The stringent upper limit on jet power in the persistent soft-state source 4U 1957+11

Maccarone, Thomas J.; Osler, Arlo; Miller-Jones, J. C. A.; Atri, P.; Russell, D. M.; Meier, David L.; McHardy, I. M.; Longa-Peña, Penélope

doi:10.1093/mnrasl/slaa120

Cited by 12 publications

(21 citation statements)

References 58 publications

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“…We did not find any Type I X-ray burst in the entire data. This provides a support against the case of a NS primary (Maccarone et al 2020). As seen in Figure 1, X-ray flux changed during the observing span.…”

Section: Light Curves and Variabilitysupporting

confidence: 70%

“…The earlier studies have provided the bounds on the distance of the binary system as the closest possible distance greater than 10 kpc (Nowak et al 2008;Maitra et al 2014) and a maximum limit of 50 kpc, for the system to reside in the galaxy (Russell et al 2010;Gomez et al 2015). In a recent study, Maccarone et al (2020) reported the most probable source distance of 7 kpc based on the posterior probability with 3 kpc and 15 kpc as the 5 th and 95 th percentile of distribution by using the Gaia parallax measurement.…”

Section: Relativistic Disc Modelmentioning

confidence: 99%

“…Generally, NSs exhibiting a soft spectra and a low root-mean square amplitude of variability show relatively high rates of Type I bursting activity. Therefore, absence of Type I X-ray bursts in 4U 1957+11 is a suggestive evidence for presence of a BH primary in this system (Wijnands et al 2002;Maccarone et al 2020). Although there have been several detailed studies exploring the nature of the compact object in 4U 1957+11, no study has been compelling and conclusive.…”

mentioning

confidence: 99%

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Broad-band spectral study of LMXB black hole candidate 4U 1957+11 with NuSTAR

Sharma,

Jain

et al. 2021

Preprint

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We present here the results of broadband spectral analysis of low-mass X-ray binary and a black hole candidate 4U 1957+11. The source was observed nine times with the Nuclear Spectroscopic Telescope Array (NuSTAR) between 2018 September and 2019 November. During these observations, the spectral state of 4U 1957+11 evolved marginally.The disc dominant spectra are well described with a hot, multicolour disc blackbody with disc temperature varying in the range kT in ∼ 1.35-1.86 keV and a non-thermal component having a steep slope (Γ = 2-3). A broad Fe emission line feature (5-8 keV) was observed in the spectra of all the observations. The relativistic disc model was used to study the effect of distance, inclination, and the black hole mass on its spin. Simulations indicate a higher spin for smaller distances and lower black hole mass. At smaller distances and higher mass, spin is maximum and almost independent of the distance. An inverse correlation exists between the spin and the spectral hardening factor for all the cases. The system prefers a moderate spin of about 0.85 for black hole masses between 4-6 M for a 7 kpc distance.

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Section: Light Curves and Variabilitysupporting

confidence: 70%

Section: Relativistic Disc Modelmentioning

confidence: 99%

mentioning

confidence: 99%

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Broad-band spectral study of LMXB black hole candidate 4U 1957+11 with NuSTAR

Sharma,

Jain

et al. 2021

Preprint

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“…During the soft state, we detect no radio emission from the compact jets, hence we can place constraints on the jet quenching factor by using the highest flux density compatible with the compact jet in hard state and the lowest upper limit on the non-detection during the following soft state. We find a ∼3.5 orders of magnitude quenching factor, which is, so far, one of the strongest constraints on the suppression of compact jets during the soft state of a BH LMXB (Coriat et al 2011;Russell et al 2019a;Maccarone et al 2020).…”

Section: Evolution Of the Compact Jetsmentioning

confidence: 52%

“…Ribó, Dhawan & Mirabel 2004;Russell et al 2015;Péault et al 2019;Saikia et al 2019;Tetarenko et al 2019). No radio emission is usually detected during the soft state, as compact jets are strongly quenched (Fender et al 1999;Corbel et al 2000), by at least 3.5 orders of magnitude (Russell et al 2019a;Maccarone et al 2020). Compact jets are then gradually re-activated as the systems transition back to the final hard state, which precedes quiescence (Miller-Jones et al 2012;Corbel et al 2013;Kalemci et al 2013;Russell et al 2014) One of the most interesting properties of BH LMXBs is the capability of launching transient jets, which are bipolar, discrete blobs of plasma ejected from the system in opposite directions.…”

mentioning

confidence: 99%

The black hole transient MAXI J1348–630: evolution of the compact and transient jets during its 2019/2020 outburst

