Issue |
A&A
Volume 502, Number 3, August II 2009
|
|
---|---|---|
Page(s) | 749 - 770 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/200912128 | |
Published online | 15 June 2009 |
Simultaneous multiwavelength observations of the second exceptional
-ray flare of PKS 2155-304 in July 2006
F. Aharonian1,13 - A. G. Akhperjanian2 - G. Anton16 - U. Barres de Almeida8,
- A. R. Bazer-Bachi3 - Y. Becherini12 - B. Behera14 - W. Benbow1 - K. Bernlöhr1,5 - C. Boisson6 - A. Bochow1 - V. Borrel3 - E. Brion7 - J. Brucker16 - P. Brun7 - R. Bühler1 - T. Bulik24 - I. Büsching9 - T. Boutelier17 - P. M. Chadwick8 - A. Charbonnier19 - R. C. G. Chaves1 - A. Cheesebrough8 - L.-M. Chounet10 - A. C. Clapson1 - G. Coignet11 - L. Costamante
1,29,31
- M. Dalton5 - M. K. Daniel8 - I. D. Davids22,9 - B. Degrange10 - C. Deil1 - H. J. Dickinson8 - A. Djannati-Ataï12 - W. Domainko1 - L. O'C. Drury13 - F. Dubois11 - G. Dubus17 - J. Dyks24 - M. Dyrda28 - K. Egberts1 - D. Emmanoulopoulos14 - P. Espigat12 - C. Farnier15 - F. Feinstein15 - A. Fiasson15 - A. Förster1 - G. Fontaine10 - M. Füßling5 - S. Gabici13 - Y. A. Gallant15 - L. Gérard12 - B. Giebels10 - J. F. Glicenstein7 - B. Glück16 - P. Goret7 - D. Göhring16 - D. Hauser14 - M. Hauser14 - S. Heinz16 - G. Heinzelmann4 - G. Henri17 - G. Hermann1 - J. A. Hinton25 - A. Hoffmann18 - W. Hofmann1 - M. Holleran9 - S. Hoppe1 - D. Horns4 - A. Jacholkowska19 - O. C. de Jager9 - C. Jahn16 - I. Jung16 - K. Katarzynski27 - U. Katz16 - S. Kaufmann14 - E. Kendziorra18 - M. Kerschhaggl5 - D. Khangulyan1 - B. Khélifi10 - D. Keogh8 - W. Kluzniak24 - T. Kneiske4 - Nu. Komin7 - K. Kosack1 - G. Lamanna11 - J.-P. Lenain6 - T. Lohse5 - V. Marandon12 - J. M. Martin6 - O. Martineau-Huynh19 - A. Marcowith15 - D. Maurin19 - T. J. L. McComb8 - M. C. Medina6 - R. Moderski24 - L. A. G. Monard30 - E. Moulin7 - M. Naumann-Godo10 - M. de Naurois19 - D. Nedbal20 - D. Nekrassov1 - J. Niemiec28 - S. J. Nolan8 - S. Ohm1 - J.-F. Olive3 - E. de Oña Wilhelmi12,29 - K. J. Orford8 - M. Ostrowski23 - M. Panter1 - M. Paz Arribas5 - G. Pedaletti14 - G. Pelletier17 - P.-O. Petrucci17 - S. Pita12 - G. Pühlhofer14 - M. Punch12 - A. Quirrenbach14 - B. C. Raubenheimer9 - M. Raue1,29 - S. M. Rayner8 - M. Renaud12,1 - F. Rieger1,29 - J. Ripken4 - L. Rob20 - S. Rosier-Lees11 - G. Rowell26 - B. Rudak24 - C. B. Rulten8 - J. Ruppel21 - V. Sahakian2 - A. Santangelo18 - R. Schlickeiser21 - F. M. Schöck16 - R. Schröder21 - U. Schwanke5 - S. Schwarzburg18 - S. Schwemmer14 - A. Shalchi21 - M. Sikora24 - J. L. Skilton25 - H. Sol6 - D. Spangler8 -
.
Stawarz23 - R. Steenkamp22 - C. Stegmann16 - G. Superina10 - A. Szostek23,17 - P. H. Tam14 - J.-P. Tavernet19 - R. Terrier12 - O. Tibolla1,14 - M. Tluczykont4 - C. van Eldik1 - G. Vasileiadis15 - C. Venter9 - L. Venter6 - J. P. Vialle11 - P. Vincent19 - M. Vivier7 - H. J. Völk1 - F. Volpe
1,10,29 - S. J. Wagner14 - M. Ward8 - A. A. Zdziarski24 - A. Zech6
1 - Max-Planck-Institut für Kernphysik, PO Box 103980, 69029
Heidelberg, Germany
2 -
Yerevan Physics Institute, 2 Alikhanian Brothers St.,375036 Yerevan,
Armenia
3 -
Centre d'Étude Spatiale des Rayonnements, CNRS/UPS, 9 Av. du Colonel Roche, BP
4346, 31029 Toulouse Cedex 4, France
4 -
Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee
149, 22761 Hamburg, Germany
5 -
Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15,
12489 Berlin, Germany
6 -
LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon,
France
7 -
IRFU/DSM/CEA, CE Saclay, 91191
Gif-sur-Yvette, Cedex, France
8 -
University of Durham, Department of Physics, South Road, Durham DH1 3LE,
UK
9 -
Unit for Space Physics, North-West University, Potchefstroom 2520,
South Africa
10 -
Laboratoire Leprince-Ringuet, École Polytechnique, CNRS/IN2P3,
91128 Palaiseau, France
11 -
Laboratoire d'Annecy-le-Vieux de Physique des Particules, CNRS/IN2P3,
9 Chemin de Bellevue, BP 110,74941 Annecy-le-Vieux Cedex, France
12 -
Astroparticule et Cosmologie (APC), CNRS, Universite Paris 7 Denis Diderot,
10, rue Alice Domon et Leonie Duquet,75205 Paris Cedex 13; UMR 7164, CNRS, Université Paris VII, CEA, Observatoire de Paris, France
13 -
Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2,
Ireland
14 -
Landessternwarte, Universität Heidelberg, Königstuhl, 69117 Heidelberg, Germany
15 -
Laboratoire de Physique Théorique et Astroparticules,
Université Montpellier 2, CNRS/IN2P3, CC 70, Place Eugène Bataillon,34095
Montpellier Cedex 5, France
16 -
Universität Erlangen-Nürnberg, Physikalisches Institut,Erwin-Rommel-Str. 1,
91058 Erlangen, Germany
17 -
Laboratoire d'Astrophysique de Grenoble, INSU/CNRS, Université Joseph Fourier, BP
53, 38041 Grenoble Cedex 9, France
18 -
Institut für Astronomie und Astrophysik, Universität Tübingen,
Sand 1, 72076 Tübingen, Germany
19 -
LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot
Paris 7, CNRS/IN2P3, 4 Place Jussieu, 75252 Paris Cedex 5, France
20 -
Charles University, Faculty of Mathematics and Physics, Institute of
Particle and Nuclear Physics, V Holesovickách 2, 180 00
21 -
Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und
Astrophysik,
Ruhr-Universität Bochum, 44780 Bochum, Germany
22 -
University of Namibia, Private Bag 13301, Windhoek, Namibia
23 -
Obserwatorium Astronomiczne, Uniwersytet Jagiellonski, ul. Orla 171,
30-244 Kraków, Poland
24 -
Nicolaus Copernicus Astronomical Center, ul. Bartycka 18,00-716 Warsaw,
Poland
25 -
School of Physics & Astronomy, University of Leeds, Leeds LS2 9JT, UK
26 -
School of Chemistry & Physics,
University of Adelaide, Adelaide 5005, Australia
27 -
Torun Centre for Astronomy, Nicolaus Copernicus University, ul.
Gagarina 11, 87-100 Torun, Poland
28 -
Instytut Fizyki Jadrowej PAN, ul. Radzikowskiego 152,31-342 Kraków,
Poland
29 -
European Associated Laboratory for Gamma-Ray Astronomy, jointly
supported by CNRS and MPG
30 -
Bronberg Observatory, CBA Pretoria, PO Box 11426,
Tiegerpoort 0056, South Africa
31 - Stanford University, W.W. Hansen Experimental Physics Laboratory &
Kavli Institute for Particle Astrophysics and Cosmology,
Stanford, CA 94305-4085, USA
Received 21 March 2009 / Accepted 17 April 2009
Abstract
Aims. The X-ray-TeV connection and the evolution of the emitting particle population is studied in high-energy peaked BL Lac objects, by obtaining spectral information in both bands on sub-hour timescales.
Methods. Simultaneous observations with HESS, and the Bronberg optical observatory were performed on the BL Lac object PKS 2155-304 in the night of July 29-30 2006, when the source underwent a major -ray outburst during its high-activity state of Summer 2006. This event took place about 44 h after the other major outburst of the night of July 27-28, which is known for its ultrafast variability. An unprecedented 6 to 8 h of simultaneous, uninterrupted coverage was achieved, with spectra and light curves measured down to 7 and 2 min timescales, respectively.
Results. The source exhibited one major flare along the night, at high energies. The -ray flux reached a maximum of
11 times the Crab flux (>400 GeV), with rise/decay timescales of
1 h, plus a few smaller-amplitude flares superimposed on the decaying phase. The emission in the X-ray and VHE
-ray bands is strongly correlated, with no evidence of lags. The spectra also evolve with similar patterns, and are always soft (photon index
), indicating no strong shift of the peaks in the spectral energy distribution towards higher energies. Only at the flare maximum is there evidence that the
-ray peak is inside the observed passband, at
400-600 GeV. The VHE spectrum shows a curvature that is variable with time and stronger at higher fluxes. The huge VHE variations (
)
are only accompanied by small-amplitude X-ray and optical variations (factor 2 and 15% respectively). The source has shown for the first time in a high-energy peaked BL Lac object a large Compton dominance (
/
)
- rapidly evolving - and a cubic relation between VHE and X-ray flux variations, during a decaying phase. These results challenge the common scenarios for the TeV-blazar emission.
Key words: galaxies: active - galaxies: BL Lacertae objects: individual: PKS 2155-304 - gamma rays: observations - X-rays: galaxies
1 Introduction
Among blazars, high-energy peaked BL Lac objects (HBL, Giommi & Padovani 1994) are characterized by the highest energy particles and most violent acceleration processes. In the X-ray band, they have shown extreme spectral properties (see e.g., Costamante et al. 2001) and variability (e.g., Mkn 501, Pian et al. 1998). At very high energies (VHE,

Providing two handles on the one electron distribution responsible for both emissions,
simultaneous observations in the X-ray and VHE bands
represent both a powerful diagnostic tool and a very stringent
testbed for the model itself (Coppi & Aharonian 1999),
especially during large flares when the emission from a single region
is expected to dominate the SED.
Alternatively, hadronic scenarios explain the -ray peak as being produced by
ultra high energy protons (
eV; see e.g. Mücke & Protheroe 2001; Aharonian 2000).
Imaging atmospheric Cherenkov telescopes (IACT) provide a unique chance to study
rapidly-variable sources at -ray energies,
thanks to their large collecting area.
Multiwavelength campaigns performed on a few very bright sources
(namely Mkn 501, Mkn 421 and 1ES 1959+650)
have shown that X-ray and VHE emission are generally highly correlated
(e.g., Pian et al. 1998; Djannati-Atai et al. 1999; Sambruna et al. 2000; Giebels et al. 2007; Bazejowski et al. 2005; Krawczynski et al. 2002; Fossati et al. 2008; Aharonian et al. 1999a; Krawczynski et al. 2004; Aharonian et al. 1999b),
down to sub-hour timescales with no evidence of significant lags
(Fossati et al. 2008; Maraschi et al. 1999; Fossati et al. 2004).
Moreover, the correlation seems to tighten
when individual flares can be fully sampled (Fossati et al. 2008).
