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{{Short description|Spiral galaxy in the constellation Crater}}
{{Short description|Galaxy in the constellation Crater}}
{{Infobox galaxy
{{Infobox galaxy
| name = [[New General Catalogue|NGC]] 3511
| name = [[New General Catalogue|NGC]] 3511
Line 18: Line 18:
| h_radial_v = 1,109 ± 3 [[kilometer|km]]/[[second|s]]<ref name="ned" />
| h_radial_v = 1,109 ± 3 [[kilometer|km]]/[[second|s]]<ref name="ned" />
| appmag_v = 10.8 <ref name=seds>{{cite web |title=Revised NGC Data for NGC 3511 |url=http://spider.seds.org/ngc/revngcic.cgi?NGC3511 |website=spider.seds.org |access-date=25 November 2018}}</ref>
| appmag_v = 10.8 <ref name=seds>{{cite web |title=Revised NGC Data for NGC 3511 |url=http://spider.seds.org/ngc/revngcic.cgi?NGC3511 |website=spider.seds.org |access-date=25 November 2018}}</ref>
| size_v = 5&prime;.8 × 2&prime;.0
| size_v = 5.8{{prime}} × 2.0{{prime}}
| constellation name = [[Crater (constellation)|Crater]]
| constellation name = [[Crater (constellation)|Crater]]
| notes = Extended [[HIPASS]] source<ref name="ned" />
| notes = Extended [[HIPASS]] source<ref name="ned" />
Line 25: Line 25:
'''NGC 3511''' is an [[intermediate spiral galaxy]] located in the constellation [[Crater (constellation)|Crater]]. It is located at a distance of circa 45 million [[light year]]s from Earth, which, given its apparent dimensions, means that NGC 3511 is about 70,000 light years across. It was discovered by [[William Herschel]] on December 21, 1786.<ref name="Seligman">{{cite web |last1=Seligman |first1=Courtney |title=NGC 3511 |url=https://cseligman.com/text/atlas/ngc35.htm#3511 |website=Celestial Atlas |access-date=19 November 2018}}</ref> It lies two degrees west of [[Beta Crateris]].<ref>{{cite book |last1=Bakich |first1=Michael E. |title=1,001 Celestial Wonders to See Before You Die: The Best Sky Objects for Star Gazers |date=2010 |publisher=Springer Science & Business Media |isbn=9781441917775 |page=79 |url=https://books.google.com/books?id=qEhpS7d5ZdAC&pg=PA79 |language=en}}</ref>
'''NGC 3511''' is an [[intermediate spiral galaxy]] located in the constellation [[Crater (constellation)|Crater]]. It is located at a distance of circa 45 million [[light year]]s from Earth, which, given its apparent dimensions, means that NGC 3511 is about 70,000 light years across. It was discovered by [[William Herschel]] on December 21, 1786.<ref name="Seligman">{{cite web |last1=Seligman |first1=Courtney |title=NGC 3511 |url=https://cseligman.com/text/atlas/ngc35.htm#3511 |website=Celestial Atlas |access-date=19 November 2018}}</ref> It lies two degrees west of [[Beta Crateris]].<ref>{{cite book |last1=Bakich |first1=Michael E. |title=1,001 Celestial Wonders to See Before You Die: The Best Sky Objects for Star Gazers |date=2010 |publisher=Springer Science & Business Media |isbn=9781441917775 |page=79 |url=https://books.google.com/books?id=qEhpS7d5ZdAC&pg=PA79 |language=en}}</ref>


