Issue |
A&A
Volume 520, September-October 2010
|
|
---|---|---|
Article Number | A23 | |
Number of page(s) | 5 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/201014273 | |
Published online | 23 September 2010 |
Short-term VHE variability in blazars: PKS 2155-304
(Research Note)
F. M. Rieger1,2 - F. Volpe1
1 - Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
2 - European Associated Laboratory for Gamma-Ray Astronomy, jointly supported by CNRS and MPG
Received 17 February 2010 / Accepted 17 July 2010
Abstract
Context. The -ray
blazar PKS 2155-304 has attracted considerable attention because of its
extreme TeV variability characteristics during an exceptional
flaring period in 2006. Among the observed key findings are (i) a
minimum variability timescale as short as
s and (ii) highly variable TeV emission, which in the frequency interval [10-4 Hz, 10-2 Hz] can be described by a log-normal distribution and suggests an underlying multiplicative (and not additive) process.
Aims. Simultaneously accounting for these findings appears
difficult within conventional approaches. Following earlier suggestions
for the TeV blazar Mkn 501, we explore a possible scenario
where PKS 2155-304 is supposed to harbor a supermassive binary
black hole system and where the observed TeV variability is
dominated by emission from the less massive black hole.
Methods. We analyze the constraints on the very high energy
(VHE) source imposed by the observed variability characteristics and
the integrated VHE luminosity output, and discuss its implications
for a binary black hole system.
Results. We show that for a secondary mass of
,
fluctuations in the disk accretion rate that feed the jet could account
for the observed red-noise type variability process down to frequencies
of
Hz.
Jet curvature induced by orbital motion, on the other hand, could
further relax constraints on the intrinsic jet speeds.
Conclusions. Because a binary system can lead to different (yet
not independent) periodicities in different energy bands, a longterm
(quasi-) periodicity analysis could offer important insights into the
real nature of the central engine of PKS 2155-304.
Key words: galaxies: active - galaxies: jets - BL Lacertae objects: individual: PKS 2155-304 - black hole physics - radiation mechanisms: non-thermal
1 Introduction
Active galactic nuclei (AGNs) show significant variability over a
large range of timescales. Usually, a variety of information can
be extracted from the data with statistical methods based on Fourier
techniques. In the X-ray domain, for example, variability in
accreting compact objects has commonly been described by means of power
spectral densities (PSD), characterizing the amount of variability
power
as a function of temporal frequencies
,
or timescales
(e.g., van der Klis 1997). For (Seyfert) AGNs the resultant PSDs quite often appear to follow power laws
,
which on long timescales (small frequencies) are approximately described by
close to 1 (flicker noise), but break to a steeper slope (
)
on timescales shorter than a break timescale
.
Active galactic nuclei thus vary more strongly towards lower
frequencies (longer timescales). Recent studies have shown that the
X-ray PSDs of AGNs can be qualitatively similar to the high state of
black hole X-ray binary systems (e.g., McHardy et al. 2004, 2006). Based on these and other similarities, AGNs have sometimes been interpreted as scaled-up Galactic black hole systems.
In the very-high-energy (VHE) domain, the experimental situation is
usually much less favorable. However, one object where it became
recently possible to employ similar analysis techniques is the
TeV blazar PKS 2155-304 (z=0.116). Usually detected only with a low VHE flux of
of the Crab nebula, PKS 2155-304 underwent a dramatic outburst in
July 2006, with VHE flux levels varying between 1 and
15 Crab units, allowing an unprecedented variability analysis
(Aharonian et al. 2007; Abramowski et al. 2010; Degrange et al. 2008).
The Fourier analysis of its VHE light curve of, e.g.,
MJD 53 944 indicates a red (Brownian) noise-type VHE PSD with
an exponent close to 2 within the frequency range [10-4 Hz, 10-2 Hz] (Aharonian et al. 2007). Similar results have been obtained in X-rays (1.5-10 keV) with BeppoSAX in 1996 and 1997 (Zhang et al. 1999). Moreover, similar to findings in the X-ray domain (Zhang et al. 1999, 2005),
where linear relations between (absolute) rms variability
amplitude and (mean) X-ray flux have been previously reported,
a significant rms-flux correlation has been observed in the
VHE data set (Degrange et al. 2008).
This is known to be characteristic of a non-linear, log-normal
stochastic process where the relevant, normally distributed variable is
the logarithm of the flux
,
and not just the flux itself (see Uttley et al. 2005,
for a general treatment; and Superina et al. 2008, for
application to PKS 2155). A log-normal distribution can be
thought of as the result of many multiplicative random effects, whereas
additive effects would give rise to a normal (Gaussian) distribution.
Indeed, if the variability would be caused merely by an additive
stochastic process, the fluxes would be normally distributed and no
linear rms-flux relation would be expected, because all Fourier
coefficients would be statistically independent. Therefore,
the finding that the variations on short timescales (determining
the rms) decrease in amplitude when the long timescale variations
(determining the mean flux) decrease, indicates that the process
driving the variations is a multiplicative process (as in a
cascade) and not just an additive one (e.g., shot-noise), nor one
resulting from independent variations in many separate regions (Uttley
et al. 2005; McHardy 2008).
In accreting galactic black hole (BH) systems these variations have
been frequently related to small, independent fluctuations in the
accretion rate, occurring on local viscous timescale
over a range of disk radii r that are large compared to the inner radius of the disk (Lyubarskii 1997; King et al. 2004; Arevalo & Uttley 2006).
If not damped, these fluctuations can propagate inwards and couple
together in a way to produce the multiplicative characteristics noted
above. Any emission process linked to the the innermost region (e.g.,
as X-ray production or jet launching site) may then eventually be
modulated over a frequency interval ranging from the inverse accretion
time near the outer to the one at the innermost disk radius,
respectively. While this scenario sounds very attractive (cf. also
Giebels & Degrange 2009,
for BL Lac), a generalization to a supermassive source like
PKS 2155-304 seems challenging given the detected VHE minimum
variability (doubling) timescale of
s.
As we show below, a consistent approach along this line may
require the presence of a putative binary BH system in
PKS 2155-304 (cf. Rieger & Mannheim 2003). It is this conjecture which we wish to explore here in more detail.
2 The origin of variability in PKS 2155-304
According to the VHE variability analysis for July 2006, there are two major findings which need
explanation: (i) first, the extreme short-term variability on a timescale as low as
s (in the observer's frame)
;
and (ii) secondly, the log-normal distribution of fluxes, which
points to an underlying, multiplicative process. Consider the first
finding (i):
If the luminosity of the host galaxy of PKS 2155-304 is indeed as high as reported, i.e.,
mag (Kotilainen et al. 1998), its central BH mass is (even if one takes the scatter in the
relation into account) expected to exceed (McLure & Dunlop 2002)
![]() |
(1) |
Accounting for the observed rapid variations based on conventional assumptions has thus proved challenging (see, e.g., Levinson 2007; and Begelman et al. 2008, for detailed discussions): in the galaxy's rest frame, the characteristic scale of any disturbance produced by the central engine cannot be smaller than its minimum size




