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Crime & Deviance
Level: AS and A Level
Subject: Sociology
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Assess the right realist view that crime is the result of biological rational factors and therefore best solved by formal social control.
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Assess the right realist view that crime is the result of biological rational factors and therefore best solved by formal social In this essay, discussed is the causes and solutions for crime according to right and left realists. The questions answered are going to be, is crime a real problem or is it socially constructed according to the labelling theory or is the root cause of crime the fact that society is unequal or that control and punishment isn't strong enough. Discussed in this essay is going to be right realist ideas on society into crime and deviance. This will come from the likes of James Q Wilson and Richard J. Hernstein who believe that that crime is caused by a combination of biology and social factors. Charles Murray however believes that most crime comes from the underclass (working class people behaving in an anti social way, so one believes that people are socialised into crime. One other right realist theory is Ron Clarke's idea that people decide whether to commit crime or not based on weighing up the costs and benefits, called the Rational Choice Theory. The final theory is the tacking crime theory which was devised by Wilson and Kelling in an article 'broken windows' who believes that it is essential to maintain an ordered society as any sign of deterioration could cause further crime. On the other side of the argument, discussed will be the left realist view who see society as an unequal capitalist one. However, unlike Marxists left realists would like to reform than revolutionise. Discussed from the left realist theories so going to be Young and Lea who believe they have the answer to why crime is caused. One believed that it was a combination or relative depravation (people who believe they are deprived around others) and individualism which are the desire for freedom. These pair of sociologists believes that these two combined make a lethal combination. ...read more.
They say that any sign of deterioration, such as graffiti or vandalism must be dealt with immediately. The pair advocates a 'zero tolerance' policy towards undesirable behaviour such as prostitution, begging and drunkenness. The role of the police should be to focus on controlling the streets so that law-abiding citizens feel safe. Crime prevention policies should reduce the rewards and increase the costs of crime to the offender, for example by 'target hardening' (making public places more difficult to break into), greater use of prison and ensuring punishments follow soon after the offence to maximise their deterrent effect. There are some criticisms of Wilson and Kelling's idea of advocating a zero tolerance policy due to the fact that it gives police a free rein to discriminate against ethnic minority youth, the homeless and people underprivileged. It also results in displacement of crime to other areas. One theorists Jones notes that right realist policies in the USA failed to prevent the crime rate rising. It also overemphasises control of disorder, rather than tackling underlying causes of neighbourhood decline such as a lack of investment. Having such a formal control such as longer prison sentences and zero tolerance can have a negative impact on people having respect to society. Lower class may riot as they have not got the freedom to live with the police and CCTV watching them move. However, unlike other right realist ideas that are preoccupied with petty street crime and ignores corporate crime, which may be more costly and harmful to the public. The broken windows idea is where it is the petty street crimes that lead on to the deterioration of society which leads onto larger crimes such as prostitution and drug dealing. Left realists unlike right realists believe we need to develop explanations of crime that will lead to practical strategies for reducing crime. Lea and Young identify two related causes of crime: relative depravation and individualism. ...read more.
Young and Lea described crime being committed due to a combination of both relative depravation and individualism. The pair believes that these two combined make a lethal combination for discontent which leads to crime amongst other things. Young also described subcultures and say that they are aiming for the goals of mainstream society, however they can't achieve it legitimately, but have to immerse into the 'American Dream' illegitimately. Marginalisation is also a big contributing factor with the lower class that lack clear goals and organisations which leads to resentment and frustration leading onto violence and rioting. Young also believes that we are living in a late modern stage we are moving away from unskilled labour (working class jobs) so that they are turning unemployed. This means that they are getting excluded from society from the middle and upper class. Finally, to prevent crime, the left realist believe that police do not have a very big impact on society but it needs all the agencies to work together in order for crime to decline and a more informal social control. In answer to the essay question it has been argued that left wing realists perspectives on how to solve crime are useful, however in modern society it is very hard to get rid of relative depravation which they believe is on of the main cause. In Britain, the minimum wage and housing has never been better and to tackle crime, one idea from the left realists is to give them better housing condition and better jobs. However, with the housing getting better and the increase in pay, the lower class are able to live much better lives than what the left realists say. The right realist's perspectives are better at providing answers to why and how people commit crime due to the fact that harsher prison sentences and zero tolerance policies would deter criminals who have either committed a crime, or about to commit one. Ron Clarke's rational choice theory in particular has demonstrated why people would commit a crime by weighing out the costs and benefits. ?? ?? ?? ?? Charlie Thompson ...read more.
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Sociological Theories on Crime and Deviance
Deviant identity is the definition a person has of himself or herself as a deviant. The formation of a deviant identity, like other identities, involves a process of social transformation in which a new self-image and new public definition of a person emerges. Most often, deviant identities emerge over time.
Crime and its effects on society. Police Reform Act 2002 The police ...
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Society would then be cautious of black males and street crime. Black males would feel they are being labelled and treated unfairly, they would then turn to crime through reason of the labelling theory; therefore the media are one of the causes for the social construction of crime.
Examine some of the reasons for the existence of deviant subcultures. Assess the view ...
They developed three different groups, criminal, where an illegitimate crime structure is present and young males can learn from criminal role models and expand their criminal career. Conflict subculture, where legitimate and illegitimate opportunities are unsuccessful, which often results in gang violence.
The Justice and welfare debate.
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Assess The Contribution Of Control Theory To Our Understanding Of Crime And Criminality
as with gender, differences in self control probably outweigh differences in supervision in accounting for racial or ethnic variations. (Gottfredson and Hirschi 1990). Summary We began by discussing how crime and criminality became more political during the seventeenth century onwards and the influence of Hobbe`s.
Outline the new right view of the role of education
They believe that schools should be managed in the same way as businesses However, some theorists such as Chubb and Moe would argue that American state education has failed and they make the case for opening it up to new marker forces of supply and demand.
Analyse explanations of crime and deviance and explain the importance of social order and ...
Formal social control is enforced by authorities such as Parliament, who pass laws to determine what is and is not acceptable behaviour, police, who enforce the laws, and the courts and prison service, which impose the punishments for breaking them (Parsons, 2004, p.85).
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redpajama_set_name: RedPajamaCommonCrawl


text:
Q: How does closing a socket affects other's side read For example we have a server-client application. If the server write a message on the socket and then close it before the client's read. Will the client be able to read the message?

A: "If the server write a message on the socket and then close it before the client's read. Will the client be able to read the message?"
Yes. The client will get the data that was sent before the FIN packet that closes the socket.

A: This behavior is implementation specific, in general, you should not assume the client is able to read the message, the close(2) in the Linux manual says:
Be sure to use shutdown(2) to shut down all parts the connection before closing the socket.

If you want to ensure that a client has read that message, make that client acknowledge that action in your application protocol.
When you send data through the socket and then you close that same socket, there's no guarantee that the kernel has emptied it's internal buffers to the network or even could do so (eventual problematic network conditions).

redpajama_set_name: RedPajamaStackExchange


Manufactured between 2003 and 2010, their new supercar allowed Mercedes-Benz and its then Formula 1 partner, McLaren, to showcase their collective experience in the development, construction and production of high-performance sports cars and, just like its legendary 300 SLR predecessor of 1955, it incorporated technological developments that were ahead of their time. Yet the term 'supercar' does not do full justice to the SLR, which, its peerless performance notwithstanding, is a luxurious and finely engineered Gran Turismo in the best traditions of Mercedes-Benz. Rather than creating an all-out, no-compromise supercar, Mercedes-Benz and McLaren decided to take a slightly different route. Instead of placing the engine in behind the cabin, the car had a front-mid-engine layout, with the engine sitting behind the front wheels and just ahead of the cabin. This not only helped to improve the SLR's handling by giving it near-perfect weight distribution but also gave the car a rather spacious boot and cabin, which was not common in cars boasting such performance credentials. As it was supremely engineered and built to incredible standards at McLaren's facilities in Woking, it boasted a very high level of fit and finish, the kind befitting any Mercedes-Benz.
The heart of any car is its engine, and that of the SLR McLaren is truly outstanding. Produced at Mercedes-Benz's AMG Performance Division, it is a 5.5-litre, 24-valve, supercharged V8 producing 617bhp, making it one of the most powerful engines ever found in a series-produced road-going sports car. Impressive though this peak horsepower figure is, it is the torque produced by the Lysholm-type twin-screw supercharger that is its most remarkable feature. The torque curve is almost flat: there is already 440lb/ft by 1,500 rpm and well over 500lb/ft between 3,000 and 5,000 revs, and acceleration is equally phenomenal, with 0 to 60 mph taking just 3.8 seconds and the quarter-mile only 11 seconds. Of course, a car with such impressive speed credentials also requires an equally impressive braking system. An automatic airbrake and Mercedes-Benz's Sensotronic "brake by wire" system assist the massive carbon-ceramic disc brakes and help bring the SLR McLaren down from 120 mph to a stop in less than 240 feet.
This particular SLR was bought by our private vendor through Taylor and Crawley in 2005 and has been owned by him ever since. Finished in the SLR's quintessential colour combination of 'Crystal Laurite Silver SLR' over 'Silver Arrows 300SL Red' leather, it remains in remarkable condition, having covered just 6,700 miles from new. Naturally, it has a full service history with the most recent being in 2017 by Mercedes specialists, Avantgarde. Our vendor reports that he hasn't used the car since, hence the reason why he is selling it - this car needs to be used and enjoyed which is why it's coming to the open market for the first time in 14 years.
Offered at a very competitive and sensible guide price, when you compare it with asking prices elsewhere, this really is a fantastic opportunity to acquire a very special car that delivers in terms of both value and collectability. Though the partnership between McLaren and Mercedes-Benz, with the intention of creating world-beating road cars, was a brief one, it was also a spectacular moment that may never occur again. Given the significance of this venture and the skyrocketing appeal of the SLR's direct competitors, the Ford GT and Porsche Carrera GT, there is no doubt that this is the moment in time when a Mercedes-Benz SLR McLaren should be considered for one's collection. The Cherished Registration Number, WHO5 SLR, will pleasingly remain with the car.


