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| names = [[Uppsala General Catalogue|UGC]] 6439, [[Morphological Catalogue of Galaxies|MCG]] +07-24-004, [[Principal Galaxies Catalogue|PGC]] 35164<ref name="ned" />
| names = [[Uppsala General Catalogue|UGC]] 6439, [[Morphological Catalogue of Galaxies|MCG]] +07-24-004, [[Principal Galaxies Catalogue|PGC]] 35164<ref name="ned" />
}}
}}
'''NGC 3675''' is an [[spiral galaxy]] located in the constellation [[Ursa Major]]. It is located at a distance of circa 50 million [[light year]]s from Earth, which, given its apparent dimensions, means that NGC 3675 is about 100,000 light years across. It was discovered by [[William Herschel]] in 1788.
'''NGC 3675''' is a [[spiral galaxy]] located in the constellation [[Ursa Major]]. It is located at a distance of circa 50 million [[light year]]s from Earth, which, given its apparent dimensions, means that NGC 3675 is about 100,000 light years across. It was discovered by [[William Herschel]] in 1788.


It hosts a [[low-ionization nuclear emission-line region]] (LINER).<ref>{{cite journal|last1=McKernan|first1=B.|last2=Ford|first2=K. E. S.|last3=Reynolds|first3=C. S.|title=Black hole mass, host galaxy classification and AGN activity|journal=Monthly Notices of the Royal Astronomical Society|date=20 July 2010|volume=407|issue=4|pages=2399–2410|doi=10.1111/j.1365-2966.2010.17068.x}}</ref> In the nucleus there is a [[supermassive black hole]] with estimated mass 10-39 millions [[solar mass|M⊙]], based on the intrinsic velocity dispersion as measured by the [[Hubble Space Telescope]].<ref>{{cite journal|last1=Beifiori|first1=A.|last2=Sarzi|first2=M.|last3=Corsini|first3=E. M.|last4=Bontà|first4=E. Dalla|last5=Pizzella|first5=A.|last6=Coccato|first6=L.|last7=Bertola|first7=F.|title=Upper Limits on the Masses of 105 Supermassive Black Holes from Hubble Space Telescope/Space Telescope Imaging Spectrograph Archival Data|journal=The Astrophysical Journal|date=10 February 2009|volume=692|issue=1|pages=856–868|doi=10.1088/0004-637X/692/1/856|accessdate=17 July 2017}}</ref> Although the galaxy was reported to have a strong [[barred spiral galaxy|bar]] visible in [[infrared]] images, it has not been any indication of bar in further observations.<ref>{{cite journal|last1=Möllenhoff|first1=C.|last2=Heidt|first2=J.|title=Surface photometry of spiral galaxies in NIR:Structural parameters of disks and bulges|journal=Astronomy & Astrophysics|date=15 March 2001|volume=368|issue=1|pages=16–37|doi=10.1051/0004-6361:20000335|url=https://www.aanda.org/articles/aa/full/2001/10/aa10227/aa10227.html}}</ref> Its [[galaxy disk|spiral disk]] in of type III and there is a dust structure which is more prominent to the east.<ref>{{cite journal|last1=Gutiérrez|first1=Leonel|last2=Erwin|first2=Peter|last3=Aladro|first3=Rebeca|last4=Beckman|first4=John E.|title=The Outer Disks of Early-type Galaxies. II. Surface-brightness Profiles of Unbarred Galaxies and Trends with Hubble Type|journal=The Astronomical Journal|date=1 November 2011|volume=142|issue=5|pages=145|doi=10.1088/0004-6256/142/5/145}}</ref> The galaxy features two ring structures, with diametre 1.62 and 2.42 arcminutes.<ref>{{cite journal|last1=Comerón|first1=S.|last2=Salo|first2=H.|last3=Laurikainen|first3=E.|last4=Knapen|first4=J. H.|last5=Buta|first5=R. J.|last6=Herrera-Endoqui|first6=M.|last7=Laine|first7=J.|last8=Holwerda|first8=B. W.|last9=Sheth|first9=K.|last10=Regan|first10=M. W.|last11=Hinz|first11=J. L.|last12=Muñoz-Mateos|first12=J. C.|last13=Gil de Paz|first13=A.|last14=Menéndez-Delmestre|first14=K.|last15=Seibert|first15=M.|last16=Mizusawa|first16=T.|last17=Kim|first17=T.|last18=Erroz-Ferrer|first18=S.|last19=Gadotti|first19=D. A.|last20=Athanassoula|first20=E.|last21=Bosma|first21=A.|last22=Ho|first22=L. C.|title=ARRAKIS: atlas of resonance rings as known in the S4G|journal=Astronomy & Astrophysics|date=19 February 2014|volume=562|pages=A121|doi=10.1051/0004-6361/201321633}}</ref> The [[spiral arm]]s are tightly wound and form an inner pseudoring and they continue for one revolution outside the ring. The outer arms are very patchy and filamentary.<ref>{{cite journal|last1=Eskridge|first1=Paul B.|last2=Frogel|first2=Jay A.|last3=Pogge|first3=Richard W.|last4=Quillen|first4=Alice C.|last5=Berlind|first5=Andreas A.|last6=Davies|first6=Roger L.|last7=DePoy|first7=D. L.|last8=Gilbert|first8=Karoline M.|last9=Houdashelt|first9=Mark L.|last10=Kuchinski|first10=Leslie E.|last11=Ramirez|first11=Solange V.|last12=Sellgren|first12=K.|last13=Stutz|first13=Amelia|last14=Terndrup|first14=Donald M.|last15=Tiede|first15=Glenn P.|title=Near‐Infrared and Optical Morphology of Spiral Galaxies|journal=The Astrophysical Journal Supplement Series|date=November 2002|volume=143|issue=1|pages=73–111|doi=10.1086/342340}}</ref>
