A&A 486, 99-111 (2008)
DOI: 10.1051/0004-6361:20079111
A. I. Shapovalova1 - L. C. Popovic2,3 - S. Collin4 - A. N. Burenkov1 - V. H. Chavushyan5 - N. G. Bochkarev6 - E. Benítez7 - D. Dultzin7 - A. Kovacevic8 - N. Borisov1 - L. Carrasco5 - J. León-Tavares5,9 - A. Mercado10 - J. R. Valdes5 - V. V. Vlasuyk1 - V. E. Zhdanova1
1 - Special Astrophysical Observatory of the Russian AS,
Nizhnij Arkhyz, Karachaevo-Cherkesia 369167, Russia
2 -
Astronomical Observatory, Volgina 7, 11160 Belgrade 74, Serbia
3 - Alexander von Humboldt Fellow, presently at Max Planck Institute for
Radioastronomy, Bonn, Germany
4 -
LUTH,
Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place
Jules Janssen, 92190 Meudon, France
5 -
Instituto Nacional de Astrofísica, Óptica y
Electrónica, Apartado Postal 51, CP 72000, Puebla, Pue. México, México
6 -
Sternberg Astronomical Institute, Moscow, Russia
7 -
Instituto de
Astronomía, UNAM, Apartado Postal 70-264, CP 04510, México
8 -
Department of Astronomy, Faculty of Mathematics, University
of Belgrade, Studentski trg 16, 11000 Belgrade, Serbia
9 -
Max-Planck Institute für Radioastronomie, Auf dem Hügel
69, 53121 Bonn, Germany
10 - Universidad Politécnica de Baja
California, Av. de la Industria # 291, CP 21010, Mexicali, B.C.,
México
Received 20 November 2007 / Accepted 7 April 2008
Abstract
Aims. Results of long-term spectral monitoring of the active galactic nucleus of NGC 4151 are presented (11 years, from 1996 to 2006).
Methods. High quality spectra (S/N>50 in the continuum near H
and H
)
were obtained in the spectral range
4000 to 7500 Å, with a resolution between 5 and 15 Å, using the 6-m and the 1-m SAO's telescopes (Russia), the GHAO's 2.1-m telescope (Cananea, México), and the OAN-SPM's 2.1-m telescope (San-Pedro, México). The observed fluxes of the H
,
H
,
H
,
and HeII
4686 emission lines and of the continuum at the observed wavelength 5117 Å were corrected for the position angle, the seeing, and the aperture effects.
Results. We found that the continuum and line fluxes varied strongly (up to a factor 6) during the monitoring period. The emission was maximum in 1996-1998, and there were two minima in 2001 and in 2005. As a consequence, the spectral type of the nucleus changed from a Sy1.5 in the maximum activity state to a Sy1.8 in the minimum state. The H,
H
,
and He
4686 fluxes correlated well with the H
flux. The line profiles were strongly variable, showing changes of the blue and red asymmetry. The flux ratios of the blue/red wings and of the blue (or red) wing/core of H
and H
varied differently. We considered three characteristic periods during which the H
and H
profiles were similar: 1996-1999, 2000-2001, and 2002-2006. The line-to-continuum flux ratios were different; in particular during the first period (1996-1999),
Conclusions. We discuss the different responses of H
and H
to the continuum during the monitoring period.
Key words: galaxies: active - galaxies: individual: NGC 4151
The brightest Seyfert 1.5-type galaxy NGC 4151 has been studied in detail at all wavelengths (e.g. Peterson 1988; and Ulrich 2000). The nucleus of this galaxy shows flux variability in a wide wavelength range, with time scales from a few hours (in the hard X-ray, e.g. Yaqoob et al. 1993) to several months (in the infrared, e.g. Oknyanskij et al. 1999).
In the optical range, the active galactic nucleus (AGN) of this galaxy is also known to display flux variations of the continuum and of the lines up to a factor ten or more (e.g. Peterson 1988; Clavel et al. 1990; Maoz et al. 1991; Shapovalova et al. 1996; Ulrich & Horne 1996; Sergeev et al. 2001; Lyuty 2005). These variations occur on time scales of several days (Maoz et al. 1991).
NGC 4151 has been the subject of echo-mapping observational
campaigns. The main aim of AGN monitoring campaigns was to
determine the size of the broad line region (BLR) by measuring the
time delay between the emission line fluxes, in response to the variations in the
continuum flux (see Peterson 1993, for a review). It is interesting
that different authors have found different time lags: Antonucci &
Cohen (1983) observed NGC 4151 at least once a month from 1980 May through 1981 July. They have also found that the BLR radius
was less
than 30 lt-days. These observations were used
by Peterson & Cota (1988) in combination with their own
observations (performed from 1985 to 1986), and they found a BLR radius of lt-days. Gaskell & Sparke (1986)
applied the cross-correlation method to the ultraviolet data
of Ulrich et al. (1984) and to the optical data of Antonucci
& Cohen (1983), and they found a BLR size between 2 lt-days (for
HeII
4686) and 20 lt-days (for H
).
On the other hand, Maoz et al. (1991) analyzed the observations (optical
continuum, H,
and H
)
from 67 nights during a 216-day period
between December 15, 1987, and July 18, 1988. They found a BLR size of
lt-days. They also showed that on a time scale of
days, the wings of
H
and H
varied in phase, and they ruled out a purely
unidirectional radial motion in the BLR (either inflow or outflow).
A 10-year long monitoring campaign (1988-1998) of the NGC 4151
nucleus was performed with a sampling of 1-2 observations per month, using
the CCD spectrograph of the 2.6-m CrAO telescope, which covers the
H
and H
spectral range (Malkov et al. 1997;
Sergeev et al. 2001). The time delays between the broad lines and the continuum at 5100 Å were 1.5-10 days for the Balmer lines and 0.0-2.6 days for the HeII
4686 line
(Sergeev et al. 2001). Bentz et al. (2006) analyzed the
observations performed between February 27 and April 10, 2005. They obtained a time lag for the H
line
of
6.6+1.1-0.8 days.
NGC 4151 was also monitored in the UV. Clavel et al. (1990)
analyzed the spectra obtained with the IUE satellite during two months from November 29, 1988, to January 30, 1989 (with a 4 day sampling time) and found
a time lag of
days between the continuum and the lines CIV
1549 and Mg II
2798. In addition, NGC 4151 was observed with IUE from November 9 to
December 15, 1991 (35 days), with a one-day sampling time (see Ulrich &
Horne 1996). Ulrich & Horne (1996) found that the time delay in the continuum at
3000 Å with respect to that at 1320 Å was less than one day (i.e. the UV
continuum is emitted by a region with a dimension less than one light day). The broad UV emission lines showed large variations that
closely followed the continuum ones. For CIV
1549,
the time lag relative to the continuum was 2.4-3.8 days.
Ulrich & Horne (1996) also observed deep
blue-shifted absorption lines. They are produced by a low-velocity gas that covers the major part of the rapidly varying
continuum source and the emission-line regions. This material is moving
outwards along the line of sight and may be located anywhere
beyond 15 lt-days. Kaspi et al. (1996) observed NGC 4151
during two months in 1993, with a time resolution of about one day. They
found no evidence of any time lag between the optical and UV continuum, and a time lag of 0-2 days for
H
and 0-3 days for H
.
Metzroth et al.
(2006) re-analyzed the IUE spectra of NGC 4151 obtained in 1988
(Clavel et al. 1990) and in 1991 (Ulrich & Horne 1996), using the
New Spectral Image Processing System (NEWSIPS). This allowed the photometric precision to
be improved and the S/N ratio to be increased by 10%-50%.
They found that the time lags of the revised responses to changes of the continuum were
3-7 days for
CIV
1549, HeII
1640,
CIII]
1909, and MgII
2798.
The results mentioned above indicate that the dimension of the BLR varies among the emission lines (radial stratification) and is changing with time. Contradictory results have been obtained, even for the same species, after using the modified processing system and re-analyzing old data (for instance, Antonucci & Cohen 1983; Gaskell & Sparke 1986; Peterson & Cota 1988; Ulrich & Horne 1996; Metzroth et al. 2006). Inconsistent time lags from different monitoring campaigns might be caused by the short duration of the campaigns, but might also indicate real changes in the BLR size and geometry; for example Lyuty (2005) analyzed photometric observations performed during more than 30 years and concluded that the NGC 4151 nucleus goes through different levels of activity. They could be related to a total destruction of the accretion disk (AD) that took place in cycle A (from 1968 to 1984) and to the formation of a new AD in cycle B (from 1989 to 1996). Nevertheless, most UV and optical monitoring campaigns confirmed that the BLR is small and is radially stratified.
Unfortunately, spectral optical monitoring of NGC 4151 were mostly carried out during periods that were too short (less than one year), to trace real changes in the BLR structure. More than 10 years of spectral monitoring is needed to study the evolution of the BLR. Such observations have been made since 1986 in CrAO (Malkov et al. 1997; Sergeev et al. 2001) and SAO RAS (Bochkarev et al. 1988, 1991; Shapovalova et al. 1996; Nazarova et al. 1998).
In this paper we present the analysis of the spectral monitoring of NGC 4151 which covers a 11-year period from 1996 to 2006.
The paper is organized as follows. In Sect. 2 the observations, data
reduction and calibration are explained. In Sect. 3 we study the correlations between the
continuum, the Balmer (H,
H
,
H
), and the
HeII
4686 fluxes for both the whole lines
and the line wings. In Sect. 4 we discuss different possible
interpretations, and the results are summarized in Sect. 5.
Observatory | Code | Tel. and equip. | Aperture | Focus |
SAO(Russia) | L(N) | 6 m+Long slit | 2.0 ![]() |
Nasmith |
SAO(Russia) | L(U) | 6 m+UAGS | 2.0 ![]() |
Prime |
SAO(Russia) | L(S) | 6 m+Scorpio | 1.0 ![]() |
Prime |
Gullermo Haro(México) | GH | 2.1 m+B![]() |
2.5 ![]() |
Cassegrain |
San-Pedro(México) | S-P | 2.1 m+B![]() |
2.5 ![]() |
Cassegrain |
SAO(Russia) | L1(G) | 1 m+GAD | 4.2(8.0) ![]() |
Cassegrain |
SAO(Russia) | L1(U) | 1 m+UAGS+CCD2K | 4.0 ![]() |
Cassegrain |
Spectroscopic observations of NGC 4151 were carried out between
January 11, 1996 (Julian Date = JD 2 450 094) and April 20, 2006 (JD 2 453 846), thus covering a period of more than 10 years. In total 180 blue and
137 red spectra were taken during 220 nights (i) with the 6-m and 1-m
telescopes of SAO, Russia (1996-2006); (ii) with the 2.1-m telescope of the Guillermo Haro Astrophysical Observatory (GHAO)
at Cananea, Sonora, México (1998-2006); and (iii) with the 2.1-m telescope of
the Observatorio Astronómico Nacinal at San Pedro Martir (OAN-SMP), Baja
California, México (2005-2006).
The spectra were obtained with a long-slit spectrograph equipped with CCDs.
The typical wavelength range was 4000-7500 Å, the spectral
resolution was R=5-15 Å, and the S/N ratio was >50 in the
continuum near H
and H
.
Note that from 2004 to 2006,
the spectral observations with the GHAO's 2.1-m telescope
were carried out with two variants of the equipment:
1) with a grism of 150 l/mm (a low dispersion of R=15 Å,
like the observations of 1998-2003);
2) with a grism of 300 l/mm (a moderate dispersion of R=7.5 Å).
As a rule, the observations were performed with the moderate dispersion
in the blue or red bands during the first night of each set.
During the next night, we usually used the low dispersion
in the whole range 4000-7500 Å, and
the moderate dispersion was used the following night.
Since the shape of the continuum of active galaxies practically
does not change during adjacent nights, it was easy to link
the blue and red bands obtained with the moderate dispersion, using
the data obtained for the continuum with the low dispersion
in the whole wavelength range.
The photometric accuracy is thus considerably improved with respect
to a link obtained by overlapping the extremities of the continuum
(3-5% instead of 5-10%).
Spectrophotometric standard stars were observed every night. Information on the source of spectroscopic observations is listed in Table 1. Log of the spectroscopic observations is given in Table 2 (available only in electronic form).
The spectrophotometric data reduction was carried out either with the software developed at the SAO RAS by Vlasyuk (1993) or with IRAF for the spectra observed in México. The image reduction process included bias subtraction, flat-field corrections, cosmic ray removal, 2D wavelength linearization, sky spectrum subtraction, addition of the spectra for every night, and relative flux calibration based on standard star observations.
The standard technique of flux calibration spectra (i.e. comparison with
stars of known spectral energy distribution) is not precise enough for the study
of AGN variability, since even under good photometric conditions, the
accuracy of spectrophotometry is not better than .
Therefore we used standard
stars only for a relative calibration.
For the absolute calibration, the fluxes of the narrow emission lines are
adopted for scaling the AGN spectra, because they are known to remain constant on time scales of tens of
years (Peterson 1993).