Al Turtle offers so many great resources. One of them is an article, Safety and the Lizard, in which he discusses "The Logic, Science, and Art of Maintaining Safety between People."
He does a beautiful job explaining how our brain works when we are triggered into the fight or flight response.


text:
\section{Introduction}
\label{intro}
Observations of intensity variations at different wavelengths
constitute a highly effective probe of the physics of active
galactic nuclei (AGN). In the optical domain, numerous such
studies have been carried out, covering time scales down to hours
and even minutes, sometimes coordinated with monitoring in other
wavebands (e.g., \citealt*{1989Natur.337..627Miller}; \citealt*{1995ARA&A..33..163Wagner};
\citealt{1995ApJ...452..582Jang,1997AJ....114..565Jang}; \citealt*{1999A&AS..135..477Romero};
\citealt{2002A&A...390..431Romero}; \citealt*{1993MNRAS.262..963GK, 1993A&A...271...89GK, 1995MNRAS.274..701GK};
\citealt{2000MNRAS.314..815GK,2003ApJ...586L..25GK,2011MNRAS.416..101GK};
\citealt*{1996MNRAS.281.1267Sagar}; \citealt{2004MNRAS.348..176Sagar};
\citealt{1991AJ....101.1196Carini, 1992AJ....104...15Carini, 2007AJ....133..303Carini};
\citealt*{1990AJ....100..347Carini, 1992ApJ...385..146Carini, 1998AJ....116.2667Carini, 2003AJ....125.1811Carini};
\citealt{2004MNRAS.350..175Stalin, 2004JApA...25....1Stalin, 2005MNRAS.356..607Stalin};
\citealt{1997AJ....113.1995Noble};
\citealt{2007BASI...35..141AG, 2009MNRAS.399.1622AG, 2010MNRAS.401.2622AG, 2012A&A...544A..37AG};
\citealt*{2005A&A...440..855Gupta, 2009NewA...14...88Gupta};
\citealt{1998ApJ...501...69Diego}; \citealt{2009AJ....138..991Ramirez}; \citealt{2011MNRAS.412.2717Joshi};
\citealt{2008AJ....136.2359Gupta, 2008AJ....135.1384Gupta, 2012MNRAS.425.1357Gupta};
\citealt{2010ApJ...719L.153Rani, 2010MNRAS.404.1992Rani, 2011MNRAS.413.2157Rani};
\citealt{2010ApJ...718..279Gaur, 2012MNRAS.425.3002Gaur}).
Since 1990, most observations of intra-night optical
variability (INOV) have been made using CCD detectors, which allow
simultaneous recording of a number of stars within the same chip.
Not only are some of these simultaneously monitored stars used
for measuring any variations in the seeing disk during the course
of the monitoring session, but, more importantly, they are used
as non-varying standards relative to which the light curve of the
target AGN can be drawn.  Such `differential light curves' (DLCs) are
also drawn for the candidate `comparison stars' themselves and used
to check for the presence of INOV of those stars, in which case they
are disqualified as comparison stars (e.g.,
\citealt{1991Sci...254R1238Miller}; \citealt{2004JApA...25....1Stalin,
2006ASPC..350..183Wiita}).
A key advantage of using DLCs is that the effects of any
fluctuations in the atmospheric attenuation and even in the seeing
disk are mostly canceled out, and this way the
variability detection threshold is pushed down enormously (e.g.,
\citealt*{1986PASP...98..802Howell}; \citealt*{1989Natur.337..627Miller};
\citealt{1993AJ....106.2441Gilliland};
\citealt{2005PASP..117.1187Howell}). Thus, intra-night optical
variability (INOV) with amplitudes as low as 1 to 2 per cent can be
routinely detected using 1-metre class telescopes.
(e.g., see \citealt{2012A&A...544A..37AG} and references therein).
Since 1998, a large body of such sensitive observations has been
accumulated, in a fairly uniform manner, using the 104-cm
Sampurnanand telescope of ARIES in Nainital (India)
(\citealt{2004MNRAS.350..175Stalin, 2004JApA...25....1Stalin, 2005MNRAS.356..607Stalin};
\citealt{2008AJ....136.2359Gupta, 2008AJ....135.1384Gupta, 2012MNRAS.425.1357Gupta};
\citealt{2003ApJ...586L..25GK,2011MNRAS.416..101GK};
\citealt{2007BASI...35..141AG, 2009MNRAS.399.1622AG, 2010MNRAS.401.2622AG, 2012A&A...544A..37AG}
). Usually, the
targets monitored in these studies are optically luminous and relatively bright
point-like AGN, namely, quasars (both radio-loud and radio-quiet)
and BL Lacs, in the magnitude range $m_v$ = 15 - 17 mag.
\\
A number of statistical tests have been employed in the
literature for detecting the presence of variability in DLCs.
Until recently, the most popular test has been the, so called,
$C$-test (\citealt*{1997AJ....114..565Jang};
\citealt{1999A&AS..135..477Romero}).
Basically, this involves computation of a factor `C' for a given DLC
of a target object,
where C is the ratio of the standard deviation of the AGN light
curve to the standard deviation of the comparison star-star light curve, i.e.,
\begin{equation}
C = \frac{\sigma_{t-s}}{\sigma_{s-s}} =
\frac{\sigma_{t-s}}{\langle \sigma_{t-s} \rangle}
\end{equation}
where $\sigma_{t-s}$ is the standard deviation of the `target-star' DLC,
and $\langle \sigma_{t-s} \rangle$ is the mean of the (formal) rms errors
of the individual data points in the `target-star' DLC.
\\
This ratio `C' has been taken to have a Gaussian (normal) distribution (e.g.,
\citealt*{1997AJ....114..565Jang}, \citealt{1999A&AS..135..477Romero}).
Thus, an AGN DLC found to have `C' greater than
2.576 (corresponding to significance level, $\alpha=$ 0.01)
is declared to be `variable'. Similarly, an AGN
DLC having computed `C' value greater than 1.950 and less than 2.576
(corresponding to $\alpha=$ 0.05) is termed as `probable variable'.
However, recently, \citet{2010AJ....139.1269Diego} has questioned the validity
of this test on the ground that C-statistics does not have
a normal distribution and the two tailed p-values of
normal distribution should not be
used as a statistical indicator of INOV at a given $\alpha$
(variable vs. non-variable). The argument is as follows :\\
(a) The C-statistic is always positive, making it a
{\it one-sided} comparison, unlike the normal
Gaussian distribution which is {\it two-sided} comparison. \\
(b) For a test statistic to have a standard
normal distribution, the expected value is distributed around
0 while in case of `C' statistic it is distributed around 1
when $\sigma_{t-s} = \sigma_{s-s}$ is satisfied.  \\
(c) One cannot compare two standard deviations using the normal
distribution as they are not lineal statistical operators.
\\
Thus, \citet{2010AJ....139.1269Diego} has argued in favour of {\it F}-test
which relies on the computation of {\it F}-factor, being the ratio of
two variances, as follows (see also, \citealt*{2010ApJ...723..737Villforth}):
\\
\begin{equation}
\label{ftest}
F =\frac{Var_{observed}}{Var_{expected}}= \frac{Var_{t-s}}{Var_{s-s}}
=\frac{Var_{t-s}}{\langle \sigma_{t-s}^2 \rangle}
\end{equation}
\\
where $Var_{t-s}$ is the variance of the `target-star' DLC, and
$\langle \sigma_{t-s}^2 \rangle$,
is the mean of the squares of the (formal) rms errors of the individual data
points in the `target-star' DLC.
\\
\\
Clearly, both the {\it C}-test and the {\it F}-test require a precise estimate
of the rms error ($\sigma$) associated with individual data points,
which is usually determined using the {\sc APPHOT} routine in the
{\emph IRAF}\footnote{\textrm
{Image Reduction and Analysis Facility (http://iraf.noao.edu/) }} software.
Many years ago, it was pointed out that the
$\sigma$ returned by this algorithm is systematically too low by
a factor, $\eta$, for which a value of 1.75 was estimated using
the DLCs derived for pairs of steady stars (\citealt{1995MNRAS.274..701GK}).
This inference ($\eta \neq $ 1) has been borne out in several
independent studies from atleast 4 different observatories
and the derived values of this parameter range
between 1.3 and 1.75 (\citealt{1995MNRAS.274..701GK}; \citealt{1999MNRAS.309..803Garcia};
\citealt{2005MNRAS.358..774Bachev}; \citealt{2004JApA...25....1Stalin};
\citealt{2007BASI...35..141AG}).
The most recent attempt to determine $\eta$ used DLCs for 73 pairs of steady
stars and a best-fit value of $\eta$ = 1.5 was obtained
(\citealt{2012A&A...544A..37AG}).
Clearly, a neglect of $\eta$ factor (i.e., setting
$\eta$ = 1) might often lead to spurious claims of INOV (above
a preset statistical significance threshold). It is therefore
important to achieve a greater precision in the determination of $\eta$,
by avoiding the use of any photometric data that fall within a
parameter space that is more prone to introducing larger uncertainty in
the $\eta$ determination.
\\
A prime candidate for a part of this `undesirable' parameter space is the
mismatch between the brightness of the chosen steady comparison
stars which are paired to derive the DLCs which are collectively
used for $\eta$ determination.
The mismatch can be represented by $\Delta m_{s}$ = $m_{s1} - m_{s2}$.
The purpose of the present study is to identify the `safe'
parameter space for $\Delta m_{s}$, outside which
a significant distortion of the
$\eta$ estimate can occur. This has important implications for the INOV
search since several claims of large INOV of AGN have been questioned
because of a large mismatches between their brightnesses and those of the
comparison stars used for deriving the differential light curves (e.g., \citealt{2007MNRAS.374..357Cellone}).
\\
\section{The sample of intra-night optical DLCs}
\label{sample}
Using the 1-m Sampurnanand telescope (ST) of ARIES, a long-term programme
was launched in 1998, for characterizing the INOV properties of important
AGN classes.
Results of this ongoing study have been reported in a
series of publications and in the Ph.D. theses of C. S. Stalin (\citeyear{2003PhDT.......263Stalin})
and Arti Goyal (\citeyear{2010PhDT.......263Arti}) (\citealt{2012A&A...544A..37AG} and references
therein; \citealt{2005MNRAS.356..607Stalin} and references therein).
Optical intra-night monitoring data from other optical observatories
in India, such as the 2-m Himalayan Chandra Telescope
(HCT) and the 2.4m Vainu Bappu Telescope (VBT) of IIA, the 1.2m telescope
at the Gurushikhar observatory of PRL and the 2-m IUCAA Girawali
Observatory (IGO) telescope of IUCAA were also obtained to augment the
data taken with the 1-m ST. Nearly always, just one target AGN was monitored
on a given night.
\\
The above intra-night monitoring program has covered 22 radio-quiet
quasars (RQQs), 10 radio-intermediate quasars (RIQs),
9 radio lobe-dominated quasars (LDQs), 11 radio core-dominated
quasars showing high optical polarization (HPCDQs)
and 12 showing low optical polarization (LPCDQs), as well
as 13 TeV detected BL Lac objects. Sources in the various
classes were chosen from the catalog of
\citet{2001yCat.7224....0Veron} and its subsequent releases.
All the sources lie at $z$ $> 0.14$ and have a listed
$m_B < 18$mag, which allows enough signal-to-noise ratio (SNR) in a typical
exposure time of $\sim10$ minutes.
Each source was monitored for a minimum duration of $\sim$4 hours.
These CCD monitoring observations, aided by a careful and uniform
data analysis procedure, have routinely allowed INOV detection with
amplitude ($\psi$) as low as 1 - 2 per cent.
The present sample consists of 262 such intra-night observations
obtained from the entire data set from our ARIES AGN INOV programme.
\\
\section{Observations and data analysis}
\label{obs}
The observations were made mostly in the {\it R} filter and
occasionally in the {\it V} filter.
The exposure time was typically between 10 to 20 minutes for
the ARIES and Gurushikar observations and ranged between 3 to 6 minutes for
the observations from VBT, IAO and IGO, depending on the
brightness of the source, the phase of the moon and the sky
transparency on that night. The field positioning was adjusted
so as to also have within the CCD frame at least 2--3 comparison stars.
For all the telescopes, bias frames were taken intermittently,
and twilight sky flats were also obtained.
\\
The pre-processing of the images (bias subtraction, flat-fielding and
cosmic-ray removal) was done by applying the standard procedures in the
{\textrm IRAF} and {\textrm MIDAS}\footnote{\textrm {Munich Image and
Data Analysis System (http://www.eso.org/sci/data-processing/software/esomidas/) }}
software packages. The instrumental magnitudes
of the target AGN (all point-like) and the stars in
the image frames were determined by aperture photometry, using
{\textrm APPHOT}.
The magnitude of the target AGN was measured relative to
a few apparently steady comparison
stars present on the same CCD frame. In this way
DLCs for each AGN were derived
relative to 2-3 comparison stars designated as S1, S2, S3.
\\
These comparison stars mostly lie within about 1.5 magnitude
of the target AGN, this being an important criterion for minimizing
the possibility of spurious INOV detection
(e.g., \citealt{2007MNRAS.374..357Cellone}).
Spurious variability
on account of different second-order
extinction coefficients for the AGN and their comparison
stars is a possible problem if the colours of the objects are different.
Although the {\it B-R} colors of the AGN and the comparison
stars used in our study often differ
significantly, it was shown by \citet{1992AJ....104...15Carini}
and \citet{2004JApA...25....1Stalin} that  even though their
photons travel through varying airmass
during the course of monitoring, this has a negligible effect on DLCs.
For each night, an optimum aperture radius for photometry
was chosen by minimizing the dispersions in the star-star DLCs,
that were found using different aperture radii, starting
from the median seeing (FWHM) value on that night to 4
times that value (Fig. \ref{aper_rad}). For very small
aperture radii, the scatter will be large due to improper photon
counting statistics, as the total photon count from the source will
be small. On the other hand, at very large aperture radii,
the scatter will increase as the on-source measurement will be affected by the
emission from the sky background (\citealt*{1989PASP..101..616Howell}).
At intermediate aperture radii, a minimum will occur as shown in Fig. \ref{aper_rad}.
We selected the appropriate aperture for each night
as the one that provided the minimum dispersion for the DLC found among all pairs of
the comparison stars, as the same stars would be used to produce DLCs
against the target quasars to check for their INOV. Thus, using the aperture which
provides minimum dispersion will set a threshold for INOV detection
on that night (e.g., \citealt{2004JApA...25....1Stalin}).
Typically, the selected aperture radius was
$\sim$4$^{\prime\prime}$ and the seeing was $\sim$2$^{\prime\prime}$.
\\
\\
\begin{figure}
\includegraphics[height=  10.0cm, width = 12.0cm]{fig_scatter.jpg}
\caption{
The rms of the DLCs derived for a pair of (steady) comparison stars used
for the target quasar J2203$+$3145, versus photometric aperture radius,
monitored on 15-Sep-2007. The minimum in standard deviation on that
night is seen to occur for an aperture radius $\simeq$ 3.8 arcsec. }
\label{aper_rad}
\end{figure}
\\
\\
\section{Determination of $\eta$}
\label{eta_comp}
As mentioned in Sect. \ref{intro}, the photometric errors
returned by {\sc APPHOT} are significantly underestimated.
In this work, we make a fresh attempt to determine
$\eta$ using our enlarged dataset of 262 DLCs from our
ARIES AGN monitoring program
(see \citealt{2012A&A...544A..37AG}; Sect.\ \ref{sample}).
Out of the 3 star-star DLCs available for each night
(using the 3 comparison stars monitored), we first
selected the steadiest (one having minimum variance) star$-$star DLC. Thus, for
our entire dataset we have got 262 `steady' DLCs, whose 524 stars
appear to have not varied on the corresponding
nights. For each selected DLC, with $N_p$ points, we then computed
$\chi^2$ corresponding to its degree of freedom, $\nu$ =
$N_p - 1$, which is given as;

