it does exist, then the mass is estimated as {{Val|8.5e8|1.9|ul=solar mass}},<ref name=Graham2008/> or around 850&nbsp;million times the mass of the Sun.


Radio observations at the ] hydrogen line show the gaseous disk of M63 extends outward to a radius of {{Convert|40|kpc|ly|abbr=off|order=flip}}, well past the bright optical disk. This gas shows a symmetrical form that is warped in a pronounced manner, starting at a radius of {{Convert|10|kpc|ly|order=flip|abbr=off}}. The form suggests a ] halo that is offset with respect to the inner region. The reason for the warp is unclear, but the position angle points toward the smaller companion galaxy, UGC 8313.<ref name=Battaglia2006/> Radio observations at the ] hydrogen line show the gaseous disk of M63 extends outward to a radius of {{Convert|40|kpc|ly|abbr=off|order=flip}}, well past the bright optical disk. This gas shows a symmetrical form that is warped in a pronounced manner, starting at a radius of {{Convert|10|kpc|ly|order=flip|abbr=off}}. The form suggests a ] halo that is offset with respect to the inner region. The reason for the warp is unclear, but the position angle points toward the smaller companion galaxy, UGC 8313.<ref name=Battaglia2006/>


The distance to M63, based upon the luminosity-distance measurement is {{Convert|8.99|Mpc|ly|order=flip|abbr=off}}.<ref name=Tully2016/> The ] relative to the ] yields an estimate of {{Convert|4.65|Mpc|ly|order=flip|abbr=off}}.<ref name=Ann2015/> Estimates based on the ] range over {{Convert|5.0|–|10.3|Mpc|ly|abbr=off|order=flip}}. The ] technique gives a distance of {{Convert|8.87|±|0.29|Mpc|ly|order=flip|abbr=off}}.<ref name=McQuinn2017/> M63 is part of the ], a group of galaxies that also includes ] (the 'Whirlpool Galaxy').<ref name=Tikhonov2009/> The distance to M63, based upon the luminosity-distance measurement is {{Convert|8.99|Mpc|ly|order=flip|abbr=off}}.<ref name=Tully2016/> The ] relative to the ] yields an estimate of {{Convert|4.65|Mpc|ly|order=flip|abbr=off}}.<ref name=Ann2015/> Estimates based on the ] range over {{Convert|5.0|–|10.3|Mpc|ly|abbr=off|order=flip}}. The ] technique gives a distance of {{Convert|8.87|±|0.29|Mpc|ly|order=flip|abbr=off}}.<ref name=McQuinn2017/> M63 is part of the ], a group of galaxies that also includes ] (the 'Whirlpool Galaxy').<ref name=Tikhonov2009/>


In 1971, a supernova with a magnitude of 11.8 appeared in one of the arms of M63. It was discovered May 24, 1971 and reached peak light around May 26.<ref name=Barbon1973/> The spectrum of {{nowrap|SN 1971 I}} is consistent with a supernova of ]. However, the spectroscopic behavior appeared anomalous.<ref name=Deming1973/> One ] has been observed in M63: {{nowrap|SN 1971I}} (], mag. 11.8) was discovered by Glenn Jolly on 24 May 1971, and was discovered independently by Roger Clark on 29 May 1971.<ref name=Deming1973 /><ref>{{cite web | website=Transient Name Server | title=SN{{nbsp}}1971I | url=https://www.wis-tns.org/object/1971I | publisher = ] | access-date=2 December 2024}}</ref> It reached peak light around 26 May.<ref name=Barbon1973/> While the spectrum was consistent with a supernova of type I, the spectroscopic behavior appeared anomalous.<ref name=Deming1973/>


==Gallery== ==Gallery==
<gallery widths="220px" heights="220px"> <gallery widths="220px" heights="220px">
File:Messier 63 GALEX WikiSky.jpg|M63 from ] Sky Survey, Credit ] / ] File:Messier 63 GALEX WikiSky.jpg|M63 imaged in ] light by the ] satellite. The UV light is produced primarily by young, massive stars, so the UV-bright areas are regions where stars are currently forming.<ref name="Bai"/> Credit ] / ]