We thus assumed that the flux of the [O III] 5007 line was
constant during the monitoring period. One can indeed check that
it did not change between 1980 (Antonucci & Cohen 1983) and 1992 (Malkov et al. 1997).
This is due to the fact that the forbidden line emitting region is
very extensive
(more than a hundred light-years). All blue spectra were thus scaled to
the constant flux F([O III]
erg s-1 cm-2 determined by Malkov et al.
(1997), and corrected for the position angle (PA), seeing,
and aperture effects, as described in Sect. 2.3. The scaling of the
blue spectra was performed by using the method of Van Groningen
& Wanders (1992)
modified by Shapovalova et al. (2004)
.
This method allowed us to obtain a homogeneous set
of spectra with the same wavelength calibration and the same
[OIII]
5007 flux.
The spectra obtained using the GHAO 2.1-m telescope (México) with
a resolution of 15 Å contain both the H
and
H
regions. These spectra were scaled using the
[O III]
5007 line. In this case the red region
was also automatically scaled by the [O III]
5007 flux.
However, the
accuracy of such a scaling depends strongly on the correct
determination of the continuum slope within the whole wavelength
range (4000-7500), i.e. on a correct correction for the spectral
sensitivity of the equipment, which is determined by a comparison star.
If the night of the observation did not have good
photometric conditions (clouds, mist, etc.), the reduction can
give a wrong spectral slope and, consequently, the errors in
scaling the H
wavelength band can be large. Most of the
spectra from the 1-m and 6-m SAO telescopes were obtained
separately in the blue (H
)
and in the red (H
)
bands, with
a resolution of 8-9 Å. Usually, the red
edge of the blue spectra and the blue edge of the red spectra
overlapped within an interval of
300 Å. Therefore, as
a zero approximation (the first stage), the majority of red
spectra was scaled using the overlapping continuum region with
the blue spectra, which were scaled with the
[O III]
5007 line. In this case the scaling
uncertainty is about 5%-10%. However, for some red spectra, this method
could not be used because (i) some spectra
obtained with a higher resolution (
5 Å) did not overlap
with blue spectra; (ii) some spectrum ends were distorted by
the reduction procedures of the instrumental set-up; or (iii) the blue and red
spectra were not taken during the same night. Therefore, to
increase the precision of the H
spectral region (the second
stage), all red spectra were once more scaled to a constant flux
value of the
narrow emission line [OI]
,
using the modified method of Van
Groningen & Wanders (1992; see also Shapovalova et al.
2004). As a reference, we used a red spectrum
obtained with the GHAO 2.1-m telescope during a good photometric
night, and well-scaled by the [OIII]
5007 line. After
scaling all red spectra using the [OI]
Å line, we
were able to estimate the quality of each spectrum by comparing the [OI] and the [OIII] scalings, and we eliminated the low quality spectra in the
further
analysis. The
uncertainty of the scaling of red spectra by the line
[OI]
6300 (i.e. actually by the flux of the [OIII]
5007
line)
was then about (2-3)%.
Then from the scaled spectra we determined an average flux in the
continuum at the observed wavelength 5117 Å (i.e. at
5100 Å in the rest frame of NGC 4151, z=0.0033), by
averaging the fluxes in the band 5092-5142 Å.
To determine the observed H
and H
fluxes, it is
necessary to subtract the continuum. The continuum was estimated in 30 Å windows, and
was fitted by a straight
line between two windows
centered at 4590 Å and 5125 Å for H
,
and
at 6200 Å and 6830 Å for H
.
After subtracting the
continuum, we measured the observed
fluxes in the lines, in the following wavelength intervals: 4780-4950 Å for the H
and 6415-6716 Å for
H
.
To measure the fluxes of H
and HeII
4686, we used only
115 blue spectra
from a total of 180. The
remaining 65 blue spectra were not suitable, because
they begin at
Å, or had a bad correction for
spectral sensitivity at the edge of the blue region (for example,
because of bad weather).
The underlying continuum for
H
and HeII
4686 was fitted by a straight
line using estimates of the continuum in a 30 Å window
centered at 4230 Å and 5125 Å respectively.
After continuum
subtraction, the H
and HeII
4686 fluxes were
measured in the
following wavelength intervals: 4268-4450 Å for H
and 4607-4783 Å for
HeII
4686.
To investigate the long-term spectral variability of NGC 4151, it is necessary to have a consistent set of spectra. Since NGC 4151 was observed with different telescopes, in different position angles, and with different apertures, we first had to perform corrections for the position angle (PA), seeing, and aperture effects. A detailed discussion on the necessity for these corrections is given in Peterson et al. (1995), so will not be repeated here.
The position angle corresponds to the position of the slit of the spectrograph
on the sky (from North to East). Usually, the
observations were performed with
,
but sometimes it was not
possible, e.g. at the 6 m - Nesmith focus, etc. Note that the atmospheric
dispersion was very small, since the object was always observed close to the meridian (<2 h and
).
To make the correction for the position angle, 80 spectra of NGC 4151
were taken with the 1-m and 6-m SAO
telescopes on May 8 and 9,
2003, under photometric conditions and a good seeing
(1.2''-1.5''), in different position angles (
,
45, 90, 135
degrees), and with different spectrograph entrance slits (1'', 1.5'',
2'', 4'', 8''). Data sets with
degrees for different slits
were used as the standard, since most of the NGC 4151 spectra in our
monitoring campaign were obtained in this position angle. Then we
determined corrections for the PA effect
,
as
The narrow line region (NLR) of NGC 4151 has an extended bi-conical
structure spreading up to >2'' from the nucleus (Evans et al.
1993), while the BLR and non-stellar (AGN) continuum are
effectively point-like sources (1''). Consequently, the
measured NLR flux depends on the size of the spectrograph
entrance aperture (see Peterson et al. 1995, for a detailed
discussion). Also, since we observed with different telescopes
and apertures, for each aperture the measured ratio of the
BLR flux (a point-like source) to the NLR flux (a spatially
extended region) depends on the seeing. Therefore, in each
aperture we must find corrections for images and reduce all flux
data to some accepted standard image. The method
suggested by Peterson et al. (1995) has been used for this purpose. For the seeing
in each aperture we can write
We divided the whole range of seeing values into several
intervals, for two different apertures. For the first aperture,
,
which corresponds to the observations
with the 6-m and 2.1-m telescopes (México), we considered the
following intervals: 1''-1.5'', 1.5''-2.5'', 2.5''-3.5'', 3.5''-4.5'',
and >4.5''. The data set for the interval 1.5''-2.5'' was adopted
as a standard one since the average seeing in the period of
observations with this aperture was about 2''. A value k(s)=1and G(s)=0 was accepted for this standard data set. We
obtained the seeing correction k(s) and the extended source
correction G(s) for the seeing intervals mentioned above using
spectra observed with different seeings within a time interval
shorter than 3 days, i.e.,
,
where
is the observed flux in
for the i-seeing, and
F(1.5''-2.5'') is the flux for the seeing interval 1.5''-2.5'';
these data are separated by 3 days or less. In Table 4
(available only in electronic form), we listed the k(s) and
G(s) corrections and the data obtained from Peterson et al.
(1995, their Figs. 5 and 6) for the aperture
From
this table, one can see that our seeing corrections k(s) for an
aperture of
practically coincide (within 1%) with
those of Peterson et al. (1995) for an aperture of
.
The correction (k(s) in Table 4) for the emission line
fluxes is the same for a slit length of
and of
,
meaning that the lines are emitted by a
region smaller than
,
but there are significant
differences in the host galaxy contribution, as expected.
For the second aperture,
,
which corresponds to our
observations with the 1-m Zeiss telescope (SAO), we used the seeing
intervals 2''-4'', 4''-6'', 6''-8''.
They are large because with this telescope it is
impossible to determine the seeing quality with a good precision,
owing to the small scale along the spectrograph slit (2.2''/px).
The data set for the interval 2''-4'' was used as a standard. The seeing
corrections k(s) and G(s) for the aperture
were
obtained with the same procedure described above for the
aperture
.
The results are given in Table 5
(available only in electronic form), together with those of Peterson et al. (1995) for the aperture
(their Figs. 5 and 6).
Emission line and continuum fluxes were scaled to the mean seeing
2'' for the apertures
)
and to the
mean seeing 3'' for the aperture
,
using the
seeing corrections from Tables 4 and 5. After that, we scaled all spectra
to the
aperture (cf. below).
To correct the observed fluxes for aperture effects, we determined a
point-source correction factor
using the equation (see
Peterson et al. 1995, for a detailed discussion):
The contribution of the host galaxy to the continuum flux also depends
on the aperture size. The continuum fluxes (5117)
were corrected for different amounts of host-galaxy contamination,
according to the following expression (see Peterson et al. 1995):
Sample | Years | Aperture | Point-source | Extended source |
(arcsec) | Scale factor | Correction | ||
(![]() |
G(g)a | |||
L(U,N) | 1996-2005 | 2.0 ![]() |
1.000 | 0.000 |
GH,S-P | 1996-2005 | 2.5 ![]() |
1.000 | 0.000 |
L(S) | 2004-2006 | 1.0 ![]() |
0.950 ![]() |
-0.391 |
L1(G) | 1996-2003 | 4.2 ![]() |
1.035 ![]() |
1.133 ![]() |
L1(G) | 1996-2003 | 8.0 ![]() |
1.112 ![]() |
1.623 ![]() |
L1(U) | 2004-2006 | 4.0 ![]() |
0.962 ![]() |
0.750 ![]() |
The fluxes listed in Table 7 were not corrected for contamination by the
narrow-line emission components of H,
HeII
,
H
,
H
,
and
6548,
6584. These contributions are expected to be constant and to have
no influence on the broad line variability.
The mean error (uncertainty) in our flux determinations for H
and H
and for the continuum is <3%,
while it is
5% for H
and
8% for
HeII
4686. These quantities were estimated by comparing
the results from spectra obtained within time intervals
shorter than 2 days. The estimated mean errors for every year and
for the total period of monitoring are given in
Table 8 (available only in electronic form).
To estimate the narrow line contributions
to the broad line fluxes, we constructed a spectral
template for the narrow lines. To this end, we used the blue and
red spectra in the minimum activity state (May 12,
2005), obtained with a spectral resolution of .
In
these spectra, the broad H
component was very weak, and
the broad components from the higher Balmer line series were
absent.
Both the broad and the
narrow components of H,
HeII
,
H
,
and
H
were fitted by Gaussians. The template spectrum contains the
following lines: for H
:
the narrow component of
H
and [O III]
4363; for H
:
the narrow component of H
and
[O III]
4959, 5007; for H
:
the
narrow component of H
,
[N II]
6548, 6584,
[O I]
6300, 6364)
[S II]
6717, 6731 and HeI
6678. Table 9 lists the narrow line
contributions obtained from the template spectrum in the same
wavelength integration intervals as for integral fluxes. Our
results are in good agreement with those given by Sergeev et al. (2001).
The spectra for the high- and
low-activity states, obtained respectively on January 15, 1996 (6 m
SAO's telescope) and on June 8, 2005 (2.1 m GHAO's telescope) are
presented in Fig. 1. As can be seen, the continuum flux decreased
by a large factor (5.6 times) in the
low-activity state, and the slope of the
continuum in the blue was significantly flatter than in the
high-activity state. Besides, the
wings of H
and H
became
extremely weak in the minimum state, and those of
H
and of the higher Balmer line series
could not be detected at all. These profiles correspond to a
Sy 1.8 type and not to a Sy1-Sy1.5, as this AGN could be classified
in the maximum state; hence, the spectral type of the object is
changing with time. This was noted earlier. In 1984-1989, the
nucleus of NGC 4151 went through a very deep minimum. At that time, the
brightness of the source fell down to the level of the
host galaxy for an aperture of 27'' in the V-band, the broad wings of hydrogen
lines became much weaker (they almost completely vanished in April 1984) and the spectrum of the nucleus was identified as a Sy 2
(Penston & Perez 1984).
![]() |
Figure 2:
The light curves of H![]() ![]() ![]() ![]() ![]() ![]() ![]() |
In Fig. 2 the light curves obtained from
Table 7 are presented for the H,
H
,
H
,
and
HeII
4686 integrated line fluxes and for the
continuum at the observed wavelength 5117 Å. The
fluxes of
H
,
HeII
4686, H
,
and H
were not corrected
for contamination by the constant contributions of the narrow lines.
The contributions of the narrow lines given in Table 9 are also shown.
It is clearly seen that, if the fluxes of the narrow lines
are subtracted from H
and HeII
4686 during the
minimum of activity, these lines disappear.
The continuum flux
presented in Table 7 and in Fig. 2 also contains
a constant contribution from the starlight of the host galaxy, which is estimated as
through an
aperture of
(Peterson & Cota 1988), and
through an aperture of
(Mal'kov et al. 1997). Bochkarev et al. (1991) determined that
the host galaxy contributed to about 40% of the total flux of NGC 4151
in the H
wavelength band though an aperture
,
near the
minimum state (1987). As can be seen from
Table 7, the minimum flux in the continuum (
)
obtained with an
aperture
was observed from November 29 to December 17, 2000. If
we assume that the host galaxy contribution is about 40% of the continuum (Bochkarev
et al. 1991), it gives
(i.e.
lower limit). Using a linear regression between the continuum
flux and the H
and H
broad line fluxes (the
narrow line flux being subtracted) near the low-activity state, and
extrapolating the broad line flux to zero, we estimated
F(host
.