These results provide strong support to the idea that
both emissions during flares
are produced by a single electron population (``one zone'' SSC scenario).
On the other hand, the same campaigns have also unveiled a more complex and puzzling behaviour, which represents a challenge to the SSC scenario. Two main problems have recently emerged:
- 1)
- the X-ray and VHE emissions do not always correlate
(e.g., in Mkn 421; Bazejowski et al. 2005).
In particular, VHE flares seem to occur also without any visible X-ray counterpart
(so-called ``orphan'' flares). The most striking example has been provided by 1ES 1959+650
during the high state of 2002, when a strong (>4 Crab) and rapid TeV flare
(7 h of doubling timescale) was not accompanied by detectable variations
in the RXTE band (Krawczynski et al. 2004).
True orphan events are quite difficult to explain with a standard SSC scenario.
However, the generally sparse sampling does not allow the exclusion of
lagged counterparts (Bazejowski et al. 2005)
or counterparts emerging in a different energy band (Krawczynski et al. 2004).
- 2)
- Mkn 421 exhibited a quadratic relation between VHE and X-ray flux variations during both the rising and decaying phases of a flare (Fossati et al. 2008,2004). This is not expected if the source is in the Klein-Nishina (KN) regime.

![[*]](/icons/foot_motif.png)


To investigate these issues, a multiwavelength study of single flares is essential. Although many efforts have been made to achieve a good sampling, so far the short variability timescales have been difficult to study, because of the lack of sensitivity of the past-generation of IACTs. However, these are extremely interesting timescales: the results of HEGRA on Mkn 421, for example, have already revealed an entire ``zoo'' of intra-night flares with different rise and decay times (Aharonian et al. 2002b), indicative of a complex interplay between acceleration/injection and cooling processes (e.g., Kirk & Mastichiadis 1999)
When the IACT array HESS became operational,
a project was therefore developed
with specific ToO proposals, to investigate the fast variability timescales with
a whole night (6-8 h) of continuous, simultaneous observations during a bright -ray state.
To achieve this aim, was chosen because it is the only X-ray satellite
capable of a full coverage of the entire HESS visibility window during most of the year,
and without the interruptions on sub-hour timescales
which are typical of low-orbit satellites.
The efforts paid off in July 2006, when the HBL PKS 2155-304 (z=0.116)
became highly active at VHE, with a flux level a factor of
10 higher than
its typical quiescent flux of
4
10-11 cm-2 s-1 above 200 GeV.
PKS 2155-304 is one of the brightest and
most studied BL Lacs
in the Southern Hemisphere, at every wavelength,
and it can be detected by HESS on almost a nightly basis since 2002
(see Aharonian et al. 2005b,a, and references therein).
In the first days of activity, ToO observations were also triggered
for other X-ray satellites such as RXTE and Swift, to sample
the source behaviour over several days and weeks.
Then, in the early hours of July 28 2006,
a giant outburst occurred at VHE
(
above the quiescent level),
with a peak flux of 15 Crab above 200 GeV (corresponding to 9.9 Crab above 400 GeV)
and repeated flares with doubling timescales of few minutes (Aharonian et al. 2007a).
Unfortunately, this dramatic outburst occurred too early with respect to the
already-triggered but not-yet-started X-ray observations
(which were acquired from the night after).
Therefore, the event of most exceptional variability remained
without multiwavelength coverage.
Two days later however, on the night of July 29-30,
the source underwent a second major VHE flare, this time in coincidence
with our planned Chandra-HESS ToO campaign, and with the further coverage
in the optical band provided by the Bronberg Observatory in South Africa.
Snapshot observations of few ks were also taken with RXTE and Swift.
This second outburst has reached even higher fluxes
than the first one (11 Crab above 400 GeV).
As a result, in this single night the most dense and sensitive X-ray/TeV campaign
to date was obtained, during one of the brightest states ever observed from an HBL at VHE.
This paper focuses on the multiwavelength results of this exceptional night, presenting new optical, X-ray and VHE data. The results of the whole VHE activity of PKS 2155-304 between July and October 2006 will be presented in forthcoming papers, together with the overall multiwavelength coverage.
Since this is a very rich and complex dataset, the
data have been divided into several subsets of different time windows,
to highlight specific aspects
(e.g., different VHE thresholds, integration times, or X-ray coverage).
These subsets and their rationale will be introduced in the relevant Sects.,
but a summary list with corresponding time windows
is given in Table 1, for reference.
Throughout the paper, the following cosmological parameters are used:
H0 =70 km s-1 Mpc-1,
,
and
.
Conforming to the convention adopted in all previous HESS publications,
unless otherwise indicated, all errors are given at the 1
confidence level
for one parameter of interest (
). For simplicity,
in the text the values of MJD are given as MJD
MJD-53 900.
2 Observations and data reduction
2.1 HESS
HESS is an array of four Imaging Atmospheric Cherenkov Telescopes located in the Khomas Highlands of Namibia (23






The recorded signal in the field of view is dominated by the constant background from hadronic
cosmic rays entering the atmosphere.
Most of the hadronic background can be identified from
by the shape of the shower images and the arrival direction of the recorded showers.
The remaining hadronic background can be statistically removed by
estimating it from sky regions with no -ray signal.
In the analysis shown here, loose cuts and the reflected background
method were applied for background substraction (Aharonian et al. 2006b).
Light curve and spectra were derived following the
standard HESS analysis also described in this reference.
HESS observed PKS 2155-304 throughout the night of July 29-30.
A total of 15 runs (each 28 min long) were taken, all
passing the standard quality criteria specified in
Aharonian et al. (2006b).
The total lifetime after dead-time corrections is 6.58 h.
A -ray excess of 32 612 events was detected with a
significance
of 254
following Eq. (17) in Li & Ma (1983). The
excess is point-like, taking into account the point spread function of HESS, with a
best fit position of
,
,
consistent with the position of PKS 2155-304
(
;
Ma et al. 1998).
Because of the long duration of the observations,
the zenith angle of the source varied
strongly during the night, going from 53
at the beginning,
to 8
at the middle, and back to 50
at the end of the night.
Observations at larger zenith angles imply
a higher energy threshold of the analysis.
For the observations discussed here the energy
threshold varies between 200 and 700 GeV for the applied energy
reconstruction (Aharonian et al. 2006b). This results in a tradeoff between energy
and time coverage for the analysis, as we discuss later.
HESS has a systematic uncertainty in the normalization of its
energy scale of 15%. The main source of this systematic error are
uncertainties in the atmospheric conditions
(for a more detailed discussion see Aharonian et al. 2006b). During the night the atmospheric
conditions were stable. This can be verified to timescales
shorter than one minute in the overall trigger rate and background
rates in regions off the source.
The differential energy spectrum
of PKS 2155-304 at
VHE energies is generally steep,
with a photon index of about 3.4 in a power-law model
(Aharonian et al. 2007a,2005b,a). The
systematic error in the energy scale of the detector therefore transforms into an error
of
40% in the overall flux normalization. The systematic error
in the slope of differential energy spectra is
0.1 for the
photon index
(see Aharonian et al. 2006b).
2.2 Chandra
PKS 2155-304 was observed with (Weisskopf et al. 2000) for a total duration of 30 ks with the Low Energy Transmission Grating (LETG) spectrometer coupled with the ACIS-S detector (ObsId 6874; set-up with 1/8 subarray and 6 active chips, for a 0.7 s frametime). Because of difficulties in placing our constrained ToO observation within the schedule, the observation started later than requested, missing the first 1.7 h of the HESS window. Unfortunately, the main flare occurred in the first few hours of the HESS window. As a result, the rising part of the main VHE flare has no X-ray coverage.
Data reduction was performed according to the standard CXC procedures,
using the CIAO software version 3.4 with the
corresponding Calibration Database CALDB version 3.3.0 and HEASOFT v6.3.2.
Event files on timescales as short as 2 min
were obtained using dmcopy
, which propagates all deadtime corrections
correctly.
Grating spectra were then extracted with tgextract
and their ancillary files were generated with fullgarf
for each arm;
then added together to obtain the first-order spectrum.
The scientific analysis was completed mainly on the first-order spectrum,
because of its higher S/N and photon statistics.
A check was performed that the centroid of the source
obtained from the zero-order image was indeed coincident
with the coordinates of the source on the detector.
The response matrix was produced using mkgrmf
applied to the entire observation,
since no difference was found from files created in different epochs during the night.
The analysis was optimized and performed only on the continuum properties: the study
of the total grating spectrum at its highest resolution is beyond the scope of this paper
and is left to future publications.
The background and source spectra in each time-bin were then extracted with
the tool tg_bkg
for use in XSPEC.
The hundreds of spectra (one for each time bin, down to 2-min bins)
have been routinely fitted in XSPEC version 11.3.2,
using a source model plus photoelectric absorption (wabs
), with the
equivalent hydrogen column density fixed at Galactic values
(
cm-2; Dickey & Lockman 1990).
This is also the
value obtained from the best
fit to the total exposure with free absorption, to within 1 sigma.
The integrated flux and its error
were calculated from the spectral fit using the specific error routine in XSPEC.
The error in the unabsorbed flux was then obtained from the percentage error
of the absorbed fit. The results of this procedure were later checked
to be fully consistent with the values from the specific Tcl routine
fluxerror.tcl
recently provided by HEASARC with XSPEC v12, for calculating the error in the flux from single
components of the model.
In the following, all X-ray fluxes are quoted as unabsorbed values.
The time analysis was also performed using the direct count rate and its error
in the energy band of interest, for each time-bin,
obtaining fully consistent results.
The average count rate observed from PKS 2155-304 in the LETG
is 8 cts/s, ranging between 12 and 6 cts/s.
These count rates allow the spectra to be extracted down to 2-4 min
timescales with typically 1000-2000 counts each.
For the observed flux, the grating spectra do not suffer from pile-up problems:
the total fraction of piled-up events estimated at the peak of the
effective area (1-2 keV) and source peak flux is less than 5%.
![]() |
Figure 1: VHE fluxes integrated in different energy bands, as a function of time, in time bins of two minutes. The time windows corresponding to the different energy thresholds are given in Table 1 (labelled accordingly, from top to bottom: T200 to T700). The dotted lines mark the positions of rapidly varying events on-top of the main flare (see text). |
Open with DEXTER |
One of the calibration issues with the ACIS instrument is the excess absorption seen below 1 keV due to the build-up of contaminants on the optical blocking filter. These contaminants (thought to be carbon compounds) cause a significant absorption in the 0.3-0.4 keV range, which is taken into account by the calibration but which also severely reduces the count rate in that range, yielding very few counts during short exposures. Therefore, for the spectra extracted on 2 and 4 min timescales, the interval 0.3-0.4 keV was excluded from the analysis. At high energies, data were included in the fit up to the energy where positive net source counts were present. As a result, short-timescale spectra were fitted in the range 0.23-0.3 and 0.4-6 keV, while longer-exposure spectra could be fitted from 0.23 to 8-9 keV. The spectra were generally rebinned to have more than 30 counts per bin, using different schemes. A fixed coarse binning was used for all the spectra on short timescales (<7 min). Various checks have shown that, within the uncertainties, the obtained results are independent of the adopted rebinning.
The analysis of the total exposure shows evidence of a slight residual
excess absorption in the 0.3-0.4 keV range,
not yet fully accounted for by the calibration. The effect is small, and does not affect
the fit values significantly. Nevertheless, it was taken into account
by simply adding an edge model at the carbon K edge, 0.31 keV, with a fixed value of .
These are the best-fit parameters obtained from the fit of the total spectrum
(see Sect. 4.2).
