{'fraction_non_alphanumeric': 0.0446142338106433, 'fraction_numerical': 0.036439410130369734, 'mean_word_length': 3.9739569492426257, 'pattern_counts': {'":': 0, '<': 0, '<?xml version=': 0, '>': 0, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 0, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
Orbital modulations of X-ray light curves of Cygnus X-1 in its low/hard and high/soft states

The black hole binary Cygnus X-1 has a 5.6 day orbital period. We first detected a clear intensity modulation with the orbital period in its high/soft state with 6 year MAXI data, as well as in its low/hard state. In the low/hard state, the folded light curves showed an intensity drop at the superior conjunction of the black hole by a modulation factor (MF), which is the amplitude divided by the average, with 8+-1%, 4+-1% and 3+-2% for 2-4 keV, 4-10 and 10-20 keV bands, showing a spectral hardening at the superior conjunction of the black hole. Spectral analysis with a model consisting of a power law and a photoelectric absorption, showed that the hydrogen column density increased from (2.9+-0.4)E+21 to (4.7+-1.1)E+21 cm^-2 around the superior conjunction, although more complex spectral variation, such as a partial absorption, was suggested, and the flux of the power law component decreased with 6+-1%. On the other hand, the MFs of the folded light curves in the high/soft state, were 4+-1% and 4+-2% for 2-4 keV and 4-10 keV bands, respectively. We applied a model consisting of a power law and a diskblackbody with a photoelectric absorption and found a modulation of the flux of the power law component with 7+-5% in MF, while the modulation of the hydrogen column density was less than 1E+21 cm^-2. These results can be interpreted as follows; the modulation of both states can be mainly explained by scattering of the X-rays by an ionized stellar wind, but only at the superior conjunction in the low/hard state, a large photoelectric absorption appears, because of a low ionization state of the wind in the line of sight at the phase. Such a condition can be established by reasonable parameters of an in-homogeneous wind and the observed luminosities.


Introduction
The black hole (hereafter BH) binary Cygnus X-1 (hereafter Cyg X-1) is persistently bright in the X-ray band. It shows typically two spectral states (Oda 1977;Remillard & McClintock 2006;Done et al. 2007), the low/hard state (hereafter LHS) which is dominated by a power law spectrum with a high energy cutoff, and the high/soft state (hereafter HSS) which is dominated by optically-thick thermal emission from an accretion disk, i.e. the standard-disk (Shakura & Sunyaev 1973;Tanaka & Shibazaki 1996;Remillard & McClintock 2006;Done et al. 2007). Cyg X-1 repeats transitions between the two states in several days to several hundred days. The companion, HDE 2268968, is a O9Iab super giant star. An orbital period of the binary is 5.6 days (Mason et al. 1974;Bolton 1975) and the inclination angle is 27 • (Orosz et al. 2011). A strong stellar wind from the companion star is captured by the black hole and probably forms a characteristic structure around the black hole like a focused wind (Friend & Castor 1982). The wind exposed by luminous X-rays should be ionized and also considered to be clumpy (Bałucińska-Church et al. 2000;Feng & Cui 2002).
Although an eclipse is not seen in the X-ray light curve, an orbital modulation in the X-ray intensity has been observed in its LHS (Priedhorsky et al. 1995;Wen et al. 1999;Kitamoto et al. 2000;Miškovičová et al. 2016), especially in the low energy band. However, the intensity modulation has not been detected in the HSS (Wen et al. 1999;Brocksopp et al. 1999a). Boroson & Vrtilek (2010) reported that a peak of 5.61 d in the periodogram of the hardness ratio was detected during a part of the HSS period, using the RXTE/ASM data, but it was weaker than that in the LHS.
The absorption dip was first detected in the LHS (Li & Clark 1974), which is an abrupt intensity drop in the soft X-ray band around the superior conjunction of the BH. Various depth and the duration of dips have been observed (Kitamoto et al. 1984;Bałucińska-Church et al. 2000). The duration of the dip is distributed from several seconds to more than 10 min. The probability of the 2 dip is high around superior conjunction, at phase 0.9 − 0.1. The cause of the dips is interpreted by an absorption by clumpy and in-homogeneous stellar wind (Kitamoto et al. 1984;Boroson & Vrtilek 2010;Miškovičová et al. 2016). Yamada et al. (2013) discovered a dip during the HSS by a Suzaku/XIS observation. They detected Fe absorption edge at 7.5 keV and He-like and H-like Fe−K α absorption lines in the energy spectrum around the dip, indicating absorption by a highly ionized wind.
In order to clarify the wind condition and its difference between the two states, we analyzed more than 6 yr observational data with Monitor of All sky X-ray Image (MAXI) (Matsuoka et al. 2009) and compared the orbital modulation in the LHS and the HSS.

