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This could suggest that either the HBL jets have lower Lorentz actors compared to LDLs. or they are oriented al larger angles {ο theline of sight. | This could suggest that either the HBL jets have lower Lorentz factors compared to LBLs, or they are oriented at larger angles to theline of sight. |
drivers of turbulence were necessarily weaker than the MRI. a single measurement of the turbulent velocity would then distinguish between the two. | drivers of turbulence were necessarily weaker than the MRI, a single measurement of the turbulent velocity would then distinguish between the two. |
If. ou the other hand. we treat the streneth of lyvdrocdvuamic urbulence as a free parameter. then our results sugeest iat the vertical variation of turbuleut velocities iu the wdrodyvuamuc and MITD. limits can lave a qualitatively similar trend. | If, on the other hand, we treat the strength of hydrodynamic turbulence as a free parameter, then our results suggest that the vertical variation of turbulent velocities in the hydrodynamic and MHD limits can have a qualitatively similar trend. |
Of course. the plwsical mechanisims iat nüeght initiate hydrodynamic turbulence witlout arbitrary forcing could. iu principle. inupriut distinctive characteristics iuto the observable turbulent velocity field. which would allow them to be distinguished from 1ο MERI more reacülv. | Of course, the physical mechanisms that might initiate hydrodynamic turbulence without arbitrary forcing could, in principle, imprint distinctive characteristics into the observable turbulent velocity field, which would allow them to be distinguished from the MRI more readily. |
To test this. it would be useful to repeat the analysis presented here for disks iu which these other sources of turbulence are active. | To test this, it would be useful to repeat the analysis presented here for disks in which these other sources of turbulence are active. |
These calculations are currently underway and will be preseuted in future work. | These calculations are currently underway and will be presented in future work. |
We thauk Meredith Uueghes. Tilman Dirustiel. Charles Camnue. and Johu Dawley for useful diseussious auk sugeestions regarding this work. | We thank Meredith Hughes, Tilman Birnstiel, Charles Gammie, and John Hawley for useful discussions and suggestions regarding this work. |
We also thauk the anouvinous referee whose comunents ereatlv improves this paper. | We also thank the anonymous referee whose comments greatly improved this paper. |
We acknowledge support from tle NSF (AST-0s07171. AST-0907872). οι NASAs Origius of Sol Systems program CNNNO9ADBO90CU. frou: NASA's Astrophysics Theory. program (NNNILAEL2C). anc from the NSF through TeraCaid resources provider bv the Texas Advanced Computing Center aud the National Tustitute for Computational Science uuder erant nuuber TG-ASTO090106. | We acknowledge support from the NSF (AST-0807471, AST-0907872), from NASA's Origins of Solar Systems program (NNX09AB90G), from NASA's Astrophysics Theory program (NNX11AE12G), and from the NSF through TeraGrid resources provided by the Texas Advanced Computing Center and the National Institute for Computational Science under grant number TG-AST090106. |
We also acknowledge the Texas Advanced Computing Center at The University of Texas at Austin for providing TPC and visualization resources that have contributed to the research results reported within this paper. | We also acknowledge the Texas Advanced Computing Center at The University of Texas at Austin for providing HPC and visualization resources that have contributed to the research results reported within this paper. |
Computations were also performed on Kraken at the National Institute for Computational Sciences. | Computations were also performed on Kraken at the National Institute for Computational Sciences. |
(2009b).. where the separation velocities. found for the detected knots range between 15e ancl 20€. | , where the separation velocities found for the detected knots range between $c$ and $c$. |
