EDP Sciences logo
Subscriber Authentication Point
Search
Menu
Home All issues Volume 620 (December 2018) A&A, 620 (2018) A110 Full HTML
Free Access
Issue
A&A
Volume 620, December 2018
Article Number A110
Number of page(s) 16
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/201834102
Published online 07 December 2018

© ESO 2018

1. Introduction

Multiwavelength observations of black hole X-ray binaries (BHXBs) in outburst are crucial to understand the physical mechanisms at work in the different regions of the accretion flow. There is a general consensus that the X-rays are produced in the vicinity of the compact object and that the radio emission is associated with the jet. However, the optical emission in BHXBs can be generated by a variety of mechanisms that take place in different regions of the system. These may include reprocessing of X-rays in the outer regions of the accretion disc and in the optical companion, self-synchrotron emission in the inner hot flow, and synchrotron emission at the base of the jet (Lewin & van der Klis 2006; Hynes 2010; Gandhi et al. 2016).

Performing a cross-correlation analysis of the optical and X-ray light curves is an essential tool for characterising the physical mechanisms driving the observed optical fluxes and for selecting the best of competing physical models, as different emission regions would lead to different observed time lags. It is commonly accepted that in many cases the optical emission is X-ray driven, mainly as reprocessing in the accretion disc and in the optical companion (van Paradijs & McClintock 1994; Dubus et al. 1999). In this scenario, light travel-time delays between the X-rays and the optical emission are expected. Such time lags have been observed for instance in Sco X-1 (Muñoz-Darias et al. 2007; Hynes et al. 2016). However, other mechanisms (e.g. synchrotron emission from the jet) can also lead to sub-second lags and produce more complex patterns in the optical/X-ray correlation functions (as has been observed for XTE J1118+480, Kanbach et al. 2001; Hynes et al. 2003, and GX 339-4, Markoffet al. 2001; Gandhi et al. 2008).

V404 Cygni (hereafter V404 Cyg) is a transient low-mass X-ray binary (LMXB) consisting of a black hole (BH) that accretes mass from a low-mass optical companion. The distance to the system is 2.39 ± 0.14 kpc (Miller-Jones et al. 2009). The orbital period is 6.47 d and the mass function is f(M) = 6.08 ± 0.04 M⊙ (Casares & Charles 1994). The inclination of the orbit is in the range 56–67° (Shahbaz et al. 1994; Sanwal et al. 1996; Khargharia et al. 2010). The donor star is a K0 III–K2 IV (Khargharia et al. 2010; González Hernández et al. 2011), and the mass of the black hole is MBH = 9–12 M⊙.

V404 Cyg was first detected in the optical and identified as a nova-like system during its outbursts in 1938 (Wachman 1948), 1956, and probably in 1979 (Richter 1989). The X-ray source GS 2023+338, discovered in X-rays by the Ginga satellite during an X-ray outburst in May 1989 (Makino et al. 1989), was identified as the old Nova Cygni 1938 (V404 Cygni, Wagner et al. 1989). On 15 June 2015 18:32 UTC (MJD 57188.772), after 26 years of quiescence, the Burst Alert Telescope (BAT; Barthelmy et al. 2005) on board the Swift satellite (Gehrels et al. 2004) detected renewed X-ray activity from V404 Cyg (Barthelmy et al. 2015). This outburst reached its peak on 26 June 2015 and then rapidly decayed, returning to quiescence in mid-August (Sivakoff et al. 2015). The outburst was intensively observed by most of the available space telescopes and ground-based facilities worldwide. On 23 December 2015 (MJD 57379), the Swift/BAT instrument detected a new outburst from V404 Cyg (Barthelmy et al. 2005). The 2015 December outburst was shorter and fainter than the June 2015 outburst (Kajava et al. 2018).

Several studies comparing the optical and X-ray emission from these two outbursts have been performed in the past years. They found no lags or lags of only fractions of seconds to several seconds. Maitra et al. (2017) did not find lags between their optical observations and the X-ray light curves during the June 2015 outburst and proposed the origin of the optical emission to be a compact region most likely originating in a jet outflow. Gandhi et al. (2017) measured optical lags of 0.1 s in two epochs of their June 2015 observations, which they attributed to the elevation of the optical jet base of the system. Kimura et al. (2017, 2018) found evidence of lags of 22.5 and 34.8 s between the optical and X-ray emission for two epochs in their observations during the December 2015 outburst. Gandhi et al. (2015) measured lags of several seconds between the optical and X-rays during their observations from 21 June 2015. In both works, the authors attributed these optical lags of several seconds to reprocessing of the X-ray emission in the accretion disc. Rodriguez et al. (2015) studied the available INTEGRAL observations in the period from 20 to 25 June 2015, and found optical lags of several minutes; this points to a jet origin.

In this paper, we analyse all the available INTEGRAL data during the brightest period of the June 2015 outburst, that is, from 18 June 2015 to the fast decay of the optical and X-ray emission in 27 June 2015, also including NuSTAR observations performed from 25 to 26 June 2015 and some complementary public optical observations.

2. Observations

The INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL; Winkler et al. 2003) observed V404 Cyg in the period MJD 57191.5 to 57216. We analyse here the data obtained during the interval MJD 57191.75–57200.25, when intense flaring activity was detected from the system. We study the optical light curves in the V band provided by the Optical Monitoring Camera (OMC; Mas-Hesse et al. 2003), and the X-ray light curves provided by the Joint European X-Ray Monitor (JEM-X; Lund et al. 2003; 3–10 keV), and by the Imager on Board the INTEGRAL Satellite (IBIS; Ubertini et al. 2003; 20–80 keV and 80–200 keV).

The INTEGRAL data reduction was performed with the Off-line Science Analysis (OSA; Courvoisier et al. 2003) software version 10.2, using the latest calibration files. The data were processed following standard reduction procedures.

We also added to our analysis the X-ray light curves provided by the Nuclear Spectroscopic Telescope Array (NuSTAR, Harrison et al. 2013) in the 3–10 and 10–79 keV bands. These observations were performed during MJD 57197.94–57199.05 (Walton et al. 2017).

The INTEGRAL/JEM-X and IBIS light curves have been binned to provide a time resolution of 5 s. We use a time resolution of 1 s for the NuSTAR light curves.

We complement the OMC optical monitoring with public observations provided by the American Association of Variable Star Observers (AAVSO; Kafka 2018) and with data from the Variable Star Network (VSNET) Collaboration (see Kimura et al. 2016 for a description of this dataset). We converted the reference times provided by the observers in coordinated universal time (UTC) to barycentric dynamical time (TDB), in order to correctly compare the ground-based data with the INTEGRAL and NuSTAR observations. In some cases we have applied small flux corrections for some observers’ datasets, always taking the OMC fluxes as reference. All the optical observations have been corrected for interstellar extinction assuming a value of AV = 4 mag (Casares et al. 1993).

The optical monitoring mean cadences vary between 3 s and 260 s throughout the outburst.

3. Data analysis

We show the V404 Cyg optical and X-ray light curves from MJD 57191.75 to MJD 57200.25 analysed in this work in Figs. 1 and 2. In this section we describe the properties of these light curves and the analysis we have performed.

thumbnail Fig. 1.