This value is in good agreement with other estimates with
different apertures. The estimated contribution from the host galaxy
is also given in Fig. 2 (top).
The light curve of the continuum is similar to those of the
emission lines, showing
a maximum in 1996 and two minima in 2001 and 2005.
Components | Integration | NLR fluxa |
intervals (Å) | ||
H![]() |
6415-6716 | 7.93 |
H![]() |
4780-4950 | 1.00 |
H![]() ![]() |
4268-4450 | 1.04 |
HeII+[ArIV]+ | 4607-4783 | 0.36 |
![]() |
In Table 10, we give for the lines and continuum, the mean observed
maximum flux
in the interval JD = 2 450 094-2 450 402 (1996),
the mean observed minimum flux
in the intervals JD = 2 451 895-2 452 043 (December 2000-May 2001), and
(2005), the observed ratio
and this ratio for the broad lines
after subtraction of the narrow components
and the contribution of the host galaxy (agn continuum
in Table 10).
Lines or |
![]() |
![]() |
RF |
![]() |
continuuma | ||||
H![]() |
34.860 | 15.340 | 2.3 | 3.6 |
H![]() |
9.170 | 2.640 | 3.5 | 5.0 |
H![]() |
4.365 | 1.178 | 3.7 | 24!(not broad) |
HeII![]() |
3.170 | 0.714 | 4.4 | 7.9 |
cont(5117A) | 10.69 | 1.9 | 5.6 | 7.8 |
agn continuum |
The maximum amplitude ratios of the broad component line flux during
the 1996-2006 period were 3.6 for H
,
5.0 for H
line, and
7.8 for the
agn continuum
after subtraction of the host galaxy flux. In the
low-activity state, the broad component of
HeII
4686 and H
was almost absent.
![]() |
Figure 3:
The variation of the wings and core of H![]() ![]() ![]() |
![]() |
Figure 4:
The variation in the ratio of the fluxes in the line wings
and in the core of H![]() ![]() |
We divided the H
and H
profiles into three
parts: the blue wing, the core, and the red wing, each part covering
a range of 3000 km s-1. Distinct features or peaks observed
at different epochs in the wings were included,
and the corresponding narrow lines were
included in the core. In Table 11, we give the wavelength intervals used
to measure the flux in the three parts of each profile. We also
give the corresponding velocity intervals with respect to the center of the
narrow component.
Component | Integration | Integration |
interval | interval | |
in Å | in km s-1 | |
H![]() |
6486-6552 | (-4510)-(-1503) |
H![]() |
6553-6616 | (-1458)-(+1402) |
H![]() |
6617-6684 | (+1458)-(+4510) |
H![]() |
4804-4853 | (-4493)-(-1479) |
H![]() |
4854-4900 | (-1417)-(+1412) |
H![]() |
4901-4950 | (+1474)-(+4488) |
Light curves for the wings and cores of H
and H
are
presented in Fig. 3. As can be seen, the flux in the wings and cores
of both lines behaved similarly during the
monitoring period.
In Fig. 4 we present the flux ratios between the three parts of the
H
and H
profiles. In both lines,
the blue wing had a stronger flux than the red one in the period of
maximal activity (March 1996 to 1997 or
)
(F(blue)/F(red) >1, see Fig. 4, top-left). From 1997 to 2000 (or
), the H
blue/red flux ratio was very close to unity, while the H
blue/red ratio
varied from 0.95 to 0.8 (Fig. 4, top-right). In 2000-2006 (
), the red wing was the strongest
for both lines, and the H
blue/red ratio decreased
almost monotonically from 0.8 to 0.6
(Fig. 4, top-left), while it
varied from 0.6 to 0.8 for H
(Fig. 4,
top-right).
The F(blue)/F(core) ratio of both lines was decreasing nearly
monotonically from 1996 to 2001 (
). After
2002 (
), the H
ratio remained nearly
constant (
0.3), while the H
ratio decreased very slightly
(Fig. 4, middle). On the other hand, the
F(red)/F(core) ratio of both lines showed approximaly the same rapid
changes in the monitoring period.
![]() |
Figure 5:
The averaged and rms profiles of the broad H![]() ![]() |
![]() |
Figure 6:
The averaged and rms profiles of the broad H![]() ![]() |
The comparison between the averaged and the root-mean-square (rms)
spectra allows the line profile variability be investigated. We first inspected the H
and H
profiles for different periods, using spectra with a
resolution of 8 Å. With a criteria
based on the similarity of line profiles, we found three
characteristic profiles during the period 1996-2006. In the first
period (1996-1999,
2 450 094.466-2 451 515.583), where the lines were
very intense, a red asymmetry and a shoulder in the blue wing
were present. In the second period (2000-2001,
), the broad lines were weaker and the
shoulder in the blue wing is smaller and a shoulder in the red part is
present. From 2002 to 2006 (third period,
), the lines showed a blue asymmetry,
and a shoulder in the red part was dominant in the line profiles
(peak at
Å or at
2000 km s-1 relative to the narrow component, see Figs. 5-7, top).
Averaged and rms profiles of H
and H
for
each of these three periods and for the whole monitoring period
(1996-2006) were calculated after removing the continuum. They are shown
in Figs. 5-8.
We measured
the Full
Width at Half Maximum (FWHM) in the rms and averaged broad line profiles, and we defined the asymmetry A as the
ratio of the red/blue Half Width at Half Maximum (HWHM), i.e.
.
The measured values for the broad H
and
H
lines and their rms are given in Table 12.
![]() |
Figure 7:
The averaged and rms profiles of the broad H![]() ![]() |
![]() |
Figure 8:
The averaged and rms profiles of the broad H![]() ![]() |
Period | FWHM (H![]() |
![]() |
FWHM (H![]() |
![]() |
first | 4780 ![]() |
0.944 ![]() |
5980 ![]() |
0.935 ![]() |
second | 4020 ![]() |
0.872 ![]() |
5550 ![]() |
1.086 ![]() |
third | 5790 ![]() |
1.491 ![]() |
6350 ![]() |
1.282 ![]() |
mean profile | 4650 ![]() |
1.000 ![]() |
6110 ![]() |
1.056 ![]() |
Period | FWHM (rms H![]() |
![]() |
FWHM (rms H![]() |
![]() |
first | 4790 ![]() |
0.810 ![]() |
5430 ![]() |
0.596 ![]() |
second | 3100 ![]() |
1.061 ![]() |
3700 ![]() |
0.811 ![]() |
third | 3150 ![]() |
0.816 ![]() |
3760 ![]() |
1.168 ![]() |
mean rms | 4420 ![]() |
0.830 ![]() |
5490 ![]() |
0.775 ![]() |
![]() |
Figure 9:
The H![]() ![]() ![]() ![]() |
![]() |
Figure 11:
The wings and core fluxes as a function of the continuum
flux (at
![]() ![]() ![]() |
We have also plotted the H,
H
,
H
and He
4686 fluxes against the continuum flux Fc (see Fig. 10).
We find that the relationship between the line and
continuum fluxes can be divided into two separated sequences.
The first sequence, corresponding
to
,
took place in the period 1998 to
2006; there was a linear relationship between the lines and continuum
fluxes with a high correlation coefficient (0.88-0.95) for the Balmer lines.
The behavior of He
4686 vs. Fc is not clear, tending to be linear,
but with a high dispersion (r=0.79) when Fc was equal to
,
corresponding to the period 1998-1999. The second
sequence corresponds to high values of Fc (
)
and belongs to the period
from 1996 to 1997. Here the line fluxes tended to remain constant,
with a very weak correlation with Fc (see Fig. 10;
is given in the right-down corner for each line).
In Fig. 11 we show the relation between the continuum flux and
the different parts of the H
and H
profiles (the
blue, the core, and the red). As can be seen, the relation for
the core and the blue/red wing is similar to that of the whole line
(see Fig. 10).
To find an explanation for this behavior, we inspected these relationships within the three periods of observations mentioned above (see Sect. 3.3). We concluded that there was not only a difference in the line profiles, but also in the continuum vs. line flux relationships.
In the first period, when the
lines were the most intense, there was a weak
correlation between the lines and the continuum fluxes. The
H
flux changed by only
40%, while
the continuum flux changed by a factor three (see Fig. 12, left).
During the same period, H
was also very weakly correlated to
the continuum (Fig. 12, right), except for five points,
corresponding to observations between June and December 1999. At this time
the continuum and H
fluxes nearly decreased by a factor two, but
the H
and H
profiles remained almost identical.
In the second period,
a large dispersion was observed for
,
and the lines did not respond to the continuum. Some points (5) with
erg cm-2 s-1 Å-1 in Fig. 12
(middle) correspond to spectra taken in January and February 2000, and their H
and H
profiles are similar to those in
the first period (i.e. they have a red asymmetry and a shoulder in
the blue wing). In the third period, the response of the lines
to the continuum was linear.
![]() |
Figure 12:
H![]() ![]() |
To determine the time lag between the optical continuum and the line variations (line lagging continuum), we used the cross correlation function - CCF method introduced by Alexander (1997), the z-transformed discrete correlation function (ZDCF), which contains the idea of the discrete correlation function (DCF) method (Edelson & Krolik 1988) avoiding an interpolation. The ZDCF approximates the bin distribution by a bi-normal distribution. This algorithm differs from the DCF in that the data points are equally binned, and it uses Fisher's z-transform to stabilize a highly-skewed distribution of the correlation coefficient. According to Alexander (1997), ZDCF is much more efficient than DCF in detecting correlations involving the variability time scale, and it is more sensitive to under-sampled light curves than DCF and interpolated cross-correlation function (Gaskell & Sparke 1986; Gaskell & Peterson 1987).
The CCF analysis was carried out for the full data set which
covers the whole monitoring period from 1996 to 2006
and the three periods mentioned above. The
time lags and CCF for H
and H
are given in
Table 13. The CCF
coefficients are
calculated between the continuum flux and the H
,
H
fluxes
(line lagging contninuum). Positive time lags mean that the line light curve lags behind the
continuum light curve.
We also calculated the CCF and the time lags by dividing the data
set into three groups according to the continuum intensity: (i)
;
(ii)
and (iii)
.
As seen in Fig. 12,
is only present during
the first period, while
and
are present in
all three periods. Table 13 shows that, for such a division, the CCF is
small when the continuum is high.
There is a big
difference in the time lags between these three cases.
Note that the
highest CCF is obtained for the lowest continuum, but it is still
smaller than the one obtained in the third period based on the line profiles. The time lags
for H
and H
in the whole period are
5 days,
but they were different in the three periods. In the first and third
periods, the time lags were much shorter
for both lines (from 0.6 to 1.1 days) than in the second period
(11 and 21 days).
The time lags should, however, be considered as having a relative significance, since the CCF curves are very messy, as seen from the large uncertainties of the results, and some curves are asymmetrical. To illustrate this, we give the shifts of the centroïds in light-days in Table 13, when they could be measured. All these results together indicate a complex line-to-continuum response, due to complex and varying BLR.
We can summarize the CCF analysis as follows.
Period | H![]() |
CCF | H![]() |
H![]() |
CCF | H![]() |
1996-2006 |
![]() |
![]() |
80.36 ![]() |
![]() |
![]() |
69.79 ![]() |
First |
![]() |
![]() |
0.62 ![]() |
![]() |
![]() |
11.61 ![]() |
Second |
![]() |
![]() |
66.07 ![]() |
![]() |
![]() |
8.15 ![]() |
Third |
![]() |
![]() |
3.18 ![]() |
![]() |
![]() |
16.17 ![]() |
Continuum | H![]() |
CCF | H![]() |
H![]() |
CCF | H![]() |
![]() |
![]() |
![]() |
- |
![]() |
![]() |
- |
![]() |
![]() |
![]() |
0.56 ![]() |
![]() |
![]() |
2.71 ![]() |
![]() |
![]() |
![]() |
13.65 ![]() |
![]() |
![]() |
12.28 ![]() |
During the monitoring period, the spectrum of NGC 4151 underwent strong
changes, not only in the
line and continuum fluxes, but also in the H
and H
line profiles. Using the line profiles, we characterized three periods (see
Sect. 3.3, Tables 12 and 13, and Fig. 12). We found that the
FWHM of H
and H
are different, H
being
significantly broader
than H
(
1000 km s-1). This may indicate that H
is
formed deeper in the BLR, i.e. closer to the black hole. On the
other hand, the blue asymmetry in the averaged rms of H
and
H
could indicate a contribution of the emitting gas with an approaching
motion, i.e. an outflow. Finally, the presence of the central spike in the
rms spectrum is hard to explain unless it is produced by a remote component with an axisymmetric distribution and no outward motion. One suggestion is that it comes from a region heated and
ionized by the jet. In conclusion, there seems to be at least two BLR components, the first closer and in outward motion, the second located further away with no outward motions.