. Since 2007. when also and AGILE satellites could. provide crucial information to relate the radio and hieh-encrey *-rav emission. we could. follow the evolution of three additional knots. labelled NI. N2 and. N3 in Fig. 4.. | Since 2007, when also and AGILE satellites could provide crucial information to relate the radio and high-energy $\gamma$ -ray emission, we could follow the evolution of three additional knots, labelled N1, N2 and N3 in Fig. \ref{mojave_sep10}. . |
For Nl. α le separation speed of G75 pras/ve (i.e. 11.60). was reported. ον Abdo.etal.(2010b) using data between september 2008 ancl December. 2009. | For N1, a $\sigma$ separation speed of 675 $\mu$ as/yr (i.e. $c$ ) was reported by \citet{abdo10b} using data between September 2008 and December 2009. |
La our analysis we expand the time baseline to December 2010. | In our analysis we expand the time baseline to December 2010. |
We determine he angular separation speeds of these three new knots rom the core. which we assume stationary: we corive 1.060-E0.056 masvr. 1.102-250.113 masvr. and. 1.041-50.250 mas/ve for NI. N2 and N3 respectively. which correspond ο κι=1T.5x0.9. Jy»=15.0L9. Op;=17.0+ 4.0. | We determine the angular separation speeds of these three new knots from the core, which we assume stationary: we derive $\pm$ 0.056 mas/yr, $\pm$ 0.113 mas/yr, and $\pm$ 0.250 mas/yr for N1, N2 and N3 respectively, which correspond to $\beta_{\rm N1}=17.3\pm 0.9$, $\beta_{\rm N2}=18.0\pm 1.9$, $\beta_{\rm N3}=17.0\pm 4.0$ . |
For each. knot the time of zero separation obtained. from he fit is Zon,=2008.61+0.11. Zone:=2009.38+0.17. and Ton;=2009.93£0.25 (Fig. 8)). | For each knot the time of zero separation obtained from the fit is $T_{\rm
0,N1}=2008.61\pm 0.11$, $T_{\rm 0,N2}=2009.38\pm 0.17$, and $T_{\rm
0,N3}= 2009.93\pm 0.25$ (Fig. \ref{fit_mojave}) ). |
Components NI and 2 were also detected in VLBA observations at 43 Gllz by Alarscheretal.(2010). | Components N1 and N2 were also detected in VLBA observations at 43 GHz by \citet{marscher10}. |
. Given the lower spatial resolution (and larger opacity) with respect to the 43 Cillz. these components were detected at 15 Gllz a few months later when their separation from the core was large enough to »e resolved. | Given the lower spatial resolution (and larger opacity) with respect to the 43 GHz, these components were detected at 15 GHz a few months later when their separation from the core was large enough to be resolved. |
The apparent separation speeds derived. at 43 (11 are 2442 and 00.0 for NI and N2 respectively. i.c. systematically larger than our values. | The apparent separation speeds derived at 43 GHz are $\pm$ 2 and $\pm$ 0.6 for N1 and N2 respectively, i.e. systematically larger than our values. |
This discrepancy may be due to the lower resolution of the 15-ClLIz data that may cause a blending with other features. as also suggested in Abdoetal.(2010b). | This discrepancy may be due to the lower resolution of the 15-GHz data that may cause a blending with other features, as also suggested in \citet{abdo10b}. |
. Llowever. it must be noted that the higher separation speed found at 43 Cillz is not rellected in a substantially cülferent origin time of the jet components. | However, it must be noted that the higher separation speed found at 43 GHz is not reflected in a substantially different origin time of the jet components. |
In fact. in the case of NI and. N2 components the time of zero separation derived from 43-CGllz data are 40.05 and. 2009.34+0.01 respectively (Alarscheretal.2010)... Le. within the errors estimated from the 15-CGllz data. | In fact, in the case of N1 and N2 components the time of zero separation derived from 43-GHz data are $\pm$ 0.05 and $\pm$ 0.01 respectively \citep{marscher10}, i.e. within the errors estimated from the 15-GHz data. |
ln Table 5 we report the apparent separation speed and the ejection date of the superluminal knots of The population of blazar objects represents a sub-class of AGN characterized. by high. levels. of tux density variability. across the entire. electromagnetic spectrum. | In Table \ref{tabella_moto} we report the apparent separation speed and the ejection date of the superluminal knots of The population of blazar objects represents a sub-class of AGN characterized by high levels of flux density variability across the entire electromagnetic spectrum. |