Optical and X-ray light curves of V404 Cyg during the June 2015 outburst from MJD 57191.75 to MJD 57196.00. The optical observations are plotted in red, the soft X-ray emission in the 3–10 keV band is plotted in orange, and the hard X-ray emission in the 20–80 keV band for INTEGRAL/IBIS and in the 10–79 keV band for the NuSTAR observations are plotted both in green. The numbers in black refer to the optical flare identifications. Brown and blue boxes mark flares with positive and negative lags, respectively. Light green boxes represent double symmetric optical flares with simultaneous X-ray emission. Purple boxes represent epochs where heartbeat-type oscillations are observed (see text).

thumbnail Fig. 2.

Same as Fig. 1, but from MJD 57196.75 to MJD 57200.25. Grey dashed lines mark the initial and end times of the NuSTAR observations.

3.1. Identification of optical flares

We have identified all the optical flares that have simultaneous X-ray observations. These flares are flagged with identifying numbers in Figs. 1 and 2. The main properties of these optical flares are summarised in Table A.1, where for each flare we provide the time of the peak, the flare rise and decay times, the total flare duration, the peak flux, the flux increment during the flare rise (ΔFrise), and the flux decrement during the decay (ΔFdecay).

The flare start and end times were identified as the times when a change in the slope of the optical light curve is detected. The time of the peak was defined as the time when the optical flux is maximum in each flare. Flare durations, defined as the difference between the flare start and end times, typically range from 3 to 30 min, although some longer flares have been observed (e.g. flares 12 and 14, with durations of 166 and 142 min, respectively). The distribution of the optical flare durations is provided in Fig. 3.

thumbnail Fig. 3.

Histogram of the duration of the optical flares during the June 2015 outburst of V404 Cyg. Bins of 5 min are used.

In order to study the shape of the flares, we represent the ΔFrise/ΔFdecay vs. Δtrise/Δtdecay in Fig. 4. We used colours to distinguish between the different types of flares according to the classification we describe in Sect. 3.2. The horizontal dashed line corresponds to flares for which the source flux before and after the flare is the same (ΔFrise/ΔFdecay = 1). Points above this line correspond to flares for which the optical flux decays to higher fluxes than the flux measured at the flare onset. Points below this line correspond to flares for which the flare decays to lower fluxes than those measured at the flare onset. The vertical dashed line corresponds to flares for which the rise and decay times are equal (Δtrise/Δtdecay = 1). Points to the left of this line correspond to flares with shorter rise than decay times, whereas points to the right of this line correspond to flares with longer rise than decay times. Most of the flares are symmetric, showing similar ΔFrise and ΔFdecay, and similar Δtrise and Δtdecay. However, there are some highly asymmetric flares that show longer time decays, with end fluxes below the pre-flare flux values. As we show in Sect. 3.2, most of these asymmetric flares are flares with simultaneous X-ray and optical emission (green filled points: e.g. flares 20, 26, 37, 38, 44, and 55).

thumbnail Fig. 4.

ΔFrise/ΔFdecay vs. Δtrise/Δtdecay ratios for all the optical flares identified in this work. Dashed lines mark where these properties are symmetrical. Colour-coding according to the optical/X-ray lags (see Sect. 3.2): zero-lagged flares (green points), positive-lagged flares (red triangles), negative-lagged flares (blue stars), frequency-dependent lagged flares (inverted purple triangles), and uncertain (grey squares). Flare numbers of highly asymmetric flares with longer time decays are labelled.

We also computed the flare rise and decay rates, defined as (ΔF/Δt)rise and (ΔF/Δt)decay. We show these rates in Fig. 5. Most of the flares seem to present similar rise and decay flux rates, but some flares show faster rates during decay than during rise. Some of these flares (flares 29, 31, 37, 38, and 44) also displayed decays to lower flux values than those measured before the flare onset, as described before (see Fig. 4). There are also several positive-lagged flares displaying larger decay than rising decays.

thumbnail Fig. 5.

Fading vs. rising flux rates; the dashed line marks where the rates are equal. Flares numbers that deviate from this relation by more than 1σ are marked.

3.2. Cross-correlation analysis

For all the optical flares identified in this work (see Figs. 1 and 2 and Table A.1), we performed a cross-correlation analysis with the X-ray light curves of the system in order to identify possible time lags between the optical and X-ray emission. For this analysis, we used the discrete cross-correlation function (DCF; Edelson & Krolik 1988), a method that avoids interpolating in the temporal domain when the temporal binning is not regular (this is the case for some of the optical observations in this work). In the results from the DCF analysis, a positive lag means that the optical follows the X-rays, a negative lag means that the optical precedes the X-rays, and zero lag means that the optical and the X-rays are simultaneous.

The results of the DCF analysis for each flare are summarised in Table A.2. A histogram of the measured lags between the optical emission and the different X-ray bands is shown in Fig. 6.

thumbnail Fig. 6.

Histogram of the measured lags between the optical and soft X-rays (3–10 keV; top), optical and hard X-rays (20–80 keV for INTEGRAL data, 10–79 keV for NuSTAR data; middle), and optical and very hard X-rays (80–200 keV; bottom). The bin size is 1 min.

To estimate the uncertainties on the measured lags, we performed 1000 Monte Carlo simulations per flare, taking the optical and X-ray flux uncertainties and the temporal binning into account to randomly simulate each light curve. Considering the obtained uncertainties of the lags, in some parts of the outburst there could be optical lags of up to some tens of seconds, which we cannot measure with these data, while in other cases, we are able to accurately measure lags of a few seconds.

In approximately a third of the flares we find that the optical emission is well correlated with the X-ray light curve, and no lags (or lags smaller than the uncertainties) have been found. However, we also found several flares displaying positive lags from tens of seconds to several minutes (the optical emission following the X-rays), and some negative lags of several minutes (with the optical emission preceding the X-rays).

3.3. Hardness evolution

In order to complement our analysis and to search for spectral changes during the studied events, we also analysed the evolution of the X-ray hardness ratio (HR):

H R i = CR a , i − CR b , i CR a , i + CR b , i , $ HR_{i} = \frac{{\rm CR}_{a,i}-{\rm CR}_{b,i}}{{\rm CR}_{a,i}+{\rm CR}_{b,i}} , $(1)

with a, i and b, i the two energy bands for which we have calculated each HRi. We define HR1 as the ratio between the soft (3–10 keV) and the hard (20–80 keV for INTEGRAL, 10–79 keV for NuSTAR) X-ray bands, and HR2 as the ratio between the hard (20–80 keV) and very hard (80–200 keV bands) for INTEGRAL. A distribution of the values of these hardness ratios is shown in Fig. 7.

thumbnail Fig. 7.

Histogram of the hardness ratios: HR1 (solid orange) and HR2 (dark blue striped). The bin size is 0.025. N is the number of observations within each hardness ratio bin.

3.4. Classification of the flares

3.4.1. Simultaneous optical and X-ray flares

We have classified the flares according to the measured lags. For some flares, the optical and X-ray peaks do not show temporal lags within the uncertainties on the lag determination (see Table A.2). Some examples of simultaneous optical and X-ray flares are shown in Fig. 8.

thumbnail Fig. 8.

