An Application of Hilbert-Huang Transform on the Non-Stationary Astronomical Time Series: The Superorbital Modulation of SMC X-1

Journal of Astronomy and Space Sciences.
2013.
Jun,
30(2):
79-82

This is an open Access article distributed under the terms of the Creative Commons Attribution Non-Commercial License (http://creativecommons.org/licenses/by-nc/3.0/) which premits unrestricted non-commercial use, distribution, and reproduction in any medium, provided the original work is properly cited.

- Received : November 11, 2012
- Accepted : December 12, 2012
- Published : June 15, 2013

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We present the Hilbert-Huang transform (HHT) analysis on the quasi-periodic modulation of SMC X-1. SMC X-1, consisting of a neutron star and a massive companion, exhibits superorbital modulation with a period varying between ~40 d and ~65 d. We applied the HHT on the light curve observed by the All-Sky Monitor onboard
Rossi X-ray Timing Explorer
(
RXTE
) to obtain the instantaneous frequency of the superorbital modulation of SMC X-1. The resultant Hilbert spectrum is consistent with the dynamic power spectrum while it shows more detailed information in both the time and frequency domains. According to the instantaneous frequency, we found a correlation between the superorbital period and the modulation amplitude. Combining the spectral observation made by the Proportional Counter Array onboard
RXTE
and the superorbital phase derived in the HHT, we performed a superorbital phase-resolved spectral analysis of SMC X-1. An analysis of the spectral parameters versus the orbital phase for different superorbital states revealed that the diversity of
n_{H}
has an orbital dependence. Furthermore, we obtained the variation in the eclipse profiles by folding the All Sky Monitor light curve with orbital period for different superorbital states. A dip feature, similar to the pre-eclipse dip of Her X-1, can be observed only in the superorbital ascending and descending states, while the width is anti-correlated with the X-ray flux.
_{⊙}
neutron star (van der Meer et al. 2007) and a 17.2 M
_{⊙}
supergiant (Reynolds et al. 1993). The orbital period of this system is ~3.89 d obtained from the X-ray eclipse. Gruber & Rothschild (1984) found that the SMC X-1 exhibits an X-ray periodicity with a rough time scale of 60 d. This periodicity was then confirmed by Wojdowski et al. (1998) and the cycle lengths were reported to vary with time. The behavior of the period variation was investigated after several timefrequency analysis techniques, like the dynamic power spectrum (Clarkson et al. 2003) and the slide Lomb-Scargle periodogram (Trowbridge et al. 2007), were applied on the All-Sky Monitor (ASM) light curve. We present our analysis by using of a recently developed time-frequency analysis technique, the Hilbert-Huang transform (HHT), to explore the timing properties of the superorbital modulation. Furthermore, based on the phase defined in the HHT, the superorbital phase-resolved analysis on both the spectral behaviors and the variation of orbital profiles are also presented.
Rossi X-ray Timing Explorer
(
RXTE
) with ~ 90 minute timing resolution, were used to explore the detailed variation of orbital profile of SMC X-1. The data were further binned into one-day light
The Hilbert spectrum and the dynamic power spectrum of SMC X-1.
curve to investigate the variation of superorbital period. Furthermore, the data collected by the Proportional Counter Array (PCA) onboard
RXTE
were also included to obtain the variation of spectral behavior in the different superorbital states.
Folded light curve of superorbital modulation of SMC X-1.
The correlation between the superorbital modulation period and the amplitude. The rank correlation coefficient is r = 0.46 with a null hypothesis probability value of 3.2 × 10^{-6}.
between the modulation period and the amplitude shown in
Fig. 3
. This correlation is similar to that between the main-on flux and the superorbital period of Her X-1 (Still & Boyd 2004). Both of the examples are inconsistent with the prediction of radiation-induced warp disk (Wijers & Pringle 1999).
The unabsorbed flux (top panel), nH (middle panel) and power-law index (bottom panel) verse the superorbital phase. Black, blue, red, and green symbols represent the spectral parameters in the low, ascending, high, and descending states, respectively.
variation of the uneclipsed hydrogen column density (
n_{H}
) versus the superorbital phase is shown in the middle panel of
Fig. 4
. We noticed that the
n_{H}
values show great diversity in the ascending state but remain stable in the descending state. By further checking the orbital distribution of
n_{H}
in the different superorbital states, we obtained that the diversity might be caused by the dip feature occurred in orbital phase ~ 0.7.
The dip feature could be further examined by the folded light curve. Since the appearance of dip may have superorbital dependence, a two-dimensional folded light curve is a good way to investigate the dip properties. We perform this analysis method on the dwell light curve collected by the ASM. We first folded the X-ray photons in the data window of superorbital phase 0.0-0.05 according to the orbital ephemeris proposed by Wojdowski et al. (1998)
Two-dimensional dynamic folded light curve of SMC X-1.
and normalized the uneclipsed count rate to 1. Then, we move the window 0.01 superorbital cycles forward to obtain the next orbital profile. This process was repeated until the end of the data set. The combined folded light curve, drawn in a three-dimensional color map, is shown in
Fig. 5
. We can easily obtain the dip feature in the dynamic folded light curve, especially that occurred in superorbital descending state. From this figure, we also noticed that the dip width has an anti-correlation with the X-ray count rate. This dip feature could be associated with the pre-eclipse dip of Her X-1 (Moon & Eikenberry 2001).
n_{H}
and the orbital profile indicate that the system contains a pre-eclipse dip. The width variation of the dip can be interpreted by the warp and tilted disk model.