We
leave for the following paper a detailed discussion based on the study
of the line profiles, and we focus here on the global line variations.
We found that the responses of
the H
and H
fluxes to the continuum flux were different
in the
three periods, but it could be due to the limited range of fluxes in periods
2 and 3. For
low values of the continuum flux (
), there was a linear relation
between the lines and the continuum in the second and
third periods
(see Fig. 12). The dispersion of the points is larger in the second than in
the third period, so we think that the results concerning the last period
are more reliable. Note that Fc is smaller than
in period 2 and smaller than
in period 3, and that the linear
relation seems to flatten for H
between 4 and
in period 3. In the first period, there are only a few
points for
and they all
correspond almost to the same value of Fc, but if one interpolates
between these points and those at
,
about the same relation is obtained as in periods 2 and 3. Still in
the first period, when the continuum flux was more intense, i.e.
,
the linear relation
between the
line and continuum fluxes disappeared,
and the line fluxes saturated at values
for
H
and
for
H
(see Fig. 12).
Note finally that, if one extrapolates
the
continuum flux to zero linearly in the third period, it seems that the line
flux is
still larger than zero, being on the order of
erg cm-2 s-1 for H
.
It thus appears that the relation between the line and the continuum is
not
linear in the whole continuum flux range (2 to
), but it steepens at low fluxes and saturates at high fluxes.
This could occur when the ionizing incident flux is intense, so the
medium reprocesses the irradiating flux into continua (Balmer, Pashen...)
and not into lines (cf. for instance Collin-Souffrin & Lasota 1988).
Let us try to roughly model the response of the lines to a given continuum
flux. For the highest value of the continuum flux,
one gets an optical luminosity
erg s-1. One can then compute the ionizing flux incident on
the BLR, assuming it to be on the order of the optical flux,
,
where R is the radius of the BLR (of
course it is a very rough approximation, to be refined in a subsequent paper). Assuming an average energy of the ionizing photons
equal
to 2 Rydbergs, and using the grids of models computed with Cloudy published
by Korista et al. (1997) for a typical AGN spectrum (AGN3 in their list),
one finds (Fig. 13) the H
fluxes at Earth as a function of the density,
for a covering factor equal to unity, R=3 and 30 light days, and for two values of the column density. We have also used a minimum optical flux of 1042 erg s-1 to compare with the high flux.
We see that the computed line flux is of the order of the observed one only for a large (30 light-days) BLR, and for the larger flux (we recall that the observed fluxes of the broad component of
H
is (2.3-9.8)
10-12 erg cm-2 s-1). Since we know that the BLR extends in a wide range of radii, it leads to strongly suspect that a non-photoionized region is contributing to the Balmer
lines. Such a
``mechanically heated'' region was invoked by Dumont et al. (1998) to
account for
the strong intensities of the Balmer lines in NGC 5548. This region could be
associated with the radio jet. Indeed the radio image of NGC 4151 reveals a
0.2-pc
two-sided base to the well-known arc-second radio jet (Ulvestad et al.
2005)
.
Thus the BLR would be made of two-components: the usual one, ionized by the
radiation of the accretion disc and its corona, and another component,
possibly associated with a rotating outflow surrounding the
jet (Murray & Chiang 1997). In this second component, ionization and
heating
could be due either to relativistic particles or to a shock at the basis of
the jet, and they could not be directly correlated to the ionizing continuum.
It is worthwhile recalling here the results obtained from the spectro-polarimetry of
H
by Martel (1998). He presented evidence that
the scattering axes of different parts of the H
profile correlate with the major morphological axes of the host
galaxy of NGC 4151.
If scattering is the dominant
polarization mechanism in the BLR, then there are multiple lines
of sight towards large-scale structures in
the host galaxy, specifically the central bar, the radio jet, and
the dynamical axis. Martel (1998) suggests that
the line-emitting and scattering regions are cospatial, possibly
in bulk flows moving along preferential axes defined
by large-scale structures, such as streaming along
the bar and inflow/outflow along the radio jet. In this case, the
observed variability of the H
profile and flux could
be caused, at least partly, by dynamical effects, and not
by a time-variable continuum source, as is usually
assumed in reverberation mapping studies.
We have presented the results of a 11-year (1996-2006) spectral monitoring of the NGC 4151 nucleus. We have investigated the continuum and line variations during this period, and we reached the following conclusions:
Acknowledgements
This work was supported by the INTAS (grant N96-0328), RFBR (grants N97-02-17625 N00-02-16272, N03-02-17123, and 06-02-16843), State program ``Astronomy'' (Russia), CONACYT research grant 39560-F and 54480 (México), and the Ministry of Science of the Republic of Serbia through the project Astrophysical Spectroscopy of Extragalactic Objects (146002). L.C.P. is supported by the Alexander von Humboldt foundation through the Fritz Thyssen Special Programme. We would like to thank Tal Alexander for useful discussions concerning the time lags, and the referee Ian McHardy, for his comments and suggestions which contributed greatly to improving the paper.
UT-date | JD | Code | Aperture | Sp. range | Res. | PA | Seeing |
(2 400 000+) | (arcsec) | (Å-Å) | (Å) | (deg) | ('') | ||
Jan. 11, 1996 | +50 094.5 | L1(G) | 4.0 ![]() |
3840-5600 | 8 | 33 | 3 |
Jan. 15, 1996 | +50 097.6 | L1(G) | 4.0 ![]() |
3640-7140 | 10 | 77 | 3 |
Jan. 16, 1996 | +50 098.6 | L1(G) | 4.0 ![]() |
3640-7140 | 10 | 90 | 4.5 |
Feb. 14, 1996 | +50 128.0 | L(N) | 1.5 ![]() |
3400-5440 | 10 | 211 | 2.4 |
Mar. 19, 1996 | +50 162.4 | L(N) | 2.0 ![]() |
3650-5540 | 9 | 235 | 4.8 |
Mar. 20, 1996 | +50 163.3 | L(N) | 2.0 ![]() |
4750-7340 | 13 | 3.5 | |
Mar. 21, 1996 | +50 164.4 | L(N) | 2.0 ![]() |
3650-5540 | 8 | 40 | 1.6 |
Mar. 22, 1996 | +50 165.4 | L1(G) | 4.0 ![]() |
5700-7500 | 8 | 4 | |
Mar. 23, 1996 | +50 166.3 | L(N) | 2.0 ![]() |
4750-7340 | 13 | ||
Apr. 26, 1996 | +50 200.3 | L(U) | 2.0 ![]() |
4440-5200 | 5 | 353 | 2.4 |
Apr. 27, 1996 | +50 201.3 | L(U) | 2.0 ![]() |
4440-5200 | 5 | 351 | 1.6 |
Jun. 14, 1996 | +50 249.3 | L(U) | 2.0 ![]() |
4440-5240 | 5 | 131 | 2.4 |
Jul. 10, 1996 | +50 275.3 | L(U) | 2.0 ![]() |
3700-5340 | 10 | 97 | 1.2 |
Jul. 11, 1996 | +50 276.3 | L(U) | 2.0 ![]() |
6140-6950 | 6 | 131 | 1.4 |
Jul. 12, 1996 | +50 277.3 | L(U) | 2.0 ![]() |
4450-5250 | 5 | 117 | 1.6 |
Jul. 15, 1996 | +50 280.3 | L(U) | 2.0 ![]() |
4450-5250 | 5 | 123 | 1.6 |
Jul. 16, 1996 | +50 281.3 | L(U) | 2.0 ![]() |
6140-6950 | 6 | 1.3 | |
Nov. 05, 1996 | +50 392.6 | L(U) | 2.0 ![]() |
4450-5250 | 5 | 27 | 3.2 |
Nov. 15, 1996 | +50 402.6 | L(U) | 2.0 ![]() |
3700-5400 | 11 | 349 | 2 |
Mar. 02, 1997 | +50 510.4 | L(U) | 2.0 ![]() |
4390-5200 | 5 | 333 | 2.4 |
Mar. 03, 1997 | +50 511.4 | L(U) | 2.0 ![]() |
4440-5250 | 5 | 9 | 2.4 |
Apr. 05, 1997 | +50 543.6 | L1(G) | 4.2 ![]() |
4140-5850 | 8 | 90 | 4.4 |
Apr. 06, 1997 | +50 544.4 | L1(G) | 4.2 ![]() |
4140-5800 | 8 | 90 | 4.4 |
Apr. 08, 1997 | +50 547.3 | L(U) | 2.0 ![]() |
4640-5450 | 5 | 353 | 3.2 |
Apr. 13, 1997 | +50 552.3 | L(U) | 2.0 ![]() |
4440-5250 | 5 | 337 | 2 |
