Jump to content

IC 1459: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous editNext edit →
Content deleted Content added
VisualWikitext
No edit summary
++
Line 25: Line 25:


== Characteristics ==
== Characteristics ==
IC 1459 is a giant elliptical galaxy. In core has been observed to feature a fast counter-rotating stellar component.<ref name="Cappellari02">{{cite journal |last1=Cappellari |first1=M. |last2=Verolme |first2=E. K. |last3=van der Marel |first3=R. P. |last4=Kleijn |first4=G. A. Verdoes |last5=Illingworth |first5=G. D. |last6=Franx |first6=M. |last7=Carollo |first7=C. M. |last8=de Zeeuw |first8=P. T. |title=The Counterrotating Core and the Black Hole Mass of IC 1459 |journal=The Astrophysical Journal |date=20 October 2002 |volume=578 |issue=2 |pages=787–805 |doi=10.1086/342653}}</ref> The galaxy also features multible [[shell galaxy|shells]]<ref>{{cite journal |last1=Tal |first1=Tomer |last2=van Dokkum |first2=Pieter G. |last3=Nelan |first3=Jenica |last4=Bezanson |first4=Rachel |title=The Frequency of Tidal Features Associated with Nearby Luminous Elliptical Galaxies From a Statistically Complete Sample |journal=The Astronomical Journal |date=1 November 2009 |volume=138 |issue=5 |pages=1417–1427 |doi=10.1088/0004-6256/138/5/1417}}</ref> and disturbed isophotes, which indicate that has accreted material, probably by the [[galaxy merger|merger]] of smaller galaxies with the elliptical galaxy. The galaxy is characterised as [[radio galaxy|radio loud]] and has two symmetrical radio jets. Its nucleus is [[active galactic nucleus|active]] and has been characterised as a [[LINER]]. In the centre of the galaxy lies a [[supermassive black hole]] with an estimated mass {{val|2.4|1.0|e=9|ul=M_solar}} based on stellar velocities.<ref name="Cappellari02"/> In images by the [[Hubble Space Telescope]], 199 [[globular cluster]]s where recognised, with an indication of a decrease of their number near the core and statistically non-significant evidence of dimodial color distribution.<ref>{{cite journal |last1=Forbes |first1=Duncan A. |last2=Franx |first2=Marijn |last3=Illingworth |first3=Garth D. |last4=Carollo |first4=C. M. |title=Ellipticals with Kinematically Distinct Cores: WFPC2 Imaging of Globular Clusters |journal=The Astrophysical Journal |date=August 1996 |volume=467 |pages=126 |doi=10.1086/177589}}</ref>
IC 1459 is a giant elliptical galaxy. In its core has been observed a fast counter-rotating stellar component,<ref>{{cite journal |last1=Franx |first1=Marijn |last2=Illingworth |first2=Garth D. |title=A counterrotating core in IC 1459 |journal=The Astrophysical Journal |date=April 1988 |volume=327 |pages=L55 |doi=10.1086/185139}}</ref> with estimated total mass {{val|3|e=9|ul=M_solar}}. The stars of this component have circular orbits on a flat disk with a radius of less than two arcseconds. It has been suggested that the stars of the counterrotating disk are of external origin, either by the accretion of a stellar satellite or of a dense [[molecular cloud]] from which the stars were created.<ref name="Cappellari02">{{cite journal |last1=Cappellari |first1=M. |last2=Verolme |first2=E. K. |last3=van der Marel |first3=R. P. |last4=Kleijn |first4=G. A. Verdoes |last5=Illingworth |first5=G. D. |last6=Franx |first6=M. |last7=Carollo |first7=C. M. |last8=de Zeeuw |first8=P. T. |title=The Counterrotating Core and the Black Hole Mass of IC 1459 |journal=The Astrophysical Journal |date=20 October 2002 |volume=578 |issue=2 |pages=787–805 |doi=10.1086/342653}}</ref> The galaxy also features multible [[shell galaxy|shells]] and disturbed [[isophote]]s, which indicate that has accreted material, probably by the [[galaxy merger|merger]] of smaller galaxies with the elliptical galaxy.<ref>{{cite journal |last1=Tal |first1=Tomer |last2=van Dokkum |first2=Pieter G. |last3=Nelan |first3=Jenica |last4=Bezanson |first4=Rachel |title=The Frequency of Tidal Features Associated with Nearby Luminous Elliptical Galaxies From a Statistically Complete Sample |journal=The Astronomical Journal |date=1 November 2009 |volume=138 |issue=5 |pages=1417–1427 |doi=10.1088/0004-6256/138/5/1417}}</ref> Deep photography revealed the presence of a diffuse [[spiral galaxy|spiral pattern]] at the outer regions of IC 1459.<ref>{{cite book |last1=Malin |first1=D.F. |authorlink1=David Malin |title=New aspects of galaxy photometry : proceedings of the specialized meeting of the Eighth IAU European Regional Astronomy Meeting, Toulouse, September 17-21, 1984 |date=1985 |publisher=Springer-Verlag |isbn=978-3-540-39566-9 |page=28 |chapter=Food for the photometrists — faint galaxies revealed|doi=10.1007/BFb0030917}}</ref>

