Long-Term Optical and Spectral Variability of FSRQ 3C454.3.
Blazars show some extreme properties, such as violently optical variability, core dominance, and superluminal motion [1, 2]. Blazars can be divided into two subclasses: BL Lacs and FSRQs (flat spectrum radio quasars). BL Lacs are characterized by featureless optical spectra or weak emission line , and FSRQs are composed of the flat-spectrum radio spectrum and show typically broad emission lines .
Blazars have relativistic jets. Their jets can produce the nonthermal emission, which can dominate the total observed emission. Many works analyzed the relations between spectral indices (or spectrum) and flux densities (or brightness) (e.g., [4-10]). Those studies can explain the reasons behind the characteristic of blazar variability and can also help us to constrain the emitting region. BL Lacs and FSRQs show different correlations. Generally, BL Lacs show that when the sources become brighter, the spectrums become harder and when the sources become fainter, the spectrums become softer. FSRQs show that when the sources become brighter, the spectrums become softer (redder). The redder when-brighter (RWB) behavior of FSRQs can be explained as the contribution from less variable, bluer accretion disk to the variable, redder jet emission.
Kirk and Mastichiadis (1999)  put forward that, for blazars, the spectral shape can be influenced by the synchrotron particle acceleration and synchrotron cooling. The spectral shape can reflect the intrinsic variability of jet [12-15]. Fiorucci, Ciprini, and Tosti (2004)  pointed out that the optical spectrum of QSOs (subclass of Active Galactic Nuclei) consisted of two components, the first one was variable ([[alpha].sub.v], with a flatter slope), which came from synchrotron emission, and the other part was stable ([[alpha].sub.s]), which might come from the thermal emission. Fan et al. (2014)  pointed out that the correlation between brightness and spectral index can be influenced by the brightness intensity.
For blazars, the optical variable timescales can divide into three types: (1) the intraday variability (IDV), with the timescales from minutes to hours; (2) short-term variability, with the timescales of days; and (3) long-term variability, which are generally periodic, with the timescales from months to years . The variable timescales can help us to study the physical processes of blazars. The IDV timescales can constrain the size of the emitting region. The long-term periodicity can give us the information about the central black hole mass of the blazars. For example, based on a slim disk, the periodicity can be determined as P/yr = 9.0[delta][([alpha]/0.1).sup.-0.62]([M.sub.BH]/[10.sup.6][M.sub.(x)]) , where a is the viscosity coefficient and P is the periodicity, in unit of years.
FSRQ 3C454.3 (z=0.859, ) displays strong variabilities over the entire electromagnetic bands (e.g., [20-25]). Based on the B-band lightcurve, Webb et al. (1988)  obtained three periodicities, 0.8, 3.0, and 6.4 years. Based on the University of Michigan Radio Astronomy Observatory (UMRAO) database, Ciaramella et al. (2004)  obtained a periodicity of 6.3 [+ or -] 0.2 years and Fan et al. (2007)  obtained two periodicities, 4.6 [+ or -]0.1 years and 6.3 [+ or -] 0.2 years. Based on UMRAO and MRO (Metsdhovi Radio Observatory database), Kudryavtseva and Pyatunina (2006)  obtained two periodicities, [P.sub.1] = 6.2 [+ or -] 0.1 years and [P.sub.2] = 12.4 [+ or -] 0.6 years. Woo et al. (2002)  availed the optical luminosity to calculate the central black hole mass being 1.47 x [10.sup.9][M.sub.(x)], where [M.sub.(x)] is the solar mass.
This paper is arranged as follows: in Section 2, we introduce observations and data reductions; in Section 3, results are proposed; Section 4 includes discussion and conclusion.
2. Observations and Data Reductions
The data used in this work are collected from the Small and Moderate Aperture Research Telescope System (SMARTS), which is located at the Cerro Tololo Inter-American Observatory (CTIO) in Chile. The data reduction and processing had been described by Brown et al. (1989)  and Bonning et al. (2012) .