In the radio band the increase in luminosity is first detected at high frequencies. at. millimeter wavelengths. subsequentIv Followed. at lower frequencies with some delay. consistent with opacity elfects. | In the radio band the increase in luminosity is first detected at high frequencies, at millimeter wavelengths, subsequently followed at lower frequencies with some delay, consistent with opacity effects. |
Episodes of enhanced radio luminosity also seem to be related. to changes in the pe-seale radio structure where new components are ejected with apparent superluminal velocity (e.g.Wagneretal.1995:Jorstaclal.2001). | Episodes of enhanced radio luminosity also seem to be related to changes in the pc-scale radio structure where new components are ejected with apparent superluminal velocity \citep[e.g.][]{wagner95,jorstad01}. |
. In the following we discuss our results on the multi-epoch analvsis of the total intensity ancl polarimetric racio properties. and we compare the source activity at various frequency v means of the multi-epoch analysis of the parsec-scale structure of 11510-089.. various knots emerging [rom the core at eilferent times have been detected. | In the following we discuss our results on the multi-epoch analysis of the total intensity and polarimetric radio properties, and we compare the source activity at various frequency By means of the multi-epoch analysis of the parsec-scale structure of 1510-089, various knots emerging from the core at different times have been detected. |
In particular. we obtain a solid estimate for one of the components detected. between 1999 and 2001. thanks to the addition of 5 new position measurements at 4.8 and SA Cillz. | In particular, we obtain a solid estimate for one of the components detected between 1999 and 2001, thanks to the addition of 5 new position measurements at 4.8 and 8.4 GHz. |
Interestingly. comparingthe properties. of the knots analvsed in this paperwith those studied in previous works (Table 3)) we found that all the knots are separating from | Interestingly, comparingthe properties of the knots analysed in this paperwith those studied in previous works (Table \ref{tabella_moto}) ) we found that all the knots are separating from |
in Hs. extremely high velocity CO and SO (see Fig. 1(3))) | in $_2$, extremely high velocity CO and SO (see Fig. \ref{jets}) ) |
and indicated by an arrow in Figs. 4--7.. | and indicated by an arrow in Figs. \ref{ch3ohmom0}- \ref{hncomom0}. |
Interestingly. the occurrence of CH30OH emission along the OF] axis is more evident in the two lower excitation transitions (reported in Table 2)). | Interestingly, the occurrence of $_3$ OH emission along the OF1 axis is more evident in the two lower excitation transitions (reported in Table \ref{id}) ). |
Asshown by the spectra in Fig. 3.. | Asshown by the spectra in Fig. \ref{spectra-lsb}, |
this is not due to low dynamical range. since all methanol lines used 1n this analysis have a signal-to-noise ratio larger than 40 at the peak of the continuum emission, | this is not due to low dynamical range, since all methanol lines used in this analysis have a signal-to-noise ratio larger than 40 at the peak of the continuum emission. |
Also the OCS emission. and to some extent ος emission. is elongated in the direction the OF2-OF3 outflows. and shows a wisp of emission in the direction of OF1 (Fig. 5)). | Also the OCS emission, and to some extent $^{13}$ CS emission, is elongated in the direction the OF2–OF3 outflows, and shows a wisp of emission in the direction of OF1 (Fig. \ref{ocsmom0}) ). |
Figure 6 shows the zero-th moment maps derived from different lines of CH3CN. | Figure \ref{ch3cnmom0} shows the zero-th moment maps derived from different lines of $_3$ CN. |