The nucleus of IC 1459 is [[active galactic nucleus|active]] and has been characterised as a [[LINER]]. The most accepted theory for the power source of active galactic nuclei is the presence of an [[accretion disk]] around a supermassive black hole. In the centre of IC 1459 lies a [[supermassive black hole]] with an estimated mass {{val|2.6|1.0|e=9|ul=M_solar}} based on stellar velocities.<ref name="Cappellari02"/> Estimates of the mass of the black based on gas kinematics are lower, from (1-4) × 10<sup>8</sup><ref>{{cite journal |last1=Verdoes Kleijn |first1=Gijs A. |last2=van der Marel |first2=Roeland P. |last3=Carollo |first3=C. Marcella |last4=de Zeeuw |first4=P. Tim |title=The Black Hole in IC 1459 from Hubble Space Telescope Observations of the Ionized Gas Disk |journal=The Astronomical Journal |date=September 2000 |volume=120 |issue=3 |pages=1221–1237 |doi=10.1086/301524}}</ref> to 10<sup>9</sup> {{solar mass}}, although the presence of non gravitional forces acting on the circumnuclear gas renders them less accurate.<ref name="Cappellari02"/> The disturbed kinematics of the circumnuclear gas may be caused by an outflow.<ref>{{cite journal |last1=Ricci |first1=T. V. |last2=Steiner |first2=J. E. |last3=Menezes |first3=R. B. |title=IFU spectroscopy of 10 early-type galactic nuclei – III. Properties of the circumnuclear gas emission |journal=Monthly Notices of the Royal Astronomical Society |date=29 June 2015 |volume=451 |issue=4 |pages=3728–3758 |doi=10.1093/mnras/stv1156}}</ref> The galaxy is characterised as [[radio galaxy|radio loud]] and has two symmetrical radio jets.<ref>{{cite journal |last1=Tingay |first1=S. J. |last2=Edwards |first2=P. G. |title=The multifrequency parsec-scale structure of PKS 2254−367 (IC 1459): a luminosity-dependent break in morphology for the precursors of radio galaxies? |journal=Monthly Notices of the Royal Astronomical Society |date=21 March 2015 |volume=448 |issue=1 |pages=252–257 |doi=10.1093/mnras/stu2756}}</ref>

In images by the [[Hubble Space Telescope]], 199 [[globular cluster]]s where recognised, with an indication of a decrease of their number near the core and statistically non-significant evidence of dimodial color distribution.<ref>{{cite journal |last1=Forbes |first1=Duncan A. |last2=Franx |first2=Marijn |last3=Illingworth |first3=Garth D. |last4=Carollo |first4=C. M. |title=Ellipticals with Kinematically Distinct Cores: WFPC2 Imaging of Globular Clusters |journal=The Astrophysical Journal |date=August 1996 |volume=467 |pages=126 |doi=10.1086/177589}}</ref>