Dec. 27, 1997 | +50 809.7 | L(U) | 2.0 ![]() |
4540-5340 | 5 | 153 | 1.6 |
Dec. 28, 1997 | +50 810.7 | L(U) | 2.0 ![]() |
3840-7240 | 15 | 149 | 4 |
Jan. 20, 1998 | +50 833.6 | L(N) | 2.0 ![]() |
3840-6150 | 8 | 141 | 1.2 |
Jan. 21, 1998 | +50 834.6 | L(N) | 2.0 ![]() |
3840-6150 | 8 | 142 | 1.2 |
Jan. 23, 1998 | +50 836.7 | L(N) | 2.0 ![]() |
4240-5500 | 5 | 131 | 1.2 |
Jan. 23, 1998 | +50 836.7 | L(N) | 2.0 ![]() |
3840-6150 | 8 | 130 | 1.2 |
Jan. 28, 1998 | +50 842.4 | L(U) | 2.0 ![]() |
4540-5350 | 5 | 357 | 1.6 |
Feb. 22, 1998 | +50 867.4 | L(N) | 2.0 ![]() |
3840-6150 | 8 | 352 | 1.2 |
Apr. 30, 1998 | +50 934.5 | L1(G) | 8.0 ![]() |
4100-5750 | 8 | 147 | 4.4 |
May 04, 1998 | +50 938.3 | L(N) | 2.0 ![]() |
3740-6150 | 8 | 140 | 2.8 |
May 07, 1998 | +50 940.5 | L(N) | 2.0 ![]() |
3740-6150 | 8 | 90 | 3.6 |
May 08, 1998 | +50 941.5 | L(N) | 2.0 ![]() |
3740-6150 | 8 | 92 | 2 |
May 08, 1998 | +50 942.5 | L(N) | 2.0 ![]() |
3740-6150 | 8 | 119 | 1.6 |
May 08, 1998 | +50 942.5 | L(N) | 2.0 ![]() |
4140-5400 | 5 | 115 | 1.6 |
Jun. 20, 1998 | +50 985.3 | L1(G) | 8.0 ![]() |
4120-5740 | 8 | 0 | 4.4 |
Jun. 26, 1998 | +50 991.3 | L(N) | 2.0 ![]() |
3640-6040 | 8 | 2 | |
Jul. 14, 1998 | +51 008.7 | GH | 2.5 ![]() |
3970-7210 | 15 | 90 | 2 |
Jul. 16, 1998 | +51 010.7 | GH | 2.5 ![]() |
3630-6890 | 15 | 90 | 2 |
Jul. 17, 1998 | +51 011.6 | GH | 2.5 ![]() |
4210-7470 | 16 | 90 | 2 |
Jul. 21, 1998 | +51 015.7 | GH | 2.5 ![]() |
4040-7280 | 12 | 90 | 2.7 |
Jul. 30, 1998 | +51 025.3 | L(U) | 2.0 ![]() |
4540-5350 | 5 | 120 | 3.6 |
Nov. 13, 1998 | +51 130.6 | L1(G) | 8.0 ![]() |
4140-5810 | 8 | 90 | 4.4 |
Dec. 19, 1998 | +51 166.6 | L1(G) | 4.0 ![]() |
4140-5760 | 8 | 90 | 6.6 |
Jan. 12, 1999 | +51 190.7 | L(U) | 2.0 ![]() |
6250-7100 | 9 | 2.5 | |
Jan. 13, 1999 | +51 191.9 | GH | 2.5 ![]() |
4140-7420 | 15 | 90 | 1.5 |
Jan. 14, 1999 | +51 193.0 | GH | 2.5 ![]() |
4150-7430 | 15 | 90 | 1.3 |
Jan. 22, 1999 | +51 200.5 | L1(G) | 4.2 ![]() |
4100-5740 | 8 | 90 | 2.2 |
Jan. 23, 1999 | +51 201.6 | L1(G) | 4.2 ![]() |
4100-5740 | 8 | 0 | 4.4 |
Jan. 25, 1999 | +51 203.6 | L1(G) | 4.2 ![]() |
4100-5750 | 9 | 0 | 6.6 |
Feb. 09, 1999 | +51 218.6 | L(U) | 2.0 ![]() |
3640-8040 | 14 | 156 | 4 |
Feb. 12, 1999 | +51 221.7 | L(U) | 2.0 ![]() |
3640-7940 | 14 | 156 | 1.6 |
Feb. 13, 1999 | +51 222.6 | L(U) | 2.0 ![]() |
4290-5500 | 5 | 181 | 5.2 |
Feb. 14, 1999 | +51 223.6 | L(U) | 3.0 ![]() |
4290-5500 | 5 | 143 | 2.4 |
Mar. 15, 1999 | +51 252.9 | GH | 2.5 ![]() |
4200-7490 | 17 | 90 | 2.0 |
Mar. 20, 1999 | +51 258.5 | L1(G) | 4.2 ![]() |
4090-5740 | 8 | 0 | 2.2 |
Mar. 23, 1999 | +51 261.5 | L1(G) | 4.2 ![]() |
4090-5740 | 8 | 0 | 8.8 |
Mar. 24, 1999 | +51 262.3 | L1(G) | 4.2 ![]() |
5590-7300 | 9 | 4 | |
Mar. 24, 1999 | +51 262.5 | L(U) | 2.0 ![]() |
4290-5450 | 5 | 62 | 4 |
Apr. 09, 1999 | +51 277.6 | L1(G) | 4.2 ![]() |
4090-5750 | 8 | 0 | 4.4 |
Apr. 11, 1999 | +51 279.5 | L1(G) | 4.2 ![]() |
4040-5740 | 8 | 0 | 6.6 |
Apr. 15, 1999 | +51 283.5 | L1(G) | 3.0 ![]() |
4090-5770 | 8 | 50 | 4.4 |
Jun. 14, 1999 | +51 344.3 | L1(G) | 4.2 ![]() |
4090-5790 | 8 | 90 | 4.4 |
Jun. 16, 1999 | +51 346.4 | L1(G) | 4.2 ![]() |
4090-5790 | 8 | 90 | 4.4 |
Dec. 02, 1999 | +51 514.6 | L1(G) | 4.2 ![]() |
4090-5700 | 8 | 90 | 4.4 |
Dec. 03, 1999 | +51 515.6 | L1(G) | 4.2 ![]() |
4140-5750 | 8 | 90 | 4.4 |
Dec. 05, 1999 | +51 517.6 | L1(G) | 4.2 ![]() |
4090-5750 | 8 | 90 | 4.4 |
Jan. 09, 2000 | +51 552.6 | L1(G) | 4.2 ![]() |
4090-5790 | 8 | 90 | 2.2 |
Jan. 10, 2000 | +51 553.6 | L1(G) | 4.2 ![]() |
5640-7310 | 8 | 90 | 3.0 |
Jan. 27, 2000 | +51 570.9 | GH | 2.5 ![]() |
4070-7340 | 13 | 90 | 3.0 |
Jan. 28, 2000 | +51 571.9 | GH | 2.1 ![]() |
4070-7340 | 12 | 90 | 2.5 |
Feb. 11, 2000 | +51 585.5 | L1(G) | 4.2 ![]() |
4040-5740 | 8 | 90 | 4.4 |
Feb. 14, 2000 | +51 588.5 | L1(G) | 4.2 ![]() |
4040-5740 | 8 | 90 | 6.6 |
Feb. 14, 2000 | +51 589.5 | L1(G) | 4.2 ![]() |
5590-7300 | 8 | 90 | 4 |
Feb. 26, 2000 | +51 600.8 | GH | 2.1 ![]() |
4560-7590 | 12 | 90 | 2 |
Feb. 27, 2000 | +51 601.8 | GH | 2.1 ![]() |
4300-7580 | 12 | 90 | 3 |
Apr. 03, 2000 | +51 638.5 | L1(G) | 4.2 ![]() |
4090-5790 | 8 | 90 | 4.4 |
Apr. 05, 2000 | +51 640.5 | L1(G) | 4.2 ![]() |
4040-5740 | 8 | 90 | 6.6 |
Apr. 25, 2000 | +51 659.8 | GH | 2.1 ![]() |
4210-7490 | 12 | 90 | 2.5 |
Apr. 26, 2000 | +51 660.8 | GH | 2.1 ![]() |
4210-7490 | 15 | 90 | 2.5 |
May 11, 2000 | +51 676.4 | L1(G) | 4.2 ![]() |
4090-5790 | 10 | 90 | 4.4 |
May 25, 2000 | +51 689.7 | GH | 2.5 ![]() |
4140-7390 | 15 | 90 | 2.5 |
May 26, 2000 | +51 690.7 | GH | 2.5 ![]() |
4140-7390 | 15 | 90 | 3.5 |
Jul. 10, 2000 | +51 736.4 | L1(G) | 4.2 ![]() |
4060-5750 | 8 | 90 | 6.6 |
Jul. 29, 2000 | +51 755.3 | L1(G) | 4.2 ![]() |
4060-5750 | 8 | 90 | 4.4 |
Nov. 21, 2000 | +51 869.6 | L(U) | 2.0 ![]() |
4242-5398 | 5 | 90 | 1.2 |
Nov. 30, 2000 | +51 878.6 | L1(G) | 4.2 ![]() |
4090-5740 | 8 | 90 | 4.4 |
Dec. 17, 2000 | +51 895.9 | GH | 2.5 ![]() |
4010-7310 | 13 | 90 | 2 |
Dec. 18, 2000 | +51 897.0 | GH | 2.5 ![]() |
4010-7340 | 13 | 90 | 2 |
Dec. 19, 2000 | +51 898.0 | GH | 2.5 ![]() |
4000-7270 | 15 | 90 | 4 |
Jan. 26, 2001 | +51 936.5 | L1(G) | 4.2 ![]() |
5640-7300 | 8 | 90 | 2 |
Jan. 28, 2001 | +51 937.5 | L1(G) | 4.2 ![]() |
4090-5750 | 8 | 90 | 4.4 |
Jan. 31, 2001 | +51 940.6 | L1(G) | 4.2 ![]() |
4040-5700 | 8 | 90 | 4.4 |
Feb. 02, 2001 | +51 943.5 | L1(G) | 4.2 ![]() |
4140-5750 | 8 | 90 | 6.6 |
Feb. 11, 2001 | +51 952.4 | L1(G) | 4.2 ![]() |
4090-5750 | 8 | 0 | 4.4 |
Mar. 13, 2001 | +51 981.7 | GH | 2.5 ![]() |
4130-7430 | 14 | 90 | 2 |
Apr. 13, 2001 | +52 013.3 | L1(G) | 4.2 ![]() |
4090-5750 | 8 | 90 | 3.0 |
Apr. 16, 2001 | +52 016.4 | L1(G) | 4.2 ![]() |
4090-5750 | 8 | 90 | 4.4 |
Apr. 29, 2001 | +52 029.5 | L1(G) | 4.2 ![]() |
4090-5800 | 8 | 90 | 6.6 |
May 05, 2001 | +52 034.6 | GH | 2.5 ![]() |
3600-6800 | 12 | 90 | 3.5 |
May 06, 2001 | +52 036.4 | L1(G) | 4.2 ![]() |
4040-5750 | 8 | 90 | 4.4 |
May 12, 2001 | +52 041.8 | GH | 2.5 ![]() |
3600-6880 | 15 | 90 | 1.5 |
May 14, 2001 | +52 043.7 | GH | 2.5 ![]() |
4030-7340 | 13 | 90 | 2 |
Jun. 14, 2001 | +52 074.7 | GH | 2.5 ![]() |
4020-7310 | 13 | 90 | 3.5 |
Jun. 15, 2001 | +52 075.7 | GH | 2.5 ![]() |
4020-7310 | 17 | 90 | 2.5 |
Nov. 24, 2001 | +52 237.6 | L(U) | 2.0 ![]() |
3640-6000 | 10 | 91 | 3.6 |
Nov. 24, 2001 | +52 238.0 | GH | 2.5 ![]() |
4230-5900 | 8 | 90 | 2.5 |
Nov. 25, 2001 | +52 239.0 | GH | 2.5 ![]() |
5680-7380 | 7.5 | 90 | 2.5 |
Jan. 23, 2002 | +52 297.6 | L1(G) | 4.2 ![]() |
4040-5750 | 9 | 90 | 4.4 |
Jan. 24, 2002 | +52 299.4 | L1(G) | 4.2 ![]() |
4040-5750 | 8 | 90 | 2.2 |
Feb. 21, 2002 | +52 327.4 | L1(G) | 4.2 ![]() |
4040-5750 | 8 | 90 | 6.6 |
Feb. 22, 2002 | +52 327.5 | L(U) | 2.0 ![]() |
3500-5840 | 9 | 90 | 3.2 |
Mar. 05, 2002 | +52 338.7 | GH | 2.5 ![]() |
3900-7190 | 13 | 90 | 2 |
Mar. 06, 2002 | +52 339.7 | GH | 2.5 ![]() |
5690-7390 | 7.5 | 90 | 2 |
Mar. 07, 2001 | +52 340.8 | GH | 2.5 ![]() |
4260-5940 | 8 | 90 | 2 |
Mar. 17, 2002 | +52 350.8 | GH | 2.5 ![]() |
4260-5940 | 8 | 90 | 3 |
Apr. 03, 2002 | +52 367.7 | GH | 2.5 ![]() |
4280-5960 | 8 | 90 | 2 |
Apr. 04, 2002 | +52 368.7 | GH | 2.5 ![]() |
5740-7440 | 7.5 | 90 | 2 |
Apr. 05, 2002 | +52 369.7 | GH | 2.5 ![]() |
3820-7130 | 12 | 90 | 2 |
Apr. 06, 2002 | +52 370.7 | GH | 2.5 ![]() |
3820-7130 | 12 | 90 | 1.5 |
May 03, 2002 | +52 397.7 | GH | 2.5 ![]() |
4260-5940 | 8 | 90 | 2 |
May 04, 2002 | +52 398.7 | GH | 2.5 ![]() |
5680-7370 | 7.5 | 90 | 2 |
May 05, 2002 | +52 399.7 | GH | 2.5 ![]() |
4200-5880 | 8 | 90 | 2 |
May 16, 2002 | +52 411.4 | L1(G) | 4.2 ![]() |
4090-5790 | 8 | 90 | 4.4 |
Jun. 02, 2002 | +52 427.7 | GH | 2.5 ![]() |
4150-5820 | 8 | 90 | 2.5 |
Jun. 04, 2002 | +52 429.7 | GH | 2.5 ![]() |