Zoomed-in optical and X-ray light curves where optical flares are essentially simultaneous with X-ray flares (optical is shown in red, soft X-ray (3–10 keV) in orange, hard X-ray (20–80 keV for ISGRI, or 10–79 keV for NuSTAR) in green, and very hard X-ray (80–200 keV) in dark blue). For each subplot, the HRs (HR1 is plotted in orange, and HR2 in dark blue) and the DCFs (optical ACF is shown in red, optical/soft X-ray DCF in orange, optical/hard X-ray DCF in green, and optical/very hard X-ray in dark blue) are shown below the light curves. The variation in behaviour is discussed in the text.

In these cases we observe two different flare patterns that we describe in detail below.

  • The optical flares seem to envelop the X-ray flares (see flares 6, 13, 46, and 54 in Fig. 8).

  • The optical and X-ray flare peaks are simultaneous, although the optical flares show longer decay times than the X-ray flares, which decay abruptly (see flares 20, 38, and 55 in Fig. 8). These flares are the asymmetric flares in Fig. 4 that we describe in Sect. 3.1. This difference between the optical and X-ray flare profiles leads to an asymmetry in the DCF, which sometimes provides peak values slightly higher than zero. At other times we observe double flares that display a similar behaviour (flares 19–20), and also double symmetric structures in which each flare is composed of two sub-flares (flares 28–29 and 30–31). These regions are marked with light green boxes in Fig. 1.

3.4.2. Optical emission following the X-rays

In some flares we have observed that the optical emission lags the X-rays (positive lags). These lags are typically of several minutes, although time lags shorter than 2 min have also been observed. We have chosen 2 min as the limiting value to distinguish between short and long lags (>2 min), because, as we detail in the discussion, the size of the binary system is close to this value.

Short lags (<2 min)}. For some flares we measure optical lags of several tens of seconds. Given the different monitoring frequency provided by the different optical telescopes, these results should be interpreted carefully. The uncertainties on the estimation of the lags takes this effect into account.

  • Single flares: some flares have been found to be delayed by 0.5–2 min (e.g. flares 2, 43, 45, 49, and 53, see Fig. 9). In this case, the optical flares display similar but smoother shapes than the X-ray flares (in contrast to the flares with slower optical fading described in Sect. 3.4.1).

  • Heartbeat-type oscillations: in some epochs of the outburst, we have observed quasi-periodic oscillations (QPOs) in the optical and X-ray light curves (marked with purple boxes in Fig. 2). We show some examples of these heartbeat-type oscillations in Fig. 10. In all cases the optical oscillations are obvious, but the X-ray oscillations, or at least the correlation with the optical and X-ray variations, are not so clear for all of them. In the last case (Fig. 10, bottom right), the correlation between the optical and X-ray flickering is clear enough to perform a more detailed analysis. Between MJD 57199.850 and 57199.875, the average optical and X-ray fluxes were decaying, while from MJD 57199.875 to MJD 57199.905, the average optical and X-ray fluxes remained roughly constant. We calculated the period of the QPO in both epochs using Lomb-Scargle techniques (Lomb 1976; Scargle 1982), obtaining values of 8.1 min for the decay phase and 6.4 min for the stable phase, with very similar results in the optical and X-ray light curves. We derive optical lags of 1.2 ± 0.3 min, 1.5 ± 0.3 min, and 1.5 ± 0.3 min when we compared this with the soft, hard, and very hard energy bands, respectively. No significant changes have been observed in HR1 and HR2 in the single and heartbeat-type optical flares displaying short delays.

    Long lags (>2 min). The epochs where positive lags longer than 2 min have been measured are marked with brown continuous boxes in Figs. 1 and 2. A closer examination of some representative flares showing these positive lags is displayed in Fig. 11.

thumbnail Fig. 9.

Same as in Fig. 8, but for flares with optical emission following the X-rays with short lags (<2 min).

thumbnail Fig. 10.

Same as in Fig. 8, but for some regions showing heartbeat-type oscillations.

thumbnail Fig. 11.

Same as in Fig. 8, but for flares with optical emission following the X-rays with long lags (>2 min).

  • Single-peaked flares: examination of the optical and X-ray light curves shows that for most of the time, we can identify one single optical flare lagging the X-ray flare (see Fig. 11). The delayed optical flares tend to show symmetric and quasi-linear brightening and fading rise and decays (flares 15, 16, 17, 22, and 47), while in a few cases, the optical flares display smoother peaks (flares 10 and 32).

    In many cases the optical flare begins when the X-ray flare has already decayed (e.g. flares 15, 16, 17, 22, and 47). On other occasions, the optical flare begins during the X-ray flare (flares 8 and 10). In most cases the X-ray and optical flares occur after a longer-term continuous increase in the optical (e.g. flares 10, 14 15, 16, 17, 32, and 47).

  • Multi-flare complex regions: sometimes, multiple optical and X-ray flares are observed, and identifying which optical flare is related with an X-ray flare is not easy. In these cases, we cannot select an interval containing only one optical and one X-ray flare, and the DCF results can be affected by the presence of other flares.

    One of these regions is that from MJD 57197.140–57197.240 (see Fig. 12, top), where the DCF of this region gives two peaks at ∼58.5 and ∼27 min, and it is hard to be sure which optical flare is related with each X-ray flare. When we consider that flares 35–36 are related to the first two X-ray flares and calculate the DCF for shorter regions trying to avoid the presence of the other flares, we obtain time-delays of ∼34 min for flare 35, and ∼25 min for flare 36 (see Table A.2). The sum of both time delays would be in agreement with the first DCF peak at ∼59 min. After flares 35–36, two optical flares (37–38) occur with simultaneous X-ray emission. Both display very fast X-ray and slower optical decays.

    Another peculiar region is that from MJD 57198.214 to 57198.229, where several optical and X-ray flares appear (see Fig. 12, bottom). In this case, the DCF gives the main result at close to zero, but another two peaks at ∼5 and 9 min are significant. When we calculate the DCF in a region including only flares 41 and 42, the DCF indeed peaks at ∼5 min, which is the distance between the two optical flares. While flares 41 and 43 can be related with two simultaneous X-ray flares, flares 42 and 44 seem to be related with the two fainter X-ray flares. On the other hand, flares 41 and 42 are symmetric and display a similar shape in the optical, while flares 43 and 44 display large optical flux decays with longer optical than X-ray decay times (similarly to flares 37–38).

thumbnail Fig. 12.

Same as in Fig. 8, but for complex cases in which there are several optical flares that follow the X-rays.

The HR evolution of these long-delayed optical flares displays different patterns. Sometimes we observe a sudden hardening in HR1 just before the optical flares, at the beginning (see flares 8 and 15–16) or just after the end of the previous X-ray flares (flares 36 and 47). In other cases, the optical brightening takes place during a smooth softening of the X-ray emission (as for flares 10, 14, and 17). In many cases a fast X-ray flare takes place after a delayed optical flare. These flares are harder than most of the flares observed in the outburst and can be identified by spikes in the HR2 evolution that occur several minutes after the optical flares (we have observed these spikes after flares 17, 22, 29, 32, 35, 36, and 40) . Some of these fast flares also show simultaneous optical emission and have been identified as individual flares in this work (flares 23, 37, and 38).