\begin{equation}
\label{chi2}
\chi^2 = \sum\limits_{i=1}^{N_p-1} \frac{1}{\sigma_i^2} (\Delta m_i - \langle \Delta m \rangle)^2
\end{equation}
where the expected value $\langle \Delta m \rangle$ is the sample mean of the DLC.
$N_p$ is the number of data points in the lightcurve, $\Delta m_i$ is the
differential magnitude of the $i^{th}$ data point in the lightcurve
and $\sigma_i$
is the rms measurement error associated with each $\Delta m_i$.

To compute $\eta$, we use

\begin{equation}
\label{eta_equ}
\nu = \sum\limits_{i=1}^{N_p-1} \frac{1}{\eta^2 \sigma_i^2} (\Delta m_i - \langle \Delta m \rangle)^2
\end{equation}
where the degree of freedom $\nu$ is also the expected $\langle \chi^2 \rangle$ value
for a pair of non-variable stars. The simplest approach is to use
regression analysis given by

\begin{equation}
\label{regression}
\chi^2 = \eta^2 \nu + \epsilon
\end{equation}

where $\epsilon$ is the residual associated with each pair of $\chi^2$ and $\nu$.
However, we do not know that residuals are Gaussian distributed,
or are homogeneous with respect to the values of independent variable,
precluding a reliable least square fitting. As our regression analysis
exhibit an ``expected value - residual'' we can transform
the variables to stabilize the variance. The most common method is
the Box-Cox set of tranformations (\citealt*{1964AJ....113.1995Box}; \citealt*{2005drea.book.....Box}).
In our case this involves using logrithms of the $\chi^2$ values
to homogenize the variance of regression analysis and to maintain
the linear relationship
between the $\chi^2$ and $\nu$, we tranform $\nu$ to $log(\nu$). Then, we
fix the slope to 1 in the regression analysis to obtain :

\begin{equation}
\label{log_regress}
log(\langle \chi^2 \rangle) = K + log(\nu)
\end{equation}

where $\eta^2 = 10^K$. The error in $\eta^2$ is computed using \citet*{2003drea.book.....Bevington}

\begin{equation}
\label{error_eta}
\sigma_\eta^2 = \eta^2 \times (2.303 \times \sigma_K)^2
\end{equation}
where $\sigma_K$ is the error in $K$.
Using these, we obtain $\eta = 1.54 \pm 0.05$ for the
entire set of 262 steady `star-star' DLCs data listed in Table \ref{result}.

