Fixed references. Please see Category:CS1 errors: dates.
| ← Previous revision | Revision as of 15:45, 28 September 2025 | ||
| Line 2: | Line 2: | ||
|
{{Infobox galaxy|name=[[Third Cambridge Catalogue of Radio Sources|3C]] 411|epoch=[[J2000.0]]|constellation name=[[Delphinus]]|ra={{RA|20|22|08.43}}<ref name=”ned” />|dec={{DEC|+10|01|11.26}}<ref name=”ned” />|z=0.467000<ref name=”ned” />|h_radial_v=140,003 [[kilometer per second|km/s]]<ref name=”ned” />|dist_ly=4.947 [[light year|Gly]]|appmag_b=19.70|type=N galaxy HEG<ref name=”ned” />|names=[[Fourth Cambridge Survey|4C]] +09.67, [[Parkes Catalogue of Radio Sources|PKS]] 2019+09, [[Lyon-Meudon Extragalactic Database|LEDA]] 2817722, PKS B2019+098, [[NRAO VLA Sky Survey|NVSS]] J202208+100110, OW +032, DA 512, NRAO 0627, TXS 2019+098<ref name=”ned” />|image=File:Image of 3C 411.png|caption=[[Pan-STARRS]] image of 3C 411.}}
|
{{Infobox galaxy|name=[[Third Cambridge Catalogue of Radio Sources|3C]] 411|epoch=[[J2000.0]]|constellation name=[[Delphinus]]|ra={{RA|20|22|08.43}}<ref name=”ned” />|dec={{DEC|+10|01|11.26}}<ref name=”ned” />|z=0.467000<ref name=”ned” />|h_radial_v=140,003 [[kilometer per second|km/s]]<ref name=”ned” />|dist_ly=4.947 [[light year|Gly]]|appmag_b=19.70|type=N galaxy HEG<ref name=”ned” />|names=[[Fourth Cambridge Survey|4C]] +09.67, [[Parkes Catalogue of Radio Sources|PKS]] 2019+09, [[Lyon-Meudon Extragalactic Database|LEDA]] 2817722, PKS B2019+098, [[NRAO VLA Sky Survey|NVSS]] J202208+100110, OW +032, DA 512, NRAO 0627, TXS 2019+098<ref name=”ned” />|image=File:Image of 3C 411.png|caption=[[Pan-STARRS]] image of 3C 411.}}
|
||
|
”’3C 411”’ is a high-excitation [[Fanaroff–Riley classification|Fanaroff-Riley class]] Type 2 [[radio galaxy]] (HEG)<ref>{{Cite journal |last=Varano |first=S. |last2=Chiaberge |first2=M. |last3=Macchetto |first3=F. D. |last4=Capetti |first4=A. |date=2004-12-01 |title=The nuclear radio-optical properties of intermediate-redshift FR II radio galaxies and quasars |url=https://www.aanda.org/articles/aa/pdf/2004/47/aa0303-04.pdf |journal=Astronomy & Astrophysics |language=en |volume=428 |issue=2 |pages=401–408 |doi=10.1051/0004-6361:20040303 |issn=0004-6361}}</ref> located in the constellation of [[Delphinus]]. The estimated [[redshift]] for this galaxy is (z) 0.467<ref name=”ned”>{{Cite web |title=NED Search results for 3C 411 |url=https://ned.ipac.caltech.edu/byname?objname=3C+411&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1 |access-date=2025-09-28 |website=NASA/IPAC Extragalactic Database}}</ref><ref>{{Cite journal |last=Tadhunter |first=C. N. |last2=Scarrott |first2=S. M. |last3=Draper |first3=P. |last4=Rolph |first4=C. |date=1992
|
”’3C 411”’ is a high-excitation [[Fanaroff–Riley classification|Fanaroff-Riley class]] Type 2 [[radio galaxy]] (HEG)<ref>{{Cite journal |last=Varano |first=S. |last2=Chiaberge |first2=M. |last3=Macchetto |first3=F. D. |last4=Capetti |first4=A. |date=2004-12-01 |title=The nuclear radio-optical properties of intermediate-redshift FR II radio galaxies and quasars |url=https://www.aanda.org/articles/aa/pdf/2004/47/aa0303-04.pdf |journal=Astronomy & Astrophysics |language=en |volume=428 |issue=2 |pages=401–408 |doi=10.1051/0004-6361:20040303 |issn=0004-6361}}</ref> located in the constellation of [[Delphinus]]. The estimated [[redshift]] for this galaxy is (z) 0.467<ref name=”ned”>{{Cite web |title=NED Search results for 3C 411 |url=https://ned.ipac.caltech.edu/byname?objname=3C+411&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1 |access-date=2025-09-28 |website=NASA/IPAC Extragalactic Database}}</ref><ref>{{Cite journal |last=Tadhunter |first=C. N. |last2=Scarrott |first2=S. M. |last3=Draper |first3=P. |last4=Rolph |first4=C. |date=1992 |title=The optical polarizations of high- and intermediate-redshift radio galaxies |url=https://watermark02.silverchair.com/mnras256-053P.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA14wggNaBgkqhkiG9w0BBwagggNLMIIDRwIBADCCA0AGCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQMIbENvDI_DID8-qY7AgEQgIIDEYJMfvDUh1CWWbtS4OIKRtKwrCY_jZkE-BwVxcwFvkKl8JMSfWyU0j9ZhwQrtwskfj13su6Wn4NjfvikpktdkRAQfObEgvf0_KJf2zkg5V_JaVgCt3DKQZZP6URnLDO9_R0Z87sRoDbxfHNuQYpTItwE8JSAMdSkwbQWguf0uwQNK0RhDxOY8XXKtxp0SSbJ_MWwfvuisHsa2qMKOjckWpnGNpFYkfdmkUfle6wukKzsfKMqd73CkyYc7qmwkvAA3tKsB4uaO-VdXnmglqZ-N7Q6OBAXFvi3g47dgYb2kElinoi0A_C1m3OxF4SrMRySutg-P_Lrt-Ix21zWCEyh64jly2kAUDQGNxic_-DkaNZnqg7t2EWkEiTzp643NVMynmabwBXWOAU4kPy-WEKovfDBi7mkWSY_Vo3G1aXUxmTu0I0iuP1a61x-Fw5FyY5ThyR0TeK9-bT5773HE44PXkxTWWjyS1CLbzZIiZ4OjWPLwM60VZMsPDYj7y4Pdi7HYUV268QOfLv3f3Rnf-uPQnO_kEbmSBYEnezrSOvc8XUgBxIGnt-dEYZGdDoqMdTd1hcw5gBq_AX7rfSVd6XlDZplRBYp9mC_dUbHbY4TUPSmTvlgtTKe6_hBxFbK9Ue5C1nDPPFUyZ8QfBApfUa8GPHYeu-kqQOFS4FOajgYknzXyEZrzpBsDGQELbGxouQZCruzJLH6YmUg9-NRqd-rP27juEZRrXoL-gV0ERzzZ7p1696N-DB2BdYwUqNqGvfb436L6XjcWkE0czBtJ8FRiJm8ISQALSIsbq8SAW6ZI3xocS5Tam_b2lx6B6oDVFpZQT_Ym6D-ovWrgRHliyMv6if2TRoasf833MP2vXJNCjEoKqZhYavZlUunr7QwJe7RwCwwBRbSaT8jTUZ7U-3pK4dVmrX5d-smKmJaRBf4bWDjZMXN36mL-cTRrD9-OLCGEPZDJIUb_JJOxaFJ-9Ch1qPXTOoINWe3ev3i4tQYguz7WrkcL6-YWwQ_xh8yqg14MtdAwQROT5FzjpKU5II4uBhd |journal=Monthly Notices of the Royal Astronomical Society |volume=256 |issue=1 |pages=53P–58P |doi=10.1093/mnras/256.1.53p |issn=0035-8711}}</ref> and it was first discovered in the [[Third Cambridge Catalogue of Radio Sources]] in 1962.<ref>{{Cite journal |last=Bennett |first=A. S. |date=1962 |title=The revised 3C catalogue of radio sources. |url=https://ui.adsabs.harvard.edu/abs/1962MmRAS..68..163B/abstract |journal=Memoirs of the Royal Astronomical Society |language=en |volume=68 |pages=163}}</ref> Subsequently it was classified as an [[Astronomical radio source|extragalactic radio source]] in 1974 by astronomers,<ref>{{Cite journal |last=Pooley |first=G. G. |last2=Henbest |first2=S. N. |date=1974 |title=Observations of 48 extragalactic radio sources with the Cambridge 5-km telescope at 5 GHz. |url=https://ui.adsabs.harvard.edu/abs/1974MNRAS.169..477P/abstract |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=169 |pages=477–526 |doi=10.1093/mnras/169.3.477 |issn=0035-8711}}</ref> before identified as an N galaxy, that is described to have a distant redshift based on an observation by [[Hyron Spinrad]].<ref name=”:0″>{{Cite journal |last=Spinrad |first=H. |last2=Smith |first2=H. E. |last3=Hunstead |first3=R. |last4=Ryle |first4=M. |date=1975 |title=3C 411: a newly discovered N galaxy with a large redshift. |url=https://ui.adsabs.harvard.edu/abs/1975ApJ…198….7S/abstract |journal=The Astrophysical Journal |language=en |volume=198 |pages=7–11 |doi=10.1086/153571 |issn=0004-637X}}</ref>
|
||
|
== Description ==
|
== Description ==
|
||
|
