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Coordinates: Sky map 11h 11m 31.0s, +55° 40′ 27″
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{{short description|Barred spiral galaxy in the constellation Ursa Major}}
{{Short description|Galaxy in the constellation Ursa Major}}
{{Infobox Galaxy
{{Infobox Galaxy
| name=[[Messier object|Messier]] 108
| name=Messier 108
| image=Messier108 - SDSS DR 14 (panorama).jpg
| image=Messier108 - SDSS DR 14 (panorama).jpg
| image_size=250px
| caption=A [[Sloan Digital Sky Survey]] image of M108.
| caption=A [[Sloan Digital Sky Survey]] image of M108.
| credit=
| credit=
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| constellation name=[[Ursa Major]]<ref name="sinnott1988">{{cite book | editor=R. W. Sinnott | title=The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer | date=1988 | publisher=[[Sky Publishing Corporation]]/[[Cambridge University Press]] | isbn=978-0-933346-51-2}}</ref>
| constellation name=[[Ursa Major]]<ref name="sinnott1988">{{cite book | editor=R. W. Sinnott | title=The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer | date=1988 | publisher=[[Sky Publishing Corporation]]/[[Cambridge University Press]] | isbn=978-0-933346-51-2}}</ref>
| type=SB(s)cd<ref name="aaa54" />
| type=SB(s)cd<ref name="aaa54" />
| ra={{RA|11|11|31.0}}<ref name="ned">{{cite web | title=NASA/IPAC Extragalactic Database | work=Results for NGC 3556 | url=http://nedwww.ipac.caltech.edu/ | access-date=2007-06-21 }}</ref>
| ra={{RA|11|11|31.0}}<ref name="ned">{{cite web | title=NASA/IPAC Extragalactic Database | work=Results for NGC 3556 | url=http://ned.ipac.caltech.edu/byname?objname=NGC+3556 | access-date=30 March 2022 }}</ref>
| dec={{DEC|+55|40|27}}<ref name="ned" />
| dec={{DEC|+55|40|27}}<ref name="ned" />
| z=699 ± 9 km/[[second|s]]<ref name="ned" />
| z=696.1 ± 0.6 km/[[second|s]]<ref name="ned" />
| dist_ly=8.8<ref name="Sorce2014">{{cite journal|author=Sorce, J. G.|title=From Spitzer Galaxy photometry to Tully–Fisher distances|date=2014|display-authors=etal|doi=10.1093/mnras/stu1450|url=https://academic.oup.com/mnras/article/444/1/527/1017867|journal=[[Monthly Notices of the Royal Astronomical Society]]|volume=444|issue=1|pages=527–541}}</ref>
| dist_ly=14.1 Mpc (46 Mly) <ref name="Sorce2014">{{cite journal|author=Sorce, J. G.|title=From Spitzer Galaxy photometry to Tully–Fisher distances|date=2014|display-authors=etal|doi=10.1093/mnras/stu1450|url=https://academic.oup.com/mnras/article/444/1/527/1017867|journal=[[Monthly Notices of the Royal Astronomical Society]]|volume=444|issue=1|pages=527–541|doi-access=free|arxiv=1408.0729}}</ref>
| appmag_v=10.0<ref>{{cite web |url=https://messier.seds.org/m/m108.html |title=Messier 108 |access-date=30 April 2022 |website=SEDS Messier Catalog}}</ref>
| appmag_v=10.7<ref name="ned" />
| size_v=8′.7 × 2′.2<ref name="ned" />
| size_v=8′.7 × 2′.2<ref name="ned" />
| names=[[New General Catalogue|NGC]] 3556,<ref name="ned" /> [[Principal Galaxies Catalogue|PGC]] 34030,<ref name="ned" /> [[Uppsala General Catalogue|UGC]] 6225<ref name="ned" />}}
| names=[[New General Catalogue|NGC]] 3556,<ref name="ned" /> [[Principal Galaxies Catalogue|PGC]] 34030,<ref name="ned" /> [[Uppsala General Catalogue|UGC]] 6225<ref name="ned" />}}