NGC 3511 features two very diffuse, thick, and patchy [[spiral arm]]s that emanate from the bulge, while there are also other spiral arm fragments. Dark dust lanes can be seen across the spiral pattern. The [[bulge (astronomy)|bulge]] appears elliptical and is weak.<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|bibcode=2002ApJS..143...73E |arxiv=astro-ph/0206320 |s2cid=15491635 }}</ref> The galaxy is seen at a high inclination, estimated to be 70°.<ref>{{cite journal |last1=Thean |first1=A. |last2=Pedlar |first2=A. |last3=Kukula |first3=M. J. |last4=Baum |first4=S. A. |last5=O'Dea |first5=C. P. |title=High-resolution radio observations of Seyfert galaxies in the extended 12- m sample - II. The properties of compact radio components |journal=Monthly Notices of the Royal Astronomical Society |date=1 August 2001 |volume=325 |issue=2 |pages=737–760 |doi=10.1046/j.1365-8711.2001.04485.x|bibcode=2001MNRAS.325..737T |arxiv=astro-ph/0103266|s2cid=15097032 }}</ref> In the centre of the galaxy lies a [[supermassive black hole]], whose mass is estimated to be 10<sup>6.46 ± 0.33</sup> (1.3 - 6.2 million) {{solar mass|link=yes}}, based on the pitch angle of the spiral arms.<ref>{{cite journal |last1=Davis |first1=Benjamin L. |last2=Berrier |first2=Joel C. |last3=Johns |first3=Lucas |last4=Shields |first4=Douglas W. |last5=Hartley |first5=Matthew T. |last6=Kennefick |first6=Daniel |last7=Kennefick |first7=Julia |last8=Seigar |first8=Marc S. |last9=Lacy |first9=Claud H. S. |title=The Black Hole Mass Function Derived from Local Spiral Galaxies |journal=The Astrophysical Journal |date=20 June 2014 |volume=789 |issue=2 |pages=124 |doi=10.1088/0004-637X/789/2/124|bibcode=2014ApJ...789..124D |arxiv=1405.5876 |s2cid=119302157 }}</ref> The galaxy had been classified as a type 1 [[Seyfert galaxy]],<ref>{{cite journal |last1=Deo |first1=Rajesh P. |last2=Richards |first2=Gordon T. |last3=Crenshaw |first3=D. M. |last4=Kraemer |first4=S. B. |title=The Mid-Infrared Continua of Seyfert Galaxies |journal=The Astrophysical Journal |date=1 November 2009 |volume=705 |issue=1 |pages=14–31 |doi=10.1088/0004-637X/705/1/14|bibcode=2009ApJ...705...14D |arxiv=0910.1614 |s2cid=119207097 }}</ref> however it features only narrow [[emission line]]s, and has been reclassified as a [[HII region]] galaxy.<ref>{{cite journal |last1=Tommasin |first1=Silvia |last2=Spinoglio |first2=Luigi |last3=Malkan |first3=Matthew A. |last4=Fazio |first4=Giovanni |title=Spitzer-IRS High-Resolution Spectroscopy of the 12 μm Seyfert Galaxies. II. Results for the Complete Data Set |journal=The Astrophysical Journal |date=1 February 2010 |volume=709 |issue=2 |pages=1257–1283 |doi=10.1088/0004-637X/709/2/1257|bibcode=2010ApJ...709.1257T |arxiv=0911.3348 |s2cid=56219335 }}</ref> The Infrared Spectrograph (IRS) on the [[Spitzer Space Telescope]] has detected [[polycyclic aromatic hydrocarbon]] (PAH) emission.<ref>{{cite journal |last1=Gallimore |first1=J. F. |last2=Yzaguirre |first2=A. |last3=Jakoboski |first3=J. |last4=Stevenosky |first4=M. J. |last5=Axon |first5=D. J. |last6=Baum |first6=S. A. |last7=Buchanan |first7=C. L. |last8=Elitzur |first8=M. |last9=Elvis |first9=M. |last10=O'Dea |first10=C. P. |last11=Robinson |first11=A. |title=Infrared Spectral Energy Distributions of Seyfert Galaxies: Spitzer Space Telescope Observations of the 12 μm Sample of Active Galaxies |journal=The Astrophysical Journal Supplement Series |date=1 March 2010 |volume=187 |issue=1 |pages=172–211 |doi=10.1088/0067-0049/187/1/172|bibcode=2010ApJS..187..172G |arxiv=1001.4974 |s2cid=119223756 }}</ref>
NGC 3511 features two very diffuse, thick, and patchy [[spiral arm]]s that emanate from the bulge, while there are also other spiral arm fragments. Dark dust lanes can be seen across the spiral pattern. The [[bulge (astronomy)|bulge]] appears elliptical and is weak.<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|bibcode=2002ApJS..143...73E |arxiv=astro-ph/0206320 |s2cid=15491635 }}</ref> The galaxy is seen at a high inclination, estimated to be 70°.<ref>{{cite journal |last1=Thean |first1=A. |last2=Pedlar |first2=A. |last3=Kukula |first3=M. J. |last4=Baum |first4=S. A. |last5=O'Dea |first5=C. P. |title=High-resolution radio observations of Seyfert galaxies in the extended 12- m sample - II. The properties of compact radio components |journal=Monthly Notices of the Royal Astronomical Society |date=1 August 2001 |volume=325 |issue=2 |pages=737–760 |doi=10.1046/j.1365-8711.2001.04485.x|doi-access=free |bibcode=2001MNRAS.325..737T |arxiv=astro-ph/0103266|s2cid=15097032 }}</ref> In the centre of the galaxy lies a [[supermassive black hole]], whose mass is estimated to be 10<sup>6.46 ± 0.33</sup> (1.3 - 6.2 million) {{solar mass|link=yes}}, based on the pitch angle of the spiral arms.<ref>{{cite journal |last1=Davis |first1=Benjamin L. |last2=Berrier |first2=Joel C. |last3=Johns |first3=Lucas |last4=Shields |first4=Douglas W. |last5=Hartley |first5=Matthew T. |last6=Kennefick |first6=Daniel |last7=Kennefick |first7=Julia |last8=Seigar |first8=Marc S. |last9=Lacy |first9=Claud H. S. |title=The Black Hole Mass Function Derived from Local Spiral Galaxies |journal=The Astrophysical Journal |date=20 June 2014 |volume=789 |issue=2 |pages=124 |doi=10.1088/0004-637X/789/2/124|bibcode=2014ApJ...789..124D |arxiv=1405.5876 |s2cid=119302157 }}</ref> The galaxy had been classified as a type 1 [[Seyfert galaxy]],<ref>{{cite journal |last1=Deo |first1=Rajesh P. |last2=Richards |first2=Gordon T. |last3=Crenshaw |first3=D. M. |last4=Kraemer |first4=S. B. |title=The Mid-Infrared Continua of Seyfert Galaxies |journal=The Astrophysical Journal |date=1 November 2009 |volume=705 |issue=1 |pages=14–31 |doi=10.1088/0004-637X/705/1/14|bibcode=2009ApJ...705...14D |arxiv=0910.1614 |s2cid=119207097 }}</ref> however it features only narrow [[emission line]]s, and has been reclassified as a [[HII region]] galaxy.<ref>{{cite journal |last1=Tommasin |first1=Silvia |last2=Spinoglio |first2=Luigi |last3=Malkan |first3=Matthew A. |last4=Fazio |first4=Giovanni |title=Spitzer-IRS High-Resolution Spectroscopy of the 12 μm Seyfert Galaxies. II. Results for the Complete Data Set |journal=The Astrophysical Journal |date=1 February 2010 |volume=709 |issue=2 |pages=1257–1283 |doi=10.1088/0004-637X/709/2/1257|bibcode=2010ApJ...709.1257T |arxiv=0911.3348 |s2cid=56219335 }}</ref> The Infrared Spectrograph (IRS) on the [[Spitzer Space Telescope]] has detected [[polycyclic aromatic hydrocarbon]] (PAH) emission.<ref>{{cite journal |last1=Gallimore |first1=J. F. |last2=Yzaguirre |first2=A. |last3=Jakoboski |first3=J. |last4=Stevenosky |first4=M. J. |last5=Axon |first5=D. J. |last6=Baum |first6=S. A. |last7=Buchanan |first7=C. L. |last8=Elitzur |first8=M. |last9=Elvis |first9=M. |last10=O'Dea |first10=C. P. |last11=Robinson |first11=A. |title=Infrared Spectral Energy Distributions of Seyfert Galaxies: Spitzer Space Telescope Observations of the 12 μm Sample of Active Galaxies |journal=The Astrophysical Journal Supplement Series |date=1 March 2010 |volume=187 |issue=1 |pages=172–211 |doi=10.1088/0067-0049/187/1/172|bibcode=2010ApJS..187..172G |arxiv=1001.4974 |s2cid=119223756 }}</ref>