In Fig. \ref{etafig}, we plot for all 262 `steady' star-star DLCs,
the computed $\chi^{2}$ values against the respective values of $\nu$.
Accodingly, we adopt $\eta=$1.54, for scaling up the $\emph IRAF$
photometric rms errors (see Sect.\ 5).
\\
\begin{figure}
\hspace*{0.0cm}
\includegraphics[height=9.0cm,width=11.0cm]{chi_nu.jpg}
\caption{
Plot of $\chi^2$ values against degrees of freedom, computed for our entire data
set of 262 night. The solid line gives the slope fixed at 1
(see sect. \ref{eta_comp}). }
\label{etafig}
\end{figure}
\\
\\
As mentioned in Sect.\ref{intro}, a principal goal of the present
study is to check the dependence of $\eta$ on the brightness
mismatch between the stars which are paired to derive the
`steady' star-star DLCs. For this, we divide our sample of
262 DLCs into  subsamples corresponding to three intervals of
the apparent magnitude difference ($\Delta m_s$) between the star-pair
(see column 7 of Table \ref{result}).
These subsamples have $\Delta m_s$ in the ranges 0.00-0.40 mag (148 DLCs),
0.40-0.80 mag (69 DLCs) and 0.80 to 1.50 mag (39 DLCs).
Out of the 262 DLCs star-star DLCs considered here, only 6 have $\Delta m_s > 1.50$ mag.
The computed values of $\chi^2$ for the three subsamples are
plotted in Fig. \ref{etamag}. We apply the regression
analysis, as explained above, to compute the $\eta$ values
for these subsamples. These values of $\eta$ are found to be
1.56 $\pm$ 0.07, 1.50 $\pm$ 0.09 and 1.56 $\pm$ 0.13
for the subsamples defined by
0.00 $< \Delta m_s < $0.40, 0.40 $< \Delta m_s < $0.80
and 0.80 $< \Delta m_s < $1.50, respectively.
We note that these values of $\eta$ are mutually consistent
for the three magnitude bins.
We thus conclude that the determination of $\eta$ is essentially independent of the brightness
mismatch of at least up to 1.5 mag between the comparison stars used.
\\
\begin{figure}
\hspace*{0.0cm}
\includegraphics[height=5.0cm,width=7.0cm]{m1.jpg}
\includegraphics[height=5.0cm,width=7.0cm]{m2.jpg}
\includegraphics[height=5.0cm,width=7.0cm]{m3.jpg}
\caption{
Plot of $\chi^2$ values against degrees of freedom,
computed for the 3 ranges of apparent magnitude
difference between the (steady) stars paired to derive the DLCs. (a)
$\chi^2$ for the $\Delta m_{s} = 0.00 - 0.40$ (148 DLCs);
(b) $\chi^2$ for the $\Delta m_{s} = 0.40 - 0.80$ (69 DLCs) and
(c) $\chi^2$ for the $\Delta m_{s} = 0.80 - 1.50$ (39 DLCs).
The solid line shows slope of regression analysis fixed at 1
(see Sect.\ \ref{eta_comp}). }
\label{etamag}
\end{figure}
\\
\\
\section{Discussion}

In order to counter-check these findings, we now subject our analysis
to a {\it sanity check} (Table \ref{result}).
For this we have computed the expected number of {\it false
positives} ({\it `Type 1 error'}) for our dataset of 262 DLCs. We have
thus performed the $F-test$ (Eq.\ \ref{ftest}) on the 262 steady star-star
DLCs after accounting for the photometric error underestimation factor (i.e.,
replacing the denominator with $\eta^2 \sigma^2$ in Eq.\ \ref{ftest}).
The expression for $F$ is given by $F_{\nu_1,\nu_2}^{\alpha} = \sigma_1^2/\sigma_2^2 $
where $\sigma_1$ and $\sigma_2$ are the variances of the numerator and
the denominator and the $\nu_1$ and $\nu_2$ are the corresponding
degrees of freedom.
In our analysis, we have simplified the $F$ expression to $F_{\nu}^{\alpha}$ as
$\nu_1$ = $\nu_2 = \nu$ is the degree of freedom for the `star-star' DLC.
In this way, the  $F$-value was computed for each DLC and compared with
the critical $F$-value. Recall that smaller the $\alpha$,
the less likely is it to occur by chance. For the present study, we
have used two values of significance level, $\alpha$ = 0.01 and 0.05.
Thus we claim a spurious INOV detection for a DLC,
when the computed $F-$ value exceeds
the critical $F-$value at $\alpha = $ 0.01. We thus assign a `variable'
designation (V) to it. We assign a `probable variable' (PV) designation when
the computed $F-$ value is found to be between the
critical $F-$ values at $\alpha = $ 0.01 and 0.05, otherwise
`non-variable' (N) designation as assigned to the `star-star' DLC.
\\
Following this analysis, out of 262 steady `star-star' DLCs,
6 DLCs were found to be of `V' type, while 12 were designated
as `PV' (Table \ref{result}).  At $\alpha = 0.01$ (i.e., $p>$  0.99),
we expect among the 262 `star-star' DLCs, $\sim$3 DLCs to
be falsely classified as `V'. Similarly, at $\alpha = 0.05$
(i.e., $p>$ 0.95), the expected number of false positives
is $\sim$13. We find that for our analysis, the {\it observed}
number of false positive is 6 at $\alpha =$ 0.01 and 18 at 0.05.
Since the distribution of false positives (Type 1 errors)
is binomial, we expect its actual number for a given test will be between 0
and 9 and in most cases between 3$\pm$2 at $\alpha = 0.01$. Similarly, at $\alpha = 0.05$,
the actual number of false positives will be between 2 and 24 and
in most cases will be 13$\pm$ 4. The good match between the {\it observed}
and {\it expected} values of {\it false positives} validates our
analysis procedure adopting $\eta$ = 1.54 as determined here.
\\

Also, for our three subsamples defined in Sect. 4, we find the
expected numbers of false postives for most cases will be
2$\pm$1 (148 DLCs in the magnitude bin $ 0.0 < \Delta m_s < 0.4 $),
1$\pm$1 (69 DLCs in the magnitude bin $ 0.4 < \Delta m_s < 0.8 $) and
1$\pm$1 (39 DLCs in the magnitude bin $ 0.8 < \Delta m_s < 1.5 $) at $\alpha = 0.01$.
We find that the {\it observed} numbers for false positives are 4, 1 and 1.
Similarly, at $\alpha = 0.05$, expected numbers of false postives for most cases will be
7$\pm$3 (148 DLCs in the magnitude bin $ 0.0 < \Delta m_s < 0.4 $),
4$\pm$2 (69 DLCs in the magnitude bin $ 0.4 < \Delta m_s < 0.8 $) and
2$\pm$2 (39 DLCs in the magnitude bin $ 0.8 < \Delta m_s < 1.5 $) at.
We find that the {\it observed} numbers for false positives are 10, 3 and 5, respectively.
This again shows a close match between the observed
and expected values of {\it false positives}, validating the
estimate of $\eta = 1.54$ up to a magnitude mismatch of $\sim$1.5
mag between the comparison star pairs.

The vast majority of the data analyzed here comes from ST and therefore
our results strictly apply to those observations. The data from the HCT, IGO, GSO
and VBT all seem consistent with the ST results, but each of these
telescopes contributed measurements that are not numerous enough
to perform useful separate analyses for these telescopes.
Therefore we cannot yet determine whether
the value of $\eta$ we have found is a fundamental feature of $\textrm IRAF$'s
$\textrm APPHOT$ and thus universal, or somewhat dependent on
the telescope and the instrument used. Over the next couple of years we
anticipate obtaining comparably large data sets with a new ARIES 1.3 m
telescope located at a different site near Nainital. We will perform a similar
analysis of the values of $\eta$ for those additional data and that will
lead us to a better grasp of the root of this error underestimation.
We do, however, note that because the seeing varied substantially
(from 0.7 to 3.5 arc sec) for the data we have employed here, the value
of $\eta$ does seem to be fairly independent of this important aspect of
the differential photometry process.

\section{Summary}
In this study, we have determined the photometric error underestimation factor
$\eta$ applicable to point-source aperture photometry carried out
using the {\emph IRAF} (APPHOT) software. For this we have used an
unprecedentedly large set of 262 DLCs taken on 262 nights, about 85 per cent
of which are taken with the 1-m telescope (ST) of ARIES. By subjecting
this large database to
a $\chi^2$ analysis we
find that $\eta$ = 1.54$\pm$0.05, which is consistent with the
most recently published estimate of this important parameter,
which was derived using a $\sim$4 times smaller sample of DLCs than we
have used here
(see, \citealt{2012A&A...544A..37AG}). A sanity check, based on
the computation of `false positives' employing the $F$-test,
was performed and it has validated the estimate of $\eta$ = 1.54.
\\
We have further checked for any dependence of the $\eta$ factor on the
apparent magnitude mismatch ($\Delta m_{s}$) between the comparison stars
paired (taking them to be steady, as inferred from inspection of their DLCs).
For this we divided our sample of DLCs into three subsamples, characterized
by $0.0 < \Delta m_s < 0.40$ (148 DLCs),  $0.40 < \Delta m_s < 0.80$ (69)
and $0.80 < \Delta m_s < 1.50$ (39 DLCs).
For each subsample the sanity check again showed consistency with $\eta$ = 1.54.
It is thus concluded that $\eta$ = 1.54
remains valid even when the magnitudes of the `steady' stars paired to
derive a DLC differ by as much as 1.5 mag. In other words, even a magnitude
difference of up to 1.5-mag between the two stars paired to derive a DLC and $\eta$,
should not result in a spurious claim of INOV for either of the two stars.
As a corollary, it can be reasonably asserted that deriving DLCs of (point-like) AGN
using a comparison star that is within about 1.5 magnitude of the AGN, should
not lead to spurious claim of INOV for the AGN. However, this could well
be the case for significantly larger magnitude mismatches, as argued
by \citet{2007MNRAS.374..357Cellone} in the context of some claims of
dramatic INOV.