'''Messier 108''' (also known as '''NGC 3556''') is a [[barred spiral galaxy]] about 28 million [[light-years]] away from Earth<ref name="Sorce2014" /> in the [[celestial hemisphere|northern]] [[constellation]] [[Ursa Major]]. It was discovered by [[Pierre Méchain]] in 1781 or 1782.<ref name="NSOG">{{cite book | last=Kepple | first=George Robert |author2=Glen W. Sanner | date=1998 | title=The Night Sky Observer's Guide | volume=2 | page=399 | publisher=[[Willmann-Bell]] | isbn=978-0-943396-60-6}}</ref> From the Earth, this galaxy is seen almost edge-on.
'''Messier 108''' (also known as '''NGC 3556''', nicknamed the '''Surfboard Galaxy'''<ref name = guide/>) is a [[barred spiral galaxy]] about 46 million [[light-years]] away from Earth<ref name="Sorce2014" /><ref>{{cite web |title=Messier 108 |url=https://science.nasa.gov/mission/hubble/science/explore-the-night-sky/hubble-messier-catalog/messier-108/ |website=NASA |access-date=17 November 2024}}</ref> in the [[celestial hemisphere|northern]] [[constellation]] [[Ursa Major]]. It was discovered by [[Pierre Méchain]] in 1781 or 1782.<ref name="NSOG">{{cite book | last=Kepple | first=George Robert |author2=Glen W. Sanner | date=1998 | title=The Night Sky Observer's Guide | volume=2 | page=399 | publisher=[[Willmann-Bell]] | isbn=978-0-943396-60-6}}</ref> From the Earth, this galaxy is seen almost edge-on.


This galaxy is an isolated<ref name="wang">{{cite journal | author=Wang, Q. Daniel | date=2003 | title=Chandra Observation of the Edge-on Galaxy NGC 3556 (M 108): Violent Galactic Disk-halo Interaction Revealed | arxiv=astro-ph/0308150|display-authors=etal | doi=10.1086/379010 | volume=598 | issue=2 | journal=The Astrophysical Journal | pages=969–981 | bibcode=2003ApJ...598..969W| s2cid=49349099 }}</ref> member of the [[Ursa Major Cluster]] of galaxies in the [[Virgo supercluster|local supercluster]]. It has a [[Galaxy morphological classification|morphological classification]] of type SBbc in the [[Gérard de Vaucouleurs|de Vaucouleurs]] system, which means it is a barred spiral galaxy with somewhat loosely wound arms. The maximum angular size of the galaxy in the optical band is 11[[arcminute|′]].1 × 4′.6, and it is inclined 75° to the line of sight.<ref name="aaa54">{{cite journal | author=Tully, R. B. | author2=Fisher, J. R. | date=1977 | title=A new method of determining distances to galaxies | journal=[[Astronomy and Astrophysics]] | volume=54 | issue=3 | pages=661–673 | bibcode=1977A&A....54..661T}}</ref>
This galaxy is an isolated<ref name="wang">{{cite journal | author=Wang, Q. Daniel | date=2003 | title=Chandra Observation of the Edge-on Galaxy NGC 3556 (M 108): Violent Galactic Disk-halo Interaction Revealed | arxiv=astro-ph/0308150|display-authors=etal | doi=10.1086/379010 | volume=598 | issue=2 | journal=The Astrophysical Journal | pages=969–981 | bibcode=2003ApJ...598..969W| s2cid=49349099 }}</ref> member of the [[Ursa Major Cluster]] of galaxies in the [[Virgo Supercluster|local supercluster]]. It has a [[Galaxy morphological classification|morphological classification]] of type SBbc in the [[Gérard de Vaucouleurs|de Vaucouleurs]] system, which means it is a barred spiral galaxy with somewhat loosely wound arms. The maximum angular size of the galaxy in the optical band is 11[[arcminute|′]].1 × 4′.6, and it is inclined 75° to the line of sight.<ref name="aaa54">{{cite journal | author=Tully, R. B. | author2=Fisher, J. R. | date=1977 | title=A new method of determining distances to galaxies | journal=[[Astronomy and Astrophysics]] | volume=54 | issue=3 | pages=661–673 | bibcode=1977A&A....54..661T}}</ref>