3.4.3. Optical emission leading the X-rays

We have identified several regions in which the optical emission and/or soft X-ray activity precedes the brightening in hard X-rays. These intervals are marked with blue boxes in Figs. 1 and 2. We show two examples (flares 18 and 27) in Fig. 13. In these flares we measure negative lags of ∼−11 min between the optical and hard X-ray light curves, and lags of ∼−3.1 and −0.1 min between the optical and the soft X-rays. In two epochs around MJD 57194.630 and MJD 57195.430 (also marked with blue boxes in Figs. 1 and 2), a brightening in soft X-rays precedes a sudden increase of the hard X-ray light curve by several minutes. Unfortunately, there are no optical data during these two epochs. In all these flares we can identify two clear epochs in the optical and X-ray light curves, and the transition between them is characterized by a sudden brightening of the hard X-ray light curve and a sudden hardening of the system light curves, as measured by the hardness ratio HR1 (see Fig. 13).

thumbnail Fig. 13.

Same as in previous figures, but for cases in which the optical and soft X-ray emission precedes the hard X-rays.

3.4.4. Frequency-dependent lags

We have also observed that on occasion, the measured lag is positive or negative depending on the X-ray energy band we compare it with. This is the case for flare 21, which displays a smooth peak in the optical, but during which several (at least 3) X-ray flares are detected (see Fig. 14). As these three flares display different peak fluxes in the different X-ray bands, different lags are obtained depending on the energy band that we cross-correlate with, as the DCF identifies different times for the peaks of each X-ray flare. Positive lags of ∼0.2 min and 3.01 min are obtained when we correlate the optical with the soft and hard X-ray light curves, but a negative lag of −2.34 min is obtained for the optical to very hard X-ray correlations. This effect is probably due to changes in the hardness ratio. A similar behaviour is observed in flares 28 and 29.

thumbnail Fig. 14.

Same as in Fig. 8, but for a flare with energy-dependent optical/X-ray lags.

4. Discussion

We have studied the optical and X-ray light curves of V404 Cyg during the period 18–28 June 2015, when intense flaring activity was observed. We have identified the flares observed in both energy ranges. We used the DCF technique to search for time lags between the observed optical and X-ray variability.

4.1. Flares displaying no time lags

For a large portion of the flares we analysed, we did not find time lags between the optical and X-ray light curves (taking the uncertainties in the determination of the lags into account; see Fig. 6). This suggests that in these flares, the optical and X-ray emission are produced in the same regions, or at least in regions that lie very closely together in the system, which can include emission from the inner hot flow (the corona or the base of the jet).

For V404 Cyg, the contribution of the jet synchrotron emission to the optical is controversial. It has been found to reach more extreme values than other BHXBs, which exhibit an optically thick to optically thin jet synchrotron break at lower frequencies (Russell et al. 2013). Maitra et al. (2017) found evidence that the break frequency was higher than the optical frequencies during their observations at ∼MJD 57200. However, Russell et al. (2013) measured νb ∼ 1.8 × 1014 Hz during the 1989 outburst. Koljonen et al. (2015) studied the relation between the photon index of the X-ray continuum and the break frequency for BHXBs and AGNs, assuming that the X-ray emission comes from the coronal power-law. From their analysis, it can be inferred that for the hardest power-law indexes observed during the 2015 outburst, a break frequency of νb ∼1015 –1016 Hz can be reached. This implies that the break frequency can vary during the outburst, and the optical contribution from the jet could be significant for the hardest events. Fast variations in the break frequency have been observed in the past for GX 339-4 by Gandhi et al. (2011), who observed changes on timescales shorter than ∼1.5 h.

We have identified a sub-class of no-lagged flares that display a characteristic profile. In these flares, the optical and X-ray light curves peak simultaneously, but the decay of the X-ray light light curve is much faster than the optical light curve decay. Simultaneous infrared, optical, and X-ray observations during one of these flares (flare 44; see Fig. 12, bottom) were analysed by Dallilar et al. (2017). They measured the infrared, optical, and X-ray decay times of this flare and concluded that they were compatible with a cooling effect that was mainly due to a non-thermal mechanism. This would likely be synchrotron emission, revealing that the corona or base of the jet contributed to the optical emission at that epoch. We propose that the flares we have observed with similar profiles could also be produced by the same mechanism.

4.2. Flares displaying positive time lags

We have classified the positive-lagged flares into two categories: short- (<2 min) and long- (>2 min) lagged flares. Optical flares displaying short lags are compatible with reprocessing of incident X-rays (emitted close to the BH) in the accretion disc, and/or in the companion star. However, longer lags would require a different explanation. We have selected 2 min as a limiting value because it would correspond roughly to the light crossing time of the physical size of the binary system. From the known orbital parameters (see Sect. 1), we can infer the mean distance from the BH to the companion star, a ∼ 2.2 × 1012 cm (∼75 light–s), and the maximum size of the disc, rmax ∼ 1.4 × 1012 cm (∼45 light–s). When reprocessing of X-rays in the accretion disc and in the companion star is the mechanism producing the optical emission, we would observe positive lags due to light travel times and smoother optical than X-ray flare profiles, since the optical emission would be the sum of the contribution from multiple regions throughout the disc. To understand the observed lags, the inclination of the system needs to be considered. In a simplified model, the measured lags will vary between zero lag to risc (1 + sini), where rdisc is the disc radius in light seconds and i the binary system inclination. The response from the companion star would oscillate within the range a (1 ± sini) throughout the binary orbit, with the binary separation a expressed in light seconds (O’Brien et al. 2002; Hynes 2010). The relative contribution of the companion response with respect to the disc would depend on the relation between the accretion disc and the companion star radii, but also on the inclination of the system and the thickness of the accretion disc, which define what fraction of the companion star is covered. For V404 Cyg, with an inclination of ∼60°1, lags of up to ∼84 s (1.4 min) would be expected from reprocessing in the accretion disc, and lags between ∼10 and 140 s (0.2–2.3 min) would be expected when reprocessing takes place in the companion star (as a function of the orbital phase).

We have found two variability patterns associated with short optical lags: single flares and heartbeat-type oscillations. Single short-lagged flares can be explained by accretion events producing an enhancement of the X-ray emission that is reprocessed at optical wavelengths within the binary system. Heartbeat-type oscillations were previously noted in the optical light curves of V404 Cyg during the period MJD 57199.840–57200.110 by Kimura et al. (2016). Here we have also identified this variability pattern in the system X-ray light curves and when possible, studied the correlation between them. During the MJD 57199.850–57199.905 epoch (see Fig. 10, bottom right), we observed optical and X-ray heartbeat-type oscillations with periods of ∼6.4–8.1 min. These oscillations are similar to the faster QPOs observed in X-rays for GRS 1915+105 and IGR J17091–3624, with timescales of tens of seconds to 1–2 min (Belloni et al. 1997; Neilsen et al. 2011; Altamirano et al. 2011; Janiuk et al. 2015). These authors proposed that they can be caused by the Lightman–Eardley viscous instabilities in the inner accretion disc. At this epoch, Jourdain et al. (2017) found that the INTEGRAL/SPI spectra were compatible with a transition from a corona-driven to a jet-driven regime. These disc instabilities could be related to the development of the jet. During this epoch, we measured short lags between the optical and X-ray emission (∼1.2 ± 0.3–1.5 ± 0.3 min for the soft and hard X-ray bands, respectively). These optical delays are compatible with light travel times due to reprocessing in the accretion disc. Using the orbital ephemeris from Casares & Charles (1994) (Porb = 6.4714 day and T0 = 2448813.873 HJD), we can calculate the orbital phase during this epoch, which is ϕ ∼ 0.93, very close to superior conjunction, when the contribution from reprocessing in the companion star would be at a minimum.