Carotenuto

Corbel

Tremou

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present the radio and X-ray monitoring campaign of the 2019/2020 outburst of MAXI J1348–630, a new black hole X-ray binary (XRB) discovered in 2019 January. We observed MAXI J1348–630 for ∼14 months in the radio band with MeerKAT and the Australia Telescope Compact Array (ATCA), and in the X-rays with MAXI and Swift/XRT. Throughout the outburst we detected and tracked the evolution of the compact and transient jets. Following the main outburst, the system underwent at least 4 hard-state-only re-flares, during which compact jets were again detected. For the major outburst, we observed the rise, quenching, and re-activation of the compact jets, as well as two single-sided discrete ejecta, launched ∼2 months apart and travelling away from the black hole. These ejecta displayed the highest proper motion (≳100 mas day−1) ever measured for an accreting black hole binary. From the jet motion, we constrain the ejecta inclination and speed to be ≤46○ and ≥0.69 c, and the opening angle and transverse expansion speed of the first component to be ≤6○ and ≤0.05 c. We also infer that the first ejection happened at the hard-to-soft state transition, before a strong radio flare, while the second ejection was launched during a short excursion from the soft to the intermediate state. After traveling with constant speed, the first component underwent a strong deceleration, which was covered with unprecedented detail and suggested that MAXI J1348–630 could be located inside a low-density cavity in the interstellar medium, as already proposed for XTE J1550–564 and H1743–322.

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Confirming NGC 6231 as the parent cluster of the runaway high-mass X-ray binary HD 153919/4U 1700-37 withGaiaDR2

Meij

Guo

Kaper

et al. 2021

A&A

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Context. A significant fraction (10–20%) of the most massive stars move through space with a high (v ≳ 30 km s−1) velocity. One of the possible physical explanations is that a supernova in a compact binary system results in a high recoil velocity of the system. If the system remains bound, it can be subsequently observed as a spectroscopic binary (SB1), a high-mass X-ray binary, a compact binary, and finally a gravitational-wave event. Aims. If such a system is traced back to its parent cluster, binary evolution models can be tested in great detail. Methods. The Gaia proper motions and parallaxes are used to demonstrate that the high-mass X-ray binary HD 153919/4U 1700-37 originates from NGC 6231, the nucleus of the OB association Sco OB1. Results. The O supergiant and its compact companion, of which the physical nature (a neutron star or a black hole) is unknown, move with a space velocity of 63 ± 5 km s−1 with respect to NGC 6231. The kinematical age of the system is 2.2 ± 0.1 Myr. The parallaxes and accurate proper motions in Gaia DR2 were used to perform a membership analysis of NGC 6231; 273 members are identified, of which 268 have good quality photometry. The distance to NGC 6231 is 1.63 ± 0.15 kpc. Isochrone fitting results in an age of 4.7 ± 0.4 Myr and an extinction AV to the cluster of 1.7 ± 0.1. With the identification of NGC 6231 as the parent cluster, the upper limit on the age of the progenitor of 4U1700-37 at the moment of the supernova explosion is 3.0 ± 0.5 Myr. Conclusions. With these constraints, the evolutionary history of the system can be reconstructed with an initial mass of the progenitor of the compact object > 60 M⊙. The high mass, the extreme mass ratio, and short orbital separation of the system make it difficult to produce possible progenitor systems through population synthesis. We propose that the system experienced a Case A mass transfer phase before the supernova, which typically widens a binary. In order to create a progenitor system that does not merge, a lot of angular momentum must be lost from the system during the phase of mass transfer and/or an asymmetry in the supernova explosion provides a kick resulting in the observed orbital parameters. Given its current high space velocity and the derived evolutionary history, the compact object in the system is more likely to have received a large natal kick, which suggests that it is more likely a neutron star than a black hole. HD 153919/4U1700-37 might be a prototype in the Milky Way for the progenitor of gravitational wave events such as GW190412.

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The stringent upper limit on jet power in the persistent soft-state source 4U 1957+11

Cited by 12 publications

References 58 publications

Broad-band spectral study of LMXB black hole candidate 4U 1957+11 with NuSTAR

Broad-band spectral study of LMXB black hole candidate 4U 1957+11 with NuSTAR

The black hole transient MAXI J1348–630: evolution of the compact and transient jets during its 2019/2020 outburst

Confirming NGC 6231 as the parent cluster of the runaway high-mass X-ray binary HD 153919/4U 1700-37 withGaiaDR2

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