Similar results are obtained if the variability is taken to be produced by the collision of shells moving at different speeds (as in classical internal shock scenarios). In all these cases, the inferred minimum source size (in the rest frame of the galaxy) becomes independent of any Doppler or Lorentz factor
![[*]](/icons/foot_motif.png)










One obvious possibility to reconcile these apparently divergent central mass estimates is related to the putative presence of a close binary BH system where the jet that dominates the high-energy emission originates from the less massive (secondary) BH. In such a case, host galaxy observations may only be indicative of the total (primary and secondary) BH mass, whereas high-energy observations could actually reveal signatures of the less massive BH. We note that the possible presence of close binary BH systems in blazar-type AGN sources has been repeatedly invoked to account for a variety of observational findings, most notably for the detection of mid-and long-term quasi-periodic variability (e.g., see Rieger 2004, for a review).
If the observed VHE output in PKS 2155-305 were be dominated by
emission from the secondary BH, however, its mass cannot be
supposed to be too small if one also wishes to account for the required
jet power. Suppose that the maximum possible jet power is constrained
by the Eddington accretion limit
erg s-1.
The maximum spin power, for example, which can be extracted from the
rotational energy of a BH (via a Blandford-Znajek-type process) is
on the order of
erg s-1. With an Eddington equipartition magnetic field strength
,
the extractable spin power thus becomes comparable to
,
i.e.,
.
The average VHE gamma-ray flux detected by HESS implies
an isotropic VHE luminosity
1046 erg s-1 (Aharonian et al. 2007). If the radiation is produced within two, oppositely directed, conical jets of an opening angle
rad, the required (minimum) jet power would be
erg s-1.
For a BH accreting at close to the Eddington limit
(see below) or with maximal spin power, the required minimum mass
thus becomes
which would be consistent with the variability constraints (Eq. (2)) and be suggestive of a binary mass ratio