This galaxy has an estimated mass of 125 billion [[solar mass]]es ({{solar mass}}) and bears about 290 ± 80 [[globular cluster]]s.<ref>{{cite journal | author=Rhode, Katherine L. |display-authors=etal | date=2007 | title=Global Properties of the Globular Cluster Systems of Four Spiral Galaxies | journal=[[Astronomical Journal]] | volume=134 |issue=4 | pages=1403–1418 | doi=10.1086/521397| bibcode=2007AJ....134.1403R|arxiv = 0708.1166 |s2cid=15834447 }}</ref> Examination of the distribution of neutral hydrogen in this galaxy shows discrete shells of expanding gas extending for several kiloparsecs, known as H1 supershells. These may be driven by currents of [[dark matter]], dust and gas contributing to large star formation, having caused supernovae explosions. Alternatively they may result from an infall from the [[intergalactic medium]] or arise from radio jets.<ref>{{cite journal | author=Gopal-Krishna | author2=Irwin, Judith A. | date=2000 | title=Radio jet-blown neutral hydrogen supershells in spiral galaxies? | journal=[[Astronomy and Astrophysics]] | volume=361 | pages=888–894 | bibcode=2000A&A...361..888G|arxiv = astro-ph/0008251 }}</ref>
This galaxy has an estimated mass of 125 billion [[solar mass]]es ({{solar mass}})<ref name="Rhode" />{{refn|group=note|name=first|Using an assumed distance of 7.1 [[Megaparsec]] to Messier 108, based on a 1986 study.[https://ui.adsabs.harvard.edu/abs/1986A%26A...156..157B]}} and bears about 290 ± 80 [[globular cluster]]s.<ref name="Rhode">{{cite journal | author=Rhode, Katherine L. |display-authors=etal | date=2007 | title=Global Properties of the Globular Cluster Systems of Four Spiral Galaxies | journal=[[Astronomical Journal]] | volume=134 |issue=4 | pages=1403–1418 | doi=10.1086/521397| bibcode=2007AJ....134.1403R|arxiv = 0708.1166 |s2cid=15834447 }}</ref> Examination of the distribution of neutral hydrogen in this galaxy shows discrete shells of expanding gas extending for several kiloparsecs, known as H1 supershells. These may be driven by currents of [[dark matter]], dust and gas contributing to large star formation, having caused supernovae explosions. Alternatively they may result from an infall from the [[intergalactic medium]] or arise from radio jets.<ref>{{cite journal | author=Gopal-Krishna | author2=Irwin, Judith A. | date=2000 | title=Radio jet-blown neutral hydrogen supershells in spiral galaxies? | journal=[[Astronomy and Astrophysics]] | volume=361 | pages=888–894 | bibcode=2000A&A...361..888G|arxiv = astro-ph/0008251 }}</ref>