3990-7290 | 12 | 90 | 3.5 |
Jun. 05, 2002 | +52 430.7 | GH | 2.5 ![]() |
4240-5920 | 7.5 | 90 | 3.0 |
Jun. 24, 2002 | +52 450.4 | L(U) | 2.0 ![]() |
3500-5880 | 8 | 90 | 2 |
Dec. 11, 2002 | +52 620.0 | GH | 2.5 ![]() |
4230-6070 | 7.5 | 90 | 1.5 |
Dec. 12, 2002 | +52 621.0 | GH | 2.5 ![]() |
5750-7430 | 8 | 90 | 1.8 |
Dec. 13, 2002 | +52 622.0 | GH | 2.5 ![]() |
3740-7380 | 14 | 90 | 1.8 |
Dec. 14, 2002 | +52 623.0 | GH | 2.5 ![]() |
4240-6080 | 8 | 90 | 1.8 |
Jan. 25, 2003 | +52 665.0 | GH | 2.5 ![]() |
4300-5960 | 7.5 | 90 | 1.5 |
Jan. 26, 2003 | +52 665.9 | GH | 2.5 ![]() |
5670-7360 | 7.5 | 90 | 4 |
Jan. 27, 2003 | +52 666.9 | GH | 2.5 ![]() |
3920-7240 | 15 | 90 | 1.5 |
Jan. 28, 2003 | +52 667.9 | GH | 2.5 ![]() |
3980-7300 | 12 | 90 | 2.5 |
Mar. 25, 2003 | +52 723.8 | GH | 2.5 ![]() |
4240-6070 | 7.5 | 90 | 3.5 |
Mar. 26, 2003 | +52 724.8 | GH | 2.5 ![]() |
3747-7385 | 12 | 90 | 4.5 |
Mar. 27, 2003 | +52 725.8 | GH | 2.5 ![]() |
5600-7460 | 7.5 | 90 | 2.5 |
Apr. 10, 2003 | +52 739.7 | GH | 2.5 ![]() |
5640-7500 | 8 | 90 | 4 |
Apr. 11, 2003 | +52 740.8 | GH | 2.5 ![]() |
4130-5960 | 13 | 90 | 5.4 |
Apr. 12, 2003 | +52 741.8 | GH | 2.5 ![]() |
3700-7340 | 12 | 90 | 4.0 |
Apr. 13, 2003 | +52 743.3 | L1(G) | 4.2 ![]() |
5640-7330 | 9 | 90 | 2 |
May 08, 2003 | +52 768.4 | L1(U) | 4 ![]() |
3750-6047 | 8 | 90 | 2.0 |
May 08, 2003 | +52 768.3 | L(U) | 2.0 ![]() |
3690-6044 | 9 | 90 | 1.6 |
May 9, 2003 | +52 769.3 | L(U) | 2.0 ![]() |
3690-6044 | 9 | 90 | 1.5 |
May 10, 2003 | +52 770.3 | L(U) | 2.0 ![]() |
5740-8096 | 8 | 90 | 1.5 |
May 23, 2003 | +52 782.7 | GH | 2.5 ![]() |
3540-7188 | 12 | 90 | 3.1 |
May 24, 2003 | +52 783.8 | GH | 2.5 ![]() |
4240-6070 | 7.5 | 90 | 3.5 |
May 25, 2003 | +52 784.7 | GH | 2.5 ![]() |
5582-7450 | 8 | 90 | 3.7 |
May 26, 2003 | +52 785.7 | GH | 2.5 ![]() |
4230-6075 | 7.5 | 90 | 2.7 |
Jun. 22, 2003 | +52 812.8 | GH | 2.5 ![]() |
4270-6970 | 7.5 | 90 | 1.8 |
Jun. 23, 2003 | +52 813.7 | GH | 2.5 ![]() |
5620-7330 | 7.5 | 90 | 1.8 |
Nov. 22, 2003 | +52 965.6 | L1(G) | 4.2 ![]() |
4089-5798 | 9 | 90 | 2.0 |
Nov. 23, 2003 | +52 966.6 | L1(G) | 4.2 ![]() |
4090-5748 | 9 | 90 | 1.5 |
Nov. 24, 2003 | +52 967.9 | L1(G) | 4.2 ![]() |
4090-5748 | 9 | 90 | 1.5 |
Dec. 22, 2003 | +52 995.6 | L1(U) | 4.0 ![]() |
3750-6950 | 10 | 90 | 3.5 |
Jan. 28, 2004 | +53 032.9 | GH | 2.5 ![]() |
4238-5950 | 12 | 90 | 2 |
Feb. 17, 2004 | +53 053.0 | GH | 2.5 ![]() |
3736-7120 | 17 | 90 | 1.6 |
Mar. 17, 2004 | +53 081.8 | GH | 2.5 ![]() |
4205-5920 | 12 | 90 | 2 |
Mar. 18, 2004 | +53 082.7 | GH | 2.5 ![]() |
5664-7400 | 14 | 90 | |
Apr. 12, 2004 | +53 107.6 | Z2K | 4.0 ![]() |
3784-7170 | 7.5 | 90 | 4.0 |
Apr. 13, 2004 | +53 108.7 | GH | 2.5 ![]() |
4216-5930 | 12 | 90 | 2.5 |
Apr. 14, 2004 | +53 109.7 | GH | 2.5 ![]() |
5622-7320 | 14 | 90 | |
May 20, 2004 | +53 145.7 | GH | 2.5 ![]() |
4193-5910 | 12 | 90 | 2.22 |
May 21, 2004 | +53 146.7 | GH | 2.5 ![]() |
5664-7390 | 7.5 | 90 | |
Jun. 12, 2004 | +53 168.7 | GH | 2.5 ![]() |
4208-5920 | 10 | 90 | 2.73 |
Jun. 13, 2004 | +53 169.7 | GH | 2.5 ![]() |
5592-7320 | 8 | 90 | |
Jun. 17, 2004 | +53 173.7 | GH | 2.5 ![]() |
4213-5920 | 11 | 90 | 2.50 |
Dec. 15, 2004 | +53 355.0 | GH | 2.5 ![]() |
4185-5870 | 7.5 | 90 | 2.96 |
Dec. 16, 2004 | +53 356.0 | GH | 2.5 ![]() |
5739-7440 | 7.5 | 90 | |
Dec. 18, 2004 | +53 357.6 | L(S) | 1.0 ![]() |
3900-7537 | 12. | 270 | 1.6 |
Dec. 22, 2004 | +53 361.5 | L(S) | 1.0 ![]() |
3900-7537 | 14 | 270 | 2.5 |
Jan. 16, 2005 | +53 386.9 | GH | 2.5 ![]() |
3707-7096 | 12 | 90 | 3.05 |
Jan. 17, 2005 | +53 388.0 | GH | 2.5 ![]() |
4183-5900 | 9 | 90 | 2.4 |
Jan. 18, 2005 | +53 388.9 | GH | 2.5 ![]() |
5577-7320 | 12 | 90 | |
Feb. 07, 2005 | +53 408.8 | S-P | 2.5 ![]() |
5722-7590 | 6.5 | 90 | 2.3 |
Feb. 15, 2005 | +53 416.9 | S-P | 2.5 ![]() |
3708-5807 | 7 | 90 | 2.5 |
Feb. 15, 2005 | +53 417.5 | L1(U) | 4.0 ![]() |
3750-7400 | 8 | 90 | 4.0 |
Mar. 17, 2005 | +53 446.8 | GH | 2.5 ![]() |
5557-7300 | 13 | 90 | |
Mar. 18, 2005 | +53 447.8 | GH | 2.5 ![]() |
3689-7090 | 13 | 90 | 3.0 |
Mar. 21, 2005 | +53 451.3 | L1(U) | 4.0 ![]() |
3750-7400 | 9 | 90 | 8 |
Apr. 13, 2005 | +53 474.4 | L1(U) | 4.0 ![]() |
3750-7400 | 8 | 90 | 2.5 |
Apr. 15, 2005 | +53 475.8 | GH | 2.5 ![]() |
4245-5960 | 9 | 90 | 2.82 |
Apr. 16, 2005 | +53 476.8 | GH | 2.5 ![]() |
5521-7256 | 10 | 90 | |
Apr. 16, 2005 | +53 477.3 | L1(U) | 4.0 ![]() |
3750-7400 | 8 | 90 | 5.5 |
Apr. 18, 2005 | +53 478.7 | GH | 2.5 ![]() |
3745-7190 | 13 | 90 | |
May 12, 2005 | +53 503.3 | L1(U) | 4.0 ![]() |
3750-7400 | 8 | 90 | 2.0 |
May 13, 2005 | +53 503.7 | GH | 2.5 ![]() |
4216-5910 | 9 | 90 | 3.0 |
May 14, 2005 | +53 504.7 | GH | 2.5 ![]() |
5583-7300 | 7 | 90 | |
May 16, 2005 | +53 507.4 | L1(U) | 4.0 ![]() |
3750-7400 | 8 | 90 | 3.2 |
Jun. 09, 2005 | +53 530.7 | GH | 2.5 ![]() |
3714-7070 | 12 | 90 | 1.94 |
Jun. 10, 2005 | +53 531.6 | GH | 2.5 ![]() |
4274-5970 | 9 | 90 | 3.37 |
Jun. 11, 2005 | +53 531.6 | GH | 2.5 ![]() |
5676-7395 | 7.5 | 90 | |
Jun. 16, 2005 | +53 538.3 | L1(U) | 4.0 ![]() |
3740-7350 | 9 | 90 | 2.5 |
Nov. 28, 2005 | +53 703.0 | GH | 2.5 ![]() |
3590-6900 | 15 | 90 | 3.0 |
Nov. 29, 2005 | +53 704.0 | GH | 2.5 ![]() |
4230-5910 | 7 | 90 | 2.8 |
Dec. 06, 2005 | +53 711.0 | S-P | 2.5 ![]() |
3690-5780 | 7 | 90 | 2.5 |
Dec. 07, 2005 | +53 712.0 | S-P | 2.5 ![]() |
3690-5780 | 7 | 90 | 2.5 |
Dec. 27, 2005 | +53 732.0 | GH | 2.5 ![]() |
3890-7270 | 17 | 90 | 3 |
Dec. 28, 2005 | +53 733.0 | GH | 2.5 ![]() |
3880-7260 | 17 | 90 | 2.4 |
Jan. 21, 2006 | +53 756.9 | GH | 2.5 ![]() |
4330-6040 | 9 | 90 | 2.7 |
Jan. 22, 2006 | +53 757.9 | GH | 2.5 ![]() |
4330-6040 | 9 | 90 | 3 |
Jan. 24, 2006 | +53 760.5 | L1(U) | 4.0 ![]() |
3740-7400 | 9 | 90 | 3.5 |
Jan. 25, 2006 | +53 761.5 | L1(U) | 4.0 ![]() |
3740-7400 | 9 | 90 | 2.5 |
Feb. 20, 2006 | +53 786.9 | GH | 2.5 ![]() |
3740-7120 | 17 | 90 | 2.8 |
Feb. 21, 2006 | +53 787.5 | L1(U) | 4.0 ![]() |
3740-7400 | 8 | 90 | 2 |
Feb. 22, 2006 | +53 788.5 | L1(U) | 4.0 ![]() |
3740-7400 | 8 | 90 | 2 |
Feb. 23, 2006 | +53 789.5 | GH | 2.5 ![]() |
3740-7400 | 15 | 90 | 2.5 |
Mar. 09, 2006 | +53 803.8 | GH | 2.5 ![]() |
3730-7100 | 14 | 90 | 5.1 |
Mar. 21, 2006 | +53 816.4 | L1(U) | 4.0 ![]() |
3740-7400 | 8 | 90 | 5 |
Mar. 22, 2006 | +53 817.4 | L1(U) | 4.0 ![]() |
3740-7400 | 8 | 90 | 4 |
Apr. 18, 2006 | +53 843.7 | GH | 2.5 ![]() |
3720-7090 | 9 | 90 | 2.7 |
Apr. 19, 2006 | +53 844.8 | GH | 2.5 ![]() |
4240-5940 | 7 | 90 | 2.5 |
Apr. 20, 2006 | +53 845.7 | GH | 2.5 ![]() |
4240-5940 | 7 | 90 | 2.1 |
Apr. 20, 2006 | +53 846.4 | L1(U) | 4.0 ![]() |
3740-7400 | 8 | 90 | 2.5 |
PA | Aperture | kp(H![]() |
![]() |
kp(cnt) | ![]() |
deg. | arcsec | ||||
90 | 2.0 ![]() |
1 | 1 | ||
90 | 4.0 ![]() |
1 | 1 | ||
0 | 2.0 ![]() |
0.969 | 0.035 | 0.968 | 0.017 |
0 | 4.0 ![]() |
1.011 | 0.018 | 1.019 | 0.009 |
45 | 2.0 ![]() |
1.062 | 0.006 | 1.098 | 0.024 |
45 | 4 ![]() |
1.048 | 0.003 | 1.071 | 0.006 |
135 | 2.0 ![]() |
0.954 | 0.018 | 0.943 | 0.011 |
135 | 4.0 ![]() |
0.974 | 0.004 | 0.981 | 0.005 |
Interval | Mean | ks(our) | ![]() |
ks(Pet) | Gs(our) | ![]() |
Gs(Pet) |
seeings | seeing | (
![]() |
(
![]() |
(
![]() |
(
![]() |
||
arcsec | arcsec | H![]() |
H![]() |
10-14 | 10-14 | ||
1''-1.5'' | 1.25'' | 0.965 | 0.046 | -0.160 | 0.197 | -0.070 (1.3'') | |
1.5'' | 0.977* | 0.973 | |||||
1.5''-2.5'' | 2.0'' | 1.000 | 1.000 | 0 | 0 | ||
2.5''-3.5'' | 3.0'' | 1.042 | 0.030 | 1.052 | -0.039 | 0.130 | |
3.5''-4.5'' | 4.0'' | 1.069 | 0.063 | 1.086 | |||
3.5''-5.2'' | 0.329 | 0.203 | |||||
5'' | 1.096 | 1.105 | 0.31 |
Interval | Mean | ks(our) | ![]() |
ks(Pet) | Gs(our) | ![]() |
Gs(Pet) |
seeings | seeing | H![]() |
H![]() |
10-14 | 10-14 | ||
arcsec | arcsec | (