For the flares that display optical lags longer than 2 min, the optical emission cannot be due to reprocessing of X-rays in the binary system. These long lags could be explained by X-ray reprocessing in the surrounding material (ejected as wind or jet), by the interaction of blob ejections with this surrounding material, or with previously ejected blobs. Re-heating of ejected blobs as a result of internal shocks has been observed in radio wavelengths in Sco X–1 (Fomalont et al. 2001), and re-brightening of ejected material has been seen in other microquasars, such as SS 433, in different energy ranges from X-rays (Migliari et al. 2005) to radio (Mioduszewski et al. 2004).

Discrete jet ejections have been detected in V404 Cyg during the June 2015 outburst at radio and submillimeter wavelengths (Tetarenko et al. 2017) and inferred from optical and IR polarimetry (Shahbaz et al. 2016; Tanaka et al. 2016). Tetarenko et al. (2017) found groups of 2–4 ejections (separated by at most ∼20 min) with the ejecta travelling at bulk speeds varying between events (from 0.08 to 0.8 c). Internal shocks between ejected blobs could produce some of the optical flares analysed in this work. Moreover, if the ejection is accompanied by an X-ray flare, positive lags would result because of the difference between the ejection time (X-ray flare) and the subsequent shock (optical flare). Re-brightening of ejected blobs by the irradiation by an intense X-ray flare could also lead to long-lagged optical flares.

The presence of surrounding material around V404 Cyg is known from previous studies of the June 2015 outburst, which suggest that a substantial fraction of the outer accretion disc was launched away by the strong disc winds detected at several epochs during the outburst in the optical (Muñoz-Darias et al. 2016) and in X-rays (King et al. 2015). These authors measured wind velocities of 1000–3000 km s−1, which would be compatible with the presence of material surrounding the system at distances varying from a few to tens of light–minutes over the outburst. The interaction of ejected blobs with the surrounding material or the re-brightening of this material by irradiation from an X-ray flare could also produce optical lags of several minutes. Potential reprocessing of X-rays in a source distant to the system was inferred by Walton et al. (2017) in the spectral fitting to NuSTAR data. If reprocessing of X-rays takes place in a distant source, it would be expected to contribute to the optical emission as well, and some of the observed optical lags could be explained by this mechanism. Significant absorption by Compton-thick material was reported by Motta et al. (2017a,b), and Sánchez-Fernández et al. (2017) at several epochs during the June 2015 outburst. X-ray reprocessing and extreme absorption values were also observed during the 1989 outburst (Oosterbroek et al. 1996; Zycki et al. 1999). The material ejected by the disc wind may be partly responsible for these extreme absorption values. It should be noted that occasionally an optical flare might erroneously be associated with an X-ray flare. This may happen if the driving X-ray flare was obscured from our direct view, whereas the optical response would be visible as it arises in more distant regions that were not obscured.

Likewise, some of the observed optical flares might also have been due to synchrotron emission from discrete ejections, as has been observed in the past from the correlations between the X-ray, near-IR, and radio flares of GRS 1915+105 (Mirabel & Rodríguez 1998). In this system, hard X-ray dips and soft X-ray flares on timescales of minutes were initially explained by repeated refilling and ejection of the inner accretion disc (Mirabel & Rodríguez 1998). More recent studies have shown that it is the corona that is probably ejected during these events, and the observed X-ray spectrum softening would mark the disappearance of the Comptonisation component (Rodriguez et al. 2008a,b). A bright X-ray spike is usually detected during the recovery of the X-ray emission (Mirabel & Rodríguez 1998), which coincides with the beginning of the IR flares. According to the synchrotron bubble model (van der Laan 1966), the near-IR emission would originate as synchrotron emission from the ejections.

We have identified some multi-flare complex cases in which several optical and X-ray flares are observed, such as the interval MJD 57197.140–57197.240 (see Fig. 12, top). Just before flares 35–36, a polarised optical flare at MJD 57197.142 was measured by Shahbaz et al. (2016). These authors related this event with two radio flares observed at 16GHz and 5GHz peaking at ∼2 h and ∼3.8 h after the polarised flare, respectively, and interpreted it as the birth of a major ejection event. According to our analysis, flares 35–36 lag the first two X-ray flares by ∼34 and ∼26 min (see Sect. 3.4.2). Optical flares 35 and 36 might be related to jet ejection events, due either to synchrotron emission or to the interaction of these ejections with the surrounding material or with previous ejected blobs. After flares 35–36, two simultaneous optical/X-ray flares (37–38) occur with very fast X-ray decay and slower optical decays. From the HR2 (defined between the 80–200 keV and 20–80 keV INTEGRAL/IBIS energy bands), we can also see that flares 37–38 are harder and display faster decays than flares 35–36 (associated with the long lags), and display very bright relative fluxes in the 80–200 keV band. Similar rapid non-thermal flares have also been observed in blazars and have been explained by synchrotron self-Compton (SSC) processes in the jet (Sokolov et al. 2004).

Another complex region identified during this outburst is the interval MJD 57198.200–57198.240, during which several optical and X-ray flares are observed (see Fig. 12, bottom). Optical flares 41 and 43 are simultaneous with two bright X-ray flares, and flare 44 is simultaneous with a fainter X-ray flare. The profile of optical flare 42 is very similar to flare 41 and takes place during a period of faint X-ray emission. This flare displays a delay of ∼5 min with respect to flare 41 and the simultaneous X-ray flare. Flare 41 corresponds to flare 1 in Walton et al. (2017). These authors proposed that the brightest flares observed in their NuSTAR observations (including flare 1 and the subsequent X-ray flares) are produced by jet ejections. Furthermore, a reflection component from an unspecified distant region was also required in their X-ray spectral fitting. These authors also showed that the radio activity in the Arcminute Microkelvin Imager Large Array (AMI-LA) light curve starts just when the X-ray flaring activity begins in the NuSTAR data. A state transition was also measured at this time by Gandhi et al. (2017), who found that sub-second optical/X-ray delays appeared together with a brightening of the radio jet. Flare 44 was explained by synchrotron cooling processes by Dallilar et al. (2017). All these results suggest that various physical mechanisms, including jet ejections and reprocessing, might contribute to the observed complex pattern.