Observations with the [[Chandra X-ray Observatory]] have identified 83 [[X-ray]] sources, including a source at the nucleus. The brightest of these is consistent with an [[intermediate-mass black hole]] accreting matter. The galaxy is also emitting a diffuse soft X-ray radiation within 2.6 [[arcminutes]] of the optical galaxy.<ref name="wang" />{{refn|group=note|name=first|This is the [[angular size]] of the feature as it appears on the sky. The physical size depends on the distance to Messier 108, which is more difficult to measure. At the time of the study that discovered this feature (in 2003),<ref name="wang" /> the accepted distance to Messier 108 was based on a 1997 work,[https://iopscience.iop.org/article/10.1086/313041/meta] which gave a value of 14.1 [[Megaparsec|Megaparsec]] (Mpc). This has been substantially revised down to 8.8 Mpc in a 2014 study.<ref name="Sorce2014" /> At 14.1 Mpc, an angular size of 2.6 arcminutes would correspond to a physical size of <math>2.6/60 \cdot \pi/180 \cdot 14100=10.7</math> kpc, or roughly 10 [[kiloparsec|kiloparsec]] (kpc), which is the value given in the 2003 study. Using the more recent distance estimate, this would be <math>2.6/60 \cdot \pi/180 \cdot 8800=6.7</math> kpc.}} The spectrum of the source at the core is consistent with an [[active galactic nucleus]], but an examination with the [[Spitzer Space Telescope]] showed no indication of activity. The [[supermassive black hole]] at the core has an estimated mass of 24 million solar masses ({{solar mass}}).<ref>{{cite journal | author=Satyapal, S. |display-authors=etal | date=2008 | title=Spitzer Uncovers Active Galactic Nuclei Missed by Optical Surveys in Seven Late-Type Galaxies | journal=[[Astrophysical Journal]] | volume=677 | issue=2 | pages=926–942 | doi=10.1086/529014| bibcode=2008ApJ...677..926S|arxiv = 0801.2759 |s2cid=16050838 }}</ref>
Observations with the [[Chandra X-ray Observatory]] have identified 83 [[X-ray]] sources, including a source at the nucleus. The brightest of these is consistent with an [[intermediate-mass black hole]] accreting matter. The galaxy is also emitting a diffuse soft X-ray radiation within 2.6 [[arcminutes]] of the optical galaxy.<ref name="wang" />{{refn|group=note|name=second|This is the [[angular size]] of the feature as it appears on the sky. The physical size depends on the distance to Messier 108, which is more difficult to measure. At the time of the study that discovered this feature (in 2003),<ref name="wang" /> the accepted distance to Messier 108 was based on a 1988 work,[https://ui.adsabs.harvard.edu/abs/1988cng..book.....T/abstract] which gave a value of 14.1 Megaparsec (Mpc). This has been substantially revised down to 8.8 Mpc in a 2014 study.<ref name="Sorce2014" /> At 14.1 Mpc, an angular size of 2.6 arcminutes would correspond to a physical size of <math>2.6/60 \cdot \pi/180 \cdot 14100=10.7</math> kpc, or roughly 10 [[kiloparsec]] (kpc), which is the value given in the 2003 study. Using the more recent distance estimate, this would be <math>2.6/60 \cdot \pi/180 \cdot 8800=6.7</math> kpc. Compare the list of distance measurements in the NASA/IPAC Extragalactic Database.<ref name="ned" />}} The spectrum of the source at the core is consistent with an [[active galactic nucleus]], but an examination with the [[Spitzer Space Telescope]] showed no indication of activity. The [[supermassive black hole]] at the core has an estimated mass of 24 million solar masses ({{solar mass}}).<ref>{{cite journal | author=Satyapal, S. |display-authors=etal | date=2008 | title=Spitzer Uncovers Active Galactic Nuclei Missed by Optical Surveys in Seven Late-Type Galaxies | journal=[[Astrophysical Journal]] | volume=677 | issue=2 | pages=926–942 | doi=10.1086/529014| bibcode=2008ApJ...677..926S|arxiv = 0801.2759 |s2cid=16050838 }}</ref>


