Disc and wind in black hole X-ray binary MAXI J1820+070 observed through polarized light during its 2018 outburst

Kosenkov, Ilia A.; Veledina, Alexandra; Berdyugin, A.; Kravtsov, Vadim; Piirola, V.; Berdyugina, S. V.; Sakanoi, Takeshi; Kagitani, Masato; Poutanen, Juri

doi:10.1093/mnrasl/slaa096

Cited by 17 publications

(18 citation statements)

References 31 publications

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“…For example, Paice et al (2019) presented optical (g s band; equivalent to 6.4 × 10 5 GHz) observations of MAXI J1820+070, taken 5 d after our observations. The g s band PSD displays a break ∼5-50 Hz, whereas our model predicts the PSD break at 12.4 Hz (although we note that there may be other sources of optical emission from the system; Veledina et al 2019;Kosenkov et al 2020). Additionally, Markoff et al (2020)p r e s e n t an upper limit of <0.1 mas for the size scale of the infrared emitting region (in the plane of the sky) in MAXI J1820+070, from direct imaging with the GRAVITY instrument on the VLT Interferometer (observations taken between 2018 May 31 and June 1, while the system was still in the hard state).…”

Section: Jet Size-scalescontrasting

confidence: 60%

“…These results, combined with the broad-band spectrum shown in Fig. 2, suggest that the infrared and optical emission may both originate in the optically thin innermost jet base region (although the jet may not be the only contributor to the optical emission from the system; Veledina et al 2019;Kosenkov et al 2020), and that any lag between the optical/infrared bands may be attributed to the synchrotron cooling time of the electrons in the jet. In this case, we can use the optical/infrared lag to estimate the magnetic field strength in the jet base region (B).…”

Section: X-ray-optical-infrared Lagsmentioning

confidence: 78%

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Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070

Tetarenko

Casella

Miller-Jones

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present multi-wavelength fast timing observations of the black hole X-ray binary MAXI J1820+070 (ASASSN-18ey), taken with the Karl G. Jansky Very Large Array (VLA), Atacama Large Millimeter/Sub-Millimeter Array (ALMA), Very Large Telescope (VLT), New Technology Telescope (NTT), Neutron Star Interior Composition Explorer (NICER), and XMM-Newton. Our data set simultaneously samples ten different electromagnetic bands (radio – X-ray) over a 7-hour period during the hard state of the 2018–2019 outburst. The emission we observe is highly variable, displaying multiple rapid flaring episodes. To characterize the variability properties in our data, we implemented a combination of cross-correlation and Fourier analyses. We find that the emission is highly correlated between different bands, measuring time-lags ranging from hundreds of milliseconds between the X-ray/optical bands to minutes between the radio/sub-mm bands. Our Fourier analysis also revealed, for the first time in a black hole X-ray binary, an evolving power spectral shape with electromagnetic frequency. Through modelling these variability properties, we find that MAXI J1820+070 launches a highly relativistic ($\Gamma =6.81^{+1.06}_{-1.15}$) and confined ($\phi =0.45^{+0.13}_{-0.11}$ deg) jet, which is carrying a significant amount of power away from the system (equivalent to ∼0.6 L1 − 100keV). We additionally place constraints on the jet composition and magnetic field strength in the innermost jet base region. Overall, this work demonstrates that time-domain analysis is a powerful diagnostic tool for probing jet physics, where we can accurately measure jet properties with time-domain measurements alone.