For 3C454.3, the monitoring time is in the range from June 23, 2008 to November 30, 2015, and the observations cover five optical and near-IR bands, B, V, R, J, and K bands. The BVRJK lightcurves have been shown in Figure 1, which are built by
(1) 753 observations at B band, within [DELTA][T.sub.B] [approximately equal to] 1015 days, the largest variations [DELTA]B = 3.37 [+ or -] 0.08 mag (from 17.34 [+ or -] 0.12 mag to 13.96 [+ or -] 0.002 mag);
(2) 739 observations at V band, within [DELTA][T.sub.V] [approximately equal to] 1014 days, the largest variations [DELTA]V = 3.31 [+ or -] 0.07 mag (from 16.76 [+ or -] 0.10 mag to 13.45 [+ or -] 0.002 mag);
(3) 745 observations at R band, within [DELTA][T.sub.R] [approximately equal to] 679 days, the largest variations [DELTA]R = 3.62 [+ or -] 0.12 mag (from 16.59 [+ or -] 0.17 mag to 12.97 [+ or -] 0.002 mag);
(4) 744 observations at J band, within [DELTA][T.sub.J] [approximately equal to] 763 days, the largest variations [DELTA]J = 4.08 [+ or -] 0.01 mag (from 15.09 [+ or -] 0.019 mag to 11.01 [+ or -] 0.004 mag);
(5) 680 observations at K band, within [DELTA][T.sub.K] [approximately equal to] 2715 days, the largest variations [DELTA]K = 5.03 [+ or -] 0.03 mag (from 14.26 [+ or -] 0.03 mag to 9.24 [+ or -] 0.002 mag).
3.1. Periodicity Analysis. It is very important to choose suitable methods to analyze the long-term optical variability. Considering the uneven lightcurves, we avail the power spectrum to deal with this question and choose the common part as the quasiperiodicity.
The mostly common tool for periodicity analysis of both evenly and unevenly sampled signals is the Periodogram method, which is an estimator of the signal energy in the frequency domain by Deeming (1975) . Lomb (1976)  introduced a modified form of this method, and additionally it was elaborated by Scargle (1982) , which can be described in the following. Considering a series x(n) with N points, f is the frequency and r is a variable timescale. Their mean and deviation are given by [bar.x] = (1/N) [[summation].sup.N.sub.n=1] x(n) and [[sigma].sup.2] = (1/N) [[summation].sup.N.sub.n=1] [(x(n) - [bar.x]).sup.2]. The normalized Lomb's [P.sup.L], i.e., the power spectrum as a function of the angular frequency [omega] = 2[pi]f >0 is defined as
[mathematical expression not reproducible] (1)
and [tau] is defined by the equation:
tan (2[omega][tau]) = [[summation].sup.N-1.sub.n=0] sin 2[omega][t.sub.n]/[[summation].sup.N-1.sub.n=0] cos 2[omega][t.sub.n] (2)
The errors of the period are estimated by the half width at half-maximum (HWHM) of the minimum standard deviation ([V.sup.2.sub.m]). We use the Periodogram method to analyze the BVRJK lightcurves and obtain the periodicities [P.sub.1] = 86.92 [+ or -] 2.21 days, [P.sub.2] = 204 [+ or -] 8.1 days, [P.sub.3] = 1.24 [+ or -] 0.19 years. The periodic signals are shown in Figure 2. Red noise is a random signal, which has been filtered in order to generate a lot of energy at low frequencies. In order to check the strength of the periodic signal, we compare the periodic signal with the red noise. The red noise  with the noise levels 80%, 90%, 95%, and 99% is shown in Figure 2. Based on the results, we can find that at the whole five bands, [P.sub.1] is higher than 99% noise level, at J and K bands, [P.sub.2] is higher than 90% noise level, and only K band [P.sub.3] are higher than 99%.