2.3 RossiXTE
As part of the ToO campaign for a daily monitoring, RossiXTE (Jahoda et al. 1996) pointed PKS 2155-304 twice during the night of July 29-30, for a total exposure of
![[*]](/icons/foot_motif.png)
The RXTE spectrum was then fitted in XSPEC together with the spectrum extracted from the same time window, obtaining a spectral measurement over two decades in energy (0.2-20 keV). Without adjustments, the two spectra have very similar normalizations, indicative of a very good inter-calibration between the two instruments. To obtain the most accurate spectral determination, the RXTE / normalization was fixed at the value measured by fitting the same power-law model in the overlapping energy range (3-7 keV), namely 1.08 (see Sect. 4.2).
2.4 Optical data
Optical observations in the V filter were performed using the 32 cm Schmidt-Cassegrain telescope at Bronberg Observatory, Pretoria, South Africa (see Imada et al. 2008, for details about observations of variable sources with this telescope). After de-biasing and flat fielding, data were analyzed using relative aperture photometry with a K-type star of similar magnitude (12.6). Frames were taken every 30 s and then smoothed over 6 successive data points to calculate the mean value in each bin. Each point of the optical light curve therefore has a time duration of
The comparison with the reference star shows that the rise in optical
intensity is highly significant. The K-star light curve is constant with an
intrinsic scatter in the datapoints - using the same smoothing procedure - of
0.02 mag.
The errors were determined from the variance of each 6 successive data points
for both the source and reference star. No time variability in the intensity of
the reference star is seen.
The optical fluxes were corrected for Galactic extinction with
mag.
3 Temporal analysis
3.1 TeV light curves
The measured VHE light curve in two-minute time bins is shown in Fig. 1, divided into five different energy bands. The time coverage increases with threshold energy, due to the aforementioned zenith-angle effect. A full coverage of the observation is thus reached for an energy threshold of 700 GeV, while light curves (and spectra) down to
The source underwent a major flare in the first hours of observation,
reaching a peak flux of 9.9
10-10 cm-2 s-1 (>400 GeV) at MJD
45.90,
corresponding to
11 times the Crab Nebula flux (Aharonian et al. 2006b)
above the same threshold. This peak flux is about 20% higher than the peak
flux measured during the night of July 27-28, above the same threshold
(
9 Crab,
8
10-10 cm-2 s-1 > 400 GeV).
The fluxes measured in these two nights (July 27-28 and 29-30)
are the highest ever observed at VHE from PKS 2155-304.
The total amplitude of flux variation during this night
was about a factor of
20, above 400 GeV
(T400 covers both the highest and lowest flux epochs),
similar to the flux variation observed in the night of July 27-28
(
).
The main flare seems to occur with similar rise and decay timescales,
of the order of 1 h
(half-to-maximum amplitudes, measured using a ``generalized Gaussian'' function as in Aharonian et al. 2007a).
After the peak, the VHE flux decreased overall during the night reaching
its minimum around MJD 46.12,
but with two other smaller-amplitude flares superimposed:
a short burst around MJD
45.96 of duration
20 min, and a
longer flare or plateau between MJD
46.0 and 46.1, with a duration of 2-3 h.
In addition, two further sub-flares are evident in all covered energy bands,
around MJD 45.885 and MJD
45.920 (dotted lines in Fig. 1).
These structures have a duration of
10 min, similar to the flares
of the night of July 27-28.
Although there are hints of even shorter variability (few minutes),
the significance is limited.
![]() |
Figure 2:
Overall light curves of PKS 2155-304 in the night of July 29-30 2006,
as seen by HESS (T700, upper panel),
( lower panel, blue circles), and
the Bronberg Observatory (optical V band, red squares). Time bins of
4 min (3 for the V band).
The segments on the upper x-axis also show the two intervals corresponding to the
RXTE exposure (R label), and the two intervals of the Swift pointing (S label) reported in
Foschini et al. (2007). The vertical scales differ in each panel,
and have been adjusted to highlight the specific variability patterns.
Lower panel: the left axis gives the integrated
0.5-5 keV flux, the right axis gives the V-band
|
Open with DEXTER |
![]() |
Figure 3:
Light curves of the
|
Open with DEXTER |
Table 1:
Summary of the subsets of VHE data used in this
paper (MJD = MJD-53 900).
3.2 Comparison with X-ray and optical light curves
The combined VHE, X-ray and optical light curves are shown in
Figs. 2 and 3. Significant
flaring activity is
visible in all three bands, but with different amplitudes.
To emphasize the specific variability patterns,
the vertical scales in Fig. 2 were adjusted
differently for each band.
Fig. 3 shows instead the light curves on the same flux scale,
but with a
representation. They correspond to slices of the SED at
the three energies of 0.3 TeV, 0.3 keV, and 2.25 eV
(i.e. 5500 Å).
In this way, it is possible to highlight the overall changes and time evolution
SED-wise.
The 0.3 TeV fluxes were calculated from the integrated >300 GeV light curve
(T300 window) using the average power-law spectrum measured in the respective epochs
(namely, the T300-High spectral index in the high state,
and the T300-Low index elsewhere, see Sect. 4.1).
The same procedure was used to calculate the 0.3 TeV fluxes
from the >500 GeV light curve (T500 window),
during the epoch not covered by T300 (empty circles in Fig. 3).
A comparison with the results of the >300 GeV light curve
in the overlapping window
shows that the extrapolation from 500 GeV does not introduce differences
of more than 2%.
The 0.3 TeV fluxes were then corrected for the absorption effect
caused by
-
interactions
with the Extragalactic Background Light (EBL), using
the model by Franceschini et al. (2008)
(discussed in Sect. 4.1.1).
This corresponds to a low density of the EBL, close to the
lower limits obtained by galaxy counts.
The plotted fluxes therefore can be considered as lower limits to the
intrinsic VHE emission of the source.
The X-ray fluxes at 0.3 keV were calculated with the same procedure,
using the power-law spectrum fitted in each of the individual bins.
Anticipating the result that both the VHE and X-ray spectra are steep
(
;
see Sect. 4), the plotted
fluxes
- at the low-energy end of the respective passbands -
provide an estimate of the emission closer to the respective SED peaks
than the
fluxes in the hard band.
Several remarkable features can be noted.
The first is the huge difference in amplitude between the variations in the three energy bands.
In few hours, the VHE flux changed by more than an order of magnitude,
whereas the X-ray flux varied by only a factor 2 and the optical flux by
less than 15%
(the contribution of the host galaxy is negligible, see Sect. 6.3).
The source thus shows a dramatic increase in variability with photon energy.
Secondly, the VHE emission dominates the energy output by far in
the three bands.
In Fig. 3, the comparison
between the 0.3 TeV and 0.3 keV fluxes
shows the evolution of the Compton dominance of the source,
i.e. the ratio of the IC -ray luminosity to the synchrotron power (
).
The
-ray luminosity dominates the synchrotron luminosity by a factor
8 close to the flare maximum,
evolving rapidly towards comparable levels at the end of the night.
This is the first time that such high and rapidly variable Compton dominance
is observed in an HBL, irrespective of the choice of EBL density.
The swiftness of the changes in the
-ray emission and SED properties
also underlines the danger in modeling X-ray and VHE data
taken even only a few hours apart, during such events.
As shown in Fig. 2, both RXTE and Swift observations
occurred when the Compton dominance had already decreased significantly.
Thirdly, despite this difference in amplitude, the X-ray and VHE
light curves are strongly correlated, with the X-ray emission following closely the same pattern
traced by the VHE light curve (see next section).
The optical light curve, instead, does not correlate on short timescales with
the other two bands. However, there is a rise of 15% in flux, which appears
to begin at the same time as the main VHE flare.
A conservative estimate of the chance probability of coincidence
- considering only the data of this night - is of the order of
a few percent. We discuss
in Sect. 8.2 the possible implications if this simultaneity is genuine.
3.3 Inter-band time lags
The degree of correlation and possible time lags between different light curves have been quantified by means of cross-correlation functions. The correlation analysis was performed between X-ray and
![]() |
Figure 4: Cross-correlation analysis of the hard versus soft bands at VHE ( upper panel) and at X-ray energies ( lower panel). Upper panels: a) DCF of the 300-700 GeV and the >700 VHE band. The line around the peak shows the best fit Gaussian plus linear function, with a maximum at 28 s. b) Corresponding cross-correlation peak distribution (CCPD) of 10 000 simulated light curves. The rms of the distributions is 30 s. The dotted line marks the position of the maximum in a). Lower panels: c) DCF of the 0.2-1.0 keV and 2.0-6.0 keV X-ray band. The line around the peak shows the best fit Gaussian plus linear function, with a maximum at -82 s. d) Corresponding CCPD of 10 000 simulated light curves. The rms of the distributions is 202 s. The dotted line marks the position of the maximum in c). |
Open with DEXTER |
![]() |
Figure 5: Cross-correlation between the X-ray and VHE light curves: a) DCF of the >300 GeV light curve and the LETG 0.2-6 keV band.The blue line shows the best fit Gaussian plus linear function, with a maximum at -10 s. b) Corresponding cross-correlation peak distribution of 10 000 simulated light curves. The rms of the distributions is 76 s. The dotted line marks the position of the maximum in a). |
Open with DEXTER |
![]() |
Figure 6: HESS and Chandra light curves in the simultaneous time windows corresponding to a 300 GeV threshold (T300-X in Table 1). Two-minute time bins. Upper panel: integral fluxes above 300 GeV. Lower panel: 1st-order LETG count rate in the 0.2-6 keV band. |
Open with DEXTER |
At VHE, the analysis was performed on the simultaneous light curves between 300-700 GeV and above 700 GeV in two-minute time bins (Fig. 1).
This choice yields a
good compromise between event statistics, time coverage, and a maximum
energy difference between the bands. The resulting time lag between
the higher and lower energy band is
(
) s (see Fig. 4).
This time lag does not differ significantly from zero,
as for the flare of two nights before (Aharonian et al. 2008b),
and we derive a 95% confidence upper limit of 129 s.
This value was calculated by assuming a Gaussian
probability distribution around the measured time lag. The width of the distribution was set
to be the linear sum of the statistical and systematic error, to
be conservative. Afterwards
symmetric intervals around zero were integrated, until a 95%
containment was achieved.
In the X-ray band, an analogous procedure was applied.
The total light curve was divided into a soft (0.2-1.0 keV) and
hard (2.0-6.0 keV) band. Because of the larger errors, in this case
4-min time bins were used. The measured time lag is
(
) s.
This value again does not differ significantly from zero,
resulting in a 95% upper limit of 482 s.
The cross-correlation analysis between the X-ray and -ray emission was
performed on the simultaneous light curves with two-minute time bins
shown in Fig. 6 (in the T300-X time window).
The resulting cross-correlation is shown in Fig. 5.
The two light curves overall are highly correlated, with a maximal correlation of
DCF
,
and no significant lag is found.
The time lag of the X-rays with respect to the
-ray is
(
) s, yielding
a 95% confidence upper limit to a time lag of 208 s.
To test whether this result was caused by an averaging of lags with opposite signs, the
correlation analysis was also performed on sub-intervals,
namely in the interval around the first small flare at MJD
45.96 (MJD
45.94-46.0)
and after MJD
46.0.
The two emissions are again highly correlated
(DCF
), with no evidence of time lags.
The strong correlation is determined not merely by the overall decaying trend
of both light curves, but also by their specific patterns:
a DCF max value of
0.7-0.8 is still obtained after whitening the light curves
by removal of either a linear or quadratic trend.
On the shortest timescales (<4-8 min), however, the VHE light curve
shows few small flares apparently not mirrored in the X-ray band
(see e.g. MJD
45.925 and 46.060 in Fig. 6).
Although this might indicate a more complex correlation on the fastest timescales,
at present no firm conclusions can be drawn, since
the significance of these structures is low.