4.3. Optical emission preceding X-rays

Finally, we have also observed intervals where a gradual increase of the optical emission and soft X-rays precede a sudden rise of the hard X-ray flux by several minutes (marked with blue boxes in Figs. 1 and 2, with zoomed-in views of some of them in Fig. 13). We note that they usually occur after optical and X-ray low-flux states. Just at the end of these quiet intervals, the optical and soft X-ray fluxes brighten smoothly during several minutes before a sudden rise is detected in the hard X-ray light curve. As a consequence of this sudden rise, HR1 changes abruptly as well. One possible explanation of this previous soft state could be that an instability in the accretion flow approaches the BH, producing an increase in the optical and soft X-ray emission, and the sudden hardening could represent an ejection event. Previous identification of soft states was made by Radhika et al. (2016) with Swift data for V404 Cyg at some points of the outburst, and these authors explained them as thermal disc emission. A complete spectral analysis and a more detailed discussion of these events will be included in Kajava et al., in prep.

In the overall light curve evolution, these negative-lagged events usually take place before some long positive-lagged flares and before the symmetrical simultaneous double flares reported above (see Figs. 1 and 2). In the picture described before, if the negative-lagged events are caused by an instability propagating through the accretion disk, the instability would eventually enter the corona and could result in discrete jet ejection events. Tetarenko et al. (2017) observed discrete ejections precisely just after one of the negative-lagged events we have identified at MJD 57194.430. If discrete ejections are also produced after the other intervals when the optical and/or soft X-rays precede the hard X-rays (i.e. around MJD 57194.250, and after flares 18, 27, and 34), the presence of some single-lagged optical flares (e.g. flares 21, 22, 32, and 33) and some double symmetric flares (e.g. flares 15–16, 19–20, 24–25, 28–29 and 30–31, and 35–36) that we observed subsequently could be explained by these discrete jet ejections. Some of these single and double optical flares occur simultaneously with the X-ray flares, while others appear delayed with respect to the X-ray flares. Different geometries and ejection angles could help explain the differences between the time delays we found. The comparison with the radio emission during these epochs will be crucial for probing this scenario further.

5. Summary and conclusions

We have studied in detail the simultaneous optical and X-ray observations of the first V404 Cyg 2015 outburst from 18 June to 27 June 2015 performed with the IBIS, JEM-X, and OMC instruments on board the INTEGRAL observatory, complemented with additional data. From our analysis it is clear that the optical emission cannot always be explained by one physical mechanism alone. We classified the flares during the outburst with optical and X-ray observations according to the results of the cross-correlation analysis. We distinguished between the following behaviours.

Simultaneous optical and X-ray emission. For most flares, we have measured time delays that are compatible with no lags between the optical and X-ray emission. We interpret this emission as coming from the same region or from close regions (less than one light–minute distance). Some of these flares display longer optical than X-ray flux decays, which could be produced by synchrotron emission and cooling from the corona or the base of the jet.

Optical emission delayed from the X-rays. We found two different cases in which the optical emission appears to be delayed with respect to the X-rays.

  • Short-lagged optical flares (with lags <2 min). We have observed these lags in single flares and in intervals with flickering (heartbeat-type) oscillations. We interpret these short lags as light travel times when optical emission is due to reprocessing of the X-ray emission in the accretion disc and/or in the companion star. In one of these flickering intervals (MJD 57199.850–57199.905), we observed QPOs with frequencies of several minutes, and we measured optical lags up to 1.5 min. We propose that in this case, the optical lags are probably due to reprocessing of the X-ray emission in the external regions of the accretion disc. The mechanism producing these heartbeat-type oscillations could be related with disc instabilities and/or with the developing of a jet.

  • Long-lagged optical flares (with lags from 3 to 55 min). We propose that some of these events are related to the interaction of discrete jet ejections with wind-ejected material or with previously ejected blobs. In other cases, the optical flares could be produced by reprocessing of the X-rays in the surrounding material. Other flares could correspond to synchrotron emission from discrete jet ejections.

Optical emission preceding the X-ray emission. In some cases we have observed that the optical and soft X-rays brighten before a sudden brightening of the hard X-rays. Lags of ∼11 min have been observed between the two brightenings. These events take place before epochs in which there is radio evidence of jet ejections and/or we have observed optical flares delayed from the X-ray flares by several minutes. We propose that this effect could be produced by some instability propagating in the accretion flow, which could eventually reach the corona and eventually lead to the subsequent observed jet ejections.

From this analysis, we conclude that the optical emission observed for V404 Cyg during the June 2015 outburst is driven by a wide variety of mechanisms, including reprocessing of the X-ray emission into the accretion disc and the companion star, interaction of the ejected material with the surrounding material and/or with previously ejected blobs, and synchrotron emission from the jet. A more detailed multiwavelength analysis of each individual flare, ideally including radio observations and/or spectral information, should be performed to distinguish between the proposed scenarios.

Acknowledgments

The authors would like to thank the referee, Jan-Uwe Ness, for his very valuable comments and suggestions on the original manuscript. This work has been supported by Spanish MINECO grant ESP2015-65712-C5-1-R. This research has made use of data from the INTEGRAL/OMC Archive at CAB (INTA–CSIC), pre-processed by ISDC. PAC is grateful to the Leverhulme Trust for the award of a Leverhulme Emeritus Fellowship. PG thanks STFC (ST/R000506/1) for support. We acknowledge with thanks the variable star observations from the AAVSO and VSNET International Databases contributed by observers worldwide and used in this research.

1

Quiescence studies of V404 Cyg have yielded estimates of the binary inclination in the range 56–67° (Shahbaz et al. 1994; Sanwal et al. 1996), with systematic differences likely due to residual accretion disc contamination, as discussed by Charles et al. (2018). Hence we use a value of ∼60° here.