NGC 3511 forms a pair with [[NGC 3513]], which lies 10.5 arcminutes away from NGC 3511.<ref name=Carnegie>Sandage, A., Bedke, J. (1994), ''The Carnegie Atlas of Galaxies. Volume I'', Carnegie Institution of Washington</ref> The two galaxies form a small group, known as the NGC 3511 group, which also includes the galaxy ESO 502-024.<ref name=Makarov>{{cite journal|last1=Makarov|first1=Dmitry|last2=Karachentsev|first2=Igor|title=Galaxy groups and clouds in the local (z∼ 0.01) Universe|journal=Monthly Notices of the Royal Astronomical Society|date=21 April 2011|volume=412|issue=4|pages=2498–2520|doi=10.1111/j.1365-2966.2010.18071.x|url=http://www.sao.ru/hq/dim/groups/galaxies.dat|bibcode=2011MNRAS.412.2498M|arxiv = 1011.6277 |s2cid=119194025}}</ref>
NGC 3511 forms a pair with [[NGC 3513]], which lies 10.5 arcminutes away from NGC 3511.<ref name=Carnegie>Sandage, A., Bedke, J. (1994), ''The Carnegie Atlas of Galaxies. Volume I'', Carnegie Institution of Washington</ref> The two galaxies form a small group, known as the NGC 3511 group, which also includes the galaxy ESO 502-024.<ref name=Makarov>{{cite journal|last1=Makarov|first1=Dmitry|last2=Karachentsev|first2=Igor|title=Galaxy groups and clouds in the local (z~ 0.01) Universe|journal=Monthly Notices of the Royal Astronomical Society|date=21 April 2011|volume=412|issue=4|pages=2498–2520|doi=10.1111/j.1365-2966.2010.18071.x|doi-access=free |bibcode=2011MNRAS.412.2498M|arxiv=1011.6277|s2cid=119194025}}</ref>