1. INTRODUCTION

The high-mass X-ray binary SMC X-1 consists of a 1.06 M
2. OBSERVATIONS

The dwell data, collected by the ASM onboard
Lager Image

3. THE HILBERT-HUANG TRANSFORM

The HHT, which is proposed by Huang et al. (1998), is designed to analyze the non-linear and non-stationary time series. The normalized Hilbert transform was used to obtain the instantaneous frequency of the superorbital modulation. However, the Hilbert transform can only be applied on the intrinsic mode functions (IMFs) to get meaningful instantaneous frequency. We used the ensemble empirical mode decomposition, proposed by Wu & Huang (2009), to decompose the ASM light curve into several IMFs.
4. TIME-FREQUENCY ANALYSIS

After decomposing the light curve into several IMFs, we applied the normalized Hilbert transform on them to obtain the Hilbert spectrum.
Fig. 1
shows the Hilbert spectrum that contains information of frequency and amplitude variation in a color map, which is stacking with the dynamic power spectrum in contour for comparison. We noticed that the Hilbert spectrum is basically consistent with the dynamic power spectrum, but the resolutions are better in both the time and frequency domains. Since the HHT provided us a well-defined phase of the superorbital modulation, we folded the light curve according to the superorbital phase to obtain the asymmetric superorbital profile, which is shown in
Fig. 2
. Furthermore, we obtained a significant correlation
Lager Image

Lager Image

5. SUPERORBITAL PHASE-RESOLVED ANALYSIS

We further studied the superorbital phase-resolved spectroscopic properties of SMC X-1 by using all the PCA observations during 1996 and 2004. The standard-2 mode spectrum can be fitted with a cutoff power law continuum and a Gaussian emission line centered at 6.4 keV. The
Lager Image

Lager Image

6. CONCLUSIONS

This research demonstrated a time-frequency analysis of the non-stationary superorbital modulation of SMC X-1 by the HHT. The Hilbert spectrum shows great detail in both the time and frequency domains. Furthermore, we found a correlation between the superorbital period and amplitude, which is inconsistent with the outer warp model. Based on the phase derived in the HHT, we studied the phaseresolved spectra and the variation of orbital profile. The variation in both the
Acknowledgements

This research made use of theRXTE/PCAdata provided by the High Energy Astrophysics Science Archive Research Center of NASA’s GSFC. The data collected by the ASM were provided by the ASM/RXTE teams at MIT and at the RXTE SOF and GOF at NASA’s GSFC. This research was supported by grant NSC 97-2112-M-008-012-MY3, NSC 100-2119-M- 008-025, and NSC 101-2112-M-008-010 from the National Science Council of Taiwan.

Reynolds AP
,
Hilditch RW
,
Bell SA
,
Hill G
(1993)
Optical spectroscopy of the massive X-ray binary SM X-1/Sk 160
MNRAS
261
337 -
345

Citing 'An Application of Hilbert-Huang Transform on the Non-Stationary Astronomical Time Series: The Superorbital Modulation of SMC X-1
'

@article{ OJOOBS_2013_v30n2_79}
,title={An Application of Hilbert-Huang Transform on the Non-Stationary Astronomical Time Series: The Superorbital Modulation of SMC X-1}
,volume={2}
, url={http://dx.doi.org/10.5140/JASS.2013.30.2.079}, DOI={10.5140/JASS.2013.30.2.079}
, number= {2}
, journal={Journal of Astronomy and Space Sciences}
, publisher={The Korean Space Science Society}
, author={Hu, Chin-Ping
and
Chou, Yi
and
Wu, Ming-Chya
and
Yang, Ting-Chang
and
Su, Yi-Hao}
, year={2013}
, month={Jun}