The correlation analysis was also performed using the task CROSSCOR of the Xronos 5.21 package, which measures the correlation function (CCF) with a direct Fourier algorithm. This algorithm requires a continuous light curve without interruptions, therefore the few gaps were filled with the running mean value calculated over the 8 closest bins (e.g., Ravasio et al. 2004). The results are fully consistent with the DCF analysis, indicating that the small gaps in the VHE light curves - the X-ray light curve is continuous - do not introduce significant distortions for such well sampled data.
The cross-correlation analysis between VHE and X-ray light curves
was limited to the strictly simultaneous window, to avoid artifacts in the
lag determination due to the different timespans and the light curves characteristics.
Because both light curves have each one main flaring feature, the cross-correlation
performed on different intervals tends simply to match the maxima of the two emissions
in those intervals, irrespective of the smaller amplitude patterns.
This would yield an artificial, window-dependent ``lag'' with typically
lower correlation values (as is the case here, with a timespan of 3200 s
between the maxima of the overall VHE and X-ray light curves
and lower DCF/CCF values
0.7).
![]() |
Figure 7:
Left panel: integral flux >300 GeV and photon index
as a function of time (T300 dataset). Horizontal error bars show the time
interval of each bin, going from 7 to 14 min before and after MJD |
Open with DEXTER |
![]() |
Figure 8:
Left panel: integral flux >500 GeV and photon index
as a function of time (T500 dataset). Horizontal error bars show the time
interval of each bin, going from 14 min. at the beginning to
28 min. towards the end of the night. The shaded area shows the time window
where the |
Open with DEXTER |
4 Time-resolved spectral analysis
4.1 VHE spectra
A search for spectral variations in the VHE data was performed by fitting a
power-law spectrum to a fixed energy range in fixed time bins. The
unprecedented statistics of this dataset allow the sampling
in 7 to 14-min bins in the T300 time window (Table 1).
On these short integration times, the power-law function gives a
statistically good description of the data.
The results are shown in Fig. 7.
The spectrum generally hardens with increasing flux.
The fit to a constant photon index
results in a
probability of only 1.6%.
These spectra are also used for comparison with
the X-ray spectra extracted in exactly the same time bins,
and discussed in Sect. 5.
![]() |
Figure 9: Selected VHE spectra: average spectra for the T300-Low ( left) and T300-High ( middle) datasets (see Fig. 7), and the average spectrum above 200 GeV (T200, right). Open symbols corresponds to the spectra corrected for EBL absorption as described in Sect. 4.1.2. |
Open with DEXTER |
Table 2: Spectral fit of the measured VHE spectra extracted in different epochs (see Table 1).
Table 3: Spectral fit of the same VHE spectra given in Table 2, but corrected for EBL absorption (statistical errors only).
A study of the spectral variations was also performed
on the T500 dataset, which allows the sampling
of a wider time span and in particular of both the rise and decay phases
of the main -ray flare. However, the lower number statistics requires
longer integration times, yielding a lower time resolution.
The result is shown in Fig. 8, where spectra
were extracted
in 14 and 28 min bins. The spectral variations follow the same pattern as for the
T300 spectra, both in time and in the flux-index relation.
No significant spectral changes are observed between the rising and decaying
part of the flare, with the possible exception of a hardening event that precedes
the peak of the
-ray emission by
28 min.
The study of the spectral shape in more detail requires higher event
statistics. To achieve this, the dataset was divided into similar spectral
states, namely a high and a low flux state
(T300-High and T300-Low, respectively; see Fig. 7).
In addition, spectra were extracted in three other important epochs:
a) around the peak of the -ray emission (see Fig. 8),
yielding a spectrum with a threshold of 400 GeV (T400-Peak);
b) in the central five hours characterized by a threshold as low as 200 GeV (T200 dataset);
c) in the epoch simultaneous with the RXTE exposure
(T300-RXTE window, 44 min overall, see Table 1),
where the combined X-ray spectrum can be measured over 2 decades in energy.
The results of the spectral fits are given in Table 2,
with a selection shown in Fig. 9.
The spectra present a significant curvature with respect to the pure power-law.
The
probabilities show that the latter is completely excluded
in the high states, and is unlikely in the low state.
The spectral curvature is generally well described either
by a power-law model with an exponential cutoff around 1 TeV
(
), or a log-parabolic function
(
).
Most remarkably, the curvature of the spectrum is strongly variable with time.
In particular, the curvature is more pronounced (i.e., the parameter b is larger)
in the brightest state and decreases as the source dims.
This represents direct proof that the curvature of the VHE spectrum in PKS 2155-304
is also of intrinsic origin, inside the emitting region,
and cannot be attributed entirely to
-
absorption on the EBL
or on any local external field that is constant on the observed timescales.
Besides providing the widest energy coverage,
the T200 spectrum
allows a direct comparison with the spectrum measured during the first exceptional
flare on the night of July 27-28.
The latter has the same energy threshold (200 GeV) and is well described by a broken
power-law (
for
and
for
)
with
,
,
and
GeV.
Fitting this function to the T200 spectrum
yields almost identical results, of the same break energy, slopes
and change in spectral index by
(Table 2). This shows that the source was in a similar state,
even though the overall average normalization is about
30%
lower than two nights before. As for the July 27-28 night, the T200 spectrum
is not well fitted by a power-law model with exponential cutoff or a
log-parabolic function (F-test >99% compared to the broken power-law).
Both functions underestimate significantly the
-ray flux at higher energies.
4.1.1 Correction for intergalactic
-
absorption
The VHE 

The EBL waveband that affects the observed VHE band the most is dominated by the direct starlight emission. To correct for EBL absorption, as reference we adopted the model of the EBL spectral energy distribution by Franceschini et al. (2008), which is based on the emission from galaxies. This model takes into account the most recent results on galaxy properties and evolution and is consistent with both the lower limits from source counts - in the UV-optical (Madau & Pozzetti 2000) as well as near-mid infrared waveband (Dole et al. 2006; Fazio et al. 2004) - and with the upper limits derived from the TeV spectra of high-redshift blazars (Aharonian et al. 2007b,2002a,2007c,2006a). It is similar in shape to both the model by Primack et al. (2005) and the ``low-IR'' calculation by Kneiske et al. (2004). The spectra were corrected by applying the optical depth calculated for the average observed photon energy in each energy bin.
However, it is important to recall that
a significant uncertainty in the SED of the EBL
still remains, since it could be both lower and higher than assumed:
either down to the absolute lower limits given by HST galaxy counts (Madau & Pozzetti 2000)
(as in the model by Primack et al. 2005), or up to the upper limits given by TeV blazars
(Aharonian et al. 2006a). To estimate this uncertainty in both shape and normalization,
we also used the shape of the model by Primack et al. (2005), rescaled to these two levels.
In the energy range around the starlight peak (1-3 m),
the residual uncertainty in the EBL absolute normalization is of the order of 50%
(from
8 to
12 nW m-2 sr-1 at 2.2 micron, while our reference model gives
9.4 nW m-2 sr-1).
This translates into a systematic uncertainty of the order of
in the reconstructed
-ray spectrum.
Namely, the reconstructed spectra (which we call ``intrinsic'') discussed in the following
Sects. can actually be up to
0.2 steeper or harder than indicated.
When relevant, we take this systematic uncertainty into consideration, but
as we show in the following, it does not change the main properties of the
-ray spectrum
and Compton peak frequency of PKS 2155-304.
![]() |
Figure 10:
Evolution of the X-ray spectrum with time, for the whole
exposure. Left panel: each 8-min bin is fitted with
a single power-law model plus galactic absorption.
The HESS window ends at MJD |
Open with DEXTER |
4.1.2 Absorption-corrected
-ray spectra
For the power-law spectra measured on short timescales
(as given in Fig. 7),
the intrinsic spectra are again well fitted by a power-law model
with a slope that is typically harder by -0.8
(namely,


When a spectrum shows a relatively uniform curvature
as in this case, however, the log-parabolic model is generally preferable.
It has the advantage of providing a more direct measure of the curvature
in the true observed band, whereas the exponential cutoff model tends
to match a given curvature in the observed passband
by using a specific section of its cutoff region, and pushing the power-law
component outside the actual observed range.
This often yields artificial values for the slope, which are typically too hard.
The log-parabolic fit allows also a straightforward estimate of the location of the
SED peak (
,
defined by
)
from the curvature itself, with a minimum of free parameters.
To this aim we used the functional form described in Tramacere et al. (2007),
where b and
are the independent free parameters instead of b and
.
The comparison of the curvatures among different states and between
the synchrotron and IC components can also provide important clues about the source emission
regime (Thomson or KN) and the acceleration mechanisms (Massaro et al. 2006).
By comparing the spectra in the 3 different flux states
(T400-Peak, T300-High and T300-Low),
one can see that the curvature changes significantly along the night
(at a confidence level >99.99%) and so does the Compton peak energy.
A clear trend emerges: both the curvature parameter b and
increase with the VHE flux.
At the maximum of the VHE flare, the spectrum is strongly curved
(
), with the Compton peak estimate at
GeV.
As the flux decreases, the curvature flattens (b=0.62 to 0.35),
while the IC peak shifts to lower energies (
GeV to
GeV, respectively).
A lower/higher EBL level does not change these results substantially:
a higher level yields similar curvatures (b=1.4, 0.76, and 0.48, respectively)
and slightly higher IC peak energies because of the generally harder spectra
(
0, 370, and 180 GeV, respectively).
It is important to recall that the absolute value of the curvature b
depends on the particular choice of the EBL spectrum used, but not the trend itself.
This trend is opposite to what is generally observed and expected
for the synchrotron emission in TeV blazars. For example,
in Mkn 421 the curvature b decreases as both
and the flux increase
(Massaro et al. 2004).
We also note that the spectral index
does not correlate (and possibly anti-correlate) with the curvature b,
in contrast to what is observed in the X-ray band for this (see next section)
and other HBL (Massaro et al. 2004).
4.2 X-ray spectra
The spectra were extracted
both by a uniform sampling of the whole exposure,
in different time bins (2-4-8-16 min), and strictly coincident with the VHE time bins.
The spectra were all fitted using an equivalent hydrogen column density
fixed at Galactic values (
cm-2)
with different source models.
On short integration times (<1 h), a single power-law model
provides statistically good fits for all datasets,
while evidence of curvature is found only when larger exposures are considered
or a wider energy band is available (for example including the RXTE data).
![]() |
Figure 11:
Left panel: spectrum for the total exposure, fitted with a broken power-law
plus galactic column density. The additional absorption feature in the 0.3-0.4 keV range is due
to the contaminants on the ACIS optical blocking filter, not yet fully accounted by the calibration.
It can be accounted for with a simple edge model at 0.31 keV and
|
Open with DEXTER |
Table 4: Fit of the X-ray spectra simultaneous to the VHE data.
The time evolution in the X-ray spectrum during the entire pointing - which extends few hours beyond the end of the HESS observation- is shown in Fig. 10. There is a clear trend of ``harder-when-brighter'' behaviour in the first part of the dataset, corresponding to the decaying phase of the main VHE flare. This behaviour is also followed by the small-amplitude flares, whose paths in the flux-index plane overlap tightly with the overall trend of the decaying phase (Fig. 10 right panel).
However, the relation changes in the last part of the observation
(MJD > 46.16):
as the X-ray flux starts to increase again, the spectral index continues to soften.
This ``softer-when-brighter'' behaviour in the rising phase of a new flare
reveals a change in conditions for the emitting region.
It is indicative of a slow acceleration/injection process,
whose timescale is comparable with the other timescales of the system (
).
The information about the flare then propagates from lower to higher energies as particles
are gradually accelerated (Ravasio et al. 2004; Kirk et al. 1998).
If the optical variations are indeed associated with the flaring zone,
the optical data would support this scenario as well, exhibiting
increasing flux just before the X-ray rise
at the end of the observation.
Together, the two patterns of the X-ray data draw part of a counter-clockwise
loop in the flux-index plane (Fig. 10).
Figure 11 shows the spectra of both the total exposure and
the RXTE simultaneous window.