The present analysis is dominated by the $R-$band data taken using the
ARIES 1-m telescope (ST). Therefore, the present conclusion strictly
apply only to the $R-$band taken with this telescope.
In the coming years, we plan to expand the present analysis to observation
taken with the 1.3-m Devasthal Optical Telescope (DOT) recently installed
at a site well removed from that of the ST.
\\
\begin{deluxetable}{ccccccccccccc}
\tablecolumns{13}
\tabletypesize{\tiny}
\tablecaption{Summary of observations and derived variability status for the `steady' star-star DLCs \label{result}}
\tablewidth{0pt}
\tablehead{
AGN  & Obs. date    & Tel.{$^\P$}  &  Filter.  & Dur. & $N_p$ & $\Delta m_{s}$   & $\sigma $  &  std dev. & $\chi^2_{s}$   &  $F_{s}$ &  Status$^\dag$ & Ref$^\pounds$.  \\
name    &  dd.mm.yy& used      & used     &   (hr)  &      &  (mag) & ($10^{-2}$ mag)  & ($10^{-2}$ mag)     &    &           &         &                       \\
        (1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9)  & (10) & (11) & (12) & (13) \\ }
\startdata
\multicolumn{13}{l}{\small Radio quiet quasars (RQQs)[22 sources; 68 DLCs]}\\ \hline
&&&&&&&&&&&&\\
J0045$+$0410 & 21.10.98 & ST  & R & 2.39 & 14 & 0.376 & 0.5 & 0.2  &  4.37  & 0.13 &N  &  (a) \\
J0045$+$0410 & 05.11.98 & ST  & R & 3.21 & 30 & 0.369 & 0.8 & 1.0  & 40.05  & 0.55 &N  &   (a)\\
J0045$+$0410 & 16.10.04 & HCT & R & 6.04 & 25 & 1.859 & 0.1 & 0.2  & 79.36  & 1.24 &N  &   (b)\\
&&&&&&&&&&&&\\
J0103$+$0321 & 05.11.05 & HCT & R & 5.94 & 21 & 1.093 & 0.3 & 0.4  & 36.32  & 0.72 &N  &   (b)\\
J0103$+$0321 & 05.11.05 & ST  & R & 5.83 & 20 & 0.570 & 0.4 & 0.6  & 44.09  & 1.02 &N  &   (b)\\
&&&&&&&&&&&&\\
J0239$-$0001 & 06.11.05 & HCT & R & 6.42 & 19 & 0.779 & 0.1 & 0.2  & 53.90  & 1.26 &N  &   (b)\\
&&&&&&&&&&&&\\
J0516$-$0027 & 10.12.01 & ST  & R & 5.77 & 23 & 0.160 & 0.3 & 0.3  & 32.50  & 0.56 &N  &   (c)\\
J0516$-$0027 & 19.12.01 & ST  & R & 7.52 & 35 & 0.210 & 0.3 & 0.5  & 131.13 & 1.16 &N  &   (c)\\
J0516$-$0027 & 20.11.03 & HCT & R & 7.28 & 39 & 0.264 & 0.1 & 0.2  & 96.37  & 1.07 &N  &   (b)\\
J0516$-$0027 & 18.11.04 & ST  & R & 6.29 & 34 & 0.282 & 0.1 & 0.2  & 79.19  & 1.01 &N  &   (b)\\
J0516$-$0027 & 16.12.04 & HCT & R & 6.79 & 34 & 1.256 & 0.2 & 0.2  & 63.96  & 0.60 &N  &   (b)\\
&&&&&&&&&&&&\\
J0751$+$2919 & 14.12.98 & ST  & R & 7.41 & 40 & 1.569 & 0.3 & 0.6 & 145.70  & 1.57 &N  &   (c)\\
J0751$+$2919 & 13.01.99 & ST  & R & 8.32 & 56 & 0.362 & 0.3 & 0.5  & 134.70 & 0.93 &N  &   (c)\\
J0751$+$2919 & 24.11.99 & ST  & R & 5.39 & 28 & 0.702 & 0.3 & 0.3  & 42.90  & 0.62 &N  &   (c)\\
J0751$+$2919 & 09.12.99 & ST  & R & 6.21 & 31 & 0.710 & 0.2 & 0.5  & 144.38 & 2.13 &PV &   (c)\\
J0751$+$2919 & 01.12.00 & ST  & R & 5.95 & 32 & 0.372 & 0.3 & 0.4  & 63.30  & 0.78 &N  &   (c)\\
J0751$+$2919 & 25.12.01 & ST  & R & 5.44 & 30 & 0.372 & 0.4 & 0.4  & 36.78  & 0.54 &N  &   (c)\\
J0751$+$2919 & 17.12.04 & HCT & V & 3.69 & 15 & 0.318 & 0.1 & 0.2  & 24.61  & 0.74 &N  &   (b)\\
J0751$+$2919 & 17.12.04 & ST  & R & 7.02 & 34 & 0.238 & 0.1 & 0.3  & 130.66 & 1.56 &N  &   (b)\\
J0751$+$2919 & 12.01.05 & ST  & R & 7.15 & 16 & 0.129 & 0.1 & 0.2  & 22.10  & 0.61 &N  &   (b)\\
J0751$+$2919 & 07.03.06 & HCT & R & 8.06 & 29 & 0.046 & 0.1 & 0.2  & 55.95  & 0.84 &N  &   (b)\\
J0751$+$2919 & 07.03.06 & ST  & R & 8.33 & 46 & 0.079 & 0.1 & 0.2  & 141.20 & 1.32 &N  &   (b)\\
&&&&&&&&&&&&\\
J0827$+$0942 & 27.12.98 & ST  & R & 8.15 & 60 & 0.415 & 0.3 & 0.4  & 119.04 & 0.88 &N  &   (a)\\
J0827$+$0942 & 13.01.05 & HCT & V & 6.47 & 16 & 0.061 & 0.1 & 0.2  & 24.02  & 0.67 &N  &   (b)\\
J0827$+$0942 & 13.01.05 & ST  & R & 6.94 & 17 & 0.000 & 0.1 & 0.2  & 44.74  & 1.18 &N  &   (b)\\
&&&&&&&&&&&&\\
J0835$+$2506 & 25.12.98 & ST  & R & 4.68 & 26 & 0.911 & 0.4 & 0.6  & 67.49  & 1.13 &N  &   (a)\\
J0835$+$2506 & 14.01.99 & ST  & R & 8.91 & 78 & 0.206 & 0.4 & 0.6  & 169.41 & 0.92 &N  &   (a)\\
J0835$+$2506 & 10.12.99 & ST  & R & 6.72 & 33 & 0.714 & 0.4 & 0.6  & 59.65  & 0.75 &N  &   (a)\\
&&&&&&&&&&&&\\
J0853$+$4349 & 17.02.99 & ST  & R & 7.70 & 39 & 0.234 & 0.4 & 0.7  & 91.50  & 0.99 &N  &   (a)\\
&&&&&&&&&&&&\\
J0935$+$4331 & 20.02.99 & ST  & R & 4.47 & 26 & 0.883 & 0.2 & 0.3  & 106.91 & 1.69 &N  &   (a)\\
&&&&&&&&&&&&\\
J0938$+$4128 & 27.03.99 & ST  & R & 2.73 & 17 & 0.000 & 0.5 & 0.6  & 34.40  & 0.73 &N  &   (a)\\
&&&&&&&&&&&&\\
J0948$+$4335 & 15.01.99 & ST  & R & 7.97 & 44 & 0.209 & 0.3 & 0.5  & 79.10  & 0.80 &N  &   (c)\\
J0948$+$4335 & 26.02.00 & ST  & R & 7.97 & 39 & 0.490 & 0.4 & 0.6  & 82.44  & 0.91 &N  &   (c)\\
J0948$+$4335 & 23.01.01 & ST  & R & 6.73 & 25 & 0.505 & 0.3 & 0.6  & 77.02  & 1.20 &N  &   (c)\\
&&&&&&&&&&&&\\
J1019$+$2744 & 14.03.99 & ST  & R & 7.32 & 43 & 0.304 & 0.5 & 0.7  & 92.57  & 0.86 &N  &   (c)\\
J1019$+$2744 & 14.01.00 & ST  & R & 7.08 & 34 & 0.441 & 0.2 & 0.2  & 42.28  & 0.52 &N  &   (c)\\
J1019$+$2744 & 27.02.00 & ST  & R & 8.81 & 37 & 0.442 & 0.2 & 0.3  & 63.77  & 0.61 &N  &   (c)\\
&&&&&&&&&&&&\\
J1032$+$3240 & 13.03.99 & VBT & V & 8.40 & 45 & 0.503 & 0.5 & 0.8  & 158.00 & 1.16 &N  &   (c)\\