In reality, the variability constraint of Eq. (2)
is probably too optimistic, in particular if one wishes to account
for the second finding (ii) (i.e., the log-normal
VHE flux distribution) based on fluctuations in the accretion flow
that feeds the jet. Consider again the fluctuating disk model
(Lyubarskii 1997), where
fluctuations of the disk parameters at some radius, which occur on
local viscous timescale, can lead to variations in the accretion rate
at smaller radii that are of the flicker- or red-noise type. Then the
relevant timescale to be employed is the viscous timescale
close to the inner radius of the disk, and not the
dynamical timescale
.
In terms of the
parameter and the disk scale height to radius ratio (h/r), this timescale can be expressed as
![]() |
(4) |
where







In order to account for the observed VHE variability characteristics,
suppose therefore that fluctuations in the disk accretion rate on
timescales as short as
are efficiently transmitted to the jet, leading to red noise-type
fluctuations in the injection rate for Fermi-type particle
acceleration. Obviously we will only be able to observe emission with
red noise-characteristics if these signatures do not get blurred by
processes occurring on a longer timescale within the source:
For an observer, flux changes will always appear to be convolved
and thus dominated by the longest timescales (Salvati et al. 1998), i.e.,
![]() |
(5) |
where



![]() |
(6) |
where




Consider next the radiative timescale and assume synchrotron losses to
dominate the high-energy branch of the energetic particle
distribution
that is responsible for the up-scattering of soft photons to the VHE regime. The radiative timescale thus is
![]() |
(7) |
Hence, in order to work successfully, the proposed scenario requires co-moving magnetic field strengths that are sufficiently high (



3 Possible implications of a binary BH model
Following the above analysis, let us suppose that PKS 2155-304
harbors a close binary system consisting of a primary BH with mass
and a secondary one with mass
(mass ratio
). Evidence for a possible longterm period of
yr in the optical V band (Fan & Lin 2000; cf. also Brinkmann et al. 2000,
for soft-X-ray hints) might possibly fit well into such a framework:
if one requires the secondary to be on an orbit that could
intersect the accretion disk around the primary with a typical
(maximum) disk size of
,
with
and
(Goodman 2003), possible Keplerian periods
are constrained to be smaller than
yr,
a condition that seems well satisfied for PKS 2155-304. This
suggests that binary disk interactions could indeed result in optical
QPOs on the timescale of several years (see Rieger 2007, for more details). Accordingly, we may derive an upper limit on the intrinsic Keplerian orbital period of the binary
by assuming that the observed optical longterm periodicity is caused by the secondary crossing the disk around the primary twice per orbital period, a situation expected to occur during the initial stage of interaction. In reality, however, this may not be fully appropriate because an alignment of the binary's orbital and primary's disk plane typically occurs on comparatively short timescales (e.g., Ivanov et al. 1999). One may thus expect quasi-coplanar orbits, with the binary possibly surrounded by a circumbinary disk, to be much more common. Yet, granted that to be the case, periodically modulated mass transfer across the gap (see below) could still lead to QPOs in the standard disk-dominated infrared-optical regime. Most circumbinary disk simulations suggest that the accretion rate is pulsed over one orbital period, although occasionally two peaks per period are found (e.g., Artymowicz & Lubow 1996; Bate & Bonnell 1997; Kley 1999; Hayasaki et al. 2007). This indicates that Eq. (8) still provides us with a reasonable constraint on the maximum intrinsic orbital period. If so, then the residual lifetime


![]() |
(9) |
Once the secondary becomes embedded in the outer disk around the primary, it starts clearing up an annular gap of a radial size