The results of the fits performed on the HESS -simultaneous datasets
are given in Table 4.
All datasets correspond to strictly simultaneous windows except
for the T300-High spectra, for which the X-ray window
does not include the first 10 min of the 1.3-h VHE window above 300 GeV.
Since there are no significant spectral changes at VHE in that window,
the VHE spectrum can be considered to accurately represent the
-ray spectral shape in the X-ray window.
For all spectra in Table 4, there is clear evidence of curvature,
and the single power-law model is rejected with high confidence (F-test > 99.99%).
The spectra show a continuous steepening towards higher energies up to
20 keV,
which is well represented by both a broken power-law and log-parabolic models.
A power-law with an exponential cutoff is excluded as well (
)
for the spectra with the highest statistics
(T200 and total spectrum).
The drop rate in the cutoff region is significantly slower than
and also slightly slower than
,
as indeed expected for the synchrotron emission of a particle distribution
with an exponential cutoff (Aharonian 2000).
As is clear from Fig. 10 and Table 4, during all times the X-ray spectrum of PKS 2155-304 remains steep, with a convex shape and no signs of flattening at high energies (as instead found in XMM-Newton observations performed in November 2006; Zhang 2008; Foschini et al. 2008). This means that the peak of the synchrotron emission has not entered the observed energy range at any time, and that there is no sign of the possible emergence of the IC component in the hard X-ray band.
It is interesting to compare the curvature parameters and SED peak
location given by the log-parabolic fits.
Both the spectral index and the curvature increases (slightly) as the flux decreases.
This is also corroborated by the fits of spectra extracted in even shorter intervals at
the two extreme of the X-ray flux range (namely T300-Xmax and T400-Xmin).
The log-parabolic fit yields
and
versus
and
,
respectively, for an integrated
flux
and 1.65
10-10 erg cm-2 s-1.
The change in the two spectral parameters, however, is such that the estimate
of the location of the SED peak remains basically constant:
for all spectra, the synchrotron
falls within the range 40-50 eV
(with a typical 1-
statistical error of
20 eV).
In contrast to the behaviour in
-rays, in the X-ray band
the photon index shows a positive correlation with the curvature b,
as typically observed for example in Mkn 421 (Massaro et al. 2004).
The absolute values of the curvature are similar to those found
for most other HBL (Massaro et al. 2008).
![]() |
Figure 12:
Plot of the simultaneous spectral and flux variability
in the X-ray (blue circles) and VHE (red triangles) bands, in the T300-X window.
The spectra have been extracted in the same time-bins,
with integration times of 7 and 14 min (before and after MJD |
Open with DEXTER |
5 X-ray vs. TeV correlations
5.1 Spectral variability
The exceptional -ray brightness observed in this night,
coupled with the sensitivity of the HESS array and the continuous coverage provided
by ,
allows the emission in the two bands to be compared
with unprecedented time resolution in the spectral domain as well.
Figure 12 shows the simultaneous flux and spectral properties
measured in 7 and 14 min time bins, in the T300-X window.
Inside this window, the VHE spectral index can be well constrained (0.1) over
approximately a decade in energy (0.3-2 TeV).
The different binning was chosen to achieve comparable S/N ratio during the night,
and as a good compromise between spectral determination at VHE and time resolution
(see Sect. 4.1).
Both X-ray and VHE spectra have been extracted in exactly the same time bins.
The spectra were fitted with a single power-law model, which provides
a good fit for each time bin. The integrated energy fluxes were
calculated using the specific spectral value measured in each bin.
Two general properties can immediately be noted.
The first is that the VHE emission shows a definite correlation with the X-ray emission
not only in flux but also spectrally.
The spectral evolution follows the same overall pattern in the two bands, although
with different amplitudes. The correlation coefficient between the X-ray and -ray
spectra is r=0.65, with a probability P<0.1% of a chance correlation.
The second property, as previously illustrated by Fig. 3,
is that the source shows amplitude variations much larger in -rays than in X-rays.
This is now evident also for the spectra, although not as dramatically as for the flux:
the spectral variation at VHE
is about 3 times the variations in the X-ray band
(
vs.
).
The combination of such large-amplitude variability at VHE with correlated but small-amplitude variations in X-rays yields one of the most striking features of this dataset: the VHE flux varies more than quadratically with respect to the X-ray flux during a decaying phase.
5.2 Cubic relation between X-ray and TeV fluxes
Figure 13 shows the VHE flux as a function of the X-ray flux, in a log-log diagram. The data are divided into three subsets (``A'', ``B'', and ``C'') corresponding to three characteristic epochs: epoch ``A'' covers the first 35 min of the simultaneous window; epoch ``B'' corresponds to the full rise and decay phases of the small-amplitude flare at MJD
The data were fitted with a linear relationship in the log-log space
(
), for the total dataset and in each subset separately.
The results are reported in Table 5, together with the fits of the same
datasets with a finer sampling (4-min bins).
The -ray flux traces the variations in the X-ray flux
far more than quadratically, namely approximately as
.
With the exception of the first few minutes of epoch A,
all points lie on a narrow path, also during
the small flare on MJD
45.96 (epoch B).
In epoch A, instead, the two emissions do not seem to correlate.
The lack of correlation is limited to a few points and in a short interval;
however, one may speculate whether this is caused by the rapid, low-significance
structures in the VHE light curve,
which are not evident in X-rays (as discussed in Sect. 3.3).
One of these subflares is indeed present in epoch A
around MJD
0 =45.925 (see Fig. 6), and its exclusion
does bring the -ray emission more in line with the X-ray pattern.
This type of
-ray subflares on top of correlated emissions
have been recently envisaged by Ghisellini et al. (2009), but more sensitive
instruments are required to draw any conclusions.
![]() |
Figure 13:
Plot of the |
Open with DEXTER |
In the epochs B and C, the cubic correlation is obtained by considering both
the two zones separately and together, for which an even steeper slope of
is obtained.
This cubic correlation is robust with respect to the inclusion
or exclusion of single data points and, in particular,
does not depend on the lowest VHE point.
The flux-flux correlation is plotted using the same units for both X-ray and VHE bands, namely the integrated energy fluxes. Compared to previous studies, which used the observed event rates, our approach is more consistent and it is allowed by the good spectral determination in each time bin. However, we remark that the measured relation does not depend significantly on the particular approach used (see discussion in Fossati et al. 2008): a cubic relation is also obtained by using the event rates, both in the VHE band (as photons cm-2 s-1) and in the X-ray band (count rate).
The correlation found in the total dataset is less steep than in each subset, while in the B+C epoch it is slightly steeper than for each of B and C separately. This can be caused by a possible shift in the flux-flux paths among different datasets/epochs. While individual paths still obey a specific steep trend, taken together they can produce a flatter (or steeper) envelope. This effect was indeed observed in Mkn 421 (Fossati et al. 2008), when considering data for different days.
During the decaying phase of a flare,
a cubic relation between the -ray and X-ray fluxes
is not easy to explain even for a source in Thomson condition,
if both fluxes sample the emission beyond the respective SED peaks
(Katarzynski et al. 2005).
It is the first time that such a steep slope has been observed in the history of
the X-ray/TeV correlation studies,
though indication of a super-quadratic relation was recently
reported for Mkn 421 (Fossati et al. 2008), during single flares.
Table 5:
Values of the slope
of the correlation
.
Fluxes integrated over each respective energy band (0.5-5 keV and 0.3-3 TeV)
and in strictly simultaneous bins. The parameter is shown for fits performed with two different binnings
(4 min and 7-14 min) and over three different intervals, as shown in
Fig. 12.
Table 6:
Values of the slope
of the correlation
,
for fluxes integrated over different energy bands, as indicated.
The 3-15 keV flux is obtained by extrapolation of the power-law model in the passband.
Fit of the dataset ``B+C'' in the 7-14 min binning.
These correlations have been studied so far mainly with the RXTE -PCA instrument, which samples higher energies than those observed here. If the spectrum changes with the flux, and with a ``harder-when-brighter'' behaviour as in this case, the amplitude of the variations changes with energy, and thus the slope of the correlation can depend on the observed band.
To quantify this effect, we also investigated the flux-flux relation
by extrapolating the spectrum in the RXTE band
(namely, integrating the best-fit model in the 3-15 keV range),
and dividing the VHE range into soft and hard bands
(0.3-0.7 and >0.7 TeV, respectively).
The result is shown in Table 6.
The same cubic correlation observed in and HESS translates into a
quadratic relation (in fact quite similar to that observed in Mkn 421)
between the hard X-ray and soft VHE bands, while
an even steeper slope ()
is obtained between the soft X-ray band and hard VHE band.
We note however that the cubic relation is not simply the effect of
a pivoting type of variability seen in different energy bands.
The VHE band is closer to the IC peak (i.e. the pivoting point)
than the X-ray band to the synchrotron one, thus the X-ray variations
should be larger than the VHE ones,
in contrast to what is observed.
It is the entire IC peak that has actually varied far
more than the synchrotron peak, as shown also by the nearly constant and cubic
values of the correlation between corresponding bands
(i.e., soft-soft and hard-hard, see Table 3).
Comparing these 2006 data (low state) with the
X-ray/TeV campaign of 2003 (Aharonian et al. 2005b),
the overall brightening
in the X-ray (2-10 keV) and VHE
(>300 GeV) bands is similar (a factor of 2.7 and 5, respectively),
and corresponds to a relation
between the two epochs.
Thus PKS 2155-304 has varied its overall synchrotron and IC luminosity
sub-quadratically on very long timescales, but super-quadratically
on intra-night timescales, at least during this major flaring event.
![]() |
Figure 14:
Gallery of simultaneous X-ray and VHE SED-pairs
in different states along the night. Left panel:
maximum (T300-Xmax blue triangles) and minimum (T400-Xmin, red squares)
states (see Table 1 and Fig. 2).
Right panel: simultaneous
+ RXTE and HESS spectra (T300-RXTE, blue squares).
For comparison, the following data are also plotted:
the VHE spectrum at the peak of the |
Open with DEXTER |
6 Spectral energy distributions
6.1 X-ray/
-ray spectra pairs
To highlight the evolution of the SED during the night,
a gallery of selected pairings of simultaneous X-ray and VHE spectra
is shown in Fig. 14.
The scales on both axes are kept the same for both X-ray and -ray energies,
to enable visually a correct comparison of the spectral slopes.
For reference, a selection of historical observations is also plotted,
in particular the data from the first X-ray/TeV multiwavelength campaign
performed on PKS 2155-203 in October 2003 (Aharonian et al. 2005b).
These data (obtained with RXTE and HESS) correspond to one of the historically lowest
states ever observed from this object.
The panels show the SED-snapshots taken in
the brightest/hardest state (T300-Xmax), in the faintest/softest state (T400-Xmin),
and simultaneously with the RXTE pointing (T300-RXTE).
In addition, Fig. 14 also shows
the T400-Peak spectrum (i.e., extracted around the maximum of the -ray flare;
see Table 3 and Fig. 8).
This spectrum unfortunately lacks X-ray coverage (the pointing started a few minutes later),
but it corresponds to the brightest
-ray emission ever recorded from PKS 2155-304.
Both synchrotron and IC peaks do not shift across
the observed passbands, despite the large flux variations.
There is no evidence of the dramatic changes displayed by Mkn 501 or 1ES 1959+650.
Only at the flare maximum does the Compton peak become visible in the
observed passband (between 400 and
600 GeV, depending on the EBL normalization).
The X-ray spectrum hardens apparently pivoting around the UV band.
This behaviour is typically observed also in Mkn 421, Mkn 501 and
1ES 1959+650, but in these sources the amplitude of the spectral hardening
tends to be significantly more pronounced, leading to a shift
of the synchrotron peak in the hard X-ray band.
In the VHE band instead the behaviour is more complex,
since the hardening at higher fluxes is also accompanied
by a stronger curvature/cutoff (see Fig. 14, right panel).