The spatial distribution of the 114 line. the lowest CH;:CN excitatior line used in our analysis. extends in the direction of the OF] jet and along the axis of the OF2-OF3 outflows. while the other transitions are more compact. | The spatial distribution of the $12_4-11_4$ line, the lowest $_3$ CN excitation line used in our analysis, extends in the direction of the OF1 jet and along the axis of the OF2–OF3 outflows, while the other transitions are more compact. |
Also in thiscase we cai exclude a bias due to different signal-to-noise ratios for the different CH3CN lines. | Also in thiscase we can exclude a bias due to different signal-to-noise ratios for the different $_3$ CN lines. |
The C+HsCN and HNCO (109- 90) line maps are also elongated along the direction of the OF2-OF3 axes. but their emission Is nore compact than for the other species discussed above. | The $_2$ $_5$ CN and HNCO $10_0-9_0$ ) line maps are also elongated along the direction of the OF2–OF3 axes, but their emission is more compact than for the other species discussed above. |
In conclusion. the spatial distribution of CH;OH. OCS. and CH;CN emission could be affected by the presence of the outflows. | In conclusion, the spatial distribution of $_3$ OH, OCS, and $_3$ CN emission could be affected by the presence of the outflows. |
In particular. for CH:OH and CH3CN we find. besides an elongation along the OF2-OF3 axes. also a good correlation with the direction of the OF! outflow. | In particular, for $_3$ OH and $_3$ CN we find, besides an elongation along the OF2–OF3 axes, also a good correlation with the direction of the OF1 outflow. |
Emission at the position RI. the peak of the CO (2- I) red-shifted emission at extremely high velocity in OFI. is detected from the CH:OH (8.,— 7o) and (85— 7,9) lines and the CHsCN (124- 114) transition. | Emission at the position R1, the peak of the CO $2-1$ ) red-shifted emission at extremely high velocity in OF1, is detected from the $_3$ OH $8_{-1}-7_0$ ) and $8_{0}-7_1$ ) lines and the $_3$ CN $12_4-11_4$ ) transition. |
In Sect. | In Sect. |
ον we will analyse the first moment maps to investigate the kinematics of the gas and better constrain the association of molecular emission with the molecular outflows from the 117233 cluster. | \ref{mom1} we will analyse the first moment maps to investigate the kinematics of the gas and better constrain the association of molecular emission with the molecular outflows from the 17233 cluster. |
For transitions analysed in Sect. | For transitions analysed in Sect. |
22. with emission larger than 3 beam widths along the minor axis of the beam. we also computed the first moment distribution. | \ref{mom0}
with emission larger than 3 beam widths along the minor axis of the beam, we also computed the first moment distribution. |
This excludes the HC3N transitions from the analysis. | This excludes the $_3$ N transitions from the analysis. |
The detected velocity shifts are of the order of ἂν~ 6 km s. ie. values larger than velocity resolution of the data cubes (0.5 km s). | The detected velocity shifts are of the order of $\Delta \rm{v} \sim$ 6 km $^{-1}$, i.e. values larger than velocity resolution of the data cubes (0.5 km $^{-1}$ ). |
All CH3CN maps are blue-shifted compared to the systemic velocity (V4) of —3.4. km |1996).. | All $_3$ CN maps are blue-shifted compared to the systemic velocity $V_{\rm sys}$ ) of –3.4 km $^{-1}$. |
However. there is a large uncertainty in the determination of V4, (between —3.7 and -2.5 km sv! from single dish N:H and ΟἱΟ observations. 2011). probably due to the outflow multiplicity in the region. | However, there is a large uncertainty in the determination of $V_{\rm sys}$ (between $-3.7$ and $-2.5$ km $^{-1}$ from single dish $_2$ $^+$ and $^{17}$ O observations, ), probably due to the outflow multiplicity in the region. |
As suggested by the analysis of the integrated intensity distributions. CH3OH clearly presents a velocity gradient along the direction of the OF2-OF3 outflows. with blue-shifted emission to the north-east and red-shifted emission to the south-west. | As suggested by the analysis of the integrated intensity distributions, $_3$ OH clearly presents a velocity gradient along the direction of the OF2–OF3 outflows, with blue-shifted emission to the north-east and red-shifted emission to the south-west. |