J1032$+$3240 & 02.03.00 & ST  & R & 4.95 & 19 & 0.887 & 0.2 & 0.4  & 64.64  & 1.45 &N  &   (c)\\
J1032$+$3240 & 05.04.00 & ST  & R & 6.17 & 24 & 0.136 & 0.1 & 0.3  & 108.19 & 1.85 &PV &   (c)\\
J1032$+$3240 & 23.03.01 & ST  & R & 6.84 & 25 & 0.303 & 0.5 & 0.6  & 51.32  & 0.83 &N  &   (c)\\
J1032$+$3240 & 06.03.02 & ST  & R & 8.53 & 34 & 0.134 & 0.2 & 0.3  & 185.91 & 1.28 &N  &   (c)\\
J1032$+$3240 & 08.03.02 & ST  & R & 8.31 & 24 & 0.127 & 0.2 & 0.3  & 75.22  & 1.17 &N  &   (c)\\
&&&&&&&&&&&&\\
J1104$+$3141 & 12.03.99 & ST  & R & 8.80 & 43 & 0.551 & 0.6 & 0.7  & 51.55  & 0.48 &N  &   (c)\\
J1104$+$3141 & 14.04.00 & ST  & R & 5.61 & 22 & 0.035 & 0.3 & 0.5  & 62.25  & 1.01 &N  &   (c)\\
J1104$+$3141 & 21.04.01 & ST  & R & 6.40 & 27 & 0.032 & 0.5 & 0.5  & 28.59  & 0.41 &N  &   (c)\\
J1104$+$3141 & 22.04.01 & ST  & R & 5.58 & 24 & 0.037 & 0.5 & 0.5  & 27.08  & 0.43 &N  &   (c)\\
&&&&&&&&&&&&\\
J1119$+$2119 & 14.04.05 & ST  & R & 5.02 & 30 & 0.065 & 0.1 & 0.2  & 48.37  & 0.70 &N  &   (b)\\
J1119$+$2119 & 30.03.06 & ST  & R & 6.17 & 41 & 0.072 & 0.1 & 0.3  & 149.11 & 1.57 &N  &   (b)\\
J1119$+$2119 & 31.03.06 & ST  & R & 4.25 & 26 & 0.070 & 0.1 & 0.2  & 49.47  & 0.83 &N  &   (b)\\
&&&&&&&&&&&&\\
J1246$+$0224 & 13.04.05 & ST  & R & 5.51 & 10 & 0.046 & 0.1 & 0.3  & 48.90  & 2.01 &N  &   (b)\\
&&&&&&&&&&&&\\
J1255$+$0144 & 22.03.99 & ST  & R & 7.46 & 43 & 0.483 & 0.4 & 0.5  & 64.91  & 0.59 &N  &   (c)\\
J1255$+$0144 & 09.03.00 & ST  & R & 6.14 & 29 & 0.144 & 0.1 & 0.2  & 80.28  & 1.05 &N  &   (c)\\
J1255$+$0144 & 03.04.00 & ST  & R & 4.32 & 21 & 0.154 & 0.1 & 0.4  & 109.28 & 2.53 &V  &   (c)\\
J1255$+$0144 & 26.04.01 & ST  & R & 4.60 & 20 & 0.107 & 0.2 & 0.5  & 136.56 & 1.88 &N  &   (c)\\
J1255$+$0144 & 18.03.02 & ST  & R & 7.88 & 25 & 0.130 & 0.4 & 0.3  & 73.50  & 0.36 &N  &   (c)\\
&&&&&&&&&&&&\\
J1424$+$4214 & 03.04.99 & ST  & R & 7.22 & 41 & 0.056 & 0.3 & 0.6  & 158.64 & 1.48 &N  &   (a)\\
J1424$+$4214 & 07.03.00 & ST  & R & 3.88 & 15 & 0.380 & 0.2 & 0.3  & 55.01  & 1.34 &N  &   (a)\\
J1424$+$4214 & 08.03.00 & GSO & V & 3.05 & 30 & 0.385 & 0.6 & 0.8  & 54.71  & 0.76 &N  &   (a)\\
&&&&&&&&&&&&\\
J1524$+$0958 & 11.04.99 & ST  & R & 6.55 & 38 & 0.491 & 0.2 & 0.3  & 78.81  & 0.96 &N  &   (a)\\
&&&&&&&&&&&&\\
J1528$+$2825 & 10.05.05 & ST  & R & 7.75 & 16 & 0.065 & 0.2 & 0.2  & 27.00  & 0.33 &N  &   (b)\\
&&&&&&&&&&&&\\
J1631$+$2953 & 15.06.04 & HCT & V & 6.21 & 28 & 1.110 & 0.2 & 0.4  & 64.31  & 1.00 &N  &   (b)\\
J1631$+$2953 & 11.05.05 & ST  & R & 6.92 & 29 & 0.006 & 0.3 & 0.4  & 53.36  & 0.62 &N  &   (b)\\
J1631$+$2953 & 01.06.05 & ST  & R & 7.36 & 15 & 1.369 & 0.2 & 0.4  & 30.35  & 0.93 &N  &   (b)\\
&&&&&&&&&&&&\\
J1632$+$3737 & 12.05.05 & ST  & R & 6.60 & 29 & 0.289 & 0.2 & 0.2  & 53.95  & 0.72 &N  &   (b)\\
&&&&&&&&&&&&\\
J1751$+$5045 & 03.06.98 & ST  & R & 4.72 & 46 & 0.373 & 0.2 & 0.3  & 109.29 & 1.00 &N  &   (a)\\
J1751$+$5045 & 06.06.98 & ST  & R & 1.65 & 17 & 0.384 & 0.3 & 0.4  & 32.15  & 0.93 &N  &   (a)\\
J1751$+$5045 & 08.06.98 & ST  & R & 6.15 & 36 & 0.021 & 0.2 & 0.3  & 157.64 & 1.78 &PV &   (a)\\
&&&&&&&&&&&&\\\hline
\multicolumn{13}{l}{\small Radio intermediate quasars (RIQs)[10 sources; 31 DLCs]}\\ \hline
J0005$+$1609 & 03.11.00 & ST  & R & 6.55 & 30 & 0.302 & 0.3 & 0.3  & 44.85  & 0.61 &N  &   (a)\\
J0005$+$1609 & 05.11.00 & ST  & R & 7.74 & 39 & 0.028 & 0.4 & 0.3  & 28.94  & 0.30 &N  &   (a)\\
&&&&&&&&&&&&\\
J0748$+$2200 & 19.01.07 & ST  & R & 5.20 & 19 & 0.030 & 0.3 & 0.3  & 28.12  & 0.62 &N  &   (d)\\
J0748$+$2200 & 23.01.07 & ST  & R & 7.21 & 25 & 0.149 & 0.3 & 0.4  & 38.97  & 0.64 &N  &   (d)\\
J0748$+$2200 & 19.02.07 & ST  & R & 6.42 & 24 & 0.614 & 0.3 & 0.4  & 77.17  & 1.24 &N  &   (d)\\
J0748$+$2200 & 29.01.08 & IGO & R & 5.41 & 19 & 0.627 & 0.1 & 0.1  & 17.96  & 0.42 &N  &   (d)\\
J0748$+$2200 & 30.01.08 & IGO & R & 6.03 & 20 & 0.805 & 0.1 & 0.2  & 33.25  & 0.67 &N  &   (d)\\
&&&&&&&&&&&&\\
J0832$+$3707 & 23.01.07 & HCT & R & 4.91 & 29 & 0.265 & 0.2 & 0.2  & 60.16  & 0.88 &N  &   (d)\\
J0832$+$3707 & 21.02.07 & ST  & R & 4.70 & 21 & 0.193 & 0.1 & 0.2  & 43.88  & 0.92 &N  &   (d)\\
J0832$+$3707 & 10.03.07 & IGO & R & 5.04 & 10 & 0.203 & 0.2 & 0.2  & 11.06  & 0.59 &N  &   (d)\\
J0832$+$3707 & 11.03.07 & IGO & R & 5.09 & 10 & 0.204 & 0.2 & 0.3  & 23.95  & 1.16 &N  &   (d)\\
&&&&&&&&&&&&\\
J0836$+$4426 & 22.01.07 & ST  & R & 5.61 & 24 & 1.288 & 0.2 & 0.2  & 19.63  & 0.35 &N  &   (d)\\
J0836$+$4426 & 10.02.07 & IGO & R & 5.58 & 15 & 0.815 & 0.2 & 0.3  & 36.26  & 1.00 &N  &   (d)\\
J0836$+$4426 & 09.03.07 & IGO & R & 5.16 & 16 & 0.864 & 0.2 & 0.3  & 39.16  & 1.49 &N  &   (d)\\
&&&&&&&&&&&&\\
J0907$+$5515 & 04.02.08 & IGO & R & 8.99 & 24 & 0.247 & 0.2 & 0.3  & 47.80  & 0.75 &N  &   (d)\\
J0907$+$5515 & 05.02.08 & IGO & R & 7.48 & 13 & 0.365 & 0.1 & 0.3  & 40.08  & 1.33 &N  &   (d)\\
&&&&&&&&&&&&\\
J1259$+$3423 & 19.04.07 & ST  & R & 5.40 & 21 & 0.673 & 0.2 & 0.4  & 95.09  & 1.63 &N  &   (d)\\
J1259$+$3423 & 20.04.07 & ST  & R & 6.40 & 27 & 0.673 & 0.2 & 0.3  & 66.00  & 0.80 &N  &   (d)\\