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Section: Jet Size-scalescontrasting

confidence: 60%

Section: X-ray-optical-infrared Lagsmentioning

confidence: 78%

Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070

Tetarenko

Casella

Miller-Jones

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…The optical/infrared emission also appears to be highly correlated, displaying a strong CCF peak that indicates a lag consistent with zero (−18 +30 −50 ms). These results, combined with the broad-band spectrum shown in Figure 2, suggest that the infrared and optical emission may both originate in the optically thin innermost jet base region (although the jet may not be the only contributor to the optical emission from the system; Veledina et al 2019;Kosenkov et al 2020), and that any lag between the optical/infrared bands may be attributed to the synchrotron cooling time of the electrons in the jet. In this case, we can use the optical/infrared lag to estimate the magnetic field strength in the jet base region (𝐵).…”

Section: Sub-mm -Radio Lagsmentioning

confidence: 85%

Measuring fundamental jet properties with multi-wavelength fast timing of the black hole X-ray binary MAXI J1820+070

Tetarenko,

Casella,

Miller-Jones

et al. 2021

Preprint

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We present multi-wavelength fast timing observations of the black hole X-ray binary MAXI J1820+070 (ASASSN-18ey), taken with the Karl G. Jansky Very Large Array (VLA), Atacama Large Millimeter/Sub-Millimeter Array (ALMA), Very Large Telescope (VLT), New Technology Telescope (NTT), Neutron Star Interior Composition Explorer (NICER), and XMM-Newton. Our data set simultaneously samples ten different electromagnetic bands (radio -X-ray) over a 7-hour period during the hard state of the 2018-2019 outburst. The emission we observe is highly variable, displaying multiple rapid flaring episodes. To characterize the variability properties in our data, we implemented a combination of cross-correlation and Fourier analyses. We find that the emission is highly correlated between different bands, measuring time-lags ranging from hundreds of milliseconds between the X-ray/optical bands to minutes between the radio/sub-mm bands. Our Fourier analysis also revealed, for the first time in a black hole X-ray binary, an evolving power spectral shape with electromagnetic frequency. Through modelling these variability properties, we find that MAXI J1820+070 launches a highly relativistic (Γ = 6.81 +1.06 −1.15 ) and confined (𝜙 = 0.45 +0.13 −0.11 deg) jet, which is carrying a significant amount of power away from the system (equivalent to ∼ 0.6 𝐿 1−100keV ). We additionally place constraints on the jet composition and magnetic field strength in the innermost jet base region. Overall, this work demonstrates that time-domain analysis is a powerful diagnostic tool for probing jet physics, where we can accurately measure jet properties with time-domain measurements alone.

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“…Reprocessing of the X-rays may also take place in the cool outflowing material -the disc wind, which spectroscopic and polarization signatures have been detected during the hard state (Muñoz-Darias et al 2019;Kosenkov et al 2020). This additional component may affect the flux at the core of the line and its variability.…”

Section: Variability Of the Iron Linementioning

confidence: 99%

Accretion geometry of the black hole binary MAXI J1820+070 probed by frequency-resolved spectroscopy

Axelsson,

Veledina

2021

Preprint

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The geometry of the inner accretion flow in the hard and hard-intermediate states of X-ray binaries remains controversial. Using NICER observations of the black hole X-ray binary MAXI J1820+070 during the rising phase of its 2018 outburst, we study the evolution of the timing properties, in particular the characteristic variability frequencies of the prominent iron K𝛼 line. Using frequency-resolved spectroscopy, we find that reflection occurs at large distances from the Comptonizing region in the bright hard state. During the hard-to soft transition, the variability properties suggest the reflector moves closer to the X-ray source. In parallel, the peak of the iron line shifts from 6.5 to ∼7 keV, becoming consistent with that expected of from a highly inclined disc extending close to the black hole. We additionally find significant changes in the dependence of the root-mean-square (rms) variability on both energy and Fourier frequency as the source softens. The evolution of the rms-energy dependence, the line profile, and the timing properties of the iron line as traced by the frequency-resolved spectroscopy all support the picture of a truncated disc/inner flow geometry.

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Disc and wind in black hole X-ray binary MAXI J1820+070 observed through polarized light during its 2018 outburst

Cited by 17 publications

References 31 publications

Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070

Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070

Measuring fundamental jet properties with multi-wavelength fast timing of the black hole X-ray binary MAXI J1820+070

Accretion geometry of the black hole binary MAXI J1820+070 probed by frequency-resolved spectroscopy

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