Optical Precursors to Black Hole X-Ray Binary Outbursts: An Evolving Synchrotron Jet Spectrum in Swift J1357.2–0933

Russell, D. M.; Qasim, Ahlam Al; Bernardini, F.; Plotkin, Richard M.; Lewis, Fraser; Koljonen, K. I. I.; Yang, Yi

doi:10.3847/1538-4357/aa9d8c

Cited by 19 publications

(23 citation statements)

References 47 publications

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“…Photometric variability, even in quiescence, is expected for BH LMXB systems, and is sometimes attributed to a jet (e.g. Russell et al 2018). Some BH LMXBs have shown flux increases in the optical and NIR on the order of ∼ 0.05 mag yr −1 as they approach an outburst (e.g.…”

Section: Quiescencementioning

confidence: 99%

“…Some BH LMXBs have shown flux increases in the optical and NIR on the order of ∼ 0.05 mag yr −1 as they approach an outburst (e.g. Bernardini et al 2016;Russell et al 2018). However, the ASAS-SN and ATLAS light curves are consistent with no systematic brightening since 2015.…”

Section: Quiescencementioning

confidence: 99%

“…The smaller accretion disk is less likely to be unstable for a given donor star, and even when unstable, these smaller disks result in lower amplitude outbursts than those seen in BH LMXBs (Done et al 2007). BH LMXBs can exhibit optical outbursts of 5 mags (Corral-Santana et al 2016), and go years between consecutive outbursts (e.g., Russell et al 2018). These outbursting LMXBs are well-described by the classical disk insta- * Carnegie Fellow bility model (DIM) with modifications to account for selfirradiation (DIM+irradiation, Dubus et al 2001).…”

Section: Introductionmentioning

confidence: 99%

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ASASSN-18ey: The Rise of a New Black Hole X-Ray Binary

Tucker

Shappee

Holoien

et al. 2018

ApJL

110

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We present the discovery of ASASSN-18ey (MAXI J1820+070), a new black hole low-mass X-ray binary discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN). A week after ASAS-SN discovered ASASSN-18ey as an optical transient, it was detected as an X-ray transient by MAXI/GCS. Here, we analyze ASAS-SN and Asteroid Terrestrial-impact Last Alert System (ATLAS) pre-outburst optical light curves, finding evidence of intrinsic variability for several years prior to the outburst. While there was no long-term rise leading to outburst, as has been seen in several other systems, the start of the outburst in the optical preceded that in the X-rays by 7.20 ± 0.97 days. We analyze the spectroscopic evolution of ASASSN-18ey from pre-maximum to > 100 days post-maximum. The spectra of ASASSN-18ey exhibit broad, asymmetric, double-peaked Hα emission. The Bowen blend (λ ≈ 4650Å) in the post-maximum spectra shows highly variable double-peaked profiles, likely arising from irradiation of the companion by the accretion disk, typical of low-mass X-ray binaries. The optical and X-ray luminosities of ASASSN-18ey are consistent with black hole low-mass X-ray binaries, both in outburst and quiescence.

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Section: Quiescencementioning

confidence: 99%

Section: Quiescencementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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ASASSN-18ey: The Rise of a New Black Hole X-Ray Binary

Tucker

Shappee

Holoien

et al. 2018

ApJL

110

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“…Swift J1357.2−0933 (hereafter J1357) has been observed to go into outburst twice -once in 2011 (Krimm et al 2011), and again recently in 2017 (Drake et al 2017). However, even during quiescence, an additional component in the system dominates the light from the companion , Russell et al 2018. For this reason, the mass of the system has not been dynamically determined; instead, it was inferred by measuring the Full Width at Half-Maximum (FWHM) of the Hα profiles from the accretion disc.…”

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confidence: 99%

Puzzling blue dips in the black hole candidate Swift J1357.2 − 0933, from ULTRACAM, SALT, ATCA, Swift, and NuSTAR

Paice

Gandhi

Charles

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present rapid, multiwavelength photometry of the low-mass X-ray binary Swift J1357.2-0933 during its 2017 outburst. Using several sets of quasi-simultaneous ULTRACAM/NTT (optical), NuSTAR (X-ray), XRT/Swift (X-ray), SALT (optical), and ATCA (radio) observations taken during outburst decline, we confirm the frequent optical dipping that has previously been noted both in outburst and in quiescence. We also find: (1) that the dip frequency decreases as the outburst decays, similar to what was seen in the previous outburst, (2) that the dips produce a shape similar to that in binary systems with partial disc occultations, (3) that the source becomes significantly bluer during these dips, indicating an unusual geometry compared to other LMXB dippers, and (4) that dip superposition analysis confirms the lack of an X-ray response to the optical dips. These very unusual properties appear to be unique to Swift J1357.2−0933, and are likely the result of a high binary inclination, as inferred from features such as its very low outburst X-ray luminosity. From this analysis as well as X-ray/optical timing correlations, we suggest a model with multicomponent emission/absorption features with differing colours. This could include the possible presence of a sporadically occulted jet base and a recessed disc. This source still hosts many puzzling features, with consequences for the very faint X-ray transients population.

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“…For the NS systems Aql X–1 and MAXI J0556–332, the optical rise of the outbursts was detected by our Faulkes monitoring about a week before the X‐ray flux brightened to sufficient fluxes to be detected by the all‐sky monitors (Russell et al , ; Russell & Lewis ). For the BH LMXB Swift J1357.2–0933 (Russell et al ), the X‐ray all‐sky monitors did not detect the outburst at all (except one single MAXI point 26 days after the first optical detection).…”

Section: Examples Of Optical Rises Before X‐ray Detectionsmentioning

confidence: 97%

Optical precursors to X‐ray binary outbursts

et al. 2019

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Disc instability models predict that for X-ray binaries in quiescence, there should be a brightening of the optical flux prior to an X-ray outburst. Tracking the X-ray variations of X-ray binaries in quiescence is generally not possible, so optical monitoring provides the best means to measure the mass accretion rate variability between outbursts, and to identify the beginning stages of new outbursts. With our regular Faulkes Telescope/Las Cumbres Observatory (LCO) monitoring we are routinely detecting the optical rise of new X-ray binary outbursts before they are detected by X-ray all-sky monitors. We present examples of detections of an optical rise in X-ray binaries prior to X-ray detection. We also present initial optical monitoring of the new black hole transient MAXI J1820+070 (ASASSN-18ey) with the Faulkes, LCO telescopes, and Al Sadeem Observatory in Abu Dhabi, UAE. Finally, we introduce our new real-time data analysis pipeline, the "X-ray Binary New Early Warning System (XB-NEWS)" which aims to detect and announce new X-ray binary outbursts within a day of first optical detection. This will allow us to trigger X-ray and multiwavelength campaigns during the very early stages of outbursts, to constrain the outburst triggering mechanism. KEYWORDS

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Optical Precursors to Black Hole X-Ray Binary Outbursts: An Evolving Synchrotron Jet Spectrum in Swift J1357.2–0933

Cited by 19 publications

References 47 publications

ASASSN-18ey: The Rise of a New Black Hole X-Ray Binary

ASASSN-18ey: The Rise of a New Black Hole X-Ray Binary

Puzzling blue dips in the black hole candidate Swift J1357.2 − 0933, from ULTRACAM, SALT, ATCA, Swift, and NuSTAR

Optical precursors to X‐ray binary outbursts

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