{{Short description|Radio galaxy in the constellation Draco}} {{Infobox galaxy|name=Beaver galaxy|epoch=[[J2000.0]]|constellation name=[[Draco (constellation)|Draco]]|ra={{RA|17|13|16.00}}<ref name="ned" />|dec={{DEC|+63|47|37.56}}<ref name="ned" />|z=0.082955|h_radial_v=24,869 [[kilometer per second|km/s]] ± 4<ref name="ned" />|dist_ly={{convert|369.65 ± 25.88|Mpc|Mly|abbr=on|lk=on|order=flip}}<ref name="ned" />|group_cluster=[[Abell 2255]]|mag_j=12.97<ref name="ned" />|type=Radio galaxy<ref name="ned" />|size=~{{convert|110.9|kpc|ly|abbr=on|lk=on|order=flip}} (estimated){{r|ned}}|names=14W 119, [[Principal Galaxies Catalogue|PGC]] 59867, [[2MASX]] J17131603+6347378, [[Seventh Cambridge Survey|7C]] 1712+6352, 1712+638, ABELL 2255:[ZBO89] O4, [GMF2006] J1713.3+6347<ref name="ned" />|image=File:Image of Beaver galaxy.png|caption=[[Sloan Digital Sky Survey|SDSS]] image of the Beaver galaxy}}

The '''Beaver galaxy''' known as '''7C 1712+6352''' or '''1712+638''', is a [[radio galaxy]] located in the constellation of [[Draco (constellation)|Draco]]. The [[redshift]] of the galaxy is (z) 0.082<ref name="ned">{{Cite web |title=NED Search results for Beaver galaxy |url=https://ned.ipac.caltech.edu/byname?objname=LEDA+59867&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1 |access-date=2026-02-15 |website=NASA/IPAC Extragalactic Database}}</ref> and it was first discovered by [[Astronomer|astronomers]] in 1980. It is also considered to be a member of [[Abell 2255]] alongside the [[Goldfish galaxy]], [[Original TRG]] and the [[Embryo galaxy]].<ref name=":0">{{Cite journal |last1=Harris |first1=D. E. |last2=Kapahi |first2=V. K. |last3=Ekers |first3=R. D. |date=February 1980 |title=Westerbork synthesis observations of 8 clusters of galaxies which contain tailed radio galaxies. |url=https://articles.adsabs.harvard.edu//full/1980A%26AS...39..215H/0000219.000.html |journal=Astronomy and Astrophysics Supplement Series |language=en |volume=39 |pages=215–233 |bibcode=1980A&AS...39..215H |issn=0365-0138}}</ref><ref>{{Cite journal |last1=Burns |first1=Jack O. |last2=Roettiger |first2=Kurt |last3=Pinkney |first3=Jason |last4=Perley |first4=Rick A. |last5=Owen |first5=Frazer N. |last6=Voges |first6=Wolfgang |date=June 1995 |title=Evidence for an On-going Cluster/Group Merger in Abell 2255 |url=https://articles.adsabs.harvard.edu/pdf/1995ApJ...446..583B |journal=The Astrophysical Journal |language=en |volume=446 |pages=583 |doi=10.1086/175817 |issn=0004-637X}}</ref>