The slopes of the X-ray (above 1 keV) and VHE spectra are very similar,
going from
(
0.04) to 2.9 (
0.11) between the high and low states.
It is also interesting to note that the X-ray spectrum is
significantly less curved than the spectrum measured by BeppoSAX
during the high state of 1998 (Chiappetti et al. 1999).
While the slopes above few keV are quite similar (see Fig. 14),
the flare in this night seems characterized by a higher luminosity in the soft X-ray band.
6.2 Compton dominance
The time evolution
of the
fluxes close to the SED peaks
is provided by Fig. 3.
As one can see, the
/
ratio is of the order of
8,
but it is rapidly variable - on the same timescales as the flux variations -
decreasing to the usual values of
1 in a few hours.
We estimated the Compton dominance using also the more detailed
spectral shape obtained for the T300-High dataset,
and renormalizing the flux to the 2 and 4-min light curves.
Considering the integrated luminosity over a decade in energy,
namely 0.3-3 TeV and 0.3-3 keV, the
/
ratio
is
10 in the first minutes of the simultaneous window.
Assuming that the cubic trend between
-ray and X-ray fluxes is
maintained up to the flare maximum
(which occurred
25 min before the start of the X-ray observation),
one obtains
/
14 at the flare maximum.
The
flux at the peak of the SED can instead be estimated from
the log-parabolic fit, based on the assumption that the curvature of the spectrum
also remains the same outside the observed energy band.
Using the aforementioned procedure,
one obtains a
/
5 in the simultaneous window,
increasing to
6 at the flare maximum.
The values are lower because
the estimate of the synchrotron peak
energy (
45 eV) locates the X-ray band farther away from the synchrotron peak
than the VHE band is from the Compton peak (
400-600 GeV).
This is the first time that such high /
ratios are observed
in an HBL, irrespective of the amount of the intergalactic EBL absorption.
While the Compton dominance can be up to 100 in powerful FSRQ,
boosted by the IC emission on the intense external photon fields from the disk
and the BLR (Ghisellini et al. 1998; Sikora et al. 1994), so far it has been of the order of unity or less
in HBL.
High Compton dominances in HBL were previously obtained only in the presence of
a very high density of the EBL (Aharonian et al. 2002a,2006a), which is now considered
very unlikely (Franceschini et al. 2008; Madau & Silk 2005; Aharonian et al. 2006a).
![]() |
Figure 15: Synthetic SED of PKS 2155-304 showing the highest and lowest simultaneous states during this night, together with historical data (shown in grey, see Aharonian et al. 2005b; Bertone et al. 2000; Chiappetti et al. 1999, and references therein). The hard X-ray data (butterfly) corresponds to the RXTE -HEXTE spectrum in the high state of 1996 (Urry et al. 1999). The right axis gives the luminosity scale in erg/s. Highest state (blue triangles): T300-High spectrum scaled to the highest VHE flux in the 4-min light curve. Lowest state (red squares): T300-Low spectrum scaled to the lowest VHE flux in the 4-min light curve. The X-ray states in the corresponding time bins are practically equal to the T300-Xmax and T400-Xmin spectra, which are thus plotted here. The dashed line shows the one-zone SSC fit of the 2003 multiwavelength campaign (black circles, Aharonian et al. 2005b). |
Open with DEXTER |
6.3 Overall SED properties
The overall SED of PKS 2155-304 in the highest and lowest states during this night
is shown in Fig. 15, together with historical data.
To plot the -ray spectral shape in more detail
while preserving the amplitude variation,
the VHE spectra shown in Fig. 15 are the T300-High and T300-Low average spectra
described in Sect. 4.1 (see Figs. 7 and 9),
rescaled to match the highest and lowest fluxes in the 4-min light curve.
Since within these two subsets, the spectra are compatible with a constant value
(see Fig. 7),
this procedure should not introduce significant distortions in the VHE spectral shape.
For clearer visibility, the SED focuses on data above
1011 Hz,
thus excluding the radio frequencies (VLBI range).
With the flux and variability timescale (
3 h)
shown at optical (and higher) frequencies,
the synchrotron emission coming from this region becomes self-absorbed
already at frequencies below
1012 Hz, and is thus not expected
to contribute significantly in the radio range.
From the results of the log-parabolic fits,
it is possible to estimate the peak frequency and luminosity
of both the synchrotron and Compton emission.
By considering the highest state, the synchrotron and Compton peak luminosities
are estimated to be at
and
erg/s, respectively,
with peak frequencies of
50 eV and
260 GeV.
Extrapolating the X-ray data with
the observed trends up to the flare maximum,
one obtains
and
erg/s at
50 eV and
500 GeV, respectively.
In the lowest state, instead, the peak luminosities
become comparable
(
and
erg/s, respectively,
at
50 eV and
70 GeV).
As discussed in Sect. 4.1, even the lowest possible EBL density
does not alter substantially these estimates.
In the optical band, the contribution of the host galaxy is
negligible: the host galaxy is resolved in optical
(Falomo et al. 1991; Falomo 1996) and NIR (Kotilainen et al. 1998),
and found to be a giant elliptical galaxy of M(R)=-24.4.
This translates into an apparent
using the typical
colours for an elliptical galaxy (
V-R=0.61-0.71, Fukugita et al. 1995).
The optical flux of PKS 2155-304 is thus always dominated by the jet emission
(see e.g., Dolcini et al. 2007):
the historical light curves from long-term photometric monitoring in the V band
show variations in the range 12.3-13.9 mag (Carini & Miller 1992; Osterman et al. 2007).
During this night, the optical flux is very high but still far from
the highest fluxes observed from this object.
In the X-ray band, instead, the flux
is close to the highest state observed historically, as measured by
RXTE -PCA in 1996 (
1.6
10-10 erg cm-2 s-1, Urry et al. 1999).
PKS 2155-304 is observed frequently in the X-ray band, since it is a calibration
and monitoring source for XMM-Newton, , and Swift,
but was never found at the level observed during this night,
in the 2-10 keV band (see e.g. Massaro et al. 2008; Donato et al. 2001).
Quite interestingly, the spectrum in the highest state also seems to connect
smoothly with the flux and spectrum measured by RXTE -HEXTE in 1996
(Urry et al. 1999, butterfly in Fig. 15).
It is also interesting to note that the extrapolation to lower energies of the
log-parabolic fit for the average T200 spectrum matches quite well the flux
in the optical band.
7 Summary of the main observational findings
Before discussing the implications in the context of blazar physics, it is useful to summarize the main observational findings of this phenomenologically rich dataset.
- Large-amplitude
-ray variations are accompanied by small X-ray and optical changes. In a few hours, the
-ray flux changes by more than an order of magnitude, reaching a luminosity of
1047 erg/s, while the X-ray flux varies by only a factor
2 overall, and the optical V flux by less than 15%.
- The X-ray and
-ray emission correlate strongly, overall and on short (sub-hour) timescales. On very short timescales (few minutes), the behaviour might be more complex.
- There is no evidence of time lags between the X-ray and
-ray emissions, with a 95% upper limit of
3 minutes for the overall light curve. In addition, no lags are found between the hard and soft energies of each passband.
- The optical light curve shows a
15% rise that appears to start simultaneously with the
-ray flare, but develops on much longer timescales, reaching a plateau about 2 h later than the VHE peak. The optical emission does not show any correlation with the other two bands on short timescales.
- When correlated, the
-ray flux decreases as the cube of the X-ray flux (
). This cubic relation holds both during the overall decaying phase and considering shorter intervals separately.
- The X-ray and
-ray (>300 GeV) spectra correlate as well, following similar patterns in their time evolution, but again of different amplitudes. The VHE variations (
) are wider by a factor of 3 than those in the X-ray band (
).
- The
-ray spectra are significantly curved, and the curvature changes with time, in correlation with the flux state: the higher the flux, the more curved the spectrum (the curvature parameter b goes from
at the maximum to
in the low state).
- The synchrotron and Compton peaks show no strong shift in frequency
across the observed bands, despite the dramatic luminosity
changes (
the quiescent state,
in this single night), remaining close to their historical values. From the curvature of the spectra, the synchrotron peak can be estimated at
40-50 eV constantly along the night, while the Compton peak shifts from
GeV at the maximum to
70+110-10 GeV at the end of the night (uncertainties given by the range on the EBL normalization).
- A very large Compton dominance is observed
(
). This is the first time that such a high
ratio is seen in an HBL, irrespective of the level of intergalactic EBL absorption. However, it also evolves rapidly, decreasing in a few hours to the more usual values of
1.
- X-ray and VHE spectra shows a similar ``harder-when-brighter'' behaviour
in the simultaneous window. The X-ray data alone also sample the start
of another flare, characterized instead by a ``softer when brighter'' behaviour.
8 Discussion
The results obtained from this campaign seem to both corroborate and challenge the one-zone SSC interpretation at the same time.On the one hand, the strong correlation between variations in the X-ray and VHE bands - the emission follow the same variability patterns in terms of both flux and spectrum, and without apparent lags - do indicate that the same particle distribution, in the same physical region, is likely responsible for the activity in both energy bands. The simultaneity of the occurrence of the optical and VHE flares also suggests that the emission in all three bands is responding to the same flaring event.
On the other hand, the cubic relation during the decaying phase
cannot be easily accounted for
within a one-zone SSC scenario.
This is shown for example by Katarzynski et al. (2005),
who investigated the different X-ray/VHE correlations
achievable in a one-zone SSC scenario,
for a plausible range of physical parameters
and considering all possible combinations of fluxes from both sides of the SED peaks.
The relation between X-ray and -ray fluxes
when both bands sample the emission above their respective SED peaks
is typically less than quadratic. Even imposing the Thomson condition
for the IC scattering of X-ray photons, which in this case would require
the extreme values of
and
mG (see next par.),
at most a quadratic relationship can be obtained,
but not in the decaying phase if the latter is due to radiative cooling.
In general, correlations steeper than quadratic (cubic or even more)
are indeed possible, but only when the X-ray band corresponds to
frequencies below or close to the synchrotron peak, as in the case of the 1997 flare of Mkn 501
(see e.g., Tavecchio et al. 2001).
A further ingredient is therefore needed to obtain a cubic relation, in a one-zone SSC scenario. It is important to remind here that ``one-zone'' does not mean the request that the entire SED is produced by a single zone. It is generally understood that the SED is always formed by the superposition of radiation from different zones along the jet, both in space (e.g., the radio emission has to come from a much larger region than for the rapidly variable X-ray or optical emission, to avoid synchrotron self-absorption) and in time (multiple injections). What is generally tested with a ``one-zone scenario'' is the hypothesis that at any given time - but during large flares in particular - it is one single region or population that dominates the entire radiative output, determining both peaks of the SED. This scenario has been very successful in explaining so far the spectral and temporal properties of blazars, both among different objects and in single sources during large flares (e.g., Mkn 501, 1ES 1959+650). We now consider if this can also be the case for this flare of PKS 2155-304.
8.1 One-zone SSC analysis
8.1.1 Thomson condition and beaming factor
In a single-zone, homogeneous SSC model, the knowledge of the frequencies of the synchrotron and Compton SED peaks (








With the parameters measured for this flare (
eV,
TeV,
erg/s,
erg/s),
the Thomson limit for photons in the middle of the passband
(
keV)
requires that
,
mG and
cm.
This solution seems unrealistic: besides the quite extreme values
of the beaming factor and severe efficiency problems,
it is not consistent with the VHE spectra.
The Thomson
-ray spectrum should extend to 10 TeV
with the same slope shown by the X-ray spectrum up to 1 keV, in contrast
to observations.
For electrons emitting at the SED peaks, instead,
PKS 2155-304 is almost certainly in the Thomson regime.