File:M63 3.6 8.0 24 microns spitzer.png|Messier 63 seen in infrared by the ].
File:M63 3.6 8.0 24 microns spitzer.png|Messier 63 seen in the ] by the ]. The infrared radiation traces the dust within the spiral arms, which does not radiate visible light. A small dust ring can be seen just outside of the galaxy's center.<ref name="spitzer">{{cite web |last1=spitzer |title=Spitzer's Sunflower |url=https://www.spitzer.caltech.edu/image/sig11-002-spitzers-sunflower |website=Spitzer Space Telescope |publisher=JPL-Caltech |access-date=21 October 2021}}</ref>
⚫ File:A galactic sunflower.jpg|"A galactic sunflower"
File:Sunflower_galaxy.png|Sunflower Galaxy (M63) as photographed by the ]. Unrelated objects have been edited out.
</gallery> </gallery>


==References== ==See also==
* ]


==References==
{{reflist|refs= {{reflist|refs=


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| volume=447 | issue=1 | pages=49–62 | date=February 2006 | volume=447 | issue=1 | pages=49–62 | date=February 2006
| doi=10.1051/0004-6361:20053210 | bibcode=2006A&A...447...49B | doi=10.1051/0004-6361:20053210 | bibcode=2006A&A...447...49B
| arxiv=astro-ph/0509382 | postscript=. }}</ref> | arxiv=astro-ph/0509382 | s2cid=119353199 | postscript=. }}</ref>




<ref name=McQuinn2017>{{citation <ref name=McQuinn2017>{{citation
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| volume=154 | issue=2 | id=51 | pages=13 | date=August 2017 | volume=154 | issue=2 | id=51 | pages=13 | date=August 2017
| doi=10.3847/1538-3881/aa7aad | bibcode=2017AJ....154...51M | doi=10.3847/1538-3881/aa7aad | bibcode=2017AJ....154...51M
| arxiv=1706.06586 | s2cid=119449804 | postscript=. }}</ref> | arxiv=1706.06586 | s2cid=119449804 | postscript=. | doi-access=free }}</ref>

<ref name="Bai">{{cite journal |last1=Bai |first1=Yu |last2=Zou |first2=Hu |last3=Liu |first3=JiFeng |last4=Wang |first4=Song |title=An Updated Ultraviolet Catalog of Galex Nearby Galaxies |journal=The Astrophysical Journal Supplement Series |date=September 2015 |volume=220 |issue=1 |page=6 |doi=10.1088/0067-0049/220/1/6 |url=ttpsh://doi.org/10.1088/0067-0049/220/1/6 |access-date=21 October 2021|arxiv=1508.07071 |bibcode=2015ApJS..220....6B |s2cid=118402184 }}</ref>


<ref name=Garfinkle1997>{{citation <ref name=Garfinkle1997>{{citation
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<ref name=Ann2015>{{citation <ref name=Ann2015>{{citation
| title=A Catalog of Visually Classified Galaxies in the Local (z ∼ 0.01) Universe | title=A Catalog of Visually Classified Galaxies in the Local (z ~ 0.01) Universe
| last1=Ann | first1=H. B. | last2=Seo | first2=Mira | last1=Ann | first1=H. B. | last2=Seo | first2=Mira
| last3=Ha | first3=D. K. | display-authors=1 | last3=Ha | first3=D. K. | display-authors=1
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<ref name=NASA>{{citation <ref name=NASA>{{citation
| title=Hubble Sees a Galactic Sunflower | title=Hubble Sees a Galactic Sunflower
| publisher=NASA | date=September 11, 2015 | publisher=NASA | date=11 September 2015
| editor1-first=Ashley | editor1-last=Morrow | editor1-first=Ashley | editor1-last=Morrow
| url=https://www.nasa.gov/image-feature/goddard/hubbles-galactic-sunflower | url=https://www.nasa.gov/image-feature/goddard/hubbles-galactic-sunflower
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| volume=152 | issue=2 | id=50 | pages=21 | date=August 2016 | volume=152 | issue=2 | id=50 | pages=21 | date=August 2016
| doi=10.3847/0004-6256/152/2/50 | bibcode=2016AJ....152...50T | doi=10.3847/0004-6256/152/2/50 | bibcode=2016AJ....152...50T
| arxiv=1605.01765 | postscript=. }}</ref> | arxiv=1605.01765 | s2cid=250737862 | postscript=. | doi-access=free }}</ref>


<ref name=Masegosa2011>{{citation <ref name=Masegosa2011>{{citation
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{{Sky|13|15|49.3|+|42|01|45|37000000}} {{Sky|13|15|49.3|+|42|01|45|37000000}}
{{Portal bar|Astronomy|Stars|Outer space}}
{{Messier objects}} {{Messier objects}}
{{Ngc55}}{{Stars of Canes Venatici}} {{Ngc55}}{{Stars of Canes Venatici}}
{{DEFAULTSORT:Messier 63}}
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Latest revision as of 16:31, 3 December 2024