3.2. The Spectral Indices. We use the following method to obtain the spectral indices. Firstly, we make Galactic Extinction correction, using [A.sub.B] = 0.382 mag, [A.sub.V] = 0.289 mag, [A.sub.R] = 0.228 mag, [A.sub.J] = 0.075 mag, and [A.sub.K] = 0.032 mag, which are collected from NED (http://ned.ipac.caltech.edu/); then we convert the magnitudes ([m.sub.v]) into flux densities ([F.sub.v]), where v is frequency; and at last, based on the relation [F.sub.v] [varies] [v.sup.-[alpha]], the spectral indices ([alpha]) can be calculated by the linear relation: log([F.sub.v]) = -[alpha] log(v) + const.
After calculation, there are 752 spectral indices ([alpha]), which are in the range from 0.33 [+ or -] 0.01 to 2.02 [+ or -] 0.07, with the averaged value [bar.[alpha]] = 1.26 [+ or -] 0.31.
3.3. Relations between Flux Densities and Spectral Indices. Because the linear relations can clearly show the interdependence between the two parameters, so many works used the linear correlations to analyze the relations between spectral indices (a) and flux densities ([F.sub.v]). To compare with the others, we use linear correlations to analyze [alpha] = k log [F.sub.v] + b, with the correlation coefficient r and the chance probability p, the slope k, and the intercept b. When the absolute value of r is higher than 0.5 and p is lower than 0.05, the correlations show strong correlation.
The results are as follows:
at B band, [alpha] = (0.80 [+ or -] 0.03) log [F.sub.B] + (0.92 [+ or -] 0.01), with r=0.68, p = 4.23 x [10.sup.-13.];
at V band, [alpha] = (0.79 [+ or -] 0.03) log [F.sub.V] + (0.83 [+ or -] 0.02), with r=0.70, p = 1.19 x [10.sup.-18.];
at R band, [alpha] = (0.75 [+ or -] 0.03) log [F.sub.R] + (0.78 [+ or -] 0.02), with r=0.72, p = 9.95 x [10.sup.-22.];
at J band, [alpha] = (0.69 [+ or -] 0.02) log [F.sub.J] + (0.60 [+ or -] 0.02), with r=0.75, p = 6.08 x [10.sup.-26.];
at K band, [alpha] = (0.63 [+ or -] 0.01) log [F.sub.K] + (0.44 [+ or -] 0.01), with r=0.91, p = 7.24 x [10.sup.-34.].
The fitting results are shown in Figure 3, with the red lines standing for the fitting lines.
4.1. Optical Variability. The optically variable timescale is an important physical quantity and is often used to probe the physics process of blazars. Based on the optical-infrared lightcurves, we obtain the spectral indices ([alpha]) and analyze the long-term [alpha] variability; see Figure 4 (the upper subpicture). The spectral variability shows quasiperiodic properties, [P.sub.[alpha]|1] = 0.55 [+ or -] 0.08 years, [P.sub.[alpha]|2] = 0.85 [+ or -] 0.07 years, and [P.sub.[alpha]|3] = 1.21 [+ or -] 0.06 years, among which [P.sub.[alpha]|3] shows the strongest signal and is consistent with the result calculated from the lightcurves; see Figure 4 (the lower subpicture). The upper results show that the lightcurves and spectral variability have the same long-term variation tendencies.
If the long-term periodicity (P) is caused by a slim disk, the periodicity can be expressed as P/yr = 9.0[delta][([alpha]/0.1).sup.-0.62][([M.sub.BH]/[10.sup.6][M.sub.(x)]).sup.1.37], where [alpha] is the viscosity coefficient , P is periodicity (in unit of years), and [M.sub.BH] is the central black hole mass. The mass calculated from this method is about ~ [10.sup.6][M.sub.(x)], which is smaller than the others, such as 1.49 x [10.sup.9][M.sub.(x)] calculated by Woo et al. (2002)  and 5.01 x [10.sup.9][M.sub.(x)] calculated by Sbarrato et al. (2012) .
Long-term periodicity might come from the influence of binary black hole. OJ287 is considered as a binary black system . Some authors [39,40] consider PKS 1510-089 as a binary black hole.