The Thomson regime is already satisfied for
,
but
the condition of transparency for 1-TeV photons (see e.g., Begelman et al. 2008; Dondi & Ghisellini 1995)
requires
,
adopting for reference the variability timescale of the
main
-ray flare (
h).
The Thomson regime for the SED peaks is also indicated by the absence of a significant
change of
(<
)
in the presence of an inferred
shift of
.
Since in the KN regime
the ratio
,
the change in
should have been accompanied
by an increase in
by
(vs.
in Thomson),
bringing it well within the band.
Therefore, the SED peaks of PKS 2155-304 are in the Thomson regime,
but a part of the passband is most likely affected by KN effects.
With
,
consistency between the size of the emitting region
estimated from both the observed Compton dominance and the variability timescale is obtained,
yielding
cm,
mG and a Thomson condition
at
keV.
This is also the result obtained by an analysis on the
plane
following the analytical approach described in Tavecchio et al. (1998).
However, this solution is not consistent with the cooling times of the peak electrons
being equal to or shorter than the escape timescales.
Because of the low values of the magnetic field and high beaming factors,
in all the above cases the energy of the electrons cooling within the variability timescale
(
),
either by synchrotron or IC, is extremely high, namely
.
This value is well above
,
meaning that the whole
electron distribution up to the energies sampled by our observations
did not have time to cool.
In the one-zone frameset, therefore, the peaks of the SED cannot be explained by
radiative cooling. This result is quite different from all previous estimates
for the SSC parameters in PKS 2155-304, and is mainly due to the increase
by a factor 10 in the separation between the synchrotron and Compton peak frequencies.
8.1.2 Expanding blob
An intriguing possibility
is to explain the observed decrease of both synchrotron and IC emission
as adiabatic cooling due to a rapid expansion
of the emitting region from an initially very compact size (``explosion''),
with the total number of particles N roughly constant.
This hypothesis has two immediate advantages:
1) it accounts for the initial high value of the Compton dominance as well as its
rapid decrease
(since in the Thomson limit
,
where
is the average over the electron distribution,
see e.g. Ghisellini & Tavecchio 2008b);
2) it can explain in a natural way the change of curvature of the VHE spectra
through a change of internal transparency to
-
interactions.
The initial region cannot be too compact, or otherwise
it would not be transparent to -ray photons.
However, in the case of PKS 2155-304, the steep and curved VHE spectra
can allow for a moderate amount of possible internal absorption to be
considered (
-2, as obtained for example with
-40),
without requiring anomalous spectral shapes.
The optical depth
increases with
-ray photon energy as
,
where
is the energy spectral index of the synchrotron target photons
(
;
),
and has a radial dependence
R-2, for a constant N.
Therefore, internal absorption can explain the stronger curvature
in the brightest state and a rapid expansion would decrease the optical depth
making the
-ray spectrum less curved at lower fluxes, as observed.
In fact, the observed change of curvature is opposite to that expected
from radiative cooling (e.g., Massaro et al. 2008), though it could
also be due to a change of the maximum electron energy.
To obtain the cubic correlation, however, one must assume correlated variations
of a second parameter, in order to shift the radiative output
from the IC to the synchrotron channel.
This can be achieved by varying the magnetic field B (see e.g. Coppi & Aharonian 1999):
for a given particle injection, an increase of the magnetic field can lead to a reduction
(B-2)
of the flux of the inverse Compton
-rays while increasing the synchrotron emission.
Using the same formalism as in Katarzynski et al. (2005),
it is possible to find the relation that yields
.
The evolution of the radius R and magnetic field Bcan be parameterized as
R=R0 (t/t0)r and
B=B0 (t/t0)-m
(see also Atoyan & Aharonian 1999). The adiabatic losses sustained by the particles during
the expansion are taken into account.
With the values for the spectral indices before and after the synchrotron peak
of
(assumed for the optical spectrum) and
(as measured in the X-ray band), respectively,
a cubic correlation is obtained with
(
0.1 considering
between 0.5 to 0.9).
Namely, the magnetic field must increase as the blob expands
at a rate
,
and on the same timescales as the flux variations.
This implies that the total energy of the magnetic field
in the region must increase substantially, as
.
Thus it should be created either locally (presumably by turbulent dynamo effects)
or supplied from outside (see e.g., discussion in Atoyan & Aharonian 1999).
However, such strong and rapid amplification of the magnetic field
seems not consistent with the optical data.
Rapid variations of B within the emitting region are also bound to
affect the synchrotron emission before the peak, produced by particles not yet cooled.
With the previous parameters, the observed decay of a factor 2 in the X-ray band
would cause a decrease of the optical flux by 15%
(compare
vs.
in Katarzynski et al. 2005),
and on the same timescales as the X-ray and VHE variations.
This disagrees with the optical light curve,
which is still slightly rising (by
5%) and then remains
basically constant during the overall X-ray/VHE decay
(see Fig. 2).
While it might be possible to further trim this scenario
to cancel out any variation in the optical band,
this would require an extreme fine-tuning.
For all of these reasons, it is very unlikely that both of the peaks in the PKS 2155-304 SED during this night are produced by the synchrotron and SSC emission of one single zone.
8.2 Two-SED scenario
A simpler and possibly more realistic explanation is provided by the superposition of two SEDs, produced by two different emitting zones. The first is responsible for the usual ``persistent'' SED of PKS 2155-304, which, presumably, peaks in the UV and at a few tens GeV, but with rather low VHE fluxes. It is typically variable on longer timescales (

A two-zone scenario is rather common for explaining major flares in blazars. The main novelty of this event with respect to all previous HBL flares is that the bulk of the luminosity of the new component is now emitted in the Compton channel instead of the synchrotron channel. The synchrotron emission of this flare is not bright enough to ``break through'' the persistent emission and thus dominate both peaks of the SED.
Within this scenario, one can try to estimate the SED
of this new component at its brightest state during the simultaneous observations,
assuming that the flux of the persistent component is roughly constant.
This is shown in Fig. 16.
In the -ray domain, the flux of the persistent component
is supposed to be negligible with respect to the observed flare.
The spectrum of the flaring region is therefore given, to a first order,
by the highest VHE state directly observed (the same as in Fig. 15).
In the optical band, at the maximum of the flare the detected variation
is
15%, so the flux in the flaring zone should be 0.15
of the observed flux.
In the X-ray band, we have used the lowest-state spectrum
observed at the end of the night as background file for the highest-state spectrum.
As a result, a spectrum with flux
F0.5-5=1.98
10-10 erg cm-2 s-1 is obtained,
which is well fitted by a log-parabolic model with
and curvature
.
This gives the estimate for the synchrotron
peak position around 0.4 keV, which is also consistent with the optical flux being
much lower than the X-ray flux (see Fig. 16).
This underlying SED yields comfortable values for the synchrotron-Compton modeling, and becomes consistent with the peak being due to radiative cooling. Such scenario also agrees with the spectral variations being larger in the VHE band than in the X-ray band (for the same diluting effect), and would naturally account for the behaviour of the optical data as well, if the optical rise is indeed associated with the VHE flare. The optical band would be reacting to the electron injection in the rising phase but not in the decaying phase, due to the much longer cooling times. The variations at VHE can then be allowed to scale linearly or quadratically with the X-ray variations, as required by the specific modeling.
![]() |
Figure 16: Possible SED of the new flaring component in PKS 2155-304, which would vary ``up and down'' beneath the persistent emission of PKS 2155-304 (see text). Blue triangles: SED of the flaring component at the flux maximum inside the X-ray/VHE simultaneous window. Red squares: expected level of the X-ray flux assuming a linear relation between X-ray and VHE flux variations. For reference, the same T300-Xmax spectrum and optical data shown in Fig. 15 are plotted as well (highest black points). |
Open with DEXTER |
8.3 Diagnostic of the flaring region
Although the amplitude of the synchrotron variations of the new component is unknown, important constraints can still be derived on its properties in both cases of a quadratic or linear relationship between X-ray and
With the new parameters, a quadratic decay obtained through radiative cooling
is readily possible with a pure SSC scenario
because the peak of the synchrotron emission falls now directly within the passband.
Indeed a solution in the Thomson regime can be obtained with the
comfortable values of
,
Gauss,
and
.
However, the high Compton dominance requires
the emitting region to be very compact, with
cm.
The flare therefore would originate in a region whose size is
of the same order as the Schwarzschild radius of the putative central black hole,
which is estimated to be
(see discussion in Aharonian et al. 2007a).
If instead the X-ray flux scaled linearly with the VHE flux,
it implies that the new component has a high Compton dominance (20)
constant in time, during all flux variations.
This behaviour points towards
an origin of the
-ray peak from
external Compton emission rather than a pure SSC mechanism.
This is indeed expected in scenarios with a strong radiative interplay
between different parts of the jet, such as the ``Needle/Jet'' model proposed
by Ghisellini & Tavecchio (2008a): a compact and fast region moving throughout
a larger jet sees the dense target field produced by the latter
(which is thought to be responsible for the persistent SED), boosting significantly its Compton emission.
Unlike the way it is envisaged by the authors, however,
the SED of such needle should also contribute significantly in the X-ray band,
in order to explain the small-amplitude but correlated variability.
Alternatively, the dominant seed photons could come from
regions further down inside the jet, where the flow has already strongly decelerated
(i.e., at the VLBI scale, Piner & Edwards 2004; Georganopoulos & Kazanas 2003), or by circumnuclear radiation fields
if the flaring region is close to the central engine.
In the latter case, -
interactions with these photon fields
could leave a distinct absorption feature imprinted onto the broad-band
-ray spectrum (Aharonian et al. 2008a),
which the combined observations with Fermi-LAT and IACT might be able to
reveal (Costamante et al. 2007).
More complex models with several interacting zones or jet stratification
have also been developed, and recently applied to the variability
of PKS 2155-304 in 2006 (see e.g. Katarzynski et al. 2008; Boutelier et al. 2008).
They seems capable of reproducing some features of the present observations
(e.g., Boutelier et al. 2008).
8.4 New mode of flaring in HBL
On a more general basis, it is interesting to compare this flare of PKS 2155-304 with the other major flaring events observed in both X-ray and VHE bands, namely from Mkn 421 in 2000 (Fossati et al. 2008), Mkn 501 in 1997 (Krawczynski et al. 2002; Tavecchio et al. 2001) and 1ES 1959+650 in 2002 (Krawczynski et al. 2004).There are many common traits: they all display a pre-flare, ``persistent'' SED with the synchrotron emission peaking in the UV/soft-X-ray band, a steep X-ray spectrum that hardens during the flare pivoting around the UV/soft-X-ray band, and a flare luminosity approximately one order of magnitude higher than the typical source luminosity. The mechanisms and properties of the flare injection thus seem common. It is the radiative output that now differs significantly.
In the previous events, such a high luminosity was emitted mostly through the synchrotron process, leading to a dramatic shift of the peak position in the SED according to the new peak frequency of the emerging component. The typical Compton luminosity, even at the flare maximum, has always been equal to or less than the synchrotron power (using the same EBL model for all sources). In this event, instead, the bulk of the flare luminosity is emitted through the Compton channel, yielding only minor modifications of the overall synchrotron emission.
A bimodality therefore seems to emerge in the mode of flaring for HBL: either synchrotron dominated or Compton dominated, with the most extreme example possibly being provided by the ``orphan flare'' event of 1ES 1959+650, which likewise occurred during one single night (June 4, 2002).
It is intriguing to note that this difference might simply depend on the environment, namely
on the location of the flaring zone with respect to the region responsible
for the persistent SED: if the new injection/flare is taking place far away,
there is little radiative interplay between the two zones, leading to a typical SSC-type
flare. When the flare occurs close to it, or close to the black hole where external fields are
more intense, the outcome is external Compton-dominated flares.
More campaigns targeted on the intra-night variability are needed to address this issue,
but the diagnostic potential on the jet structure and the location of the
``-ray zone'' is very promising.