References

  1. Altamirano, D., Belloni, T., Linares, M., et al. 2011, ApJ, 742, L17 [NASA ADS] [CrossRef] [Google Scholar]
  2. Barthelmy, S. D., Barbier, L. M., Cummings, J. R., et al. 2005, Space Sci. Rev., 120, 143 [NASA ADS] [CrossRef] [Google Scholar]
  3. Barthelmy, S. D., D’Ai, A., & D’Avanzo, P. 2015, GRB Coordinates Network, Circular Service, 17929 [Google Scholar]
  4. Belloni, T., Méndez, M., King, A. R., van der Klis, M., & van Paradijs, J. 1997, ApJ, 479, L145 [NASA ADS] [CrossRef] [Google Scholar]
  5. Casares, J., & Charles, P. A. 1994, MNRAS, 271, L5 [NASA ADS] [CrossRef] [Google Scholar]
  6. Casares, J., Charles, P. A., Naylor, T., & Pavlenko, E. P. 1993, MNRAS, 265, 834 [NASA ADS] [CrossRef] [Google Scholar]
  7. Charles, P., Gandhi, P., & Alfonso-Garzon, J. 2018, 42nd COSPAR Scientific Assembly, 42, E1.4-58-18 [Google Scholar]
  8. Courvoisier, T. J., Walter, R., Beckmann, V., et al. 2003, A&A, 411, L53 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  9. Dallilar, Y., Eikenberry, S. S., Garner, A., et al. 2017, Science, 358, 1299 [NASA ADS] [CrossRef] [Google Scholar]
  10. Dubus, G., Lasota, J., Hameury, J., & Charles, P. 1999, MNRAS, 303, 139 [NASA ADS] [CrossRef] [Google Scholar]
  11. Edelson, R. A., & Krolik, J. H. 1988, ApJ, 333, 646 [NASA ADS] [CrossRef] [Google Scholar]
  12. Fomalont, E. B., Geldzahler, B. J., & Bradshaw, C. F. 2001, ApJ, 558, 283 [NASA ADS] [CrossRef] [Google Scholar]
  13. Gandhi, P., Makishima, K., Durant, M., et al. 2008, MNRAS, 390, L29 [NASA ADS] [CrossRef] [Google Scholar]
  14. Gandhi, P., Blain, A. W., Russell, D. M., et al. 2011, ApJ, 740, L13 [NASA ADS] [CrossRef] [Google Scholar]
  15. Gandhi, P., Littlefair, S., Hardy, L., et al. 2015, ATel, 7686 [Google Scholar]
  16. Gandhi, P., Littlefair, S. P., Hardy, L. K., et al. 2016, MNRAS, 459, 554 [NASA ADS] [CrossRef] [Google Scholar]
  17. Gandhi, P., Bachetti, M., Dhillon, V. S., et al. 2017, Nat. Astron., 1, 859 [NASA ADS] [CrossRef] [Google Scholar]
  18. Gehrels, N., Chincarini, G., Giommi, P., et al. 2004, ApJ, 611, 1005 [NASA ADS] [CrossRef] [Google Scholar]
  19. González Hernández, J. I., Casares, J., Rebolo, R., et al. 2011, ApJ, 738, 95 [NASA ADS] [CrossRef] [Google Scholar]
  20. Harrison, F. A., Craig, W. W., Christensen, F. E., et al. 2013, ApJ, 770, 19 [Google Scholar]
  21. Hynes, R. I. 2010, ArXiv e-prints [arXiv:1010.5770] [Google Scholar]
  22. Hynes, R. I., Haswell, C. A., Cui, W., et al. 2003, MNRAS, 345, 292 [NASA ADS] [CrossRef] [Google Scholar]
  23. Hynes, R. I., Schaefer, B. E., Baum, Z. A., et al. 2016, MNRAS, 459, 3596 [NASA ADS] [CrossRef] [Google Scholar]
  24. Janiuk, A., Grzedzielski, M., Capitanio, F., & Bianchi, S. 2015, A&A, 574, A92 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  25. Jourdain, E., Roques, J., & Rodi, J. 2017, ApJ, 834, 130 [NASA ADS] [CrossRef] [Google Scholar]
  26. Kafka, S. 2018, Observations from the AAVSO International Database, https://www.aavso.org [Google Scholar]
  27. Kajava, J. J. E., Motta, S. E., Sánchez-Fernández, C., & Kuulkers, E. 2018, A&A, 616, A129 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  28. Kanbach, G., Straubmeier, C., Spruit, H. C., & Belloni, T. 2001, Nature, 414, 180 [NASA ADS] [CrossRef] [Google Scholar]
  29. Khargharia, J., Froning, C. S., & Robinson, E. L. 2010, ApJ, 716, 1105 [NASA ADS] [CrossRef] [Google Scholar]
  30. Kimura, M., Isogai, K., Kato, T., et al. 2016, Nature, 529, 54 [NASA ADS] [CrossRef] [Google Scholar]
  31. Kimura, M., Kato, T., Isogai, K., et al. 2017, MNRAS, 471, 373 [NASA ADS] [CrossRef] [Google Scholar]
  32. Kimura, M., Kato, T., Isogai, K., et al. 2018, MNRAS, 475, 3083 [NASA ADS] [CrossRef] [Google Scholar]
  33. King, A. L., Miller, J. M., Raymond, J., Reynolds, M. T., & Morningstar, W. 2015, ApJ, 813, L37 [NASA ADS] [CrossRef] [Google Scholar]
  34. Koljonen, K. I. I., Russell, D. M., Fernández-Ontiveros, J. A., et al. 2015, ApJ, 814, 139 [NASA ADS] [CrossRef] [Google Scholar]
  35. Lewin, W., & van der Klis, M. 2006, Compact Stellar X-ray Sources (Cambridge: Cambridge University Press) [Google Scholar]
  36. Lomb, N. R. 1976, Astrophys. Space Sci., 39, 447 [Google Scholar]
  37. Lund, N., Budtz-Jørgensen, C., Westergaard, N. J., et al. 2003, A&A, 411, L231 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  38. Maitra, D., Scarpaci, J. F., Grinberg, V., et al. 2017, ApJ, 851, 148 [NASA ADS] [CrossRef] [Google Scholar]
  39. Makino, F., Wagner, R. M., & Starrfield, S. 1989, IAU Circ., 4786 [Google Scholar]
  40. Markoff, S., Falcke, H., & Fender, R. 2001, A&A, 372, L25 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  41. Mas-Hesse, J. M., Giménez, A., Culhane, J. L., et al. 2003, A&A, 411, L261 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  42. Migliari, S., Fender, R. P., Blundell, K. M., Méndez, M., & van der Klis, M. 2005, MNRAS, 358, 860 [NASA ADS] [CrossRef] [Google Scholar]
  43. Miller-Jones, J. C. A., Jonker, P. G., Dhawan, V., et al. 2009, ApJ, 706, L230 [NASA ADS] [CrossRef] [Google Scholar]
  44. Mioduszewski, A. J., Rupen, M. P., Walker, R. C., Schillemat, K. M., & Taylor, G. B. 2004, BAAS, 36, 967 [Google Scholar]
  45. Mirabel, I. F., & Rodríguez, L. F. 1998, Nature, 392, 673 [NASA ADS] [CrossRef] [Google Scholar]
  46. Motta, S. E., Kajava, J. J. E., Sánchez-Fernández, C., Giustini, M., & Kuulkers, E. 2017a, MNRAS, 468, 981 [NASA ADS] [CrossRef] [Google Scholar]
  47. Motta, S. E., Kajava, J. J. E., Sánchez-Fernández, C., et al. 2017b, MNRAS, 471, 1797 [NASA ADS] [CrossRef] [Google Scholar]
  48. Muñoz-Darias, T., Martínez-Pais, I. G., Casares, J., et al. 2007, MNRAS, 379, 1637 [NASA ADS] [CrossRef] [Google Scholar]
  49. Muñoz-Darias, T., Casares, J., Mata Sánchez, D., et al. 2016, Nature, 534, 75 [NASA ADS] [CrossRef] [Google Scholar]
  50. Neilsen, J., Remillard, R. A., & Lee, J. C. 2011, ApJ, 737, 69 [NASA ADS] [CrossRef] [Google Scholar]
  51. O’Brien, K., Horne, K., Hynes, R. I., et al. 2002, MNRAS, 334, 426 [NASA ADS] [CrossRef] [Google Scholar]
  52. Oosterbroek, T., van der Klis, M., Vaughan, B., et al. 1996, A&A, 309, 781 [NASA ADS] [Google Scholar]
  53. Radhika, D., Nandi, A., Agrawal, V. K., & Mandal, S. 2016, MNRAS, 462, 1834 [NASA ADS] [CrossRef] [Google Scholar]
  54. Richter, G. A. 1989, Inf. Bull. Variable Stars, 3362, 1 [NASA ADS] [Google Scholar]
  55. Rodriguez, J., Hannikainen, D. C., Shaw, S. E., et al. 2008a, ApJ, 675, 1436 [NASA ADS] [CrossRef] [Google Scholar]
  56. Rodriguez, J., Shaw, S. E., Hannikainen, D. C., et al. 2008b, ApJ, 675, 1449 [NASA ADS] [CrossRef] [Google Scholar]
  57. Rodriguez, J., Cadolle Bel, M., Alfonso-Garzón, J., et al. 2015, A&A, 581, L9 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  58. Russell, D. M., Markoff, S., Casella, P., et al. 2013, MNRAS, 429, 815 [NASA ADS] [CrossRef] [Google Scholar]
  59. Sánchez-Fernández, C., Kajava, J. J. E., Motta, S. E., & Kuulkers, E. 2017, A&A, 602, A40 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  60. Sanwal, D., Robinson, E. L., Zhang, E., et al. 1996, ApJ, 460, 437 [NASA ADS] [CrossRef] [Google Scholar]
  61. Scargle, J. D. 1982, ApJ, 263, 835 [NASA ADS] [CrossRef] [Google Scholar]
  62. Shahbaz, T., Ringwald, F. A., Bunn, J. C., et al. 1994, MNRAS, 271, L10 [NASA ADS] [CrossRef] [Google Scholar]
  63. Shahbaz, T., Russell, D. M., Covino, S., et al. 2016, MNRAS, 463, 1822 [NASA ADS] [CrossRef] [Google Scholar]
  64. Sivakoff, G. R., Bahramian, A., Altamirano, D., et al. 2015, ATel, 7959 [Google Scholar]
  65. Sokolov, A., Marscher, A. P., & McHardy, I. M. 2004, ApJ, 613, 725 [NASA ADS] [CrossRef] [Google Scholar]
  66. Tanaka, Y. T., Itoh, R., Uemura, M., et al. 2016, ApJ, 823, 35 [NASA ADS] [CrossRef] [Google Scholar]
  67. Tetarenko, A. J., Sivakoff, G. R., Miller-Jones, J. C. A., et al. 2017, MNRAS, 469, 3141 [NASA ADS] [CrossRef] [Google Scholar]
  68. Ubertini, P., Lebrun, F., Di Cocco, G., et al. 2003, A&A, 411, L131 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  69. van der Laan, H. 1966, Nature, 211, 1131 [NASA ADS] [CrossRef] [Google Scholar]
  70. van Paradijs, J., & McClintock, J. E. 1994, A&A, 290, 133 [NASA ADS] [Google Scholar]
  71. Wachman, A. 1948, Erg. Astron. Nachr., 11, 42 [Google Scholar]
  72. Wagner, R. M., Starrfield, S. G., Cassatella, A., et al. 1989, IAU Circ., 4783, 1 [NASA ADS] [Google Scholar]
  73. Walton, D. J., Mooley, K., King, A. L., et al. 2017, ApJ, 839, 110 [NASA ADS] [CrossRef] [Google Scholar]
  74. Winkler, C., Courvoisier, T. J., Di Cocco, G., et al. 2003, A&A, 411, L1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  75. Zycki, P. T., Done, C., & Smith, D. A. 1999, MNRAS, 309, 561 [NASA ADS] [CrossRef] [Google Scholar]

