A radio parallax to the black hole X-ray binary MAXI J1820+070

Atri, P.; Miller-Jones, J. C. A.; Bahramian, A.; Plotkin, Richard M.; Deller, Adam T.; Jonker, P. G.; Maccarone, Thomas J.; Sivakoff, G. R.; Soria, Roberto; Altamirano, D.; Belloni, T.; Fender, R. P.; Koerding, E.; Maitra, D.; Markoff, Sera; Migliari, S.; Russell, D. M.; Russell, Thomas; Sarazin, Craig L.; Tetarenko, Alexandra J.; Tudose, V.

doi:10.1093/mnrasl/slaa010

Cited by 129 publications

(183 citation statements)

References 38 publications

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“…The jet is then modeled by a truncated cone whose apex is at the central source, of 4 9 in height, 2 6 in width, and with an opening angle of 7°.1. Using 2.96 kpc as the distance to MAXIJ1820 +070 (Atri et al 2020), this corresponds to a volume of V= 1.4×10 51 cm 3 , and a jet of 1.5×10 4 au by 7.7 ×10 3 au, which is in accordance with the estimation performed by Bright et al (2020). Their estimate was obtained 40 days before by inferring it from radio flux comparisons, while we obtained directly a physical size using Chandra data.…”

Section: Energeticssupporting

confidence: 83%

“…The proper motions obtained with the ballistic fit mas day −2 . Assuming a distance of 2.96 kpc (Atri et al 2020), this corresponds to respective apparent initial velocities of 0.61c and 1.59c approximately. The superluminal apparent velocity of the south jet, which is much higher than the apparent velocity for the north jet, suggests that the south jet is the approaching component of the ejection while the north jet is the receding component.…”

Section: Motion Of the Jetsmentioning

confidence: 99%

“…MAXIJ1820+070, first known as ASASSN−18ey, is a black hole X-ray binary (Tucker et al 2018;Torres et al 2019) originally discovered in the optical band on 2018 March 6 by the All-Sky Automated Survey for Supernovae ASAS-SN (Shappee et al 2014;Kochanek et al 2017) and in X-rays on 2018 March 11 (Denisenko 2018; Kawamuro et al 2018) by the Monitor of All-sky X-ray Image MAXI on board the International Space Station (Matsuoka et al 2009). Its distance is constrained to 2.96±0.33 kpc by radio parallax measurements (Atri et al 2020). Its 2018 and 2019 outbursts were densely monitored in radio, revealing the ejection of long-lived discrete relativistic jets (Bright et al 2020).…”

Section: Introductionmentioning

confidence: 99%

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Relativistic X-Ray Jets from the Black Hole X-Ray Binary MAXI J1820+070

Espinasse

Corbel

Kaaret

et al. 2020

ApJL

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The black hole MAXIJ1820+070 was discovered during its 2018 outburst and was extensively monitored across the electromagnetic spectrum. Following the detection of relativistic radio jets, we obtained four Chandra X-ray observations taken between 2018 November and 2019 June, along with radio observations conducted with the Very Large Array and MeerKAT arrays. We report the discovery of X-ray sources associated with the radio jets moving at relativistic velocities with a possible deceleration at late times. The broadband spectra of the jets are consistent with synchrotron radiation from particles accelerated up to very high energies (>10 TeV) by shocks produced by the jets interacting with the interstellar medium. The minimal internal energy estimated from the X-ray observations for the jets is ∼10 41 erg, significantly larger than the energy calculated from the radio flare alone, suggesting most of the energy is possibly not radiated at small scales but released through late-time interactions. Unified Astronomy Thesaurus concepts: X-ray binary stars (1811); Relativistic jets (1390); Accretion (14); Radio jets (1347); Galactic radio sources (571); Stellar mass black holes (1611)

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Section: Energeticssupporting

confidence: 83%

Section: Motion Of the Jetsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Relativistic X-Ray Jets from the Black Hole X-Ray Binary MAXI J1820+070

Espinasse

Corbel

Kaaret

et al. 2020

ApJL

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“…These limits supersede the early restriction of 69 • i 77 • calculated by adopting an outer disk radius of R d ∼ 0.5R 1 and q 0.12 (Torres et al 2019). On one hand, the allowed range for i encloses those expected for an X-ray dipper binary (Frank et al 2002) and contains the 63 ± 3 • (1σ) inclination found for the radio jet (Atri et al 2020). On the other hand, it excludes the 29.8 +3.0 −2.7 • (3-σ) inclination for the inner disk obtained from modeling of X-ray spectra (Bharali et al 2019).…”

