Up: Multi-colour optical monitoring of 0716+71
Subsections
Present light curves (Fig. 3) in combination with the optical light
curves given by Wagner et al. (1996) and by
Ghisellini et al. (1997) are
used to decipher behaviour of the long-term optical variability of the blazar.
The 8 months (in 1990/1991 winter) long relative light curve given by
Wagner et al. (1996) shows a variation of about 2.5 mag in R passband. The
source remained in "low'' state for about 50 days starting from
.Then, after a slight brightening, it declined to a minimum intensity level
around
. After that it brightened (
2.5 mag in R) rapidly to
reach a maximum intensity level around
. On the other hand, over
the 5 months (November 1994 to April 1995) observational period, the light
curve in R passband given by Ghisellini et al. (1997) shows that the source
brightened after
, remained bright for
50 days, and then
faded rapidly to reach a minimum intensity level around
. Thus
in the long-term optical variability of the blazar, events with rapid
brightening as well as fading (only one in both cases) have been observed
in the above mentioned two R passband light curves. It has to be noted that
the durations of both events are almost the same about 30 days.
The average calibrated B,V,R and I magnitudes of the blazar during present
observations are
14.7, 14.2, 13.8 and 13.3 respectively. A comparison
of these numbers and the present light curve (Fig. 4)
with optical light curves given by Ghisellini et al. (1997)
indicates that during the entire period (
30 days) of our campaign,
the blazar was in a relatively low state without any rapid
large amplitude (
1 mag) brightening or fading as the exhibited
maximum variations are only
0.2 mag in all four passbands.
As seen from Fig. 3, the blazar remained moderately active during
the 4-weeks of monitoring, the observed variations often being much
larger than the rms scatter of the relative magnitudes of the
pair of comparison stars, which is found to be
0.014 mag for
all the four passbands. Table 3 lists the date, amplitude
and duration of those outbursts whose profiles are clearly defined.
There seems to be a weak correlation between amplitude and duration
of the flares in the sense larger the amplitude longer its duration.
For shorter duration flares, the rising and decaying times appear
approximately equal and profiles are symmetric with no indications of a
"plateau'' longer than one day. Similar behaviour has also been noticed by
Ghisellini et al. (1997). For the largest outburst, the profile is
asymmetric with rising time about one day and decaying time about 3 days.
Table 3:
Clearly defined outbursts of the blazar S5 0716+71
|
From the DLCs of all 4 passbands, it
appears that the blazar outbursts are superposed on a constant base
level emission. This behaviour differs from those observed during the
extended optical monitoring campaigns of Wagner et al. (1996)
and Ghisellini
et al. (1997) when the base levels were found to either drop from a "high'' to
a "low'' state or vice-versa by almost a factor of 2 or so within about a day
(see also Quirrenbach et al. 1991). The quasi-periodicity of the optical light
curve with a characteristic time scale of 1 day, which was then found to
persist for a week is not clearly evident during our observations, only some
indication of it is present during the first week (Fig. 3). A
rigorous comparison of the present data with the earlier
dataset would be difficult, because the location of this blazar
restricted the monitoring from India during the month of March to
just 4-6 hours per night, at most, thereby leaving large gaps in
the light curves. It is clear, nonetheless, that in all four
passbands the blazar exhibited variations of up to
0.2 mag between two
consecutive nights, as measured relative to both comparison stars. Furthermore,
the light curves in the four passbands are tightly correlated, indicating that
the spectrum of the flaring component is not much different from that of the
"base'' emission. Recall that a close similarity of the light curves at R, V
and B during the quasi-periodic variations was also noticed during the 1990
campaign (Quirrenbach et al. 1991; Wagner et al. 1996). However, the campaign
by Ghisellini et al. (1997) indicates that in the "low'' optical state of the
blazar, the (B-R) spectral index responds to fast optical variations occurring
on day-like time scales, the spectrum becoming bluer with increasing brightness
in R.
In order to study the correlation between flux and optical spectral index
(
) defined by the BVRI values of present observations,
we plot the standard R magnitude and
against time in Fig.
4. We determined the R values from the compressed DLCs
presented in Fig. 3 and the calibrated R magnitude of star
1 given in Table 1. The spectral index
has been
calculated by a least-square linear fit procedure, after dereddening the
observed calibrated flux of the blazar in BVRI passbands. For this,
following Ghisellini et al. (1997), the reddening corrections were taken
as AB = 0.30, AV = 0.23, AR = 0.19 and AI = 0.14 magnitudes.
The regression coefficients of the linear fit are always
1.
The values of
obtained in this way vary from 0.81 to
1.01 with a mean value of 0.84
0.043, and do not have any significant
correlation with the flux (see Fig. 4).
Ghisellini et al.
(1997) have also obtained a similar result. However, the values of their
spectral index,
have some what larger
range (from 0.81 to 1.15) and higher mean value, 0.94.