J1259$+$3423 & 24.04.07 & ST  & R & 5.30 & 22 & 0.688 & 0.2 & 0.3  & 41.81  & 0.79 &N  &   (d)\\
&&&&&&&&&&&&\\
J1312$+$3515 & 25.03.99 & ST  & R & 6.67 & 39 & 0.097 & 0.2 & 0.5  & 398.57 & 2.79 &V  &   (e)\\
J1312$+$3515 & 01.04.01 & ST  & R & 4.87 & 32 & 0.443 & 0.2 & 0.4  & 149.98 & 2.52 &V  &   (e)\\
J1312$+$3515 & 02.04.01 & ST  & R & 5.19 & 41 & 0.696 & 0.3 & 0.4  & 86.44  & 0.81 &N  &   (e)\\
&&&&&&&&&&&&\\
J1336$+$1725 & 11.04.05 & ST  & R & 7.93 & 29 & 0.305 & 0.1 & 0.2  & 53.60  & 0.80 &N  &   (d)\\
J1336$+$1725 & 08.05.05 & ST  & R & 4.47 & 17 & 0.739 & 0.2 & 0.3  & 60.18  & 1.53 &N  &   (d)\\
J1336$+$1725 & 13.04.08 & ST  & R & 8.06 & 20 & 0.731 & 0.2 & 0.3  & 56.65  & 1.33 &N  &   (d)\\
&&&&&&&&&&&&\\
J1539$+$4735 & 27.05.09 & ST  & R & 6.26 & 30 & 0.776 & 0.3 & 0.4  & 52.69  & 0.69 &N  &   (d)\\
J1539$+$4735 & 02.06.09 & ST  & R & 7.03 & 30 & 0.779 & 0.4 & 0.5  & 56.11  & 0.68 &N  &   (d)\\
J1539$+$4735 & 14.06.09 & ST  & R & 5.30 & 24 & 0.776 & 0.4 & 0.5  & 36.33  & 0.54 &N  &   (d)\\
&&&&&&&&&&&&\\
J1719$+$4804 & 29.04.06 & ST  & R & 4.88 & 25 & 0.131 & 0.1 & 0.2  & 54.32  & 0.95 &N  &   (d)\\
J1719$+$4804 & 30.04.06 & ST  & R & 5.64 & 22 & 0.195 & 0.1 & 0.2  & 61.02  & 1.22 &N  &   (d)\\
J1719$+$4804 & 30.05.06 & ST  & R & 6.06 & 26 & 0.031 & 0.2 & 0.3  & 62.64  & 0.85 &N  &   (d)\\
&&&&&&&&&&&&\\\hline
\multicolumn{13}{l}{\small Lobe dominated quasars (LDQs)[9 sources; 25 DLCs]}\\ \hline
J0015$+$3052 & 18.01.01 & ST  & R & 3.78 & 18 & 0.241 & 0.5 & 0.5  & 21.29  & 0.40 &N  &  (c) \\
J0015$+$3052 & 20.01.01 & ST  & R & 2.70 & 12 & 0.457 & 0.6 & 0.3  & 4.66   & 0.16 &N  &  (c) \\
J0015$+$3052 & 24.01.01 & ST  & R & 2.87 & 14 & 0.242 & 0.6 & 0.5  & 9.82   & 0.25 &N  &  (c) \\
J0015$+$3052 & 14.10.01 & ST  & R & 6.78 & 26 & 0.235 & 0.6 & 0.7  & 37.85  & 0.51 &N  &  (c) \\
J0015$+$3052 & 21.10.01 & ST  & R & 6.25 & 24 & 0.703 & 0.5 & 0.5  & 17.98  & 0.36 &N  &  (c) \\
&&&&&&&&&&&&\\
J0028$+$3103 & 13.10.98 & ST  & R & 3.60 & 28 & 0.241 & 0.1 & 0.2  & 57.87  & 0.90 &N  &  (a) \\
J0028$+$3103 & 01.11.98 & ST  & R & 3.35 & 26 & 0.260 & 0.2 & 0.3  & 76.98  & 1.14 &N  &  (a) \\
&&&&&&&&&&&&\\
J0137$+$3309 & 07.11.01 & ST  & R & 6.54 & 36 & 0.089 & 0.6 & 0.5  & 88.24  & 0.28 &N  &  (c) \\
J0137$+$3309 & 08.11.01 & ST  & R & 6.66 & 32 & 0.132 & 0.3 & 0.4  & 58.61  & 0.70 &N  &  (c) \\
J0137$+$3309 & 13.11.01 & ST  & R & 8.63 & 46 & 0.213 & 0.3 & 0.4  & 119.10 & 1.07 &N  &  (c) \\
&&&&&&&&&&&&\\
J0352$-$0711 & 14.11.01 & ST  & R & 6.56 & 31 & 0.617 & 0.2 & 0.3  & 70.99  & 0.80 &N  &  (c) \\
J0352$-$0711 & 15.11.01 & ST  & R & 5.54 & 26 & 0.630 & 0.2 & 0.3  & 39.30  & 0.66 &N  &  (c) \\
J0352$-$0711 & 18.11.01 & ST  & R & 5.70 & 25 & 0.628 & 0.2 & 0.4  & 106.55 & 1.42 &N  &  (c) \\
&&&&&&&&&&&&\\
J0713$+$3656 & 20.01.01 & ST  & R & 6.51 & 29 & 0.191 & 0.3 & 0.3  & 45.90  & 0.72 &N  &  (c) \\
J0713$+$3656 & 21.01.01 & ST  & R & 6.40 & 30 & 0.190 & 0.3 & 0.3  & 42.60  & 0.61 &N  &  (c) \\
J0713$+$3656 & 25.01.01 & ST  & R & 7.08 & 31 & 0.453 & 0.3 & 0.3  & 46.97  & 0.66 &N  &  (c) \\
J0713$+$3656 & 20.12.01 & ST  & R & 8.07 & 52 & 0.202 & 0.3 & 0.6  & 190.47 & 1.56 &N  &  (c) \\
J0713$+$3656 & 21.12.01 & ST  & R & 7.49 & 48 & 0.449 & 0.2 & 0.4  & 142.06 & 1.20 &N  &  (c) \\
&&&&&&&&&&&&\\
J1007$+$1248 & 16.02.99 & ST  & R & 6.51 & 36 & 1.000 & 0.1 & 0.3  & 213.36 & 2.42 &V  &  (c) \\
J1007$+$1248 & 27.02.99 & ST  & R & 4.27 & 30 & 0.996 & 0.4 & 0.4  & 39.70  & 0.51 &N  &  (c) \\
J1007$+$1248 & 29.03.00 & ST  & R & 3.81 & 21 & 1.012 & 0.1 & 0.2  & 58.34  & 1.23 &N  &  (c) \\
J1007$+$1248 & 30.03.00 & ST  & R & 4.64 & 26 & 1.007 & 0.2 & 0.3  & 71.58  & 0.83 &N  &  (c) \\
J1007$+$1248 & 18.02.01 & ST  & R & 5.54 & 42 & 1.015 & 0.2 & 0.4  & 112.96 & 1.16 &N  &  (c) \\
J1007$+$1248 & 24.03.01 & ST  & R & 6.38 & 50 & 1.011 & 0.2 & 0.4  & 297.51 & 1.91 &PV &  (c) \\
&&&&&&&&&&&&\\
J1106$-$0052 & 17.03.99 & ST  & R & 3.81 & 23 & 0.347 & 0.3 & 0.5  & 65.59  & 1.23 &N  &  (c) \\
J1106$-$0052 & 18.03.99 & ST  & R & 7.51 & 42 & 0.348 & 0.3 & 0.5  & 107.03 & 0.99 &N  &  (c) \\
J1106$-$0052 & 16.04.00 & ST  & R & 3.85 & 15 & 0.348 & 0.3 & 0.4  & 36.16  & 0.78 &N  &  (c) \\
J1106$-$0052 & 25.03.01 & ST  & R & 7.18 & 28 & 0.343 & 0.3 & 0.4  & 49.79  & 0.70 &N  &  (c) \\
J1106$-$0052 & 14.04.01 & ST  & R & 4.55 & 19 & 0.346 & 0.3 & 0.5  & 86.90  & 1.50 &N  &  (c) \\
J1106$-$0052 & 22.03.02 & ST  & R & 6.13 & 18 & 0.342 & 0.2 & 0.3  & 32.21  & 0.78 &N  &  (c) \\
&&&&&&&&&&&&\\
J1633$+$3924 & 04.06.99 & ST  & R & 5.71 & 30 & 0.293 & 0.6 & 0.6  & 28.75  & 0.45 &N  &  (a) \\
J1633$+$3924 & 30.05.00 & ST  & R & 3.54 & 14 & 0.542 & 0.5 & 0.6  & 15.95  & 0.52 &N  &  (a) \\
&&&&&&&&&&&&\\
J2351$-$0109 & 13.10.01 & ST  & R & 7.56 & 41 & 0.163 & 0.2 & 0.4  & 213.75 & 1.43 &N  &  (c) \\
J2351$-$0109 & 17.10.01 & ST  & R & 7.80 & 43 & 0.032 & 0.2 & 0.3  & 153.36 & 1.17 &N  &  (c) \\
J2351$-$0109 & 18.10.01 & ST  & R & 8.40 & 46 & 0.032 & 0.2 & 0.2  & 96.62  & 0.72 &N  &  (c) \\
