Matches in SemOpenAlex for { <https://semopenalex.org/work/W3045121679> ?p ?o ?g. }
- W3045121679 abstract "Aims. This is the second paper in our series studying the evolution of parsec-scale radio emission in radio galaxies in the Southern Hemisphere. Following our study of the radio and high-energy properties of γ -ray-emitting sources, here we investigate the kinematic and spectral properties of the parsec-scale jets of radio galaxies that have not yet been detected by the Fermi Large Area Telescope ( Fermi -LAT) instrument on board NASA’s Fermi Gamma-ray Space Telescope. For many sources, these results represent the first milliarcsecond resolution information in the literature. These studies were conducted within the framework of the Tracking Active Nuclei with Austral Milliarcsecond Interferometry (TANAMI) monitoring program and in the context of high-energy γ -ray observations from Fermi -LAT. Methods. We took advantage of the regular 8.4 GHz and 22.3 GHz Very Long Baseline Interferometry (VLBI) observations provided by the TANAMI monitoring program, and explored the kinematic properties of six γ -ray-faint radio galaxies. We complemented this with ∼8.5 years of Fermi -LAT data, deriving updated upper limits on the γ -ray emission from this subsample of TANAMI radio galaxies. We included publicly available VLBI kinematics of γ -ray-quiet radio galaxies monitored by the MOJAVE program and performed a consistent Fermi -LAT analysis. We combined these results with those from our previous paper to construct the largest sample of radio galaxies with combined VLBI and γ -ray measurements to date. The connection between parsec-scale jet emission and high-energy properties in the misaligned jets of radio galaxies was explored. Results. For the first time, we report evidence of superluminal motion up to β app = 3.6 in the jet of the γ -ray-faint radio galaxy PKS 2153−69. We find a clear trend of higher apparent speed as a function of distance from the jet core, which indicates that the jet is still being accelerated on scales of tens of parsecs, or ∼10 5 R s , corresponding to the end of the collimation and acceleration zone in nearby radio galaxies. We find evidence of subluminal apparent motion in the jets of PKS 1258−321 and IC 4296, and no measurable apparent motion for PKS 1549−79, PKS 1733−565, and PKS 2027−308. For all these sources, TANAMI provides the first multi-epoch kinematic analysis on parsec scales. We then compare the VLBI properties of γ -ray-detected and undetected radio galaxies, and find that the two populations show a significantly different distribution of median core flux density, and, possibly, of median core brightness temperature. In terms of correlation between VLBI and γ -ray properties, we find a significant correlation between median core flux density and γ -ray flux, but no correlation with typical Doppler boosting indicators such as median core brightness temperature and core dominance. Conclusions. Our study suggests that high-energy emission from radio galaxies is related to parsec-scale radio emission from the inner jet, but is not driven by Doppler boosting effects, in contrast to the situation in their blazar counterparts. This implies that γ -ray loudness does not necessarily reflect a higher prevalence of boosting effects." @default.
- W3045121679 created "2020-07-29" @default.
- W3045121679 creator A5014199228 @default.
- W3045121679 creator A5015202355 @default.
- W3045121679 creator A5018740566 @default.
- W3045121679 creator A5027085734 @default.
- W3045121679 creator A5027612126 @default.
- W3045121679 creator A5027977193 @default.
- W3045121679 creator A5030905298 @default.
- W3045121679 creator A5034118511 @default.
- W3045121679 creator A5034381967 @default.
- W3045121679 creator A5042161585 @default.
- W3045121679 creator A5046265788 @default.
- W3045121679 creator A5049628687 @default.
- W3045121679 creator A5052196425 @default.
- W3045121679 creator A5060064628 @default.
- W3045121679 creator A5060291543 @default.
- W3045121679 creator A5060837837 @default.
- W3045121679 creator A5066377917 @default.
- W3045121679 creator A5067728607 @default.
- W3045121679 creator A5068757764 @default.
- W3045121679 creator A5072079600 @default.
- W3045121679 creator A5072873148 @default.
- W3045121679 creator A5073816424 @default.