Observation
MAXI is attached to the International Space Station. As the International Space Station orbits the earth in every 92 min, MAXI scans over nearly the entire sky with two kinds of X-ray cameras: the Gas Slit Camera (GSC: Mihara et al. 2011) covering the energy band of 2 − 20 keV, and the Solidstate Slit Camera (SSC: Tomida et al. 2011) covering 0.7 − 7 keV. The long term variation of Cyg X-1 using the same data has been reported by Sugimoto et al. (2016) (hereafter Paper I). The data extraction-criteria and observation details are described in Paper I. The power spectra in 2 − 4 keV in the LHS and the HSS are shown in figure 1 (b) and (c), whose data spans for the calculations were 55058-55376(MJD) and 56130-56607(MJD), respectively.
The peak of 5.6 d orbital period is clearly seen in the LHS, but, in the HSS, the signal is weak and splits into plural peaks (see Paper I for detail). Some peaks in the HSS, which are larger than that of 5.6d, are instrumental fakes.

Folded light curves and hardness ratios
We use the orbital period, P orb = 5.599829 ± 0.000016 d, and an epoch of the inferior conjunction of the O-star, T 0 = 41874.207 ± 0.009MJD, which were obtained by Brocksopp et al. (1999b). Even if P orb has the maximum error of 0.000016d, the difference of the orbital phase at the MAXI observation

Phase resolved spectrum analysis
In order to parameterize the spectral modulation, we performed a model fitting of the extracted spectra. We divided the orbital phase into ten phase intervals and extracted ten spectra for each state and for each of the GSC and SSC. The GSC and SSC spectra cover 2 − 20 keV and 0.7 − 7 keV bands, respectively. As examples, the spectra in the phase 0.0 − 0.1 and 0.5 − 0.6 in the LHS and HSS are plotted in figure 4 with their best fit models described below. The 1.5-2 keV range of the SSC was excluded to avoid the known systematic uncertainty in the effective area (see Paper I).

Spectral model fitting result in the LHS
First, we fitted a power law (powerlaw) model with a photoelectric absorption (phabs) to the GSC and the SSC spectra in the LHS. We added systematic errors of 1% to both the GSC and SSC data for taking account of uncertainty of the calibration. The resultant reduced χ 2 values ranged from 0.9 6 to 2.1, and best-fit models in several phase intervals were still not acceptable. It was thought that the applied model was not appropriate enough. Because an application of more sophisticated model would be beyond the scope of this work, we increased the systematic error to 5%, so as to include the model uncertainty. Then reduced χ 2 values became less than 1.3. The obtained parameters were plotted in figure 5 (a). As the errors were large, we did not recognize a modulation of the hydrogen column density, N H , and of the powerlaw flux in 10 −20 keV, but we found a modulation of the power law index. On the other hand, in figure 5 (b), we plotted the best-fit parameters obtained from the fitting of the GSC data only. The GSC results indicate that the power law index is not modulating within ±0.05 and N H shows a modulation. The average value of the power law index is 1.66 ± 0.02.
These facts mean that the SSC data shows an modulation which can not be well described by a simple absorption model, suggesting an partial absorption or an existence of a low temperature disk component. However, since the farther investigation of the complex spectral shape is not easy by our data, we applied again the model, phabs*powerlaw, with a fixed power law index of 1.66, which is the value determined by the GSC. Therefore the complex spectral variation of the low energy part is all approximately expressed by a change of N H . The best fit parameters were shown in figure 5 (c).
We found a marginal suggestion of an increase of N H around phase 0 with ∆N H = (1.8 ± 1.2) × 10 21 cm −2 (from (2.9 ± 0.4) × 10 21 cm −2 to (4.7 ± 1.1) × 10 21 cm −2 ). We also found that the powerlaw flux, in the 10-20 keV band, had a modulation with MF = 6 ± 1%. The large reduced χ 2 values around phase 0 suggest that spectra around phase 0 was not simulated well by the simple power law model and may need more complex model, such as a partial absorption model, due to averaging of many spectra with various N H values. The value of N H obtained from our analysis is smaller than those in previous works by Kitamoto et al. (1984) (N H = 5 × 10 21 ∼ 2 × 10 22 cm −2 ) and Grinberg et al. (2015) (N H = 1 × 10 22 ∼ 2 × 10 22 cm −2 ). Since our data covers down to 0.7 keV, the possible partial absorption may affect the resultant N H values to be small with more sensitivity than the above previous reports. This is supported by the figure 5 (b), where the N H around phase 0, obtained with the GSC only, is ∼ 1 × 10 22 cm −2 .