== Supernovae ==
⚫
SPIRITS 16tn, a [[supernova]] in Messier 108, was discovered by the Spitzer Space Telescope in August 2016. The supernova was only visible in [[infrared light]], because it was heavily obscured by [[Dust lane|dust]]. Its [[Extinction (astronomy)|extinction]] was estimated to be 8–9 mag, making it one of the most heavily obscured supernovae ever observed.<ref>{{Cite journal|author=Jencson, Jacob E.|display-authors=etal|date=2018|title=SPIRITS 16tn in NGC 3556: A Heavily Obscured and Low-luminosity Supernova at 8.8 Mpc|journal=[[The Astrophysical Journal]]|volume=863|issue=1|doi=10.3847/1538-4357/aacf8b|url=https://iopscience.iop.org/article/10.3847/1538-4357/aacf8b/pdf}}</ref>
Three [[supernova]]e have been observed in M108:
* SN 1969B (type unknown, mag. 16) was discovered by [[Paul_Wild_(Swiss_astronomer)|Paul Wild]] on 6 February 1969.<ref>{{cite web
| url = http://www.cbat.eps.harvard.edu/IAUCs/IAUC2131.jpg
| title = Circular No. 2131
| last = Marsden
| first = Brian G.
| date = 12 February 1969
| website = Central Bureau for Astronomical Telegrams
| publisher = Smithsonian Astrophysical Observatory
| access-date = 2 December 2024
}}</ref><ref>{{cite web | website=Transient Name Server | title=SN{{nbsp}}1969B | url=https://www.wis-tns.org/object/1969B | publisher = [[International_Astronomical_Union|IAU]] | access-date=2 December 2024}}</ref> It reached a [[apparent magnitude|brightness]] of mag. 13.9.<ref name = guide>{{Cite web|url=https://www.messier-objects.com/messier-108-surfboard-galaxy/|date=26 September 2015|title=Messier 108: Surfboard Galaxy|work=Messier Objects: Guide to the Bright Galaxies, Nebulae and Clusters Listed in the Messier Catalogue}}</ref>
⚫
* SPIRITS 16tn was discovered by the Spitzer Space Telescope in August 2016. The supernova was only visible in [[infrared light]], because it was heavily obscured by [[Dust lane|dust]]. Its [[Extinction (astronomy)|extinction]] was estimated to be 8–9 mag, making it one of the most heavily obscured supernovae ever observed.<ref>{{Cite journal|author=Jencson, Jacob E.|display-authors=etal|date=2018|title=SPIRITS 16tn in NGC 3556: A Heavily Obscured and Low-luminosity Supernova at 8.8 Mpc|journal=[[The Astrophysical Journal]]|volume=863|issue=1|page=20 |doi=10.3847/1538-4357/aacf8b|arxiv=1803.00574 |bibcode=2018ApJ...863...20J |hdl=10150/631110 |s2cid=56398022 |doi-access=free }}</ref>
* SN 2023dbc ([[Type Ib and Ic supernovae|Type Ic]], mag. 17) was discovered by the [[Zwicky Transient Facility]] on 13 March 2023.<ref>{{cite web | website=Transient Name Server | title=SN{{nbsp}}2023dbc | url=https://www.wis-tns.org/object/2023dbc | publisher = [[International_Astronomical_Union|IAU]] | access-date=2 December 2024}}</ref> 2023dbc is likely a stripped-envelope supernova as there is no evidence for hydrogen in these [[Spectrum|spectra]] beyond narrow emission associated with the underlying HII region. It is among the nearest type Ic supernovae discovered to date.<ref name="AstroNote2023-66">{{cite web
|date=2023-03-22
|title=AstroNote 2023-66 : SN 2023dbc as a Highly Extinguished Stripped-Envelope Supernova
|publisher=Transient Name Server
|url=https://www.wis-tns.org/astronotes/astronote/2023-66
|access-date=2023-04-03}}</ref>


[[File:M108map.png|thumb|Location of M108]]
[[File:M108map.png|thumb|Location of M108]]
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{{Portal bar|Astronomy|Stars|Outer space}}
{{Portal bar|Astronomy|Stars|Outer space}}
{{Messier objects}}
{{Messier objects}}
{{Ngc40}}
{{Ngc40}}{{Ursa Major}}

[[Category:Barred spiral galaxies]]
[[Category:Barred spiral galaxies]]
[[Category:Ursa Major (constellation)]]
[[Category:Ursa Major]]
[[Category:Messier objects|108]]
[[Category:Messier objects|108]]
[[Category:NGC objects|Messier 108]]
[[Category:NGC objects|Messier 108]]
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[[Category:Astronomical objects discovered in 1781]]
[[Category:Astronomical objects discovered in 1781]]
[[Category:Discoveries by Pierre Méchain]]
[[Category:Discoveries by Pierre Méchain]]
[[Category:Ursa Major Cluster]]