![]() |
(
![]() |
(
![]() |
(
![]() |
||
2''-4'' | 3'' | 1.000 | 1.000 | 0.000 | 0.000 | ||
4''-6'' | 5'' | 1.063 | ![]() |
1.004 | 0.031 | ![]() |
0.123 |
4''-8'' | 6'' | 1.080 | ![]() |
1.015 | 0.188 | ![]() |
|
6''-8'' | 7'' | 1.116 | |||||
0.503 | 0.245 |
JD |
![]() |
![]() |
![]() |
![]() |
![]() |
50 094.5 | 8.8 ![]() |
- | 8.03 ![]() |
4.807 ![]() |
3.136 ![]() |
50 097.6 | 9.26 ![]() |
33.41 ![]() |
8.19 ![]() |
3.893 ![]() |
2.707 ![]() |
50 098.6 | 9.26 ![]() |
35.16 ![]() |
- | - | - |
50 128 | 11.25 ![]() |
34.34 ![]() |
9.28 ![]() |
4.524 ![]() |
3.495 ![]() |
50 162.4 | 11.66 ![]() |
- | 8.9 ![]() |
3.638 ![]() |
2.22 ![]() |
50 163.3 | 11.66 ![]() |
33.79 ![]() |
- | - | - |
50 164.4 | 10.78 ![]() |
- | 8.5 ![]() |
4.044 ![]() |
3.485 ![]() |
50 165.4 | 10.78 ![]() |
33.24 ![]() |
- | - | - |
50 166.3 | 10.78 ![]() |
32.04 ![]() |
- | - | - |
50 200.3 | 9.6 ![]() |
- | 9.34 ![]() |
- | - |
50 201.3 | 8.85 ![]() |
30.97 ![]() |
8.73 ![]() |
- | - |
50 249.3 | 12.64 ![]() |
35.45 ![]() |
8.24 ![]() |
- | - |
50 275.3 | 11.99 ![]() |
35.72 ![]() |
9.83 ![]() |
4.649 ![]() |
3.313 ![]() |
50 276.3 | 11.99 ![]() |
35.88 ![]() |
- | - | - |
50 277.3 | 11.29 ![]() |
36.6 ![]() |
9.26 ![]() |
- | - |
50 280.3 | 12.19 ![]() |
35.95 ![]() |
10 ![]() |
- | - |
50 281.3 | 12.19 ![]() |
35.53 ![]() |
- | - | - |
50 392.6 | 10.04 ![]() |
- | 9.97 ![]() |
- | - |
50 402.6 | 10.65 ![]() |
39.95 ![]() |
10.8 ![]() |
5.003 ![]() |
3.792 ![]() |
50 510.4 | 7.84 ![]() |
32.4 ![]() |
9.08 ![]() |
- | - |
50 511.4 | 8.86 ![]() |
- | 9.57 ![]() |
- | - |
50 543.6 | 6.82 ![]() |
32.15 ![]() |
7.44 ![]() |
3.336 ![]() |
2.088 ![]() |
50 544.4 | 6.47 ![]() |
32.54 ![]() |
7.35 ![]() |
- | - |
50 547.3 | 6.92 ![]() |
- | 7 ![]() |
- | - |
50 552.3 | 7.38 ![]() |
- | 8.5 ![]() |
- | - |
50 809.7 | 7.56 ![]() |
- | 9.07 ![]() |
- | - |
50 810.7 | 7.22 ![]() |
- | 9.04 ![]() |
- | - |
50 833.6 | 5.91 ![]() |
31.65 ![]() |
7.31 ![]() |
3.256 ![]() |
1.912 ![]() |
50 834.6 | 6.09 ![]() |
31.03 ![]() |
7.54 ![]() |
3.466 ![]() |
2.12 ![]() |
50 836.7 | 6.4 ![]() |
- | 7.33 ![]() |
3.837 ![]() |
2.745 ![]() |
50 836.7 | 6.42 ![]() |
- | 7.82 ![]() |
3.619 ![]() |
2.524 ![]() |
50 842.4 | 6.59 ![]() |
32.87 ![]() |
8.02 ![]() |
- | - |
50 867.4 | 6.22 ![]() |
33.34 ![]() |
7.34 ![]() |
3.363 ![]() |
2.445 ![]() |
50 934.5 | 6.39 ![]() |
33.14 ![]() |
7.06 ![]() |
- | - |
50 938.3 | 6.55 ![]() |
33.6 ![]() |
6.77 ![]() |
2.643 ![]() |
1.902 ![]() |
50 940.5 | 6.27 ![]() |
30.78 ![]() |
6.82 ![]() |
2.878 ![]() |
1.457 ![]() |
50 941.5 | 5.64 ![]() |
- | 6.41 ![]() |
2.608 ![]() |
1.135 ![]() |
50 942.5 | 5.7 ![]() |
29.87 ![]() |
6.42 ![]() |
2.432 ![]() |
1.516 ![]() |
50 942.5 | 6.09 ![]() |
- | 6.25 ![]() |
2.653 ![]() |
1.157 ![]() |
50 985.3 | 8.52 ![]() |
34.03 ![]() |
8.29 ![]() |
3.118 ![]() |
2.738 ![]() |
50 991.3 | 7.43 ![]() |
- | 8.24 ![]() |
3.692 ![]() |
2.946 ![]() |
51 008.7 | 5.84 ![]() |
31.09 ![]() |
7.44 ![]() |
3.355 ![]() |
1.743 ![]() |
51 010.7 | 5.98 ![]() |
28.62 ![]() |
7.59 ![]() |
3.677 ![]() |
2.173 ![]() |
51 011.6 | 5.81 ![]() |
28.82 ![]() |
7.47 ![]() |
3.258 ![]() |
1.974 ![]() |
51 015.7 | 6.26 ![]() |
31.15 ![]() |
7.84 ![]() |
3.637 ![]() |
1.829 ![]() |
51 025.3 | 6.21 ![]() |
30.15 ![]() |
7.45 ![]() |
- | - |
51 130.6 | 5.69 ![]() |
32.59 ![]() |
7.05 ![]() |
- | - |
51 166.6 | 4.26 ![]() |
33.07 ![]() |
6.96 ![]() |
- | - |
51 190.7 | 5.56 ![]() |
29.56 ![]() |
- | - | - |
51 191.9 | 5.56 ![]() |
28.47 ![]() |
6.85 ![]() |
3.54 ![]() |
2.377 ![]() |
51 193 | 5.81 ![]() |
28.47 ![]() |
6.6 ![]() |
3.465 ![]() |
2.62 ![]() |
51 200.5 | 6.07 ![]() |
- | 7.36 ![]() |
- | - |
51 201.6 | 6.42 ![]() |
33.51 ![]() |
7.91 ![]() |
- | - |
51 203.6 | 6.57 ![]() |
34.83 ![]() |
8.05 ![]() |
- | - |
51 218.6 | 6.43 ![]() |
35.24 ![]() |
7.86 ![]() |
3.74 ![]() |
2.888 ![]() |
51 221.7 | 6.38 ![]() |
36.73 ![]() |
8.09 ![]() |
3.452 ![]() |
3.043 ![]() |
51 222.6 | 6.06 ![]() |
- | 7.92 ![]() |
- | - |
51 223.6 | 5.69 ![]() |
- | 7.34 ![]() |
- | - |
51 252.9 | 5.03 ![]() |
29.45 ![]() |
6.16 ![]() |
2.886 ![]() |
1.883 ![]() |
51 258.5 | 5.79 ![]() |
32.55 ![]() |
6.95 ![]() |
- | - |
51 261.5 | 5.81 ![]() |
31.19 ![]() |
6.93 ![]() |
- | - |
51 262.3 | 5.77 ![]() |
31.47 ![]() |
- | - | - |
51 262.5 | 5.77 ![]() |
32.2 ![]() |
7.12 ![]() |
- | - |
51 277.6 | 5.79 ![]() |
- | 7.6 ![]() |
3.425 ![]() |
3.217 ![]() |
51 279.5 | 5.5 ![]() |
34.91 ![]() |
7.51 ![]() |
- | - |
51 283.5 | 5.29 ![]() |
- | 6.56 ![]() |
- | - |
51 344.3 | 2.87 ![]() |
- | 4.2 ![]() |
1.716 ![]() |
0.998 ![]() |
51 346.4 | 2.75 ![]() |
- | 4.29 ![]() |
2.212 ![]() |
1.092 ![]() |
51 514.6 | 2.77 ![]() |
- | 3.52 ![]() |
1.668 ![]() |
1.252 ![]() |
51 515.6 | 2.79 ![]() |
22.94 ![]() |
3.6 ![]() |
1.58 ![]() |
1.193 ![]() |
51 517.6 | 3.1 ![]() |
- | 3.47 ![]() |
1.574 ![]() |
1.391 ![]() |
51 552.6 | 4.16 ![]() |
- | 4.51 ![]() |
- | - |
51 553.6 | 4.16 ![]() |
25.93 ![]() |
- | - | - |
51 570.9 | 3.86 ![]() |
25.13 ![]() |
- | - | - |
51 571.9 | 3.86 ![]() |
23.57 ![]() |
4.67 ![]() |
2.257 ![]() |
1.035 ![]() |
51 585.5 | 3.56 ![]() |
- | 4.16 ![]() |
2.615 ![]() |
1.52 ![]() |
51 588.5 | 3.6 ![]() |
- | 4.48 ![]() |
2.021 ![]() |
1.517 ![]() |
51 589.5 | 3.6 ![]() |
24.12 ![]() |
- | - | - |
51 600.8 | 2.78 ![]() |
22.51 ![]() |
4.01 ![]() |
- | - |
51 601.8 | 2.77 ![]() |
22.28 ![]() |
4.15 ![]() |
- | - |
51 638.5 | 2.53 ![]() |
- | 3.7 ![]() |
- | - |
51 640.5 | 2.3 ![]() |
- | 3.57 ![]() |
- | - |
51 659.8 | 2.63 ![]() |
20.19 ![]() |
3.6 ![]() |
1.88 ![]() |
1.156 ![]() |
51 660.8 | 2.61 ![]() |
19.04 ![]() |
3.56 ![]() |
1.943 ![]() |
1.144 ![]() |
51 676.4 | 1.88 ![]() |
- | 3.23 ![]() |
- | - |
51 689.7 | 1.95 ![]() |
17.89 ![]() |
3.09 ![]() |
1.678 ![]() |
0.649 ![]() |
51 690.7 | 1.92 ![]() |
19.68 ![]() |
3.01 ![]() |
1.528 ![]() |
0.711 ![]() |
51 736.4 | 2.31 ![]() |
- | 3.22 ![]() |
- | - |
51 755.3 | 2.72 ![]() |
- | 3.35 ![]() |
- | - |
51 869.6 | 1.86 ![]() |
- | 3.84 ![]() |
2.061 ![]() |
0.844 ![]() |
51 878.6 | 1.51 ![]() |
- | 3.14 ![]() |
1.687 ![]() |
0.918 ![]() |
51 895.9 | 1.7 ![]() |
15.92 ![]() |
2.49 ![]() |
1.203 ![]() |
0.71 ![]() |
51 897 | 1.7 ![]() |
16.61 ![]() |
2.55 ![]() |
1.18 ![]() |
0.698 ![]() |
51 898 | 1.79 ![]() |
16.22 ![]() |
2.64 ![]() |
1.2 ![]() |
0.806 ![]() |
51 936.5 | 1.79 ![]() |
20.81 ![]() |
- | - | - |
51 937.5 | 1.79 ![]() |
- | 2.96 ![]() |
- | - |
51 940.6 | 1.81 ![]() |
18.73 ![]() |
2.91 ![]() |
- | - |
51 943.5 | 1.76 ![]() |
20.09 ![]() |
2.94 ![]() |
- | - |
51 952.4 | 1.31 ![]() |
- | 2.75 ![]() |
- | - |
51 981.7 | 1.71 ![]() |
14.31 ![]() |
2.32 ![]() |
1.11 ![]() |
0.625 ![]() |
52 013.3 | 2.24 ![]() |
15.86 ![]() |
2.47 ![]() |
- | - |
52 016.4 | 2.6 ![]() |
17.27 ![]() |
2.63 ![]() |
- | - |
52 029.5 | 1.78 ![]() |
- | 2.79 ![]() |
- | - |
52 034.6 | 1.8 ![]() |
12.97 ![]() |
2.46 ![]() |
1.127 ![]() |
0.684 ![]() |
52 036.4 | 1.93 ![]() |
- | 2.61 ![]() |
1.217 ![]() |
0.86 ![]() |
52 041.8 | 1.83 ![]() |
13.31 ![]() |
2.26 ![]() |
1.107 ![]() |
0.696 ![]() |
52 043.7 | 1.99 ![]() |
13.71 ![]() |
2.25 ![]() |
1.155 ![]() |
0.608 ![]() |
52 074.7 | 2.68 ![]() |
17.38 ![]() |
3.41 ![]() |
1.667 ![]() |
0.687 ![]() |
52 075.7 | 2.84 ![]() |
15.08 ![]() |
3.13 ![]() |
1.539 ![]() |
0.798 ![]() |
52 237.6 | 3.34 ![]() |
21.66 ![]() |
5.06 ![]() |
2.221 ![]() |
1.432 ![]() |
52 238 | 3.33 ![]() |
- | 5.12 ![]() |
- | - |
52 239 | 3.33 ![]() |
20.55 ![]() |
- | - | - |
52 297.6 | 3.45 ![]() |
- | 4.23 ![]() |
- | - |
52 299.4 | 3.68 ![]() |
19.87 ![]() |
3.95 ![]() |
- | - |
52 327.4 | 3.21 ![]() |
- | 3.86 ![]() |
- | - |
52 327.5 | 3.14 ![]() |
- | 3.89 ![]() |