3C 411 is a broad-line radio galaxy (BLRG).<ref>{{Citation |last=Kataoka |first=J. |title=Broad Line Radio Galaxies Observed with Fermi-LAT: The Origin of the GeV Gamma-Ray Emission |date=2011-07-18 |url=https://arxiv.org/pdf/1107.3370 |access-date=2025-09-28 |publisher=arXiv |doi=10.48550/arXiv.1107.3370 |id=arXiv:1107.3370 |last2=Stawarz |first2=L. |last3=Takahashi |first3=Y. |last4=Cheung |first4=C. C. |last5=Hayashida |first5=M. |last6=Grandi |first6=P. |last7=Burnett |first7=T. H. |last8=Celotti |first8=A. |last9=Fegan |first9=S. J.}}</ref> It is found to contain a double lobed source. When observed through radio mapping, the source is found to contain a [[Radio wave|radio emission]] bridge of low [[surface brightness]] connecting the components, with a nuclear point source dominating over the optical object.<ref name=”:0″ /> Imaging by [[Very Large Array]] (VLA) in 1984, would show the source is heavily [[Depolarization|depolarized]] with the [[radio spectrum]] shown as steepening outside the location of its hotspots. A [[Astrophysical jet|radio jet]] is also shown linking with a central component with the hotspot feature that is located in the western radio lobe.<ref>{{Cite journal |last=Spangler |first=S. R. |last2=Pogge |first2=J. J. |date=1984
|
3C 411 is a broad-line radio galaxy (BLRG).<ref>{{Citation |last=Kataoka |first=J. |title=Broad Line Radio Galaxies Observed with Fermi-LAT: The Origin of the GeV Gamma-Ray Emission |date=2011-07-18 |url=https://arxiv.org/pdf/1107.3370 |access-date=2025-09-28 |publisher=arXiv |doi=10.48550/arXiv.1107.3370 |id=arXiv:1107.3370 |last2=Stawarz |first2=L. |last3=Takahashi |first3=Y. |last4=Cheung |first4=C. C. |last5=Hayashida |first5=M. |last6=Grandi |first6=P. |last7=Burnett |first7=T. H. |last8=Celotti |first8=A. |last9=Fegan |first9=S. J.}}</ref> It is found to contain a double lobed source. When observed through radio mapping, the source is found to contain a [[Radio wave|radio emission]] bridge of low [[surface brightness]] connecting the components, with a nuclear point source dominating over the optical object.<ref name=”:0″ /> Imaging by [[Very Large Array]] (VLA) in 1984, would show the source is heavily [[Depolarization|depolarized]] with the [[radio spectrum]] shown as steepening outside the location of its hotspots. A [[Astrophysical jet|radio jet]] is also shown linking with a central component with the hotspot feature that is located in the western radio lobe.<ref>{{Cite journal |last=Spangler |first=S. R. |last2=Pogge |first2=J. J. |date=1984 |title=VLA observations of the distant radio galaxy 3C 411. |url=https://ui.adsabs.harvard.edu/abs/1984AJ…..89..342S/abstract |journal=The Astronomical Journal |language=en |volume=89 |pages=342–349 |doi=10.1086/113519 |issn=0004-6256}}</ref> At 15 GHz, the source also shows signs of spectra steepening in both of its lobes.<ref>{{Cite journal |last=Fey |first=A. L. |last2=Spangler |first2=S. R. |last3=Myers |first3=S. T. |date=1986 |title=15 GHz VLA observations of the radio galaxies 3C 166 and 3C 411. |url=https://ui.adsabs.harvard.edu/abs/1986AJ…..91.1279F/abstract |journal=The Astronomical Journal |language=en |volume=91 |pages=1279–1285 |doi=10.1086/114103 |issn=0004-6256}}</ref>
|
||
|