Additionally. the CH3:OH (8.,— 79) and (85—Τι) E lines show red-shifted emission associated with the red lobe of the OF] jet (see Fig. 1(b)). | Additionally, the $_3$ OH $8_{-1}-7_0$ ) and $8_0-7_1$ $E$ lines show red-shifted emission associated with the red lobe of the OF1 jet (see Fig. \ref{zoom}) ). |
A wisp of red-shifted emission towards OF] is detected also in the CH:OH (10.5—9_3) line although marginally. | A wisp of red-shifted emission towards OF1 is detected also in the $_3$ OH $10_{-2}-9_{-3}$ ) line although marginally. |
For simplicity. we present the first moment distribution of the CH3CN (12,-114) line in Fig. | For simplicity, we present the first moment distribution of the $_3$ CN $12_4-11_4$ ) line in Fig. |
Ὁ while the CH3CN (125—11>) transition is presented in Fig. 10. | \ref{summary} while the $_3$ CN $12_7-11_7$ ) transition is presented in Fig. \ref{ch3cnmom1}. |
. We see the same behaviour seen 11 the CH:OH (10.5—9 nein the (124-114) transition, the lowest energy analysed line of methyl cyanide: a linear velocity gradient along the E-W axis plus a red-shifted wisp of gas extending to the north-west towards the red-shifted lobe of the OF] outflow. | We see the same behaviour seen in the $_3$ OH $10_{-2}-9_{-3}$ ) line in the $12_4-11_4$ ) transition, the lowest energy analysed line of methyl cyanide: a linear velocity gradient along the E–W axis plus a red-shifted wisp of gas extending to the north-west towards the red-shifted lobe of the OF1 outflow. |
The CH:CN (127-114) line has a more compact emission. and shows a linear velocity gradient along the E-W direction. almost perpendicular to the OF2-OF3 axis, | The $_3$ CN $12_7-11_7$ ) line has a more compact emission, and shows a linear velocity gradient along the E–W direction, almost perpendicular to the OF2–OF3 axis. |
Although not shown here. the velocity field of the CH:C (125—13) line agrees with that of the CH;CN (12;—111) transition. | Although not shown here, the velocity field of the $_3$ CN $12_8-11_8$ ) line agrees with that of the $_3$ CN $12_7-11_7$ ) transition. |
In order to further investigate the association of the CH3C (124— 114) line with the OFI outflow. in Fig. | In order to further investigate the association of the $_3$ CN $12_4-11_4$ ) line with the OF1 outflow, in Fig. |
9 we compare its first moment distribution to the H» distribution and to other tracers of kinematics in the region. | \ref{summary} we compare its first moment distribution to the $_2$ distribution and to other tracers of kinematics in the region. |
The SO blue- and red-shifted emission and the blue- and red-shifted H1O masers trace the blue and red- shifted lobes of the OF! outflow (see Fig. | The SO blue- and red-shifted emission and the blue- and red-shifted $_2$ O masers trace the blue and red- shifted lobes of the OF1 outflow (see Fig. |
9 and 2009)). | \ref{summary} and ). |
If we take into account (1) the EHV OFI red-lobe in CO (2—1). Cit) the SO red- and blue-shifted emission. and (111) the water maser spots. then the contribution of OFI to the kinematics of the CHiCN (124-114) transition. appears reasonably evident. | If we take into account (i) the EHV OF1 red-lobe in CO $2-1$ ), (ii) the SO red- and blue-shifted emission, and (iii) the water maser spots, then the contribution of OF1 to the kinematics of the $_3$ CN $12_4-11_4$ ) transition appears reasonably evident. |
Furthermore. Fig. | Furthermore, Fig. |
9 also shows red-shifted emission elongated towards the R2 red lobe of OF2-OF3 and blue-shifted emission close to the Bl peak of OF2-OF3 as observed in CO (see Fig. 1)). | \ref{summary} also shows red-shifted emission elongated towards the R2 red lobe of OF2–OF3 and blue-shifted emission close to the B1 peak of OF2–OF3 as observed in CO (see Fig. \ref{overview}) ). |
In Fig. | In Fig. |
we also show the velocity field of the CH;CN (123—113) line which hàs been excluded from our analysis because of weak blending with other features towards the centre position. | \ref{summary} we also show the velocity field of the $_3$ CN $12_3-11_3$ ) line which has been excluded from our analysis because of weak blending with other features towards the centre position. |