1.35 ![]() |
0.988 ![]() |
52 338.7 | 4.17 ![]() |
19.93 ![]() |
3.99 ![]() |
1.773 ![]() |
1.378 ![]() |
52 339.7 | 4.17 ![]() |
21.14 ![]() |
- | - | - |
52 340.8 | 3.96 ![]() |
- | 4.42 ![]() |
- | - |
52 350.8 | 2.74 ![]() |
- | 4.03 ![]() |
1.666 ![]() |
0.755 ![]() |
52 367.7 | 3.94 ![]() |
- | 3.83 ![]() |
- | - |
52 368.7 | 3.94 ![]() |
19.06 ![]() |
- | - | - |
52 369.7 | 3.79 ![]() |
19.39 ![]() |
3.73 ![]() |
1.605 ![]() |
0.863 ![]() |
52 370.7 | 3.91 ![]() |
19.29 ![]() |
3.93 ![]() |
1.671 ![]() |
0.911 ![]() |
52 397.7 | 3.3 ![]() |
- | 3.89 ![]() |
1.368 ![]() |
0.622 ![]() |
52 398.7 | 3.3 ![]() |
18.82 ![]() |
- | - | - |
52 399.7 | 3.27 ![]() |
- | 3.72 ![]() |
1.347 ![]() |
0.568 ![]() |
52 411.4 | 3.84 ![]() |
- | 4.04 ![]() |
- | - |
52 427.7 | 3.72 ![]() |
- | 4 ![]() |
1.447 ![]() |
0.693 ![]() |
52 429.7 | 3.71 ![]() |
20.55 ![]() |
4.34 ![]() |
1.718 ![]() |
0.762 ![]() |
52 430.7 | 3.75 ![]() |
- | 4.04 ![]() |
- | - |
52 450.4 | 4.24 ![]() |
21.93 ![]() |
4.5 ![]() |
1.571 ![]() |
1.325 ![]() |
52 620 | 3.36 ![]() |
- | 4.29 ![]() |
- | - |
52 621 | 3.36 ![]() |
19.15 ![]() |
- | - | - |
52 622 | 3.44 ![]() |
19.95 ![]() |
4.32 ![]() |
1.914 ![]() |
0.769 ![]() |
52 623 | 3.58 ![]() |
- | 4.76 ![]() |
- | - |
52 665 | 5.07 ![]() |
- | 4.79 ![]() |
- | - |
52 665.9 | 5.07 ![]() |
24.08 ![]() |
- | - | - |
52 666.9 | 5.07 ![]() |
22.26 ![]() |
4.79 ![]() |
2.027 ![]() |
1.21 ![]() |
52 667.9 | 5.57 ![]() |
23.24 ![]() |
4.96 ![]() |
2.246 ![]() |
1.364 ![]() |
52 723.8 | 4.54 ![]() |
- | 5.35 ![]() |
2.304 ![]() |
1.227 ![]() |
52 724.8 | 4.17 ![]() |
22.59 ![]() |
4.96 ![]() |
2.277 ![]() |
1.369 ![]() |
52 725.8 | 4.17 ![]() |
21.54 ![]() |
- | - | - |
52 739.7 | 5.17 ![]() |
23.31 ![]() |
- | - | - |
52 740.8 | 5.17 ![]() |
- | 5.97 ![]() |
2.729 ![]() |
1.347 ![]() |
52 741.8 | 5.15 ![]() |
23.5 ![]() |
5.36 ![]() |
2.603 ![]() |
1.65 ![]() |
52 743.3 | 5.15 ![]() |
22.47 ![]() |
- | - | - |
52 768.4 | 5.16 ![]() |
- | 5.67 ![]() |
- | - |
52 768.3 | 5.08 ![]() |
- | 5.44 ![]() |
2.173 ![]() |
1.277 ![]() |
52 769.3 | 5.33 ![]() |
24.39 ![]() |
5.57 ![]() |
2.064 ![]() |
1.353 ![]() |
52 770.3 | 5.33 ![]() |
23.29 ![]() |
- | - | - |
52 782.7 | 5.03 ![]() |
24.98 ![]() |
5.82 ![]() |
2.488 ![]() |
1.387 ![]() |
52 783.8 | 5.17 ![]() |
- | 5.47 ![]() |
2.714 ![]() |
1.374 ![]() |
52 784.7 | 5.55 ![]() |
23.56 ![]() |
- | - | - |
52 785.7 | 5.55 ![]() |
- | 5.31 ![]() |
- | - |
52 812.8 | 4.18 ![]() |
- | 5.74 ![]() |
2.467 ![]() |
1.429 ![]() |
52 813.7 | 4.18 ![]() |
22.76 ![]() |
- | - | - |
52 965.6 | 3.68 ![]() |
- | 4.79 ![]() |
- | - |
52 966.6 | 3.46 ![]() |
- | 4.87 ![]() |
2.428 ![]() |
1.371 ![]() |
52 967.9 | 3.3 ![]() |
- | 4.83 ![]() |
2.709 ![]() |
1.588 ![]() |
52 995.6 | 3.52 ![]() |
- | 5.55 ![]() |
2.504 ![]() |
2.258 ![]() |
53 032.9 | 3.26 ![]() |
- | 4.38 ![]() |
2.111 ![]() |
0.849 ![]() |
53 053 | 3.19 ![]() |
20.35 ![]() |
4.92 ![]() |
2.405 ![]() |
1.4 ![]() |
53 081.8 | 2.76 ![]() |
- | 4.18 ![]() |
1.861 ![]() |
0.695 ![]() |
53 082.7 | 2.76 ![]() |
17.91 ![]() |
- | - | - |
53 107.6 | 2.03 ![]() |
16.54 ![]() |
- | - | - |
53 108.7 | 2.03 ![]() |
- | 3.04 ![]() |
1.432 ![]() |
0.452 ![]() |
53 109.7 | 2.03 ![]() |
16.14 ![]() |
- | - | - |
53 145.7 | 1.92 ![]() |
- | 2.64 ![]() |
1.18 ![]() |
0.585 ![]() |
53 146.7 | 1.92 ![]() |
14.7 ![]() |
- | - | - |
53 168.7 | 2.29 ![]() |
- | 2.74 ![]() |
1.088 ![]() |
0.601![]() |
53 169.7 | 2.29 ![]() |
14.21 ![]() |
- | - | - |
53 173.7 | 2.7 ![]() |
- | 2.76 ![]() |
1.338 ![]() |
0.607 ![]() |
53 355 | 2.85 ![]() |
- | 3.72 ![]() |
1.618 ![]() |
0.857 ![]() |
53 356 | 2.85 ![]() |
18.13 ![]() |
- | - | - |
53 357.6 | 2.85 ![]() |
18.91 ![]() |
3.71 ![]() |
1.466 ![]() |
0.799 ![]() |
53 361.5 | 2.81 ![]() |
17.85 ![]() |
3.48 ![]() |
1.481 ![]() |
0.616 ![]() |
53 386.9 | 2.56 ![]() |
19.21 ![]() |
3.84 ![]() |
1.736 ![]() |
0.756 ![]() |
53 388 | 2.57 ![]() |
- | 3.79 ![]() |
1.692 ![]() |
0.625 ![]() |
53 388.9 | 2.57 ![]() |
17.64 ![]() |
- | - | - |
53 408.8 | 2.3 ![]() |
16.94 ![]() |
- | - | - |
53 416.9 | 2.04 ![]() |
- | 2.96 ![]() |
1.294 ![]() |
0.639 ![]() |
53 417.5 | 2.04 ![]() |
16.36 ![]() |
- | - | - |
53 446.8 | 1.92 ![]() |
16.16 ![]() |
- | - | - |
53 447.8 | 1.92 ![]() |
16.62 ![]() |
3.07 ![]() |
1.376 ![]() |
0.716 ![]() |
53 451.3 | 2.14 ![]() |
16.8 ![]() |
3.1 ![]() |
- | - |
53 474.4 | 1.73 ![]() |
14.01 ![]() |
- | - | - |
53 475.8 | 1.73 ![]() |
- | 2.47 ![]() |
1.014 ![]() |
0.62 ![]() |
53 476.8 | 1.73 ![]() |
13.97 ![]() |
- | - | - |
53 477.3 | 1.78 ![]() |
15.77 ![]() |
- | - | - |
53 478.7 | 1.83 ![]() |
15.08 ![]() |
2.42 ![]() |
1.071 ![]() |
0.684 ![]() |
53 503.3 | 2.16 ![]() |
14.79 ![]() |
2.51 ![]() |
- | - |
53 503.7 | 2.16 ![]() |
- | 2.74 ![]() |
1.241 ![]() |
0.796 ![]() |
53 504.7 | 2.16 ![]() |
14.65 ![]() |
- | - | - |
53 507.4 | 2.1 ![]() |
15.76 ![]() |
2.6 ![]() |
- | - |
53 530.7 | 1.89 ![]() |
15.07 ![]() |
2.62 ![]() |
1.168 ![]() |
0.681 ![]() |
53 531.6 | 1.94 ![]() |
- | 2.74 ![]() |
- | - |
53 531.6 | 1.94 ![]() |
14.92 ![]() |
- | - | - |
53 538.3 | 1.74 ![]() |
13.25 ![]() |
2.49 ![]() |
1.207 ![]() |
0.93 ![]() |
53 703 | 3.73 ![]() |
18.92 ![]() |
4.42 ![]() |
- | - |
53 704 | 3.57 ![]() |
- | 4.44 ![]() |
1.577 ![]() |
1.357 ![]() |
53 711 | 3.04 ![]() |
- | 4.3 ![]() |
2.071 ![]() |
1.036 ![]() |
53 712 | 2.79 ![]() |
- | 4.32 ![]() |
2.197 ![]() |
1.01 ![]() |
53 732 | 2.41 ![]() |
15.84 ![]() |
3.49 ![]() |
1.733 ![]() |
0.904 ![]() |
53 733 | 2.45 ![]() |
16.01 ![]() |
3.39 ![]() |
- | - |
53 756.9 | 1.88 ![]() |
- | 3.14 ![]() |
- | - |
53 757.9 | 1.92 ![]() |
- | 3.16 ![]() |
- | - |
53 760.5 | 1.8 ![]() |
15.62 ![]() |
2.81 ![]() |
- | - |
53 761.5 | 1.82 ![]() |
16.59 ![]() |
2.89 ![]() |
1.372 ![]() |
0.845 ![]() |
53 786.9 | 2.07 ![]() |
15.64 ![]() |
3.16 ![]() |
1.69 ![]() |
0.767 ![]() |
53 787.5 | 1.91 ![]() |
16.57 ![]() |
3.31 ![]() |
1.775 ![]() |
0.982 ![]() |
53 788.5 | 1.94 ![]() |
16.39 ![]() |
3.31 ![]() |
1.544 ![]() |
0.876 ![]() |
53 789.5 | 1.94 ![]() |
16.55 ![]() |
- | 1.724 ![]() |
1.027 ![]() |
53 803.8 | 3.25 ![]() |
16.9 ![]() |
3.43 ![]() |
1.684 ![]() |
1.087 ![]() |
53 816.4 | 3.22 ![]() |
17.83 ![]() |
3.98 ![]() |
1.843 ![]() |
1.471 ![]() |
53 817.4 | 3.06 ![]() |
17.79 ![]() |
4.04 ![]() |
1.755 ![]() |
1.571 ![]() |
53 843.7 | 3.53 ![]() |
19.68 ![]() |
4.55 ![]() |
2.34 ![]() |
1.407 ![]() |
53 844.8 | 3.41 ![]() |
- | 4.52 ![]() |
2.071 ![]() |
1.458 ![]() |
53 845.7 | 3.32 ![]() |
- | 4.38 ![]() |
2.054 ![]() |
1.58 ![]() |
53 846.4 | 3.31 ![]() |
19.01 ![]() |
4.6 ![]() |
2.083 ![]() |
1.887 ![]() |
Year |
![]() |
![]() ![]() |
![]() |
![]() ![]() |
![]() |
![]() ![]() |
![]() |
![]() ![]() |
![]() |
![]() ![]() |
1996 | 3.9 | 2.27 | 1.9 | 1.2 | 3.90 | 1.56 | 7.5 | 10.4 | 4.20 | |
1997 | 5.17 | 2.98 | 2.19 | 1.63 | 1.63 | 1.81 | 6.0 | 1.62 | 10.22 | 4.20 |
1998 | 2.18 | 1.37 | 3.1 | 2.4 | 1.90 | 1.42 | 5.75 | 1.62 | 10.18 | 4.70 |
1999 | 3.24 | 2.22 | 1.75 | 1.28 | 2.29 | 1.68 | 5.65 | 4.95 | 6.26 | 3.00 |
2000 | 2.3 | 3.65 | 3.62 | 2.31 | 2.12 | 0.82 | 2.88 | 2.53 | 4.65 | 4.47 |
2001 | 3.77 | 3.16 | 2.9 | 1.13 | 1.63 | 2.25 | 4.2 | 1.7 | 12.90 | 4.67 |
2002 | 2.05 | 1.38 | 2.7 | 1.66 | 3.91 | 2.44 | 5.37 | 5.9 | 5.60 | 1.56 |
2003 | 3.34 | 2.37 | 2.8 | 1.49 | 2.86 | 2.44 | 4.82 | 2.67 | 7.62 | 4.76 |
2004 | 2.65 | 2.26 | 2.6 | 0.8 | 2.25 | 3.18 | 3.85 | 4.45 | 7.28 | 4.57 |
2005 | 2.37 | 2.14 | 2.72 | 2.63 | 1.96 | 2.22 | 3.3 | 1.31 | 7.37 | 5.86 |
2006 | 2.42 | 1.76 | 2.12 | 1.68 | 1.62 | 1.34 | 6.58 | 1.97 | 8.62 | 4.71 |
mean | 2.84 | 1.23 | 2.46 | 0.75 | 2.37 | 0.84 | 4.99 | 1.46 | 7.78 | 2.51 |
(1996-2006) |