An observation conducted in 2014 by [[XMM-Newton|XMM Newton]], would find 3C 411 is a flat spectrum radio [[quasar]]. When observed, it is found to have a presence of a cold [[accretion disk]] around its central [[supermassive black hole]]. The estimated mass of the black hole is 3 x 10<sup>7</sup> [[Solar mass|M<sub>ʘ</sub>]] and the object has a total [[flux]] [[density]] of 2.20 ± 0.16 x 10<sup>-12</sup> [[erg]] cm<sup>-2</sup> s<sup>-1</sup>. A double power-law component was also found in 3C 411, mainly made up of a hard component and a [[Seyfert galaxy|Seyfert]] type-like component.<ref>{{Cite journal |last=Bostrom |first=Allison |last2=Reynolds |first2=Christopher S. |last3=Tombesi |first3=Francesco |date=2014-08-05 |title=AN XMM-NEWTON VIEW OF THE RADIO GALAXY 3C 411 |url=https://doi.org/10.1088/0004-637x/791/2/119 |journal=The Astrophysical Journal |volume=791 |issue=2 |pages=119 |doi=10.1088/0004-637x/791/2/119 |issn=1538-4357}}</ref>
|
An observation conducted in 2014 by [[XMM-Newton|XMM Newton]], would find 3C 411 is a flat spectrum radio [[quasar]]. When observed, it is found to have a presence of a cold [[accretion disk]] around its central [[supermassive black hole]]. The estimated mass of the black hole is 3 x 10<sup>7</sup> [[Solar mass|M<sub>ʘ</sub>]] and the object has a total [[flux]] [[density]] of 2.20 ± 0.16 x 10<sup>-12</sup> [[erg]] cm<sup>-2</sup> s<sup>-1</sup>. A double power-law component was also found in 3C 411, mainly made up of a hard component and a [[Seyfert galaxy|Seyfert]] type-like component.<ref>{{Cite journal |last=Bostrom |first=Allison |last2=Reynolds |first2=Christopher S. |last3=Tombesi |first3=Francesco |date=2014-08-05 |title=AN XMM-NEWTON VIEW OF THE RADIO GALAXY 3C 411 |url=https://doi.org/10.1088/0004-637x/791/2/119 |journal=The Astrophysical Journal |volume=791 |issue=2 |pages=119 |doi=10.1088/0004-637x/791/2/119 |issn=1538-4357}}</ref>
|
||
|
In March 2019, the object was thought to have a [[blazar]] core in its center. However when observed, its jet is shown as straight on a [[trajectory]] path with an [[Orbital inclination|inclination angle]] at 50°. Although [[Very-long-baseline interferometry|Very Long Baseline Interferometry]] (VLBI) observations found the core as compact, it is found to be modelled by multiple jet components instead of a blazar jet, ruling out the possibly of it being classified as a blazar.<ref>{{Cite journal |last=Perger |first=Krisztina |last2=Frey |first2=Sándor |last3=Gabányi |first3=Krisztina É |date=2019
|
In March 2019, the object was thought to have a [[blazar]] core in its center. However when observed, its jet is shown as straight on a [[trajectory]] path with an [[Orbital inclination|inclination angle]] at 50°. Although [[Very-long-baseline interferometry|Very Long Baseline Interferometry]] (VLBI) observations found the core as compact, it is found to be modelled by multiple jet components instead of a blazar jet, ruling out the possibly of it being classified as a blazar.<ref>{{Cite journal |last=Perger |first=Krisztina |last2=Frey |first2=Sándor |last3=Gabányi |first3=Krisztina É |date=2019 |title=Is There a Blazar Nested in the Core of the Radio Galaxy 3C 411? |url=https://ui.adsabs.harvard.edu/abs/2019ApJ…873…61P/abstract |journal=The Astrophysical Journal |language=en |volume=873 |issue=1 |pages=61 |doi=10.3847/1538-4357/ab040f |issn=0004-637X}}</ref>
|
||
|
== References ==
|
== References ==
|
||