- W3045121679 creator A5075150844 @default.
- W3045121679 creator A5085836400 @default.
- W3045121679 creator A5091873580 @default.
- W3045121679 date "2020-09-01" @default.
- W3045121679 modified "2023-09-30" @default.
- W3045121679 title "γ-ray emission in radio galaxies under the VLBI scope" @default.
- W3045121679 cites W1665461817 @default.
- W3045121679 cites W172390819 @default.
- W3045121679 cites W1976787957 @default.
- W3045121679 cites W1979115990 @default.
- W3045121679 cites W1979503956 @default.
- W3045121679 cites W1990401433 @default.
- W3045121679 cites W1998737144 @default.
- W3045121679 cites W1999909546 @default.
- W3045121679 cites W2007391759 @default.
- W3045121679 cites W2011183496 @default.
- W3045121679 cites W2023142861 @default.
- W3045121679 cites W2028067916 @default.
- W3045121679 cites W2036385708 @default.
- W3045121679 cites W2038367995 @default.
- W3045121679 cites W2039174758 @default.
- W3045121679 cites W2044661517 @default.
- W3045121679 cites W2045463691 @default.
- W3045121679 cites W2081906145 @default.
- W3045121679 cites W2082065985 @default.
- W3045121679 cites W2091619147 @default.
- W3045121679 cites W2098000362 @default.
- W3045121679 cites W2106234526 @default.
- W3045121679 cites W2106920781 @default.
- W3045121679 cites W2129151186 @default.
- W3045121679 cites W2135625048 @default.
- W3045121679 cites W2137354936 @default.
- W3045121679 cites W2147875900 @default.
- W3045121679 cites W2152242740 @default.
- W3045121679 cites W2168291386 @default.
- W3045121679 cites W2168541169 @default.
- W3045121679 cites W2512685471 @default.
- W3045121679 cites W2754430995 @default.
- W3045121679 cites W2950800360 @default.
- W3045121679 cites W2953270715 @default.
- W3045121679 cites W3027520426 @default.
- W3045121679 cites W3097994651 @default.
- W3045121679 cites W3098544497 @default.
- W3045121679 cites W3098605815 @default.
- W3045121679 cites W3099439273 @default.
- W3045121679 cites W3100369238 @default.
- W3045121679 cites W3100604183 @default.
- W3045121679 cites W3102874375 @default.
- W3045121679 cites W3103386697 @default.
- W3045121679 cites W3104968552 @default.
- W3045121679 cites W3105353888 @default.
- W3045121679 cites W3105442362 @default.
- W3045121679 cites W3106015352 @default.
- W3045121679 cites W3106331127 @default.
- W3045121679 cites W3121536294 @default.
- W3045121679 cites W3123578725 @default.
- W3045121679 cites W3124456551 @default.
- W3045121679 cites W4211080138 @default.
- W3045121679 cites W3150223203 @default.
- W3045121679 hasPublicationYear "2020" @default.
- W3045121679 type Work @default.
- W3045121679 sameAs 3045121679 @default.
- W3045121679 citedByCount "0" @default.
- W3045121679 crossrefType "journal-article" @default.
- W3045121679 hasAuthorship W3045121679A5014199228 @default.
- W3045121679 hasAuthorship W3045121679A5015202355 @default.
- W3045121679 hasAuthorship W3045121679A5018740566 @default.
- W3045121679 hasAuthorship W3045121679A5027085734 @default.
- W3045121679 hasAuthorship W3045121679A5027612126 @default.
- W3045121679 hasAuthorship W3045121679A5027977193 @default.
- W3045121679 hasAuthorship W3045121679A5030905298 @default.
- W3045121679 hasAuthorship W3045121679A5034118511 @default.
- W3045121679 hasAuthorship W3045121679A5034381967 @default.
- W3045121679 hasAuthorship W3045121679A5042161585 @default.
- W3045121679 hasAuthorship W3045121679A5046265788 @default.
- W3045121679 hasAuthorship W3045121679A5049628687 @default.