9 Summary and conclusions
A full night of simultaneous, uninterrupted observations
in the optical, X-ray and VHE bands was performed during an exceptionally bright state of
PKS 2155-304 in July 2006. A sampling of both light curves and spectra with
unprecedented detail is obtained.
For the first time among HBL, a high Compton dominance is observed,
with a peak luminosity reaching 1047 erg/s.
The variations in the X-ray and VHE bands are confirmed to be highly correlated,
both in flux and spectrally, but they follow a cubic relationship during the decay phase.
Homogeneous one-zone SSC scenarios do not provide a consistent explanation
for both the observed SED and the variability behaviour,
indicating that a single particle population cannot be responsible
for both peaks of the SED during this night.
We have interpreted the data as the emergence of a new component in the SED,
strongly Compton-dominated and thus without enough luminosity
in the synchrotron channel to overcome the ``persistent'' emission of PKS 2155-304.
This new component must be either very compact
- of the order of the Schwarzschild radius of the putative
central black hole (109
)
- if the emission mechanism is pure SSC,
or external-Compton dominated, as would be expected in models with
a strong radiative interplay between different parts of the jet.
The richness and quality of the data obtained from this exceptional campaign
provide a fundamental testbed for a time-dependent treatment of the emission scenarios,
which is needed to fully extract the information
on the physical conditions in the source (see e.g., Krawczynski et al. 2002; Boutelier et al. 2008; Coppi & Aharonian 1999).
This is beyond the scope of this paper, and therefore left to future studies,
but it is a necessary step forward with respect to more common parametric fits,
which simply postulate the prompt electron spectrum and treat different states
as uncorrelated emissions.
From an observational point of view,
the results from this night raise the bar for the requirements of future multiwavelength
campaigns on HBL, at least during major flaring events.
With flares as rapid as a few minutes (Aharonian et al. 2007a)
and flux changes of 1 order of magnitude in less than an hour,
sufficiently long, continuous and strictly simultaneous observations are mandatory
for a meaningful analysis.
Delays, gaps, or mismatches in the simultaneous coverage, even as short as 30 minutes,
can be fatal for the diagnostic potential.
The multiwavelength coverage should also care to sample the SED
on both sides of the emission peaks:
as shown in the present case, without the optical light curve some scenarios
could not be excluded.
In this respect, Fermi-LAT will provide the missing piece of information
on the
The flaring activity of PKS 2155-304 in July 2006
demonstrates in a compelling way that the fast, intra-night variability is
of fundamental importance to gain insights into the acceleration mechanism,
emission processes, and location and environment of the emitting regions,
which are simply lost or smeared out with a sparser, long-term sampling.
The final goal is to achieve full multiwavelength coverage of
large-amplitude and ultra-rapid events such as those observed on the night of July 27-28.
-ray hump
for many objects, though typically on longer timescales.
The all-sky monitor provided by this observatory will be of great importance
to catch the brightest Compton-dominated flares among HBL,
triggering X-ray and IACT observations and thus allowing the study of this apparent flare bimodality
(synchrotron or Compton-dominated) on a larger sample.
The support of the Namibian authorities and of the University of Namibia
in facilitating the construction and operation of HESS is gratefully
acknowledged, as is the support by the German Ministry for Education and
Research (BMBF), the Max Planck Society, the French Ministry for Research,
the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the
CNRS, the UK Science and Technology Facilities Council (STFC),
the IPNP of the Charles University, the Polish Ministry of Science and
Higher Education, the South African Department of
Science and Technology and National Research Foundation, and by the
University of Namibia. We appreciate the excellent work of the technical
support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris,
Saclay, and in Namibia in the construction and operation of the
equipment. The authors thank the team for the help and support
during the prompt response to our ToO request, as well as the RXTE and
Swift teams.
The authors wish to thank P. Coppi, G. Ghisellini and F. Tavecchio for
the support during the initial phases of the project.
This research has made use of the NASA/IPAC Extragalactic Database (NED)
which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National Aeronautics
and Space Administration.
References
Footnotes
- ...
- Supported by CAPES Foundation, Ministry of Education of Brazil.
- ... electrons
- Note that this case is different from
the condition where the observed
-rays are indeed produced by IC-scatterings occurring in the Klein-Nishina regime, or when the cooling itself is determined by Klein-Nishina losses, see e.g., Moderski et al. (2005).
- ... model
- See http://xspec.gsfc.nasa.gov/docs/xanadu/xspec/fluxerror.html
- ... 2007
- See http://www.universe.nasa.gov/xrays/programs/rxte/pca/doc/bkg/bkg-2007-saa/
All Tables
Table 1:
Summary of the subsets of VHE data used in this
paper (MJD = MJD-53 900).
Table 2: Spectral fit of the measured VHE spectra extracted in different epochs (see Table 1).
Table 3: Spectral fit of the same VHE spectra given in Table 2, but corrected for EBL absorption (statistical errors only).
Table 4: Fit of the X-ray spectra simultaneous to the VHE data.
Table 5:
Values of the slope
of the correlation
.
Fluxes integrated over each respective energy band (0.5-5 keV and 0.3-3 TeV)
and in strictly simultaneous bins. The parameter is shown for fits performed with two different binnings
(4 min and 7-14 min) and over three different intervals, as shown in
Fig. 12.
Table 6:
Values of the slope
of the correlation
,
for fluxes integrated over different energy bands, as indicated.
The 3-15 keV flux is obtained by extrapolation of the power-law model in the passband.
Fit of the dataset ``B+C'' in the 7-14 min binning.
All Figures
![]() |
Figure 1: VHE fluxes integrated in different energy bands, as a function of time, in time bins of two minutes. The time windows corresponding to the different energy thresholds are given in Table 1 (labelled accordingly, from top to bottom: T200 to T700). The dotted lines mark the positions of rapidly varying events on-top of the main flare (see text). |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Overall light curves of PKS 2155-304 in the night of July 29-30 2006,
as seen by HESS (T700, upper panel),
( lower panel, blue circles), and
the Bronberg Observatory (optical V band, red squares). Time bins of
4 min (3 for the V band).
The segments on the upper x-axis also show the two intervals corresponding to the
RXTE exposure (R label), and the two intervals of the Swift pointing (S label) reported in
Foschini et al. (2007). The vertical scales differ in each panel,
and have been adjusted to highlight the specific variability patterns.
Lower panel: the left axis gives the integrated
0.5-5 keV flux, the right axis gives the V-band
|
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Light curves of the
|
Open with DEXTER | |
In the text |
![]() |
Figure 4: Cross-correlation analysis of the hard versus soft bands at VHE ( upper panel) and at X-ray energies ( lower panel). Upper panels: a) DCF of the 300-700 GeV and the >700 VHE band. The line around the peak shows the best fit Gaussian plus linear function, with a maximum at 28 s. b) Corresponding cross-correlation peak distribution (CCPD) of 10 000 simulated light curves. The rms of the distributions is 30 s. The dotted line marks the position of the maximum in a). Lower panels: c) DCF of the 0.2-1.0 keV and 2.0-6.0 keV X-ray band. The line around the peak shows the best fit Gaussian plus linear function, with a maximum at -82 s. d) Corresponding CCPD of 10 000 simulated light curves. The rms of the distributions is 202 s. The dotted line marks the position of the maximum in c). |
Open with DEXTER | |
In the text |
![]() |
Figure 5: Cross-correlation between the X-ray and VHE light curves: a) DCF of the >300 GeV light curve and the LETG 0.2-6 keV band.The blue line shows the best fit Gaussian plus linear function, with a maximum at -10 s. b) Corresponding cross-correlation peak distribution of 10 000 simulated light curves. The rms of the distributions is 76 s. The dotted line marks the position of the maximum in a). |
Open with DEXTER | |
In the text |
![]() |
Figure 6: HESS and Chandra light curves in the simultaneous time windows corresponding to a 300 GeV threshold (T300-X in Table 1). Two-minute time bins. Upper panel: integral fluxes above 300 GeV. Lower panel: 1st-order LETG count rate in the 0.2-6 keV band. |
Open with DEXTER | |
In the text |
![]() |
Figure 7:
Left panel: integral flux >300 GeV and photon index
as a function of time (T300 dataset). Horizontal error bars show the time
interval of each bin, going from 7 to 14 min before and after MJD |
Open with DEXTER | |
In the text |
![]() |
Figure 8:
Left panel: integral flux >500 GeV and photon index
as a function of time (T500 dataset). Horizontal error bars show the time
interval of each bin, going from 14 min. at the beginning to
28 min. towards the end of the night. The shaded area shows the time window
where the |
Open with DEXTER | |
In the text |
![]() |
Figure 9: Selected VHE spectra: average spectra for the T300-Low ( left) and T300-High ( middle) datasets (see Fig. 7), and the average spectrum above 200 GeV (T200, right). Open symbols corresponds to the spectra corrected for EBL absorption as described in Sect. 4.1.2. |
Open with DEXTER | |
In the text |
![]() |
Figure 10:
Evolution of the X-ray spectrum with time, for the whole
exposure. Left panel: each 8-min bin is fitted with
a single power-law model plus galactic absorption.
The HESS window ends at MJD |
Open with DEXTER | |
In the text |
![]() |
Figure 11:
Left panel: spectrum for the total exposure, fitted with a broken power-law
plus galactic column density. The additional absorption feature in the 0.3-0.4 keV range is due
to the contaminants on the ACIS optical blocking filter, not yet fully accounted by the calibration.
It can be accounted for with a simple edge model at 0.31 keV and
|
Open with DEXTER | |
In the text |
![]() |
Figure 12:
Plot of the simultaneous spectral and flux variability
in the X-ray (blue circles) and VHE (red triangles) bands, in the T300-X window.
The spectra have been extracted in the same time-bins,
with integration times of 7 and 14 min (before and after MJD |
Open with DEXTER | |
In the text |
![]() |
Figure 13:
Plot of the |
Open with DEXTER | |
In the text |
![]() |
Figure 14:
Gallery of simultaneous X-ray and VHE SED-pairs
in different states along the night. Left panel:
maximum (T300-Xmax blue triangles) and minimum (T400-Xmin, red squares)
states (see Table 1 and Fig. 2).
Right panel: simultaneous
+ RXTE and HESS spectra (T300-RXTE, blue squares).
For comparison, the following data are also plotted:
the VHE spectrum at the peak of the |
Open with DEXTER | |
In the text |
![]() |
Figure 15: Synthetic SED of PKS 2155-304 showing the highest and lowest simultaneous states during this night, together with historical data (shown in grey, see Aharonian et al. 2005b; Bertone et al. 2000; Chiappetti et al. 1999, and references therein). The hard X-ray data (butterfly) corresponds to the RXTE -HEXTE spectrum in the high state of 1996 (Urry et al. 1999). The right axis gives the luminosity scale in erg/s. Highest state (blue triangles): T300-High spectrum scaled to the highest VHE flux in the 4-min light curve. Lowest state (red squares): T300-Low spectrum scaled to the lowest VHE flux in the 4-min light curve. The X-ray states in the corresponding time bins are practically equal to the T300-Xmax and T400-Xmin spectra, which are thus plotted here. The dashed line shows the one-zone SSC fit of the 2003 multiwavelength campaign (black circles, Aharonian et al. 2005b). |
Open with DEXTER | |
In the text |
![]() |
Figure 16: Possible SED of the new flaring component in PKS 2155-304, which would vary ``up and down'' beneath the persistent emission of PKS 2155-304 (see text). Blue triangles: SED of the flaring component at the flux maximum inside the X-ray/VHE simultaneous window. Red squares: expected level of the X-ray flux assuming a linear relation between X-ray and VHE flux variations. For reference, the same T300-Xmax spectrum and optical data shown in Fig. 15 are plotted as well (highest black points). |
Open with DEXTER | |
In the text |
Copyright ESO 2009
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.