It hosts a [[low-ionization nuclear emission-line region]] (LINER).<ref>{{cite journal|last1=McKernan|first1=B.|last2=Ford|first2=K. E. S.|last3=Reynolds|first3=C. S.|title=Black hole mass, host galaxy classification and AGN activity|journal=Monthly Notices of the Royal Astronomical Society|date=20 July 2010|volume=407|issue=4|pages=2399–2410|doi=10.1111/j.1365-2966.2010.17068.x}}</ref> In the nucleus there is a [[supermassive black hole]] with estimated mass 10-39 millions [[solar mass|M⊙]], based on the intrinsic velocity dispersion as measured by the [[Hubble Space Telescope]].<ref>{{cite journal|last1=Beifiori|first1=A.|last2=Sarzi|first2=M.|last3=Corsini|first3=E. M.|last4=Bontà|first4=E. Dalla|last5=Pizzella|first5=A.|last6=Coccato|first6=L.|last7=Bertola|first7=F.|title=Upper Limits on the Masses of 105 Supermassive Black Holes from Hubble Space Telescope/Space Telescope Imaging Spectrograph Archival Data|journal=The Astrophysical Journal|date=10 February 2009|volume=692|issue=1|pages=856–868|doi=10.1088/0004-637X/692/1/856|accessdate=17 July 2017}}</ref> Although the galaxy was reported to have a strong [[barred spiral galaxy|bar]] visible in [[infrared]] images, it has not been any indication of bar in further observations.<ref>{{cite journal|last1=Möllenhoff|first1=C.|last2=Heidt|first2=J.|title=Surface photometry of spiral galaxies in NIR:Structural parameters of disks and bulges|journal=Astronomy & Astrophysics|date=15 March 2001|volume=368|issue=1|pages=16–37|doi=10.1051/0004-6361:20000335|url=https://www.aanda.org/articles/aa/full/2001/10/aa10227/aa10227.html}}</ref> Its [[galaxy disk|spiral disk]] in of type III and there is a dust structure which is more prominent to the east.<ref>{{cite journal|last1=Gutiérrez|first1=Leonel|last2=Erwin|first2=Peter|last3=Aladro|first3=Rebeca|last4=Beckman|first4=John E.|title=The Outer Disks of Early-type Galaxies. II. Surface-brightness Profiles of Unbarred Galaxies and Trends with Hubble Type|journal=The Astronomical Journal|date=1 November 2011|volume=142|issue=5|pages=145|doi=10.1088/0004-6256/142/5/145}}</ref> The galaxy features two ring structures, with diametre 1.62 and 2.42 arcminutes.<ref>{{cite journal|last1=Comerón|first1=S.|last2=Salo|first2=H.|last3=Laurikainen|first3=E.|last4=Knapen|first4=J. H.|last5=Buta|first5=R. J.|last6=Herrera-Endoqui|first6=M.|last7=Laine|first7=J.|last8=Holwerda|first8=B. W.|last9=Sheth|first9=K.|last10=Regan|first10=M. W.|last11=Hinz|first11=J. L.|last12=Muñoz-Mateos|first12=J. C.|last13=Gil de Paz|first13=A.|last14=Menéndez-Delmestre|first14=K.|last15=Seibert|first15=M.|last16=Mizusawa|first16=T.|last17=Kim|first17=T.|last18=Erroz-Ferrer|first18=S.|last19=Gadotti|first19=D. A.|last20=Athanassoula|first20=E.|last21=Bosma|first21=A.|last22=Ho|first22=L. C.|title=ARRAKIS: atlas of resonance rings as known in the S4G|journal=Astronomy & Astrophysics|date=19 February 2014|volume=562|pages=A121|doi=10.1051/0004-6361/201321633}}</ref> The [[spiral arm]]s are tightly wound and form an inner pseudoring and they continue for one revolution outside the ring. The outer arms are very patchy and filamentary.<ref>{{cite journal|last1=Eskridge|first1=Paul B.|last2=Frogel|first2=Jay A.|last3=Pogge|first3=Richard W.|last4=Quillen|first4=Alice C.|last5=Berlind|first5=Andreas A.|last6=Davies|first6=Roger L.|last7=DePoy|first7=D. L.|last8=Gilbert|first8=Karoline M.|last9=Houdashelt|first9=Mark L.|last10=Kuchinski|first10=Leslie E.|last11=Ramirez|first11=Solange V.|last12=Sellgren|first12=K.|last13=Stutz|first13=Amelia|last14=Terndrup|first14=Donald M.|last15=Tiede|first15=Glenn P.|title=Near‐Infrared and Optical Morphology of Spiral Galaxies|journal=The Astrophysical Journal Supplement Series|date=November 2002|volume=143|issue=1|pages=73–111|doi=10.1086/342340}}</ref>