Spiral galaxy in the constellation Canes Venatici
Messier 63
Image taken by Hubble Space Telescope, on 16 November 2001 at 450 and 814 nm
Observation data (J2000 epoch)
ConstellationCanes Venatici
Right ascension13 15 49.27385
Declination+42° 01′ 45.7261″
Redshift484 km/s
Distance29.3 Mly (8.99 Mpc)
Group or clusterM51 Group
Apparent magnitude (V)9.3
Characteristics
TypeSAbc
Apparent size (V)12.6′ × 7.2′
Other designations
M63, NGC 5055, PGC 46153, UGC 8334
Center of the galaxy

Messier 63 or M63, also known as NGC 5055 or the seldom-used Sunflower Galaxy, is a spiral galaxy in the northern constellation of Canes Venatici with approximately 400 billion stars. M63 was first discovered by the French astronomer Pierre Méchain, then later verified by his colleague Charles Messier on 14 June 1779. The galaxy became listed as object 63 in the Messier Catalogue. In the mid-19th century, Anglo-Irish astronomer Lord Rosse identified spiral structures within the galaxy, making this one of the first galaxies in which such structure was identified.

The shape or morphology of this galaxy has a classification of SAbc, indicating a spiral form with no central bar feature (SA) and moderate to loosely wound arms (bc). There is a general lack of large-scale continuous spiral structure in visible light, so it is considered a flocculent galaxy. However, when observed in the near infrared, a symmetric, two-arm structure is seen. Each arm wraps 150° around the galaxy and extends out to 13,000 light-years (4,000 parsecs) from the nucleus.

M63 is a weakly active galaxy with a LINER nucleus – short for 'low-ionization nuclear emission-line region'. This displays as an unresolved source at the galactic nucleus that is cloaked in a diffuse emission. The latter is extended along a position angle of 110° relative to the north celestial pole, and both soft X-rays and hydrogen (H-alpha) emission can be observed coming from along nearly the same direction. The existence of a supermassive black hole (SMBH) at the nucleus is uncertain; if it does exist, then the mass is estimated as (8.5±1.9)×10 M☉, or around 850 million times the mass of the Sun.

Radio observations at the 21-cm hydrogen line show the gaseous disk of M63 extends outward to a radius of 130,000 light-years (40 kiloparsecs), well past the bright optical disk. This gas shows a symmetrical form that is warped in a pronounced manner, starting at a radius of 33,000 light-years (10 kiloparsecs). The form suggests a dark matter halo that is offset with respect to the inner region. The reason for the warp is unclear, but the position angle points toward the smaller companion galaxy, UGC 8313.

The distance to M63, based upon the luminosity-distance measurement is 29,300,000 light-years (8.99 megaparsecs). The radial velocity relative to the Local Group yields an estimate of 15,200,000 light-years (4.65 megaparsecs). Estimates based on the Tully–Fisher relation range over 16,000,000–34,000,000 light-years (5.0–10.3 megaparsecs). The tip of the red-giant branch technique gives a distance of 28,930,000 ± 950,000 light-years (8.87 ± 0.29 megaparsecs). M63 is part of the M51 Group, a group of galaxies that also includes M51 (the 'Whirlpool Galaxy').

One supernova has been observed in M63: SN 1971I (type Ia, mag. 11.8) was discovered by Glenn Jolly on 24 May 1971, and was discovered independently by Roger Clark on 29 May 1971. It reached peak light around 26 May. While the spectrum was consistent with a supernova of type I, the spectroscopic behavior appeared anomalous.

Gallery

  • M63 imaged in UV light by the GALEX satellite. The UV light is produced primarily by young, massive stars, so the UV-bright areas are regions where stars are currently forming. Credit NASA / WikiSky M63 imaged in UV light by the GALEX satellite. The UV light is produced primarily by young, massive stars, so the UV-bright areas are regions where stars are currently forming. Credit NASA / WikiSky
  • Messier 63 seen in the infrared by the Spitzer Space Telescope. The infrared radiation traces the dust within the spiral arms, which does not radiate visible light. A small dust ring can be seen just outside of the galaxy's center. Messier 63 seen in the infrared by the Spitzer Space Telescope. The infrared radiation traces the dust within the spiral arms, which does not radiate visible light. A small dust ring can be seen just outside of the galaxy's center.