However. being lower in energy than the (124— 114) transition. the (123— 113) line has a larger emitting size and can help the interpretation of the kinematies of the other CH3C transitions. | However, being lower in energy than the $12_4-11_4$ ) transition, the $12_3-11_3$ ) line has a larger emitting size and can help the interpretation of the kinematics of the other $_3$ CN transitions. |
In this case. the N-W velocity gradient seen in the high J CH:CN transitions and to some extent also in the (124— 114) line is less pronounced. while red-shifted emission is clearly detected towards the R1 position in OF] and towards the shifted lobe of the OF2-OF3 outflows. | In this case, the N–W velocity gradient seen in the high J $_3$ CN transitions and to some extent also in the $12_4-11_4$ ) line is less pronounced, while red-shifted emission is clearly detected towards the R1 position in OF1 and towards the red-shifted lobe of the OF2–OF3 outflows. |
As an additional check. we derived position-velocity plots along several slits placed to sample all possible directions: the OF] axis (PA. —50°). the NE-SW direction (P.A. 30°. as representative of the three possible directions of the OF2- outflows). two slits with position angles 60° and -20°. the N-S and E-W directions. | As an additional check, we derived position-velocity plots along several slits placed to sample all possible directions: the OF1 axis (P.A. $-50^\circ$ ), the NE–SW direction (P.A. $^\circ$, as representative of the three possible directions of the OF2--OF3 outflows), two slits with position angles $^\circ$ and $^\circ$, the N–S and E–W directions. |
All six slits are shown in Fig. 9.. | All six slits are shown in Fig. \ref{summary}. . |
In Fig. | In Fig. |
11. we show the PV diagram along the OF] axis which shows that CH3CN (124— 114) emission is spread over a broad range of velocities (~15 km s! ). | \ref{pv} we show the PV diagram along the OF1 axis which shows that $_3$ CN $12_4-11_4$ ) emission is spread over a broad range of velocities $\sim 15$ km $^{-1}$ ). |
We then extracted spectra of the CH3CN (12,—114) transition for each slit. and fitted the line with a Gaussian profile. | We then extracted spectra of the $_3$ CN $(12_4-11_4)$ transition for each slit, and fitted the line with a Gaussian profile. |
For each slit. we used a linear fit to reproduce the peak velocity as function of the offset position along the slit. | For each slit, we used a linear fit to reproduce the peak velocity as function of the offset position along the slit. |
Results are shown in Fig. 12.. | Results are shown in Fig. \ref{pvs}. . |
The largest velocity gradients are detected along the E-W direction (~114 km s! pe!) and the OFI jet (~99 km s! pe). | The largest velocity gradients are detected along the E–W direction $\sim114$ km $^{-1}$ $^{-1}$ ) and the OF1 jet $\sim99$ km $^{-1}$ $^{-1}$ ). |
In this paper we present results from our recent observing campaign of KWL Dra using the satellite. the Liverpool Telescope. the Isaac Newton Telescope. the Nordic Optical Telescope. the William LHerschel Telescope and the Gemini North Telescope. | In this paper we present results from our recent observing campaign of KL Dra using the satellite, the Liverpool Telescope, the Isaac Newton Telescope, the Nordic Optical Telescope, the William Herschel Telescope and the Gemini North Telescope. |
The strategy for our observations made using the 2.0m Liverpool Telescope (LE) was to obtain a single 180. sec image of KL Dra using the RATCAAL imager (Steele et al. | The strategy for our observations made using the 2.0m Liverpool Telescope (LT) was to obtain a single 180 sec image of KL Dra using the RATCAM imager (Steele et al. |
2004) in the g band filter approximately once every. week. | 2004) in the $g$ band filter approximately once every week. |
During outbursts we increased. the sampling rate to once every few days. | During outbursts we increased the sampling rate to once every few days. |