![\begin{figure}
\includegraphics [height=12cm,clip]{fig4.ps}
\end{figure}](/articles/aas/full/1999/03/ds8009/Timg27.gif) |
Figure 4:
The light curve in the R passband (lower panel) is compared with
the corresponding optical spectral index (upper panel) |
An important issue in the variability studies concerns the shape(s) of
the profiles of the flares. For some of the densely monitored blazars,
the large individual optical flares seen on the time-scale of
1 day
are characterized by exponential growth and decay profiles, as, e.g., in the
cases of the intra-day variable blazars PKS 2155-304
(Urry et al. 1993) and
S5 0954+658 (Wagner et al. 1993). In contrast, the individual flares on
day-like time scale recorded in 1990 and 1994-95 optical monitoring of the
present blazar S5 0716+71 are well described by linear profiles (cf.
Wagner
et al. 1996; Ghisellini et al. 1997). Since any dichotomy of
this nature can signify fundamentally different emission processes,
we have made an attempt to determine the shapes of the individual
optical flares of S5 0716+71 recorded during our campaign.
As seen from Figs. 1 and 2, the blazar showed on 3 nights
prominent optical flares with rates
per hour, sustained
over a minimum of two hours (see also, Fig. 5). Note that the
positive bump peaking around
UT on the DLCs of March 4 is clearly
related to the variation of the comparison star 1 (Fig. 1) and hence
we have ignored the affected portion of the blazar DLC from subsequent
analysis. Since all three flares indicate a linear temporal variation
on the magnitude scale, we have fitted least-square regression lines
to these flaring segments of the DLCs. These best-fit lines are shown in
Fig. 5 and their slopes are given in Table 4, together
with the regression coefficients. It is interesting that for each flare the
slopes are essentially the same for the different passbands. The difference
in the slopes is always
. It is therefore not statistically
significant. Moreover, the regression coefficients for the linear fits are
90% in all cases, excepting the I-band profile on March 18 which is
noisy, as evident from the DLC of the comparison stars (Fig. 1).
Thus, at least over the few hours spanned by these observations, all the three
prominent events of intra-night variability can be described by linear trends
on magnitude scale (which, therefore, corresponds to an exponential intensity
variation). Similar linear intra-night magnitude variations in B and R bands
have been noticed by Ghisellini et al. (1997) on two occasions. Unfortunately,
none of the flaring segments of the present DLCs
encompass the intensity turnover point (which is not unexpected considering
the modest durations of these DLCs). Therefore, the question of linear
vis-a-vis exponential variation cannot yet be settled conclusively, though an
exponential intensity variation seems to be consistent with all the prominent
intra-night flares recorded in the present as well as Ghisellini et al. (1997)
optical observations of S5 0716+71.
It would be of great interest to enquire if the shapes (linear/exponential)
of the outbursts of a given blazar depend on the time-scale of the
outburst and whether they vary from one occasion to another.
![\begin{figure}
\includegraphics [angle=-90,width=14.5cm,clip]{large.ps}\end{figure}](/articles/aas/full/1999/03/ds8009/Timg32.gif) |
Figure 5:
DLCs relative to the comparison star 1 in the
R and I passbands for those three nights when the
blazar intensity varied by per hour for a
minimum of 2 hours. The data for the remaining 2 passbands have
not been plotted as the temporal coverage was not so dense as in
R and I, due to lower sensitivity of the CCD. Note that the
positive bump seen in the profiles of March 4 near 19 UT is
clearly due to a variation of the comparison star (see Fig. 1) and
therefore has been ignored in the computation of the best fit-line |
Table 4:
Slopes and regression coefficients (
) of the
least-square linear fits to the intra-night magnitude variations
|
Since on many nights in the present campaign, a fairly dense temporal
coverage was achieved simultaneously in the different passbands, it is
possible to look for any ultra-rapid fluctuations on time scales shorter
than
1 hour. In particular, such events can provide important clues
to relativistic beaming of the AGN's optical radiation (e.g.,
Guilbert et al. 1983). Indeed, based on the 1990 campaign
substantial flickering of this blazar on time scales as short as
15 min was inferred from the structure function analysis
of the optical light curve (Wagner et al. 1996). A close look at
Fig. 1 reveals many events of ultra-rapid fluctuations, often occurring
in more than one passband simultaneously. Table 5 provides
a log of such individual events which were detected during almost every
observing run. However, it turned out that practically each one
of these fluctuations is due to one of the comparison stars, since
the simultaneous DLC relative to the other comparison star does not show
the corresponding fluctuation. The only exception is a 0.15 mag jump seen
at
16.5 UT on March 3; however, its reality is uncertain since
the feature is a single data point seen only on the V-band DLC
(Fig. 1). Thus, the availability of differential light curves
using multiple comparison stars serves as a powerful discriminator
and a safeguard against serious misinterpretation of the data.
It may be noted that the amplitudes of these ultra-rapid fluctuations
are typically of order of a few percent and thus the present optical data
of 1994 do not exclude the possibility of the blazar exhibiting lower level
ultra-rapid variations, similar to those inferred by Wagner et al. (1996)
from the statistical analysis of the 1990 light curves of this blazar.
Table 5:
Rapid intensity fluctuation events seen
on the DLCs, and the comparison stars most likely responsible for the events
|
Up: Multi-colour optical monitoring of 0716+71
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