== Description == The Beaver galaxy is classified to be head-tail [[radio galaxy]] or alternatively, a narrow angle tail radio galaxy, positioned in the southern region away from the center of Abell 2255.<ref name=":0" /><ref name=":1">{{Cite journal |last1=Rubeis |first1=E. De |last2=Bondi |first2=M. |last3=Botteon |first3=A. |last4=Weeren |first4=R. J. van |last5=Jong |first5=J. M. G. H. J. de |last6=Rudnick |first6=L. |last7=Brunetti |first7=G. |last8=Rajpurohit |first8=K. |last9=Gheller |first9=C. |last10=Röttgering |first10=H. J. A. |date=2025-07-01 |title=Revealing the intricacies of radio galaxies and filaments in the merging galaxy cluster Abell 2255 - I. Insights from deep LOFAR-VLBI sub-arcsecond resolution images |url=https://www.aanda.org/articles/aa/abs/2025/07/aa55268-25/aa55268-25.html |journal=Astronomy & Astrophysics |language=en |volume=699 |pages=A229 |doi=10.1051/0004-6361/202555268 |issn=0004-6361|arxiv=2505.13595 }}</ref><ref>{{Cite journal |last1=Govoni |first1=F. |last2=Murgia |first2=M. |last3=Feretti |first3=L. |last4=Giovannini |first4=G. |last5=Dolag |first5=K. |last6=Taylor |first6=G. B. |date=2006-12-01 |title=The intracluster magnetic field power spectrum in Abell 2255 |url=https://www.aanda.org/articles/aa/pdf/2006/47/aa5964-06.pdf |journal=Astronomy & Astrophysics |language=en |volume=460 |issue=2 |pages=425–438 |doi=10.1051/0004-6361:20065964 |issn=0004-6361}}</ref> When observed, the source is found to be extended over an area of 400 [[Parsec|kiloparsecs]] with two regions of [[Polarization (cosmology)|polarized]] emission located by 10 [[Minute and second of arc|arcseconds]] west and northwest from the peak of the northern radio region, in the [[position angle]] of 90°.<ref name=":0" /> The tail feature of the Beaver galaxy has been described to have a long appearance and shown to drastically increase its length to around 1 megaparsec. It also exhibits signs of steepening of the [[spectral index]] indicating the [[Electron|electrons]] lost energy after being ejected from the host. The ages of the [[Plasma (physics)|plasma]] of the tail end is estimated to be 2.2 × 10<sup>8</sup> years.<ref>{{Cite journal |last1=Pizzo |first1=R. F. |last2=Bruyn |first2=A. G. de |last3=Bernardi |first3=G. |last4=Brentjens |first4=M. A. |date=2011-01-01 |title=Deep multi-frequency rotation measure tomography of the galaxy cluster A2255 |url=https://www.aanda.org/articles/aa/pdf/2011/01/aa14158-10.pdf |journal=Astronomy & Astrophysics |language=en |volume=525 |pages=A104 |doi=10.1051/0004-6361/201014158 |issn=0004-6361}}</ref><ref>{{Cite journal |last1=Pizzo |first1=R. F. |last2=Bruyn |first2=A. G. de |date=2009-11-01 |title=Radio spectral study of the cluster of galaxies Abell 2255 |url=https://www.aanda.org/articles/aa/abs/2009/44/aa12465-09/aa12465-09.html |journal=Astronomy & Astrophysics |language=en |volume=507 |issue=2 |pages=639–659 |doi=10.1051/0004-6361/200912465 |issn=0004-6361|arxiv=0909.5198 }}</ref>

Radio imaging made by [[Very Large Array]] (VLA), showed the presence of two [[Astrophysical jet|radio jets]] bending backwards from the radio core of the Beaver galaxy.<ref>{{Cite journal |last1=O'Dea |first1=C. P. |last2=Owen |first2=F. N. |date=June 1985 |title=VLA observations of 57 sources in clusters of galaxies. |url=https://articles.adsabs.harvard.edu/pdf/1985AJ.....90..927O |journal=The Astronomical Journal |language=en |volume=90 |pages=927–953 |doi=10.1086/113801 |issn=0004-6256}}</ref> Evidence also found the inner regions of the jets displaying significant signs of polarization at 20 kiloparsecs from the core. However the eastern jet seems less polarized when imaged at 3.6 [[Centimetre|centimeters]] while the western jet is more polarized. The estimated [[fractional]] polarization of the eastern jet is 12% while the western jet has fractional polarization of 23%.<ref>{{Cite journal |last1=Govoni |first1=F. |last2=Murgia |first2=M. |last3=Feretti |first3=L. |last4=Giovannini |first4=G. |last5=Dolag |first5=K. |last6=Taylor |first6=G. B. |date=2006-12-01 |title=The intracluster magnetic field power spectrum in Abell 2255 |url=https://www.aanda.org/articles/aa/pdf/2006/47/aa5964-06.pdf |journal=Astronomy & Astrophysics |language=en |volume=460 |issue=2 |pages=425–438 |doi=10.1051/0004-6361:20065964 |issn=0004-6361}}</ref> Further radio observations also found both of the jets are shown closer to each other along the tail position, before subsequently forming a [[corkscrew]] feature. Observations at low frequencies, found the tail feature as twisted and fading away upon reaching the cluster [[Radio wave|radio emission]] halo.<ref name=":1" />

== References == <references />

== External links == {{WikiSky}} *[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=NAME%20Beaver%20Galaxy Beaver galaxy on SIMBAD]

{{Draco (constellation)}} [[Category:Radio galaxies]] [[Category:Draco (constellation)]] [[Category:Active galaxies]] [[Category:Principal Galaxies Catalogue objects|059867]] [[Category:Astronomical objects discovered in 1980]]