J/A+A/636/A62 Light curves of 3C273 during 2015-2019 (Kim+, 2020)
Investigating the connection between gamma-ray activity and relativistic jet
in 3C 273 during 2015-2019.
Kim D., Trippe S., Kravchenko E.
<Astron. Astrophys. 636, A62 (2020)>
=2020A&A...636A..62K 2020A&A...636A..62K (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Interferometry ; Radio continuum ; Gamma rays ;
Polarization
Keywords: techniques: interferometric - galaxies: jets -
quasars: individual: 3C 273 - gamma-rays: galaxies -
radio continuum: galaxies
Abstract:
The powerful radiation over the entire electromagnetic spectrum and
its radio jet activity of the blazar 3C 273 offer the opportunity of
studying the physics of γ-ray emission from active galactic
nuclei. Since the historically strong outburst in 2009, 3C 273 showed
relatively weak emission in the γ-ray band over several years.
However, recent Fermi-Large Area Telescope observations indicate
higher activity during 2015-2019.
We constrain the origin of the γ-ray outbursts toward 3C 273 and
investigate their connection to the parsec-scale jet.
We generated Fermi-LAT γ-ray light curves with multiple binning
intervals and studied the spectral properties of the γ-ray
emission. Using a 3mm ALMA light curve, we studied the correlation
between radio and γ-ray emission. The relevant activity in the
parsec-scale jet of 3C 273 was investigated with 7 mm VLBA
observations that were obtained close in time to notable γ-ray
outbursts.
We find two prominent γ-ray outbursts in 2016 (MJD 57382) and
2017 (MJD 57883) accompanied by millimeter-wavelength flaring
activity. The γ-ray photon index time series show a weak
hump-like feature around the γ-ray outbursts. The monthly
γ-ray flux-index plot indicates a transition from
softer-when-brighter to harder-when-brighter states at
1.03x10-7ph/cm2/s. A significant correlation between the
γ-ray and millimeter-wavelength emission is found, and the radio
lags the γ-rays by about 105-112 days. The 43GHz jet images
reveal the known stationary features (i.e., the core, S1, and S2) in a
region upstream of the jet. We find an indication for a propagating
disturbance and a polarized knot between the stationary components at
about the times of the two γ-ray outbursts.
Our results support a parsec-scale origin for the observed higher
γ-ray activity, which suggests that this is associated with
standing shocks in the jet.
Description:
The blazar 3C 273 was observed at two radio bands (43 and ∼100GHz) and
gamma-ray (0.1-300GeV) during 2015-2019 on the VLBA, ALMA, and
Fermi-LAT telescopes. Three binning intervals (monthly, weekly, daily)
were used to generate the gamma-ray light curves. With the data
presented below, one can reproduce the light curves (Figure 1 & 2 of
the paper).
Objects:
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RA (2000) DE Designation(s)
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12 29 06.70 +02 03 08.6 3C 273 = 3FGL J1229.1+0202
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
alma.dat 21 147 ALMA fluxes
butot.dat 25 40 VLBA (BU) total fluxes
l7.dat 54 122 LAT weekly fluxes
l7ul.dat 28 78 LAT weekly upper limits
l30.dat 54 40 LAT monthly fluxes
l30ul.dat 27 7 LAT monthly upper limits
l1-16a.dat 54 63 LAT daily fluxes during 2016A
l1-16aul.dat 27 37 LAT daily upper limits during 2016A
l1-16b.dat 54 14 LAT daily fluxes during 2016B
l1-16bul.dat 27 85 LAT daily upper limits during 2016B
l1-17a.dat 54 24 LAT daily fluxes during 2017A
l1-17aul.dat 27 74 LAT daily upper limits during 2017A
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See also:
J/A+A/601/A35 : High-fidelity VLA imaging of 3C273 (Perley+, 2017)
J/A+A/604/A111 : 22GHz image of 3C 273 (Bruni+, 2017)
J/A+A/623/A111 : 3C273 polarization over ALMA 1.3mm band (Hovatta+, 2019)
Byte-by-byte Description of file: alma.dat
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Bytes Format Units Label Explanations
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1- 7 F7.1 d Time MJD of ALMA
9- 14 F6.3 Jy Flux Flux of ALMA, 100GHz
16- 21 F6.4 Jy e_Flux Error of ALMA flux, 100GHz
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Byte-by-byte Description of file: butot.dat
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Bytes Format Units Label Explanations
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1- 7 F7.1 d Time MJD of VLBA
9- 16 F8.5 Jy Flux Total flux of VLBA, 43GHz
18- 25 F8.6 Jy e_Flux Error of VLBA flux, 43GHz
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Byte-by-byte Description of file: l7.dat
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Bytes Format Units Label Explanations
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1- 13 F13.7 d Time MJD of LAT weekly
15- 28 E14.8 ph/cm+2/s Flux Flux of LAT weekly, 0.1-300GeV
30- 43 E14.8 ph/cm+2/s e_Flux Error of LAT weekly flux, 0.1-300GeV
45- 54 F10.6 --- TS Test statistics of LAT weekly flux
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Byte-by-byte Description of file: l7ul.dat
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Bytes Format Units Label Explanations
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1- 13 F13.7 d Time MJD of LAT weekly
15- 28 E14.7 ph/cm+2/s UL Upper limits of LAT weekly flux, 0.1-300GeV
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Byte-by-byte Description of file: l30.dat
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Bytes Format Units Label Explanations
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1- 13 F13.7 d Time MJD of LAT monthly
15- 28 E14.8 ph/cm+2/s Flux Flux of LAT monthly flux, 0.1-300GeV
30- 43 E14.8 ph/cm+2/s e_Flux Error of LAT monthly flux, 0.1-300GeV
45- 54 F10.6 --- TS Test statistics of LAT monthly flux
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Byte-by-byte Description of file: l30ul.dat
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Bytes Format Units Label Explanations
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1- 13 F13.7 d Time MJD of LAT weekly
15- 27 E13.7 ph/cm+2/s UL Upper limits of LAT weekly flux, 0.1-300GeV
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Byte-by-byte Description of file: l1-16a.dat l1-16b.dat l1-17a.dat
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Bytes Format Units Label Explanations
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1- 13 F13.7 d Time MJD of LAT daily
15- 28 E14.9 ph/cm+2/s Flux Flux of LAT daily, 0.1-300GeV
30- 43 E14.9 ph/cm+2/s e_Flux Error of LAT daily flux, 0.1-300GeV
45- 54 F10.6 --- TS Test statistics of LAT daily flux
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Byte-by-byte Description of file: l1-16aul.dat l1-16bul.dat l1-17aul.dat
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Bytes Format Units Label Explanations
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1- 13 F13.7 d Time MJD of LAT daily
14- 27 E14.8 ph/cm+2/s UL Upper limits of LAT flux, 0.1-300GeV
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Acknowledgements:
Sascha Trippe, trippe(at)astro.snu.ac.kr
(End) Daewon Kim [SNU, Korea], Patricia Vannier [CDS] 12-Mar-2020