Suppose that the size
of the disk around the secondary is comparable to the Roche lobe radius (Eggleton 1983) or the Toomre stability radius (whichever is smaller). For
and
,
the viscous timescale at the outer radius
yr (standard disk) then most likely
exceeds the orbital period
yr.
Any modulation of the mass supply to the outer disk at the orbital
period may thus be damped by the viscosity of the disk, i.e., as
the next pulse comes before the former was able to propagate in,
the amplitude of variability becomes small as a result of
summation of the pulses (Zdziarski et al. 2009).
A significant modulation of the jet power (emerging from the
innermost part of the disk) solely owing to a periodically changing
mass supply (at the outer disk radius) may therefore not become
apparent. On the other hand, if variability in the disk occurs on
thermal timescale
,
optical (V band)
disk variability on orbital timescale might be possible. While a
periodically changing mass supply may thus not necessarily lead to
significant periodicities in the jet emission, geometrical effects due
to the orbital motion could introduce them: if the jet launched is
wrapped by a sufficiently strong magnetic field, for example,
its overall path can become curved due to the orbital motion of
the jet-emitting BH (leading to non-ballistic-type helical motion).
Then the constraints on the required minimum bulk Lorentz factors of
the outflow (
,
perpendicular to the disk plane) might be somewhat relaxed because the effective Doppler factor will be time-dependent, D(t),
with the strongest boosting effects occurring whenever the (changing)
angle to the line of sight becomes smallest (cf. Rieger 2004). This is illustrated in Fig. 1 for a bulk Lorentz factor (in the rest frame of the secondary) of 20 and an inclination i (defined as the angle between the line of sight and the z-axis, in a frame where the orbital plane is in the x-y plane) between
and
.
Obviously, considerable changes in the effective Doppler factor could
occur, which would further influence the detectability of high- and
low-level (intrinsic) active source stages, i.e., even if the
intrinsic flux would change only moderately, an order of magnitude
difference in measured VHE fluxes may become possible. Moreover,
the motion of components along curved trajectories could possibly
also account for the observed super-quadratic correlation between the
X-ray and VHE flux (Costamante 2008; Katarzynski & Walczewska 2010). Of course, this might only be expected as long as the lateral width of the jet remains smaller than the separation d
of the binary, so that the effects caused by orbital motion will not be
smeared out. For an expanding jet, this obviously limits the
distance up to which extreme Doppler effects may occur. This might
partly explain why on larger (radio VLBA) scales, only modest Doppler
boosting seems to be present (e.g., Piner & Edwards 2004).
Clearly, an accurate identification of active VHE source
stages in PKS 2155-304 could help to further assess the influence
of differential (geometrical) Doppler effects.
![]() |
Figure 1:
Time-dependence of the Doppler factor for motion along an idealized orbital-driven helical jet path. Chosen parameters are:
|
Open with DEXTER |
4 Conclusions
The observed, extreme VHE variability characteristics of
PKS 2155-304 provide strong constraints on the physical parameters
of its engine. We have suggested that similar to Mkn 501 (Rieger
& Mannheim 2003),
the putative presence of a close supermassive binary BH system
could allow (i) to reconcile central mass estimates based on host
galaxy observations (indicative of the total primary and secondary
mass) with those based on VHE -ray
variability (possibly only indicative of the jet-emitting secondary);
(ii) to account for the observed log-normal variability
characteristics via accretion disk fluctuations; and (iii) to
relax constraints on the jet flow velocity. Obviously, an increased
instrumental sensitivity in the TeV domain (by, e.g.,
a CTA-type instrument) that may allow us to search for even faster
variability and, complementary, an advanced QPO analysis in the
optical (e.g., Hudec & Basta 2008)
could thus be particularly useful to further assess the possibility of
a binary scenario for PKS 2155-304. If corroborated by
further observations, the analogy to X-ray binary systems might be
closer than initially anticipated.
Discussions with Felix Aharonian, Amir Levinson and Berrie Giebels are gratefully acknowledged.
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Footnotes
- ... frame)
- As shown by, e.g., Degrange et al. (2008),
this value is dependent on the telescope's sensitivity, which makes it
possible to search for even faster variability with future arrays. The
currently derived ``doubling timescale'' of
s is therefore best understood as an experimental upper limit on the real physical doubling timescale of the source.
- ... factor
- Note that the situation could be different if the variations
are produced within the relativistically moving component itself, e.g.,
via a cascade induced by internal
-absorption, cf. Aharonian et al. (2008).
All Figures
![]() |
Figure 1:
Time-dependence of the Doppler factor for motion along an idealized orbital-driven helical jet path. Chosen parameters are:
|
Open with DEXTER | |
In the text |
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