== Nearby galaxies ==
== Nearby galaxies ==

Revision as of 23:25, 23 January 2019

IC 1459
IC 1459 by Hubble Space Telescope
Observation data (J2000 epoch)
ConstellationGrus
Right ascension22h 57m 10.6s[1]
Declination−36° 27′ 44″[1]
Redshift0.006011 ± 0.000039 [1]
Heliocentric radial velocity1,802 ± 12 km/s[1]
Distance85 ± 27 Mly (26.2 ± 8.5 Mpc)[1]
Apparent magnitude (V)10.0 [2]
Characteristics
TypeE3 [1]
Apparent size (V)5′.2 × 3′.8 [1]
Notable featuresRadio galaxy
Other designations
IC 5265, ESO 406- G030, AM 2254-364, MCG -06-50-016, PKS 2254-367, PGC 070090[1]

IC 1459 (also catalogued as IC 5265) is an elliptical galaxy located in the constellation Grus. It is located at a distance of circa 85 million light years from Earth, which, given its apparent dimensions, means that IC 1459 is about 130,000 light years across. It was discovered by Edward Emerson Barnard in 1892.[3]

Characteristics

IC 1459 is a giant elliptical galaxy. In its core has been observed a fast counter-rotating stellar component,[4] with estimated total mass 3×109 M☉. The stars of this component have circular orbits on a flat disk with a radius of less than two arcseconds. It has been suggested that the stars of the counterrotating disk are of external origin, either by the accretion of a stellar satellite or of a dense molecular cloud from which the stars were created.[5] The galaxy also features multible shells and disturbed isophotes, which indicate that has accreted material, probably by the merger of smaller galaxies with the elliptical galaxy.[6] Deep photography revealed the presence of a diffuse spiral pattern at the outer regions of IC 1459.[7]

The nucleus of IC 1459 is active and has been characterised as a LINER. The most accepted theory for the power source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole. In the centre of IC 1459 lies a supermassive black hole with an estimated mass (2.6±1.0)×109 M☉ based on stellar velocities.[5] Estimates of the mass of the black based on gas kinematics are lower, from (1-4) × 108[8] to 109 M☉, although the presence of non gravitional forces acting on the circumnuclear gas renders them less accurate.[5] The disturbed kinematics of the circumnuclear gas may be caused by an outflow.[9] The galaxy is characterised as radio loud and has two symmetrical radio jets.[10]

In images by the Hubble Space Telescope, 199 globular clusters where recognised, with an indication of a decrease of their number near the core and statistically non-significant evidence of dimodial color distribution.[11]

Nearby galaxies

IC 1459 is the brightest galaxy in a galaxy group known as the IC 1459 group. It is a loose group centred at IC 1459 with a large number of spiral galaxies.[12] Other members include NGC 7418, NGC 7418A, NGC 7421, IC 5264, IC 5269, IC 5269B, IC 5270, and IC 5273.[13] IC 5264 lies 6.5 arcminutes south of IC 1459. This group, along with the NGC 7582 group form the Grus cloud, a region of elevated galaxy density.[12] The Grus cloud, along with the nearby Pavo-Indus cloud, lies between the Local Supercluster and Pavo-Indus Supercluster.[14]

The group features both diffuse X-ray emission from the intergalactic medium and HI emission. Based on the presence of both it has been suggested that the group is in its early stages of assembling from different subgroups. Three HI clouds have been found to be associated with the group, two located near IC 5270 and one near NGC 7418. These HI clouds are believed to have formed from gas stripped from the galaxies as a result of interactions.[12]