Section: Discussionsupporting

confidence: 51%

The Binary Mass Ratio in the Black Hole Transient MAXI J1820+070

Torres

Casares

Jiménez-Ibarra

et al. 2020

ApJL

119

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We present intermediate resolution spectroscopy of the optical counterpart to the black hole X-ray transient MAXI J1820+070 (=ASASSN-18ey) obtained with the OSIRIS spectrograph on the 10.4-m Gran Telescopio Canarias. The observations were performed with the source close to the quiescent state and before the onset of renewed activity in August 2019. We make use of these data and K-type dwarf templates taken with the same instrumental configuration to measure the projected rotational velocity of the donor star. We find v rot sin i = 84±5 km s −1 (1−σ), which implies a donor to black-hole mass ratio q = M 2 /M 1 = 0.072 ± 0.012 for the case of a tidally locked and Roche-lobe filling donor star. The derived dynamical masses for the stellar components are M 1 = (5.95 ± 0.22) sin −3 i M and M 2 = (0.43 ± 0.08) sin −3 i M . The use of q, combined with estimates of the accretion disk size at the time of the optical spectroscopy, allows us to revise our previous orbital inclination constraints to 66 • < i < 81 • . These values lead to 95% confidence level limits on the masses of 5.73 < M 1 (M ) < 8.34 and 0.28 < M 2 (M ) < 0.77. Adopting instead the 63 ± 3 • orientation angle of the radio jet as the binary inclination leads to M 1 = 8.48 +0.79 −0.72 M and M 2 = 0.61 +0.13 −0.12 M (1−σ).

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“…The black hole nature of the source was confirmed with a dynamical mass measurement by Torres et al (2019), who put the mass in the 7-8 M range. MAXI J1820+070 is a relatively nearby BH LMXB, with a distance of 2.96±0.33 kpc (Atri et al 2020), and it has low interstellar absorption (∼ 2 × 10 21 atoms cm −2 ; Kajava et al 2019). After spending roughly the first half of its 8 month outburst in the hard state, MAXI J1820+070 underwent a rapid state transition to the soft state in early July of 2018 (Homan et al 2018a,b).…”

Section: Introductionmentioning

confidence: 99%

A Rapid Change in X-Ray Variability and a Jet Ejection in the Black Hole Transient MAXI J1820+070

Homan

Bright

Motta

et al. 2020

ApJL

108

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We present Neutron Star Interior Composition Explorer X-ray and Arcminute Microkelvin Imager Large Array radio observations of a rapid hard-to-soft state transition in the black hole X-ray transient MAXI J1820+070. During the transition from the hard state to the soft state a switch between two particular types of quasiperiodic oscillations (QPOs) was seen in the X-ray power density spectra, from type-C to type-B, along with a drop in the strength of the broadband X-ray variability and a brief flare in the 7-12 keV band. Soon after this switch (∼1.5-2.5 hr) a strong radio flare was observed that corresponded to the launch of superluminal ejecta. Although hints of a connection between QPO transitions and radio flares have been seen in other black hole X-ray transients, our observations constitute the strongest observational evidence to date for a link between the appearance of type-B QPOs and the launch of discrete jet ejections. are usually recognized: the hard state, which shows strong rapid (subsecond) X-ray variability and a spectrum dominated by Comptonized power-law emission, and the soft state, in which rapid X-ray variability is weak and where a thermal disk blackbody component dominates the spectrum. The transitions between these two spectral states, during which sources are often classified as being in an intermediate state, are accompanied by strong evolution of the X-ray variability properties. As a source starts the transition from the hard state to the soft state, strong (type-C) low-frequency quasi-periodic oscillations (QPOs) are usually present in the power density spectra (see Wijnands et al. 1999;Remillard et al. 2002;Casella et al. 2005, for the various low-frequency QPO types). Their frequencies increase from ∼0.01 Hz to ∼10 Hz as the spectrum softens. At some point during the transition the type-C QPOs and arXiv:2003.01012v1 [astro-ph.HE]

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A radio parallax to the black hole X-ray binary MAXI J1820+070

Cited by 129 publications

References 38 publications

Relativistic X-Ray Jets from the Black Hole X-Ray Binary MAXI J1820+070

Relativistic X-Ray Jets from the Black Hole X-Ray Binary MAXI J1820+070

The Binary Mass Ratio in the Black Hole Transient MAXI J1820+070

A Rapid Change in X-Ray Variability and a Jet Ejection in the Black Hole Transient MAXI J1820+070

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