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{{short description|Quasar}}
{{Short description|Quasar in the constellation Auriga}}
{{Quasar
{{Quasar
| name = [[Third Cambridge Catalogue of Radio Sources|3C]] 147
| name = [[Third Cambridge Catalogue of Radio Sources|3C]] 147
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| ra = {{RA|05|42|36.138}}<ref name=SIMBAD>{{cite simbad
| ra = {{RA|05|42|36.138}}<ref name=SIMBAD>{{cite simbad
|title=3C 147
|title=3C 147
|accessdate=2010-04-21}}</ref>
|access-date=2010-04-21}}</ref>
| dec = {{DEC|+49|51|07.23}}<ref name=SIMBAD/>
| dec = {{DEC|+49|51|07.23}}<ref name=SIMBAD/>
| constellation name = [[Auriga (constellation)|Auriga]]
| constellation name = [[Auriga (constellation)|Auriga]]
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|work=Results for 3C 147
|work=Results for 3C 147
|url=http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=3C+147&img_stamp=yes&extend=no
|url=http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=3C+147&img_stamp=yes&extend=no
|accessdate=2010-04-21}}</ref>
|access-date=2010-04-21}}</ref>
| type = [[Quasar]]<ref name=Rossetti2009>{{cite journal
| type = [[Quasar]]<ref name=Rossetti2009>{{cite journal
|last=Rossetti |first=A.
|last=Rossetti |first=A.
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|doi=10.1051/0004-6361/200811190
|doi=10.1051/0004-6361/200811190
|arxiv=0910.2146 |bibcode=2009A&A...504..741R
|arxiv=0910.2146 |bibcode=2009A&A...504..741R
|s2cid=118716868
}}</ref><br/>Core-Dominated<ref name=ned/><br/>[[Seyfert galaxy|Seyfert 1]]<ref name=SIMBAD/><ref name=ned/>
}}</ref><br/>Core-Dominated<ref name=ned/><br/>[[Seyfert galaxy|Seyfert 1]]<ref name=SIMBAD/><ref name=ned/>
| dist_ly = 5.1 [[Giga-|billion]] [[light-year]]s<br/>([[Distance measures (cosmology)|Light travel time]])<ref name=ned/><br/>6.4 billion light-years<br/>([[Comoving distance|present]])<ref name=ned/>
| dist_ly = 5.1 [[Giga-|billion]] [[light-year]]s<br/>([[Distance measures (cosmology)|Light travel time]])<ref name=ned/><br/>6.4 billion light-years<br/>([[Comoving distance|present]])<ref name=ned/>
| appmag_v = 17.8<ref name=SIMBAD/><ref name=ned/>
| appmag_v = 17.8<ref name=SIMBAD/><ref name=ned/>
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'''3C 147''' (B0538+498) is a compact steep-spectrum (CSS) [[quasar]]<ref name=Rossetti2009/> that was discovered [[List of quasars#First quasars found|in 1964]]. It is located in the [[constellation]] [[Auriga (constellation)|Auriga]] not far in the sky from the 5th [[apparent magnitude|magnitude]] star [[Omicron Aurigae]].
'''3C 147''' (B0538+498) is a compact steep-spectrum (CSS) [[quasar]]<ref name=Rossetti2009/> that was discovered [[List of quasars#First quasars found|in 1964]]. It is located in the [[constellation]] [[Auriga (constellation)|Auriga]] not far in the sky from the 5th [[apparent magnitude|magnitude]] star [[Omicron Aurigae]].


The "distance" of a far away galaxy depends on what [[Distance measures (cosmology)|distance measurement]] you use. With a [[redshift]] of 0.545,<ref name=SIMBAD/><ref name=ned/> light from this [[Active galactic nucleus|active galaxy]] is estimated to have taken around 5.1 [[Giga-|billion]] years to reach us.<ref name=ned/> But as a result of the [[expansion of the Universe]], the present (co-moving) [[Redshift#Extragalactic observations|distance to this galaxy]] is about 6.4 billion [[light-year]]s (1974 M[[parsec|pc]]).<ref name=ned/>
The "distance" of a far away galaxy depends on the [[Distance measures (cosmology)|distance measurement]] used. With a [[redshift]] of 0.545,<ref name=SIMBAD/><ref name=ned/> light from this [[Active galactic nucleus|active galaxy]] is estimated to have taken around 5.1 [[Giga-|billion]] years to reach Earth.<ref name=ned/> But as a result of the [[expansion of the Universe]], the present (co-moving) [[Redshift#Extragalactic observations|distance to this galaxy]] is about 6.4 billion [[light-year]]s (1974 M[[parsec|pc]]).<ref name=ned/>