References

  1. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for IC 1459. Retrieved 2019-01-18.
  2. ^ "Revised IC Data for IC 1459". spider.seds.org. Retrieved 25 November 2018.
  3. ^ Seligman, Courtney. "IC 1459 (= IC 5265 = PGC 70090)". Celestial Atlas. Retrieved 19 November 2018.
  4. ^ Franx, Marijn; Illingworth, Garth D. (April 1988). "A counterrotating core in IC 1459". The Astrophysical Journal. 327: L55. doi:10.1086/185139.
  5. ^ a b c Cappellari, M.; Verolme, E. K.; van der Marel, R. P.; Kleijn, G. A. Verdoes; Illingworth, G. D.; Franx, M.; Carollo, C. M.; de Zeeuw, P. T. (20 October 2002). "The Counterrotating Core and the Black Hole Mass of IC 1459". The Astrophysical Journal. 578 (2): 787–805. doi:10.1086/342653.
  6. ^ Tal, Tomer; van Dokkum, Pieter G.; Nelan, Jenica; Bezanson, Rachel (1 November 2009). "The Frequency of Tidal Features Associated with Nearby Luminous Elliptical Galaxies From a Statistically Complete Sample". The Astronomical Journal. 138 (5): 1417–1427. doi:10.1088/0004-6256/138/5/1417.
  7. ^ Malin, D.F. (1985). "Food for the photometrists — faint galaxies revealed". New aspects of galaxy photometry : proceedings of the specialized meeting of the Eighth IAU European Regional Astronomy Meeting, Toulouse, September 17-21, 1984. Springer-Verlag. p. 28. doi:10.1007/BFb0030917. ISBN 978-3-540-39566-9.
  8. ^ Verdoes Kleijn, Gijs A.; van der Marel, Roeland P.; Carollo, C. Marcella; de Zeeuw, P. Tim (September 2000). "The Black Hole in IC 1459 from Hubble Space Telescope Observations of the Ionized Gas Disk". The Astronomical Journal. 120 (3): 1221–1237. doi:10.1086/301524.
  9. ^ Ricci, T. V.; Steiner, J. E.; Menezes, R. B. (29 June 2015). "IFU spectroscopy of 10 early-type galactic nuclei – III. Properties of the circumnuclear gas emission". Monthly Notices of the Royal Astronomical Society. 451 (4): 3728–3758. doi:10.1093/mnras/stv1156.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  10. ^ Tingay, S. J.; Edwards, P. G. (21 March 2015). "The multifrequency parsec-scale structure of PKS 2254−367 (IC 1459): a luminosity-dependent break in morphology for the precursors of radio galaxies?". Monthly Notices of the Royal Astronomical Society. 448 (1): 252–257. doi:10.1093/mnras/stu2756.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  11. ^ Forbes, Duncan A.; Franx, Marijn; Illingworth, Garth D.; Carollo, C. M. (August 1996). "Ellipticals with Kinematically Distinct Cores: WFPC2 Imaging of Globular Clusters". The Astrophysical Journal. 467: 126. doi:10.1086/177589.
  12. ^ a b c Serra, P.; et al. (25 July 2015). "ASKAP H i imaging of the galaxy group IC 1459". Monthly Notices of the Royal Astronomical Society. 452 (3): 2680–2691. arXiv:1506.04399. doi:10.1093/mnras/stv1326.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  13. ^ 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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  14. ^ Fouque, P.; Proust, D.; Quintana, H.; Ramirez, A.; Proust, D.; Quintana, H.; Ramirez, A. (1993). "Dynamics of the Pavo-Indus and Grus Clouds of Galaxies" (PDF). Astronomy and Astrophysics Supplement Series. 100 (3): 493–500. Bibcode:1993A&AS..100..493F.{{cite journal}}: CS1 maint: multiple names: authors list (link)
Retrieved from "https://en.wikipedia.org/w/index.php?title=IC_1459&oldid=879876165"