3C454.3 might be a binary black hole system. Based on the variability timescales, Li et al. (2007)  gave a method about how to calculate the masses of the primary black hole ([M.sub.1], PBH) and secondary black hole ([M.sub.2], SBH). The methods are as follows.
(1) The distance (a) between the two black holes can be calculated from the following relation:
a = 3 x [10.sup.5] x k[M.sub.2] x P/2[pi] x [DELTA]T x [M.sub.(x)] (cm) (3)
where [DELTA]T is variable timescale, P is the quasiperiodicity, and k is the ratio between the jet diameter and radius of secondary black hole.
(2) The radio (q) between the mass from the primary black hole and the one from the secondary black hole is
q = [M.sub.1]/[M.sub.2]. (4)
(3) For the binary black hole system, the following relation can be deduced
[M.sub.2](1 + q) = 4[[pi].sup.2][a.sup.3]/[GP.sup.2]. (5)
[DELTA]T = 0.685 days is collected from . Because the quasiperiodicity 1.24 years (P = 1.24) are shown both in the lightcurves and in the spectral variability, so we choose the periodicity being 1.24 years to calculate the binary black hole masses. Based on the expression (3), (4), (5), we can obtain
[M.sub.2](1 + q) = [k.sup.3][M.sup.3.sub.2]/3.11 x [10.sup.17] x [M.sub.(x).sup.2]. (6)
So, the masses should be
[mathematical expression not reproducible]. (7)
If the total mass is M = 1.49 x [10.sup.9][M.sub.(x)] , we can obtain M = [M.sub.1] + [M.sub.2] = 5.57 x [10.sup.8] [square root of ([(1 + q).sup.3]/[k.sup.3])][M.sub.(x)] = 1.49 x [10.sup.9][M.sub.(x)]. When Sillanpaa et al. (1988)  analyzed the binary black hole system of OJ287, q = 200 was used. If we take q=200, the binary black holes masses are [M.sub.1] = 1.48 x [10.sup.9][M.sub.(x)], [M.sub.2] = 7.45 x [10.sup.6][M.sub.(x)].
4.2. Time Delay among Different Bands. The analysis about the multiband time delays can help us to study the emission properties and can reflect the terms of electron cooling timescales [42,43]. For S5 0716+714, Gupta et al. (2012)  calculated the time delays between V and R bands and obtained [[tau].sub.VR] = 1.4 days and -1.4 days. For S5 0716+714, Wu et al. (2012)  obtained the time delays, [[tau].sub.BV] = -9.76 ~ 5.48 minutes and [[tau].sub.VR] = 0.77 ~ 25.35 minutes. For 1ES 1959+650, Yuan et al. (2015)  obtained [[tau].sub.RI] = 4.73 [+ or -] 2.75 days, [[tau].sub.VR] = 1.38 [+ or -] 2.92 days, and [[tau].sub.VI] = 4.97 [+ or -] 3.87 days.
We avail the DCF method [46, 47] to explore time delays among different bands. In order to get the delay time more accurately, we use three methods to fit the DCF results: local polynomial regression (LOESS) , local Kernel regression (LOCFIT) , and Gaussian regression. The fitting curves have been added in Figure 5, in which red lines stand for Gaussian regression, blue lines stand for Locfit regression, and green lines stand for Loess regression, based on which we can obtain [[tau].sub.VB] = 0.15 [+ or -] 0.12 days, [[tau].sub.RB] = 0.37 [+ or -] 0.28 days, [[tau].sub.JB] = 0.58 [+ or -] 0.40 days, and [[tau].sub.KB] = 1.02 [+ or -] 0.47 days. Our results show that the B-band lightcurves are ahead of the other bands.
4.3. Relation between Flux Density and Spectral Index. In this work, we analyze the relations between flux densities and spectral indices. At the whole five bands (B,V,R,J,K), log [F.sub.v] and [alpha] show strong correlations. When the source turn to be brighter, the spectrum turn to be redder, which is a typical RWB behavior and consistent with the other FSRQs [32,50,51].