Appendix A: Tables

Table A.1.

Flux and temporal properties of the optical flares identified.

Table A.2.

Time delays measured from the DCF for each optical flare.

All Tables

Table A.1.

Flux and temporal properties of the optical flares identified.

In the text
Table A.2.

Time delays measured from the DCF for each optical flare.

In the text

All Figures

thumbnail Fig. 1.

Optical and X-ray light curves of V404 Cyg during the June 2015 outburst from MJD 57191.75 to MJD 57196.00. The optical observations are plotted in red, the soft X-ray emission in the 3–10 keV band is plotted in orange, and the hard X-ray emission in the 20–80 keV band for INTEGRAL/IBIS and in the 10–79 keV band for the NuSTAR observations are plotted both in green. The numbers in black refer to the optical flare identifications. Brown and blue boxes mark flares with positive and negative lags, respectively. Light green boxes represent double symmetric optical flares with simultaneous X-ray emission. Purple boxes represent epochs where heartbeat-type oscillations are observed (see text).
In the text
thumbnail Fig. 2.

Same as Fig. 1, but from MJD 57196.75 to MJD 57200.25. Grey dashed lines mark the initial and end times of the NuSTAR observations.
In the text
thumbnail Fig. 3.

Histogram of the duration of the optical flares during the June 2015 outburst of V404 Cyg. Bins of 5 min are used.
In the text
thumbnail Fig. 4.

ΔFrise/ΔFdecay vs. Δtrise/Δtdecay ratios for all the optical flares identified in this work. Dashed lines mark where these properties are symmetrical. Colour-coding according to the optical/X-ray lags (see Sect. 3.2): zero-lagged flares (green points), positive-lagged flares (red triangles), negative-lagged flares (blue stars), frequency-dependent lagged flares (inverted purple triangles), and uncertain (grey squares). Flare numbers of highly asymmetric flares with longer time decays are labelled.
In the text
thumbnail Fig. 5.

Fading vs. rising flux rates; the dashed line marks where the rates are equal. Flares numbers that deviate from this relation by more than 1σ are marked.
In the text
thumbnail Fig. 6.

Histogram of the measured lags between the optical and soft X-rays (3–10 keV; top), optical and hard X-rays (20–80 keV for INTEGRAL data, 10–79 keV for NuSTAR data; middle), and optical and very hard X-rays (80–200 keV; bottom). The bin size is 1 min.
In the text
thumbnail Fig. 7.

Histogram of the hardness ratios: HR1 (solid orange) and HR2 (dark blue striped). The bin size is 0.025. N is the number of observations within each hardness ratio bin.
In the text
thumbnail Fig. 8.

Zoomed-in optical and X-ray light curves where optical flares are essentially simultaneous with X-ray flares (optical is shown in red, soft X-ray (3–10 keV) in orange, hard X-ray (20–80 keV for ISGRI, or 10–79 keV for NuSTAR) in green, and very hard X-ray (80–200 keV) in dark blue). For each subplot, the HRs (HR1 is plotted in orange, and HR2 in dark blue) and the DCFs (optical ACF is shown in red, optical/soft X-ray DCF in orange, optical/hard X-ray DCF in green, and optical/very hard X-ray in dark blue) are shown below the light curves. The variation in behaviour is discussed in the text.
In the text
thumbnail Fig. 9.

Same as in Fig. 8, but for flares with optical emission following the X-rays with short lags (<2 min).
In the text
thumbnail Fig. 10.

Same as in Fig. 8, but for some regions showing heartbeat-type oscillations.
In the text
thumbnail Fig. 11.

Same as in Fig. 8, but for flares with optical emission following the X-rays with long lags (>2 min).
In the text
thumbnail Fig. 12.

Same as in Fig. 8, but for complex cases in which there are several optical flares that follow the X-rays.
In the text
thumbnail Fig. 13.

Same as in previous figures, but for cases in which the optical and soft X-ray emission precedes the hard X-rays.
In the text
thumbnail Fig. 14.

Same as in Fig. 8, but for a flare with energy-dependent optical/X-ray lags.
In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.