Abstract
3C 279 is an archetypal blazar with a prominent radio jet that show broadband flux density variability across the entire electromagnetic spectrum. We use an ultra-high angular resolution technique - global Very Long Baseline Interferometry (VLBI) at 1.3mm (230 GHz) - to resolve the innermost jet of 3C 279 in order to study its fine-scale morphology close to the jet base where highly variable-ray emission is thought to originate, according to various models. The source was observed during four days in April 2017 with the Event Horizon Telescope at 230 GHz, including the phased Atacama Large Millimeter/submillimeter Array, at an angular resolution of ∼20 μas (at a redshift of z = 0:536 this corresponds to ∼0:13 pc ∼ 1700 Schwarzschild radii with a black hole mass MBH = 8 × 108 M⊙). Imaging and model-fitting techniques were applied to the data to parameterize the fine-scale source structure and its variation.We find a multicomponent inner jet morphology with the northernmost component elongated perpendicular to the direction of the jet, as imaged at longer wavelengths. The elongated nuclear structure is consistent on all four observing days and across diffierent imaging methods and model-fitting techniques, and therefore appears robust. Owing to its compactness and brightness, we associate the northern nuclear structure as the VLBI "core". This morphology can be interpreted as either a broad resolved jet base or a spatially bent jet.We also find significant day-to-day variations in the closure phases, which appear most pronounced on the triangles with the longest baselines. Our analysis shows that this variation is related to a systematic change of the source structure. Two inner jet components move non-radially at apparent speeds of ∼15 c and ∼20 c (∼1:3 and ∼1:7 μas day-1, respectively), which more strongly supports the scenario of traveling shocks or instabilities in a bent, possibly rotating jet. The observed apparent speeds are also coincident with the 3C 279 large-scale jet kinematics observed at longer (cm) wavelengths, suggesting no significant jet acceleration between the 1.3mm core and the outer jet. The intrinsic brightness temperature of the jet components are ≤1010 K, a magnitude or more lower than typical values seen at ≥7mm wavelengths. The low brightness temperature and morphological complexity suggest that the core region of 3C 279 becomes optically thin at short (mm) wavelengths.
| Original language | English (US) |
|---|---|
| Article number | A69 |
| Journal | Astronomy and Astrophysics |
| Volume | 640 |
| DOIs | |
| State | Published - Aug 1 2020 |
Keywords
- Galaxies: active
- Galaxies: individual: 3C 279
- Galaxies: jets
- Techniques: interferometric
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
Online availability
- 10.1051/0004-6361/202037493License: CC BY
Library availability
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In: Astronomy and Astrophysics, Vol. 640, A69, 01.08.2020.
Research output: Contribution to journal › Article › peer-review
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TY - JOUR
T1 - Event Horizon Telescope imaging of the archetypal blazar 3C 279 at an extreme 20 microarcsecond resolution
AU - Kim, Jae Young
AU - Krichbaum, Thomas P.
AU - Broderick, Avery E.
AU - Wielgus, Maciek
AU - Blackburn, Lindy
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AU - Chael, Andrew
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AU - Issaoun, Sara
AU - Janssen, Michael
AU - Chan, Chi Kwan
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AU - Pesce, Dominic W.
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AU - Chatterjee, Shami
AU - Chatterjee, Koushik
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AU - Chen, Yongjun
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AU - Conway, John E.
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AU - Crew, Geoffrey B.
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AU - Davelaar, Jordy
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AU - Dexter, Jason
AU - Doeleman, Sheperd S.
AU - Eatough, Ralph P.
AU - Falcke, Heino
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AU - Fomalont, Ed
AU - Fraga-Encinas, Raquel
AU - Friberg, Per
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AU - Galison, Peter
AU - Gammie, Charles F.
AU - García, Roberto
AU - Gentaz, Olivier
AU - Georgiev, Boris
AU - Goddi, Ciriaco
AU - Gold, Roman
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AU - Okino, Hiroki
AU - Olivares, Héctor
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AU - Park, Jongho
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AU - Ramakrishnan, Venkatessh
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AU - Ryan, Benjamin R.
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AU - Schuster, Karl Friedrich
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AU - Hao, Jinchi
AU - Hasegawa, Yutaka
AU - Henning, Jason W.
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AU - Heyminck, Stefan
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AU - Violette Impellizzeri, C. M.
AU - Jiang, Homin
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AU - Massingill, Kyle D.
AU - Matulonis, Callie
AU - Mccoll, Martin P.
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AU - Michalik, Daniel
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AU - Montgomerie, William
AU - Mora-Klein, Matias
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AU - Nadolski, Andrew
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N1 - Publisher Copyright: © J.-Y. Kim et al. 2020.