Spectral model fitting result in the HSS
The spectra in the HSS were first fitted by a model, phabs*(powerlaw+diskbb+gausian), where diskbb is a multi-color disk model (Mitsuda et al. 1984) and gaussian is for a Fe-K emission line.
As with the LHS, we added 1% systematic errors. The reduced χ 2 values were all less than 1.3, indicating reasonable fittings. Best fit parameters are shown in figure 6 (a). In the HSS, N H did not increase around phase 0 and the variation was not more than 1 × 10 21 cm −2 . The innermost radius and temperature of the disk component were ∼ 40 km and ∼ 0.5 keV, where we assumed the distance 7 of 1.86 kpc and the inclination of 27 • (Orosz et al. 2011). We did not find modulation of them. The modulation of the powerlaw flux was 7 ± 5% in MF . Here, we should note that the power law index is ∼ 3. Such a steep powarlaw model affects the spectra in the low energy band, where it is not realistic. Then, we substituted a "simpl" model, (phabs*simpl*(diskbb+gaussian)), which is an empirical model of Comptonization : a fraction of photons in an input seed spectrum is scattered into a power law component (Steiner et al. 2009). The best fit parameters are plotted in figure 6 (b). The change of N H was again less than 1 × 10 21 cm −2 , and the absolute values became small. The modulation of the flux in the 10 − 20 keV was again 7 ± 3% in MF . So far the orbital modulation of N H in the HSS was only reported by Grinberg et al. (2015). They reported that their data was still poor and their derived values of N H had large scatting with 2 ∼ 3 × 10 22 cm −2 on the average and 0 ∼ 3 × 10 22 cm −2 on the median, and no clear orbital modulation was reported.

Orbital Modulation
We first clearly detected the orbital modulation of the X-ray intensity in the HSS, which was an energy independent modulation with MF of roughly 4% up to 10 keV. In the 10 − 20 keV band, data was not in-consistent with the same amount of the modulation. On the other hand, in the LHS, an enhanced low energy modulation was notable below 4 keV, overlapping to the energy-independent modulation with MF of ∼ 4%. A reasonable interpretation is that the stellar wind is almost ionized and electron scatterings by the ionized wind make the energy independent modulation. In the LHS, the wind in the line of sight at the superior conjunction of the BH is not ionized enough and the photoelectric absorption is observed. Our data showed the increase of N H around the phase 0 in the LHS as (1.8 ± 1.2) × 10 21 cm −2 for fitting with powlaw model on the condition that the parameters of the photon index was fixed. This value was, however, smaller than the previous reports of the absorption dips, for example, 10 23 cm −2 as reported by Grinberg et al. (2015) and Kitamoto et al. (1984). It is also known that the dip depth and the dip duration have wide variety ( (b) The model fitting to the GSC and the SSC spectra with phabs*simpl*(diskbb+gaussian).
highly ionized in the HSS, but some blob-like structure with high density may still enhance the low energy absorption in a short time, and make the "so-called" absorption dip with a spectral hardening.
Since our data did not show the increase of the N H around phase 0 in the HSS, we should consider that the "so-called" absorption dip is rare in the HSS.

Density of stellar wind
We examined whether our finding of the roughly sinusoidal and energy-independent modulation can be explained by a reasonable wind-parameters or not. Although an actual wind has a complex structure such as the focusing wind (e.g. Miškovičová et al. 2016), in this work we concentrate only the overall sinusoidal modulation with the 3 ∼ 4% amplitude and assume a much simple toy model. We used the wind parameters reported by Vrtilek et al. (2008), and the inclination reported by Orosz et al. (2011), listed in table 1. We assumed that the wind is spherically symmetric, and thus the wind density, n(r), at the distance, r, from the companion star can be expressed as whereṀ is the mass loss rate as the stellar wind, m H is the mass of the hydrogen atom and v(r) is the wind velocity. If we express the ionization fraction of Hydrogen as κ, the electron column density, N e , can be calculated as where the integral is performed along the line of sight, dl, from the BH to the observer. If we approximate the wind velocity as a constant value with the terminal velocity, v ∞ , and the ionization fraction κ(l) is constant as κ 0 , the integral can be reduced as cos χ = sin i cos θ where χ is the angle between the line of sight and the line joining the centers of two stars, represented as cos −1 (sin i cos θ), i is the inclination angle and θ is the orbital phase. Since the wind condition may change between two states, we introduce a parameter η = κ 0Ṁ /Ṁ 0 v∞/v ∞,0 , whereṀ 0 and v ∞,0 are the values as listed in table 1.
Using the parameters listed in table 1 and the Thomson scattering cross section, σ T , we can calculate an optical depth for the electron scatting. The intensity variation can be roughly expressed as I = I 0 exp (−N e σ T ), as long as the optical depth is small, where I 0 is the original intensity from near the BH. In figure 7, the expected light curves for the several cases (0.5, 1, 2, 5) of the parameter