We check those distributions and find that there lie break points; see Figure 6. We use a broken power law to fit them and obtain the break points: [log.sub.10]([F.sub.b|B]) = 0.58 mJy, [log.sub.10]([F.sub.b|V]) = 0.69 mJy, [log.sub.10]([F.sub.b|R]) = 0.78 mJy, [log.sub.10]([F.sub.b|J]) = 1.12 mJy, [log.sub.10]([F.sub.b|k]) = 1.49 mJy, which are noted in Figure 6. When the source becomes fainter, the relations show correlations and when the source becomes brighter, their relations turn to be anticorrelations.
In this paper, we use the observations of 3C454.3 from SMARTs to analyze the lightcurves and calculate the optical spectral indices. Our results show that except K band, the largest variances at B, V, R, and J bands are similar (about 3.5 mag) within about 3 years. The long-term bright variability and spectral variability have the same quasiperiodicities. There lie time delays among different optical and near-IR bands (B, V, R, J, K).
The text formatting data used to support the findings of this study have been deposited in the "http://www.astro.yale.edu/ smarts/glast/home.php" repository. The data on the upper website are public and may be used by other investigators. If others intend to make use of the data, please inform the SMARTs group by email to firstname.lastname@example.org and send copies of any resulting publications, including telegrams. Please acknowledge them in your paper by including a citation to the Bonning et al. (2012), mentioned above, and with the following: "This paper has made use of upto-date SMARTS optical/near-infrared lightcurves that are available at http://www.astro.yale.edu/smarts/glast/home .php." Please also include "SMARTS" as a facility keyword.
Conflicts of Interest
The authors declare that they have no conflicts of interest.
The work is partially supported by the National Natural Science Foundation of China (NSFC 11403006, NSFC 11733001, NSFC U1831119, NSFC U1531245 and NSFC 11503004), Science and Technology Program of Guangzhou (201707010401), Innovative Training Program of Guangzhou University, Innovation Team in Guangdong Province (2014KCXD014), and the financial support for the key subject of Guangzhou City. This paper has made use of up-to-date SMARTS optical/near-infrared lightcurves that are available at http://www.astro.yale.edu/smarts/glast/home.php.
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Yu-Hai Yuan, (1,2) Ze-Xuan Chen, (1) and Yong-Xuan He (1)
(1) Center for Astrophysics, Guangzhou University, Guangzhou, Guangdong 510006, China
(2) Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province, Guangzhou 510006, China
Correspondence should be addressed to Yu-Hai Yuan; email@example.com
Received 23 June 2018; Revised 17 September 2018; Accepted 31 October 2018; Published 2 December 2018
Academic Editor: Geza Kovacs
Caption: Figure 1: The BVRJK lightcurves of 3C454.3. The black dots stand for B band, the red dots stand for V band, the green dots stand for R band, the blue dots stand for J band, and the cyan dots stand for K band.
Caption: Figure 2: Using the Periodogram method to analyze the long-term BVRJK lightcurve. The frequency is in unit of 2[pi] x [day.sup.-1]. The black line stands for periodic signal. The red line, green line, blue line, and cyan line stand for 80%, 90%, 95%, and 99% red-noise levels, respectively.
Caption: Figure 3: Relations between the logarithmic flux densities (log [F.sub.v]) and optical spectral indices (a). The red lines stand for the linear fitting.
Caption: Figure 4: The [alpha] variability and period of 3C454.3. The upper subpicture stands for [alpha] variability and the lower subpicture stands for the quasiperiodicity, which are noted by the dot lines.
Caption: Figure 5: The time delays among the different bands. The red lines stand for the Gaussian fitting, the blue lines stand for Locfit regression, and green lines stand for Loess regression.
Caption: Figure 6: Relations between the logarithmic flux densities (log([F.sub.v])) and optical spectral indices ([alpha]). The black dots and red dots stand for the different regions, with the blue line separating them.
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|Title Annotation:||Research Article|
|Author:||Yuan, Yu-Hai; Chen, Ze-Xuan; He, Yong-Xuan|
|Publication:||Advances in Astronomy|
|Date:||Jan 1, 2018|
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