PY - 2020/8/1
Y1 - 2020/8/1
N2 - 3C 279 is an archetypal blazar with a prominent radio jet that show broadband flux density variability across the entire electromagnetic spectrum. We use an ultra-high angular resolution technique - global Very Long Baseline Interferometry (VLBI) at 1.3mm (230 GHz) - to resolve the innermost jet of 3C 279 in order to study its fine-scale morphology close to the jet base where highly variable-ray emission is thought to originate, according to various models. The source was observed during four days in April 2017 with the Event Horizon Telescope at 230 GHz, including the phased Atacama Large Millimeter/submillimeter Array, at an angular resolution of ∼20 μas (at a redshift of z = 0:536 this corresponds to ∼0:13 pc ∼ 1700 Schwarzschild radii with a black hole mass MBH = 8 × 108 M⊙). Imaging and model-fitting techniques were applied to the data to parameterize the fine-scale source structure and its variation.We find a multicomponent inner jet morphology with the northernmost component elongated perpendicular to the direction of the jet, as imaged at longer wavelengths. The elongated nuclear structure is consistent on all four observing days and across diffierent imaging methods and model-fitting techniques, and therefore appears robust. Owing to its compactness and brightness, we associate the northern nuclear structure as the VLBI "core". This morphology can be interpreted as either a broad resolved jet base or a spatially bent jet.We also find significant day-to-day variations in the closure phases, which appear most pronounced on the triangles with the longest baselines. Our analysis shows that this variation is related to a systematic change of the source structure. Two inner jet components move non-radially at apparent speeds of ∼15 c and ∼20 c (∼1:3 and ∼1:7 μas day-1, respectively), which more strongly supports the scenario of traveling shocks or instabilities in a bent, possibly rotating jet. The observed apparent speeds are also coincident with the 3C 279 large-scale jet kinematics observed at longer (cm) wavelengths, suggesting no significant jet acceleration between the 1.3mm core and the outer jet. The intrinsic brightness temperature of the jet components are ≤1010 K, a magnitude or more lower than typical values seen at ≥7mm wavelengths. The low brightness temperature and morphological complexity suggest that the core region of 3C 279 becomes optically thin at short (mm) wavelengths.
AB - 3C 279 is an archetypal blazar with a prominent radio jet that show broadband flux density variability across the entire electromagnetic spectrum. We use an ultra-high angular resolution technique - global Very Long Baseline Interferometry (VLBI) at 1.3mm (230 GHz) - to resolve the innermost jet of 3C 279 in order to study its fine-scale morphology close to the jet base where highly variable-ray emission is thought to originate, according to various models. The source was observed during four days in April 2017 with the Event Horizon Telescope at 230 GHz, including the phased Atacama Large Millimeter/submillimeter Array, at an angular resolution of ∼20 μas (at a redshift of z = 0:536 this corresponds to ∼0:13 pc ∼ 1700 Schwarzschild radii with a black hole mass MBH = 8 × 108 M⊙). Imaging and model-fitting techniques were applied to the data to parameterize the fine-scale source structure and its variation.We find a multicomponent inner jet morphology with the northernmost component elongated perpendicular to the direction of the jet, as imaged at longer wavelengths. The elongated nuclear structure is consistent on all four observing days and across diffierent imaging methods and model-fitting techniques, and therefore appears robust. Owing to its compactness and brightness, we associate the northern nuclear structure as the VLBI "core". This morphology can be interpreted as either a broad resolved jet base or a spatially bent jet.We also find significant day-to-day variations in the closure phases, which appear most pronounced on the triangles with the longest baselines. Our analysis shows that this variation is related to a systematic change of the source structure. Two inner jet components move non-radially at apparent speeds of ∼15 c and ∼20 c (∼1:3 and ∼1:7 μas day-1, respectively), which more strongly supports the scenario of traveling shocks or instabilities in a bent, possibly rotating jet. The observed apparent speeds are also coincident with the 3C 279 large-scale jet kinematics observed at longer (cm) wavelengths, suggesting no significant jet acceleration between the 1.3mm core and the outer jet. The intrinsic brightness temperature of the jet components are ≤1010 K, a magnitude or more lower than typical values seen at ≥7mm wavelengths. The low brightness temperature and morphological complexity suggest that the core region of 3C 279 becomes optically thin at short (mm) wavelengths.
KW - Galaxies: active
KW - Galaxies: individual: 3C 279
KW - Galaxies: jets
KW - Techniques: interferometric
UR - http://www.scopus.com/inward/record.url?scp=85087444933&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85087444933&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202037493
DO - 10.1051/0004-6361/202037493
M3 - Article
AN - SCOPUS:85087444933
SN - 0004-6361
VL - 640
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A69
ER -