Parameter
Value Reference Mass loss rate (Ṁ0) ∼ 5 × 10 −6 M⊙ yr −1 (Vrtilek et al. 2008) Terminal velocity (v∞,0) ∼1400 km s −1 (Vrtilek et al. 2008) β of the CAK * wind model ∼0.75 (Vrtilek et al. 2008) Stellar radius (R * ) ∼ 1.5 × 10 12 cm (Vrtilek et al. 2008) Separation of the binary (a) ∼ 3.0 × 10 12 cm (Vrtilek et al. 2008) Inclination of the binary (  η are plotted as well as the observed folded light curves. All the curves were adjusted to be one at the peak intensity. Except for the light curve in the energy range 2 − 4 keV around phase 0 in the LHS, the light curves were able to be simulated with the parameter η = 2.0 (N e = (0.8 − 1.6) × 10 23 cm −2 ), in both states. This suggests that the stellar wind parameter, η, does not change between the two states within the precision of our observation. The notable discrepancy was seen around the phase 0 in the low energy band of the LHS. This is interpreted that the amount of the photoelectric absorption increases but that of electron scattering is not. Therefore, just on the line of sight around the phase 0, the ionization state of the stellar wind is low in the LHS comparing to that of HSS. Grinberg et al. (2015) calculated the wind column density of 3 ∼ 5 × 10 22 cm −2 , using more realistic model assuming the focusing wind, CAK wind model and parameters reported by Gies & Bolton (1986). Although our model is a simple toy model, the obtained parameter, N e ∼ 10 23 cm −2 , requires two of three times higher values than the above model parameters, i.e. slow velocity or high mass loss rate.

Stellar wind model
The ionization should be due to the photoionization by intense X-rays from near the BH. In such a case, the ionization state can be estimated by the ionization parameter, ξ = Lx nd 2 , where L x is the X-ray luminosity of the compact source, n is the ion density and d is the distance from the compact source (Tarter et al. 1969). According to the calculation of the model 6 and 7 by Kallman & McCray (1982), an ionization front of the He can be seen around ξ ∼ 30. If ξ exceeds 30, the majority of the metal is ionized, but if ξ is less than 30, substantial amount of the metal is not ionized and the absorption by metal becomes notable.
From the fitting result of the energy spectrum, we obtained that the luminosity in 0.7 − 7 keV was 0.4 × 10 37 erg s −1 and 2.4 × 10 37 erg s −1 for the LHS and HSS, respectively. This six times difference of the luminosity should make the difference of the ionization state of the wind between the two states. On the other hand, we considered that the energy independent intensity modulation is caused by the electron scattering and the parameter η is about 2 for the both states. Except for phase 0 of the LHS, we did not detect any orbital modulation of the amount of the photo-electric absorption in spite of non-spherical-symmetry of the wind column density seen from the BH. Therefore, we can assume, as a first approximation, that the ionization state of the wind is enough high and the unknown parameter κ 0 = 1. Then we can examine the ionization parameter at the nearest point of the companion star along the line of sight at the phase 0, using the parameters listed in table 1 and the η of 2, as where L x,38 is the X-ray luminosity with an unit of 10 38 erg s −1 . Therefore the wind is ionized well at the point in the HSS (L x,38 ∼ 0.24) . In the LHS (L x,38 ∼ 0.04), however, a delicate balance between the luminosity and the density leads large variation of the ionization state around the phase 0. Various high density blobs, in an in-homogeneous wind work as photoelectric absorbers around the superior conjunction of the BH, and cause the various dips in the LHS. In the other phase, most of the wind in the LHS, as well as the HSS, is ionized, and this is consistent to the high resolution observation in the LHS (Miškovičová et al. 2016). 13