Images which had been bias subtracted and Ilat-fielded: using the LT automatic pipeline were typically downloaded. the afternoon after the observation had. been made. | Images which had been bias subtracted and flat-fielded using the LT automatic pipeline were typically downloaded the afternoon after the observation had been made. |
We also obtained. supplementary images using the Isaac Newton “Telescope (INTE). and. the Nordic Optical Polescope (NOT). | We also obtained supplementary images using the Isaac Newton Telescope (INT) and the Nordic Optical Telescope (NOT). |
Since Wh Dra is 5.7. from the nucleus of an anonymous ealaxy (Jha et al. | Since KL Dra is $5.7^{''}$ from the nucleus of an anonymous galaxy (Jha et al. |
1998 and Fig 2 of Wood et al. | 1998 and Fig 2 of Wood et al. |
2002). differential imaging would have been an option for obtaining the photometric light curve of KL Dra. | 2002), differential imaging would have been an option for obtaining the photometric light curve of KL Dra. |
However. since the images were taken using a number of telescopes (giving different image scales. etc). we decided to. use. aperture photometry. | However, since the images were taken using a number of telescopes (giving different image scales etc), we decided to use aperture photometry. |
Care was taken to exclude as much of the galaxy as possible and to ensure a star/galaxy [ree background. | Care was taken to exclude as much of the galaxy as possible and to ensure a star/galaxy free background. |
The dillerence in magnitude between two comparison stars was constant to within a few 0.01 mag. | The difference in magnitude between two comparison stars was constant to within a few 0.01 mag. |
To place our photometry onto the standard svstem. we obtained an image of the field and several stancard stars in Oct 2009 using the INT. | To place our photometry onto the standard system, we obtained an image of the field and several standard stars in Oct 2009 using the INT. |
his allowed: us to determine the g band. magnitude of several local comparison stars. | This allowed us to determine the $g$ band magnitude of several local comparison stars. |
We show in Figure |. our optical light curve IKL Dra. | We show in Figure \ref{lt-summary} our optical light curve of KL Dra. |
Our first observation mace on 2009 July 28 showed KL Dra in à bright optical state (g 716.2). | Our first observation made on 2009 July 28 showed KL Dra in a bright optical state $g\sim$ 16.2). |
One week later the system. had faded by around —0.5 mag. after which no observations were obtained for 5 weeks. | One week later the system had faded by around $\sim$ 0.5 mag, after which no observations were obtained for 5 weeks. |
However. 63 davs after our first observation. WL Dra was again observed in a bright optical state (g 716.0) with an outburst amplitude of 73 mag. | However, 63 days after our first observation, KL Dra was again observed in a bright optical state $g\sim$ 16.0) with an outburst amplitude of $\sim$ 3 mag. |
The rise to peak brightness (maximum) was short («2 davs) with a short curation drop in brightness 5 days after maximum. | The rise to peak brightness (maximum) was short $<$ 2 days) with a short duration drop in brightness $\sim$ 5 days after maximum. |
Two weeks after maximum there was another sharp drop in brightness giving an overall duration for the outburst of ~15 clas. | Two weeks after maximum there was another sharp drop in brightness giving an overall duration for the outburst of $\sim$ 15 days. |
A thirel burst was detected from Wh Dra 61.542.0 days after the preceding one. | A third burst was detected from KL Dra $\pm$ 2.0 days after the preceding one. |
Since KL Dra shortly came too close to the Sun to be observable. we obtained. no ground-based. optical observations for nearly 9 weeks. | Since KL Dra shortly came too close to the Sun to be observable, we obtained no ground-based optical observations for nearly 9 weeks. |
However. an outburst was again seen at a time which is consistent with KL Dra showing outbursts on a repeating interval of 760 cdavs. | However, an outburst was again seen at a time which is consistent with KL Dra showing outbursts on a repeating interval of $\sim$ 60 days. |
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