See also

References

  1. Morrow, Ashley, ed. (11 September 2015), Hubble Sees a Galactic Sunflower, NASA, retrieved 2018-11-30.
  2. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.
  3. ^ "NASA/IPAC Extragalactic Database". Results for NGC 5055. Retrieved 2006-10-10.
  4. ^ Tully, R. Brent; et al. (August 2016), "Cosmicflows-3", The Astronomical Journal, 152 (2): 21, arXiv:1605.01765, Bibcode:2016AJ....152...50T, doi:10.3847/0004-6256/152/2/50, S2CID 250737862, 50.
  5. ^ Ann, H. B.; et al. (2015), "A Catalog of Visually Classified Galaxies in the Local (z ~ 0.01) Universe", The Astrophysical Journal Supplement Series, 217 (2): 27–49, arXiv:1502.03545, Bibcode:2015ApJS..217...27A, doi:10.1088/0067-0049/217/2/27, S2CID 119253507.
  6. ^ Garfinkle, Robert A. (1997), Star-Hopping: Your Visa to Viewing the Universe, Cambridge University Press, p. 258, ISBN 978-0521598897.
  7. "Messier 63 - M63 - The Sunflower Galaxy (Spiral Galaxy) | freestarcharts.com". freestarcharts.com. Retrieved 2020-06-23.
  8. Jones, K. G. (1991), Messier's Nebulae and Star Clusters (2nd ed.), Cambridge: Cambridge University Press, ISBN 978-0-521-37079-0.
  9. Thornley, Michele D. (September 1996), "Uncovering Spiral Structure in Flocculent Galaxies", Astrophysical Journal Letters, 469: L45, arXiv:astro-ph/9607041, Bibcode:1996ApJ...469L..45T, doi:10.1086/310250, S2CID 9003459.
  10. Masegosa, J.; et al. (March 2011), "The nature of nuclear Hα emission in LINERs", Astronomy & Astrophysics, 527: 28, arXiv:1011.0865, Bibcode:2011A&A...527A..23M, doi:10.1051/0004-6361/201015047, S2CID 116978210, A23.
  11. Graham, Alister W. (November 2008), "Populating the Galaxy Velocity Dispersion - Supermassive Black Hole Mass Diagram: A Catalogue of (Mbh, σ) Values", Publications of the Astronomical Society of Australia, 25 (4): 167–175, arXiv:0807.2549, Bibcode:2008PASA...25..167G, doi:10.1071/AS08013, S2CID 89905.
  12. Battaglia, G.; et al. (February 2006), "ion{H}{i} study of the warped spiral galaxy NGC 5055: a disk/dark matter halo offset?", Astronomy and Astrophysics, 447 (1): 49–62, arXiv:astro-ph/0509382, Bibcode:2006A&A...447...49B, doi:10.1051/0004-6361:20053210, S2CID 119353199.
  13. McQuinn, Kristen. B. W.; et al. (August 2017), "Accurate Distances to Important Spiral Galaxies: M63, M74, NGC 1291, NGC 4559, NGC 4625, and NGC 5398", The Astronomical Journal, 154 (2): 13, arXiv:1706.06586, Bibcode:2017AJ....154...51M, doi:10.3847/1538-3881/aa7aad, S2CID 119449804, 51.
  14. Tikhonov, N. A.; et al. (September 2009), "Stellar content of the interacting galaxies of the M51 system", Astronomy Letters, 35 (9): 599–608, Bibcode:2009AstL...35..599T, doi:10.1134/S1063773709090035, S2CID 123044805.
  15. ^ Deming, Drake; et al. (June 1973), "The Light Curve of Supernova 1971 I", Publications of the Astronomical Society of the Pacific, 85 (505): 321, Bibcode:1973PASP...85..321D, doi:10.1086/129462
  16. "SN 1971I". Transient Name Server. IAU. Retrieved 2 December 2024.
  17. Barbon, R.; et al. (1973), "Observations of five supernovae 1970-71", Memorie della Società Astronomia Italiana, 44: 65, Bibcode:1973MmSAI..44...65B.
  18. Bai, Yu; Zou, Hu; Liu, JiFeng; Wang, Song (September 2015). . The Astrophysical Journal Supplement Series. 220 (1): 6. arXiv:1508.07071. Bibcode:2015ApJS..220....6B. doi:10.1088/0067-0049/220/1/6. S2CID 118402184. Retrieved 21 October 2021.
  19. spitzer. "Spitzer's Sunflower". Spitzer Space Telescope. JPL-Caltech. Retrieved 21 October 2021.

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