== See also ==
== See also ==
Line 34: Line 34:
== Gallery ==
== Gallery ==
<gallery>
<gallery>
NGC 3511 GALEX WikiSky.jpg|NGC 3511 by [[GALEX]]
File:NGC 3511 GALEX WikiSky.jpg|NGC 3511 by [[GALEX]]
NGC 3511 PanS.jpg|[[Pan-STARRS]] image of NGC 3511
File:NGC 3511 PanS.jpg|[[Pan-STARRS]] image of NGC 3511
File:NGC 3511 legacy dr10.jpg|[[Dark Energy Spectroscopic Instrument#DESI Legacy Imaging Surveys|legacy surveys]] image of NGC 3511
</gallery>
</gallery>


Latest revision as of 23:56, 16 July 2024

NGC 3511
NGC 3511 by PanSTARRS
Observation data (J2000 epoch)
ConstellationCrater
Right ascension11h 03m 23.8s[1]
Declination−23° 05′ 12″[1]
Redshift0.003699 ± 0.000010 [1]
Heliocentric radial velocity1,109 ± 3 km/s[1]
Distance41.5 ± 6.4 Mly (12.7 ± 2.0 Mpc)[1]
Apparent magnitude (V)10.8 [2]
Characteristics
TypeSAB(s)c [1]
Apparent size (V)5.8′ × 2.0′
Notable featuresExtended HIPASS source[1]
Other designations
UGCA 223, ESO 502- G013, AM 1100-224, MCG -04-26-020, PGC 33385[1]

NGC 3511 is an intermediate spiral galaxy located in the constellation Crater. It is located at a distance of circa 45 million light years from Earth, which, given its apparent dimensions, means that NGC 3511 is about 70,000 light years across. It was discovered by William Herschel on December 21, 1786.[3] It lies two degrees west of Beta Crateris.[4]

NGC 3511 features two very diffuse, thick, and patchy spiral arms that emanate from the bulge, while there are also other spiral arm fragments. Dark dust lanes can be seen across the spiral pattern. The bulge appears elliptical and is weak.[5] The galaxy is seen at a high inclination, estimated to be 70°.[6] In the centre of the galaxy lies a supermassive black hole, whose mass is estimated to be 106.46 ± 0.33 (1.3 - 6.2 million) M☉, based on the pitch angle of the spiral arms.[7] The galaxy had been classified as a type 1 Seyfert galaxy,[8] however it features only narrow emission lines, and has been reclassified as a HII region galaxy.[9] The Infrared Spectrograph (IRS) on the Spitzer Space Telescope has detected polycyclic aromatic hydrocarbon (PAH) emission.[10]