Latest revision as of 00:28, 3 December 2024

Messier 108
A Sloan Digital Sky Survey image of M108.
Observation data (J2000 epoch)
ConstellationUrsa Major[1]
Right ascension11h 11m 31.0s[2]
Declination+55° 40′ 27″[2]
Redshift696.1 ± 0.6 km/s[2]
Distance14.1 Mpc (46 Mly) [3]
Apparent magnitude (V)10.0[4]
Characteristics
TypeSB(s)cd[5]
Apparent size (V)8′.7 × 2′.2[2]
Other designations
NGC 3556,[2] PGC 34030,[2] UGC 6225[2]

Messier 108 (also known as NGC 3556, nicknamed the Surfboard Galaxy[6]) is a barred spiral galaxy about 46 million light-years away from Earth[3][7] in the northern constellation Ursa Major. It was discovered by Pierre Méchain in 1781 or 1782.[8] From the Earth, this galaxy is seen almost edge-on.

This galaxy is an isolated[9] member of the Ursa Major Cluster of galaxies in the local supercluster. It has a morphological classification of type SBbc in the de Vaucouleurs system, which means it is a barred spiral galaxy with somewhat loosely wound arms. The maximum angular size of the galaxy in the optical band is 11′.1 × 4′.6, and it is inclined 75° to the line of sight.[5]

This galaxy has an estimated mass of 125 billion solar masses (M☉)[10][note 1] and bears about 290 ± 80 globular clusters.[10] Examination of the distribution of neutral hydrogen in this galaxy shows discrete shells of expanding gas extending for several kiloparsecs, known as H1 supershells. These may be driven by currents of dark matter, dust and gas contributing to large star formation, having caused supernovae explosions. Alternatively they may result from an infall from the intergalactic medium or arise from radio jets.[11]

Observations with the Chandra X-ray Observatory have identified 83 X-ray sources, including a source at the nucleus. The brightest of these is consistent with an intermediate-mass black hole accreting matter. The galaxy is also emitting a diffuse soft X-ray radiation within 2.6 arcminutes of the optical galaxy.[9][note 2] The spectrum of the source at the core is consistent with an active galactic nucleus, but an examination with the Spitzer Space Telescope showed no indication of activity. The supermassive black hole at the core has an estimated mass of 24 million solar masses (M☉).[12]

Supernovae

[edit]

Three supernovae have been observed in M108:

  • SN 1969B (type unknown, mag. 16) was discovered by Paul Wild on 6 February 1969.[13][14] It reached a brightness of mag. 13.9.[6]
  • SPIRITS 16tn was discovered by the Spitzer Space Telescope in August 2016. The supernova was only visible in infrared light, because it was heavily obscured by dust. Its extinction was estimated to be 8–9 mag, making it one of the most heavily obscured supernovae ever observed.[15]
  • SN 2023dbc (Type Ic, mag. 17) was discovered by the Zwicky Transient Facility on 13 March 2023.[16] 2023dbc is likely a stripped-envelope supernova as there is no evidence for hydrogen in these spectra beyond narrow emission associated with the underlying HII region. It is among the nearest type Ic supernovae discovered to date.[17]
Location of M108

See also

[edit]

Notes

[edit]
  1. ^ Using an assumed distance of 7.1 Megaparsec to Messier 108, based on a 1986 study.[1]
  2. ^ This is the angular size of the feature as it appears on the sky. The physical size depends on the distance to Messier 108, which is more difficult to measure. At the time of the study that discovered this feature (in 2003),[9] the accepted distance to Messier 108 was based on a 1988 work,[2] which gave a value of 14.1 Megaparsec (Mpc). This has been substantially revised down to 8.8 Mpc in a 2014 study.[3] At 14.1 Mpc, an angular size of 2.6 arcminutes would correspond to a physical size of kpc, or roughly 10 kiloparsec (kpc), which is the value given in the 2003 study. Using the more recent distance estimate, this would be kpc. Compare the list of distance measurements in the NASA/IPAC Extragalactic Database.[2]