Revision as of 16:10, 1 August 2017

NGC 3675
NGC 3675 in Schulman telescope
Observation data (J2000 epoch)
ConstellationUrsa Major
Right ascension11h 26m 08.6s[1]
Declination43° 35′ 09″[1]
Redshift770 ± 1 km/s[1]
Distance53 ± 10 Mly (16.2 ± 3.0 Mpc)[1]
Apparent magnitude (V)10.0
Characteristics
TypeSA(s)b [1]
Apparent size (V)5′.9 × 3′.1[1]
Other designations
UGC 6439, MCG +07-24-004, PGC 35164[1]

NGC 3675 is a spiral galaxy located in the constellation Ursa Major. It is located at a distance of circa 50 million light years from Earth, which, given its apparent dimensions, means that NGC 3675 is about 100,000 light years across. It was discovered by William Herschel in 1788.

It hosts a low-ionization nuclear emission-line region (LINER).[2] In the nucleus there is a supermassive black hole with estimated mass 10-39 millions M⊙, based on the intrinsic velocity dispersion as measured by the Hubble Space Telescope.[3] Although the galaxy was reported to have a strong bar visible in infrared images, it has not been any indication of bar in further observations.[4] Its spiral disk in of type III and there is a dust structure which is more prominent to the east.[5] The galaxy features two ring structures, with diametre 1.62 and 2.42 arcminutes.[6] The spiral arms are tightly wound and form an inner pseudoring and they continue for one revolution outside the ring. The outer arms are very patchy and filamentary.[7]

One supernova has been observed in NGC 3675, SN 1984R. NGC 3675 is belongs to the Ursa Major Cluster, part of the Virgo Supercluster.[8]

References

  1. ^ a b c d e f g "NASA/IPAC Extragalactic Database". Results for NGC 3675. Retrieved 2016-01-18.
  2. ^ McKernan, B.; Ford, K. E. S.; Reynolds, C. S. (20 July 2010). "Black hole mass, host galaxy classification and AGN activity". Monthly Notices of the Royal Astronomical Society. 407 (4): 2399–2410. doi:10.1111/j.1365-2966.2010.17068.x.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  3. ^ Beifiori, A.; Sarzi, M.; Corsini, E. M.; Bontà, E. Dalla; Pizzella, A.; Coccato, L.; Bertola, F. (10 February 2009). "Upper Limits on the Masses of 105 Supermassive Black Holes from Hubble Space Telescope/Space Telescope Imaging Spectrograph Archival Data". The Astrophysical Journal. 692 (1): 856–868. doi:10.1088/0004-637X/692/1/856. {{cite journal}}: |access-date= requires |url= (help)
  4. ^ Möllenhoff, C.; Heidt, J. (15 March 2001). "Surface photometry of spiral galaxies in NIR:Structural parameters of disks and bulges". Astronomy & Astrophysics. 368 (1): 16–37. doi:10.1051/0004-6361:20000335.
  5. ^ Gutiérrez, Leonel; Erwin, Peter; Aladro, Rebeca; Beckman, John E. (1 November 2011). "The Outer Disks of Early-type Galaxies. II. Surface-brightness Profiles of Unbarred Galaxies and Trends with Hubble Type". The Astronomical Journal. 142 (5): 145. doi:10.1088/0004-6256/142/5/145.
  6. ^ Comerón, S.; Salo, H.; Laurikainen, E.; Knapen, J. H.; Buta, R. J.; Herrera-Endoqui, M.; Laine, J.; Holwerda, B. W.; Sheth, K.; Regan, M. W.; Hinz, J. L.; Muñoz-Mateos, J. C.; Gil de Paz, A.; Menéndez-Delmestre, K.; Seibert, M.; Mizusawa, T.; Kim, T.; Erroz-Ferrer, S.; Gadotti, D. A.; Athanassoula, E.; Bosma, A.; Ho, L. C. (19 February 2014). "ARRAKIS: atlas of resonance rings as known in the S4G". Astronomy & Astrophysics. 562: A121. doi:10.1051/0004-6361/201321633.
  7. ^ Eskridge, Paul B.; Frogel, Jay A.; Pogge, Richard W.; Quillen, Alice C.; Berlind, Andreas A.; Davies, Roger L.; DePoy, D. L.; Gilbert, Karoline M.; Houdashelt, Mark L.; Kuchinski, Leslie E.; Ramirez, Solange V.; Sellgren, K.; Stutz, Amelia; Terndrup, Donald M.; Tiede, Glenn P. (November 2002). "Near‐Infrared and Optical Morphology of Spiral Galaxies". The Astrophysical Journal Supplement Series. 143 (1): 73–111. doi:10.1086/342340.
  8. ^ "The Ursa Major Groups". www.atlasoftheuniverse.com.
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