NGC 3511 forms a pair with NGC 3513, which lies 10.5 arcminutes away from NGC 3511.[11] The two galaxies form a small group, known as the NGC 3511 group, which also includes the galaxy ESO 502-024.[12]

See also

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[edit]

References

[edit]
  1. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 3511. Retrieved 2016-01-18.
  2. ^ "Revised NGC Data for NGC 3511". spider.seds.org. Retrieved 25 November 2018.
  3. ^ Seligman, Courtney. "NGC 3511". Celestial Atlas. Retrieved 19 November 2018.
  4. ^ Bakich, Michael E. (2010). 1,001 Celestial Wonders to See Before You Die: The Best Sky Objects for Star Gazers. Springer Science & Business Media. p. 79. ISBN 9781441917775.
  5. ^ 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. arXiv:astro-ph/0206320. Bibcode:2002ApJS..143...73E. doi:10.1086/342340. S2CID 15491635.
  6. ^ Thean, A.; Pedlar, A.; Kukula, M. J.; Baum, S. A.; O'Dea, C. P. (1 August 2001). "High-resolution radio observations of Seyfert galaxies in the extended 12- m sample - II. The properties of compact radio components". Monthly Notices of the Royal Astronomical Society. 325 (2): 737–760. arXiv:astro-ph/0103266. Bibcode:2001MNRAS.325..737T. doi:10.1046/j.1365-8711.2001.04485.x. S2CID 15097032.
  7. ^ Davis, Benjamin L.; Berrier, Joel C.; Johns, Lucas; Shields, Douglas W.; Hartley, Matthew T.; Kennefick, Daniel; Kennefick, Julia; Seigar, Marc S.; Lacy, Claud H. S. (20 June 2014). "The Black Hole Mass Function Derived from Local Spiral Galaxies". The Astrophysical Journal. 789 (2): 124. arXiv:1405.5876. Bibcode:2014ApJ...789..124D. doi:10.1088/0004-637X/789/2/124. S2CID 119302157.
  8. ^ Deo, Rajesh P.; Richards, Gordon T.; Crenshaw, D. M.; Kraemer, S. B. (1 November 2009). "The Mid-Infrared Continua of Seyfert Galaxies". The Astrophysical Journal. 705 (1): 14–31. arXiv:0910.1614. Bibcode:2009ApJ...705...14D. doi:10.1088/0004-637X/705/1/14. S2CID 119207097.
  9. ^ Tommasin, Silvia; Spinoglio, Luigi; Malkan, Matthew A.; Fazio, Giovanni (1 February 2010). "Spitzer-IRS High-Resolution Spectroscopy of the 12 μm Seyfert Galaxies. II. Results for the Complete Data Set". The Astrophysical Journal. 709 (2): 1257–1283. arXiv:0911.3348. Bibcode:2010ApJ...709.1257T. doi:10.1088/0004-637X/709/2/1257. S2CID 56219335.
  10. ^ Gallimore, J. F.; Yzaguirre, A.; Jakoboski, J.; Stevenosky, M. J.; Axon, D. J.; Baum, S. A.; Buchanan, C. L.; Elitzur, M.; Elvis, M.; O'Dea, C. P.; Robinson, A. (1 March 2010). "Infrared Spectral Energy Distributions of Seyfert Galaxies: Spitzer Space Telescope Observations of the 12 μm Sample of Active Galaxies". The Astrophysical Journal Supplement Series. 187 (1): 172–211. arXiv:1001.4974. Bibcode:2010ApJS..187..172G. doi:10.1088/0067-0049/187/1/172. S2CID 119223756.
  11. ^ Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
  12. ^ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv:1011.6277. Bibcode:2011MNRAS.412.2498M. doi:10.1111/j.1365-2966.2010.18071.x. S2CID 119194025.
[edit]
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