References

[edit]
  1. ^ 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 978-0-933346-51-2.
  2. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 3556. Retrieved 30 March 2022.
  3. ^ a b c Sorce, J. G.; et al. (2014). "From Spitzer Galaxy photometry to Tully–Fisher distances". Monthly Notices of the Royal Astronomical Society. 444 (1): 527–541. arXiv:1408.0729. doi:10.1093/mnras/stu1450.
  4. ^ "Messier 108". SEDS Messier Catalog. Retrieved 30 April 2022.
  5. ^ a b Tully, R. B.; Fisher, J. R. (1977). "A new method of determining distances to galaxies". Astronomy and Astrophysics. 54 (3): 661–673. Bibcode:1977A&A....54..661T.
  6. ^ a b "Messier 108: Surfboard Galaxy". Messier Objects: Guide to the Bright Galaxies, Nebulae and Clusters Listed in the Messier Catalogue. 26 September 2015.
  7. ^ "Messier 108". NASA. Retrieved 17 November 2024.
  8. ^ Kepple, George Robert; Glen W. Sanner (1998). The Night Sky Observer's Guide. Vol. 2. Willmann-Bell. p. 399. ISBN 978-0-943396-60-6.
  9. ^ a b c Wang, Q. Daniel; et al. (2003). "Chandra Observation of the Edge-on Galaxy NGC 3556 (M 108): Violent Galactic Disk-halo Interaction Revealed". The Astrophysical Journal. 598 (2): 969–981. arXiv:astro-ph/0308150. Bibcode:2003ApJ...598..969W. doi:10.1086/379010. S2CID 49349099.
  10. ^ a b Rhode, Katherine L.; et al. (2007). "Global Properties of the Globular Cluster Systems of Four Spiral Galaxies". Astronomical Journal. 134 (4): 1403–1418. arXiv:0708.1166. Bibcode:2007AJ....134.1403R. doi:10.1086/521397. S2CID 15834447.
  11. ^ Gopal-Krishna; Irwin, Judith A. (2000). "Radio jet-blown neutral hydrogen supershells in spiral galaxies?". Astronomy and Astrophysics. 361: 888–894. arXiv:astro-ph/0008251. Bibcode:2000A&A...361..888G.
  12. ^ Satyapal, S.; et al. (2008). "Spitzer Uncovers Active Galactic Nuclei Missed by Optical Surveys in Seven Late-Type Galaxies". Astrophysical Journal. 677 (2): 926–942. arXiv:0801.2759. Bibcode:2008ApJ...677..926S. doi:10.1086/529014. S2CID 16050838.
  13. ^ Marsden, Brian G. (12 February 1969). "Circular No. 2131". Central Bureau for Astronomical Telegrams. Smithsonian Astrophysical Observatory. Retrieved 2 December 2024.
  14. ^ "SN 1969B". Transient Name Server. IAU. Retrieved 2 December 2024.
  15. ^ Jencson, Jacob E.; et al. (2018). "SPIRITS 16tn in NGC 3556: A Heavily Obscured and Low-luminosity Supernova at 8.8 Mpc". The Astrophysical Journal. 863 (1): 20. arXiv:1803.00574. Bibcode:2018ApJ...863...20J. doi:10.3847/1538-4357/aacf8b. hdl:10150/631110. S2CID 56398022.
  16. ^ "SN 2023dbc". Transient Name Server. IAU. Retrieved 2 December 2024.
  17. ^ "AstroNote 2023-66 : SN 2023dbc as a Highly Extinguished Stripped-Envelope Supernova". Transient Name Server. 2023-03-22. Retrieved 2023-04-03.
[edit]
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