[[Very Long Baseline Array]] (VLBA) observations have identified a complex central region that is dominated by two bright components, A and B.<ref name=Rossetti2009/> The separation between the two central components of the source seems to be increasing with an apparent velocity ([[superluminal motion]]) of 1.2 ± 0.4 [[Speed of light|c]].<ref name=Rossetti2009/>
[[Very Long Baseline Array]] (VLBA) observations have identified a complex central region that is dominated by two bright components, A and B.<ref name=Rossetti2009/> The separation between the two central components of the source seems to be increasing with an apparent velocity ([[superluminal motion]]) of 1.2 ± 0.4 [[Speed of light|c]].<ref name=Rossetti2009/>


3C 147 is one of four primary calibrators used by the [[Very Large Array]] (along with [[3C 48]], [[3C 138]], and [[3C 286]]). Visibilities of all other sources are calibrated using observed visibilities of one of these four calibrators.<ref name="NRAO">{{cite web |last=Witz |first=Stephan W. |title=Calibration and Flux Density Scale |publisher=[[National Radio Astronomy Observatory]] |date=4 December 2015 |url=https://science.nrao.edu/facilities/vla/docs/manuals/oss/performance/fdscale |accessdate=15 May 2016}}</ref>
3C 147 is one of four primary calibrators used by the [[Very Large Array]] (along with [[3C 48]], [[3C 138]], and [[3C 286]]). Visibilities of all other sources are calibrated using observed visibilities of one of these four calibrators.<ref name="NRAO">{{cite web |last=Witz |first=Stephan W. |title=Calibration and Flux Density Scale |publisher=[[National Radio Astronomy Observatory]] |date=4 December 2015 |url=https://science.nrao.edu/facilities/vla/docs/manuals/oss/performance/fdscale |access-date=15 May 2016}}</ref>

==See also==
* [[List of quasars]]


==References==
==References==
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{{Auriga (constellation)|state=collapsed}}
{{Auriga (constellation)|state=collapsed}}


{{DEFAULTSORT:3C 147}}
[[Category:Quasars]]
[[Category:Quasars]]
[[Category:3C objects|147]]
[[Category:3C objects|147]]
[[Category:Auriga (constellation)]]
[[Category:Auriga]]

Latest revision as of 07:48, 21 July 2024

3C 147
Hubble Legacy Archive WFPC2 image of 3C 147
Observation data (Epoch J2000)
ConstellationAuriga
Right ascension05h 42m 36.138s[1]
Declination+49° 51′ 07.23″[1]
Redshift0.545[1][2]
Distance5.1 billion light-years
(Light travel time)[2]
6.4 billion light-years
(present)[2]
TypeQuasar[3]
Core-Dominated[2]
Seyfert 1[1][2]
Apparent magnitude (V)17.8[1][2]
Other designations
PGC 2355407, 2E 1506, 2MASS J05423614+4951071, QSO B0538+498[1]
See also: Quasar, List of quasars

3C 147 (B0538+498) is a compact steep-spectrum (CSS) quasar[3] that was discovered in 1964. It is located in the constellation Auriga not far in the sky from the 5th magnitude star Omicron Aurigae.

The "distance" of a far away galaxy depends on the distance measurement used. With a redshift of 0.545,[1][2] light from this active galaxy is estimated to have taken around 5.1 billion years to reach Earth.[2] But as a result of the expansion of the Universe, the present (co-moving) distance to this galaxy is about 6.4 billion light-years (1974 Mpc).[2]

Very Long Baseline Array (VLBA) observations have identified a complex central region that is dominated by two bright components, A and B.[3] The separation between the two central components of the source seems to be increasing with an apparent velocity (superluminal motion) of 1.2 ± 0.4 c.[3]

3C 147 is one of four primary calibrators used by the Very Large Array (along with 3C 48, 3C 138, and 3C 286). Visibilities of all other sources are calibrated using observed visibilities of one of these four calibrators.[4]

See also

[edit]

References

[edit]
  1. ^ a b c d e f g "3C 147". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-04-21.
  2. ^ a b c d e f g h i "NASA/IPAC Extragalactic Database". Results for 3C 147. Retrieved 2010-04-21.
  3. ^ a b c d Rossetti, A.; Mantovani; Dallacasa; Junor; Salter; Saikia (2009). "VLBA polarimetric observations of the CSS quasar 3C 147". Astronomy & Astrophysics. 504 (3): 741–749. arXiv:0910.2146. Bibcode:2009A&A...504..741R. doi:10.1051/0004-6361/200811190. S2CID 118716868.
  4. ^ Witz, Stephan W. (4 December 2015). "Calibration and Flux Density Scale". National Radio Astronomy Observatory. Retrieved 15 May 2016.
[edit]
  • Wikisky image of 3C 147 (PGC 2355407)


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