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The first estimate of radio jet proper motion at z > 5

S. Frey ; Z. Paragi ; Judit Fogasy (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; L. I. Gurvits
Monthly notices of the Royal Astronomical Society (0035-8711). Vol. 446 (2015), 3, p. 2921-2928.
[Artikel, refereegranskad vetenskaplig]

The extremely high-redshift (z = 5.3) radio source SDSS J102623.61+254259.5 (J1026+2542) is among the most distant and most luminous radio-loud active galactic nuclei (AGN) known to date. Its one-sided radio jet structure on milliarcsecond (mas) and similar to 10-mas scales typical for blazars was first imaged at 5 GHz with very long baseline interferometry (VLBI) in 2006. Here we report on our dual-frequency (1.7 and 5 GHz) imaging observations performed with the European VLBI Network (EVN) in 2013. The prominent jet structure allows us to identify individual components whose apparent displacement can be detected over the time span of 7.33 yr. This is the first time when jet proper motions are directly derived in a blazar at z > 5. The small values of up to similar to 0.1 mas yr(-1) are consistent with what is expected in a relativistic cosmological model if redshift is a measure of distance. The apparent superluminal jet speeds, considered tentative because derived from two epochs only, exceed 10 c for three different components along the jet. Based on modelling its spectral energy distribution, J1026+2542 is known to have its X-ray jet oriented close to the line of sight, with significant Doppler boosting and a large bulk Lorentz factor (Gamma approximate to 13). The new VLBI observations, indicating similar to 2.3 x 10(12) K lower limit to the core brightness temperature, are consistent with this picture. The spectral index in the core region is -0.35.

Nyckelord: Active Galactic Nuclei, Relativistic Jets, Superluminal Motion, Distant, Blazar, High-Redshift, Kinematics, Quasars, VLBI, Cosmology, Expansion



Denna post skapades 2015-05-18. Senast ändrad 2015-07-28.
CPL Pubid: 217182

 

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Projekt

Denna publikation är ett resultat av följande projekt:


Advanced Radio Astronomy in Europe (RADIONET3) (EC/FP7/283393)