&&&&&&&&&&&&\\\hline
\multicolumn{13}{l}{\small Low optical polarization core dominated quasars (LPCDQs)[12 sources; 43 DLCs]}\\ \hline
J0005$+$0524 & 23.10.06 & ST  & R & 7.05 & 16 & 0.132 & 0.3 & 0.2  & 11.64  & 0.31 &N  &  (f) \\
J0005$+$0524 & 18.11.06 & ST  & R & 4.69 & 11 & 0.394 & 0.2 & 0.1  & 6.30   & 0.24 &N  &  (f) \\
J0005$+$0524 & 14.09.07 & ST  & R & 5.31 & 12 & 0.370 & 0.2 & 0.4  & 30.33  & 1.14 &N  &  (f) \\
J0005$+$0524 & 16.09.07 & ST  & R & 6.11 & 13 & 0.240 & 0.2 & 0.4  & 81.99  & 2.15 &N  &  (f) \\
&&&&&&&&&&&&\\
J0235$-$0402 & 21.10.04 & ST  & R & 7.25 & 15 & 0.127 & 0.1 & 0.2  & 43.88  & 1.15 &N  &  (f) \\
J0235$-$0402 & 22.10.04 & ST  & R & 7.87 & 17 & 0.244 & 0.2 & 0.2  & 43.75  & 0.82 &N  &  (f) \\
J0235$-$0402 & 04.11.04 & ST  & R & 6.19 & 25 & 0.249 & 0.2 & 0.2  & 36.34  & 0.51 &N  &  (f) \\
J0235$-$0402 & 05.11.04 & ST  & R & 7.27 & 29 & 0.122 & 0.1 & 0.2  & 68.37  & 1.01 &N  &  (f) \\
&&&&&&&&&&&&\\
J0456$+$0400 & 23.11.08 & ST  & R & 5.50 & 24 & 0.405 & 0.2 & 0.3  & 43.41  & 0.79 &N  &  (f) \\
J0456$+$0400 & 29.11.08 & ST  & R & 5.51 & 20 & 0.404 & 0.2 & 0.3  & 36.82  & 0.82 &N  &  (f) \\
J0456$+$0400 & 03.12.08 & ST  & R & 5.38 & 22 & 0.529 & 0.3 & 0.3  & 28.65  & 0.59 &N  &  (f) \\
&&&&&&&&&&&&\\
J0741$+$3112 & 20.01.06 & ST  & R & 7.42 & 31 & 0.614 & 0.2 & 0.3  & 78.51  & 0.94 &N  &  (f) \\
J0741$+$3112 & 21.01.06 & ST  & R & 4.01 & 18 & 0.766 & 0.2 & 0.3  & 26.33  & 0.63 &N  &  (f) \\
J0741$+$3112 & 18.12.06 & ST  & R & 7.24 & 29 & 0.135 & 0.1 & 0.2  & 95.05  & 1.42 &N  &  (f) \\
J0741$+$3112 & 22.12.06 & ST  & R & 7.72 & 32 & 0.140 & 0.1 & 0.2  & 58.35  & 0.79 &N  &  (f) \\
&&&&&&&&&&&&\\
J0842$+$1835 & 04.02.06 & ST  & R & 7.64 & 28 & 0.274 & 0.1 & 0.2  & 59.41  & 0.92 &N  &  (f) \\
J0842$+$1835 & 16.12.06 & ST  & R & 5.96 & 14 & 0.277 & 0.1 & 0.4  & 83.30  & 2.57 &N  &  (f) \\
J0842$+$1835 & 21.12.06 & ST  & R & 6.94 & 30 & 0.279 & 0.1 & 0.2  & 92.31  & 1.23 &N  &  (f) \\
&&&&&&&&&&&&\\
J0958$+$3224 & 19.02.99 & ST  & R & 6.50 & 36 & 1.729 & 0.4 & 0.4  & 35.19  & 0.39 &N  &  (e) \\
J0958$+$3224 & 03.03.00 & ST  & R & 6.29 & 37 & 1.311 & 0.3 & 0.4  & 90.04  & 0.82 &N  &  (e) \\
J0958$+$3224 & 05.03.00 & ST  & R & 6.90 & 34 & 0.430 & 0.1 & 0.3  & 115.79 & 1.48 &N  &  (e) \\
&&&&&&&&&&&&\\
J1131$+$3114 & 18.01.01 & ST  & R & 5.73 & 31 & 0.230 & 0.3 & 0.4  & 59.11  & 0.83 &N  &  (e) \\
J1131$+$3114 & 09.03.02 & ST  & R & 8.22 & 27 & 0.435 & 0.3 & 0.3  & 41.50  & 0.52 &N  &  (e) \\
J1131$+$3114 & 10.03.02 & ST  & R & 8.33 & 28 & 0.200 & 0.2 & 0.3  & 46.60  & 0.66 &N  &  (e) \\
&&&&&&&&&&&&\\
J1228$+$3128 & 07.03.99 & ST  & R & 6.63 & 49 & 1.299 & 0.3 & 0.6  & 165.97 & 1.42 &N  &  (e) \\
J1228$+$3128 & 07.04.00 & ST  & R & 7.32 & 26 & 1.320 & 0.2 & 0.6  & 150.61 & 2.35P&V  &  (e) \\
J1228$+$3128 & 20.04.01 & ST  & R & 7.43 & 34 & 1.357 & 0.6 & 0.7  & 46.63  & 0.59 &N  &  (e) \\
&&&&&&&&&&&&\\
J1229$+$0203 & 07.03.11 & ST  & R & 5.46 & 35 & 0.084 & 0.1 & 0.2  & 61.36  & 0.72 &N  &  (f) \\
J1229$+$0203 & 10.03.11 & ST  & R & 6.72 & 49 & 0.047 & 0.1 & 0.2  & 114.60 & 1.00 &N  &  (f) \\
&&&&&&&&&&&&\\
J1357$+$1919 & 27.02.06 & ST  & R & 5.19 & 12 & 0.004 & 0.1 & 0.3  & 45.60  & 1.74 &N  &  (f) \\
J1357$+$1919 & 05.03.06 & ST  & R & 4.94 & 11 & 0.766 & 0.1 & 0.2  & 25.52  & 1.07 &N  &  (f) \\
J1357$+$1919 & 26.03.06 & ST  & R & 6.98 & 12 & 0.025 & 0.1 & 0.5  & 124.20 & 4.76 &V  &  (f) \\
J1357$+$1919 & 28.03.06 & ST  & R & 5.83 & 21 & 0.026 & 0.2 & 0.4  & 110.35 & 2.26P&V  &  (f) \\
J1357$+$1919 & 29.03.06 & ST  & R & 6.26 & 23 & 0.030 & 0.2 & 0.3  & 110.04 & 1.66 &N  &  (f) \\
J1357$+$1919 & 06.04.06 & ST  & R & 7.40 & 27 & 0.746 & 0.2 & 0.3  & 97.85  & 1.28 &N  &  (f) \\
J1357$+$1919 & 22.04.06 & ST  & R & 4.88 & 17 & 0.037 & 0.2 & 0.4  & 44.72  & 1.04 &N  &  (f) \\
J1357$+$1919 & 23.04.06 & ST  & R & 6.04 & 19 & 0.060 & 0.3 & 0.6  & 95.00  & 1.88 &N  &  (f) \\
&&&&&&&&&&&&\\
J2203$+$3145 & 08.11.05 & HCT & R & 5.62 & 18 & 0.478 & 0.2 & 0.3  & 92.02  & 1.38 &N  &  (f) \\
J2203$+$3145 & 14.09.06 & ST  & R & 5.87 & 26 & 0.158 & 0.2 & 0.3  & 78.55  & 1.27 &N  &  (f) \\
J2203$+$3145 & 15.09.07 & ST  & R & 7.74 & 33 & 0.511 & 0.2 & 0.2  & 38.25  & 0.75 &N  &  (f) \\
&&&&&&&&&&&&\\
J2346$+$0930 & 20.09.03 & HCT & R & 5.82 & 39 & 0.772 & 0.1 & 0.3  & 137.92 & 1.65 &N  &  (f) \\
J2346$+$0930 & 20.10.04 & ST  & R & 5.73 & 11 & 0.128 & 0.1 & 0.3  & 52.59  & 2.21 &N  &  (f) \\
J2346$+$0930 & 16.11.06 & ST  & R & 5.24 & 12 & 0.732 & 0.2 & 0.2  & 18.58  & 0.68 &N  &  (f) \\
&&&&&&&&&&&&\\\hline
\multicolumn{13}{l}{\small High optical polarization core dominated quasars (HPCDQs)[11 sources; 31 DLCs]}\\ \hline
J0238$+$1637 & 12.11.99 & ST  & R & 6.57 & 40 & 1.016 & 0.4 & 0.7  & 95.28  & 1.08 &N  &  (e) \\
J0238$+$1637 & 14.11.99 & ST  & R & 6.16 & 34 & 1.020 & 0.2 & 0.4  & 88.31  & 1.13 &N  &  (e) \\
J0238$+$1637 & 18.11.03 & HCT & R & 7.80 & 41 & 0.251 & 0.3 & 0.5  & 129.42 & 1.34 &N  &  (f) \\
&&&&&&&&&&&&\\
J0423$-$0120 & 19.11.03 & HCT & R & 6.69 & 38 & 0.402 & 0.2 & 0.3  & 153.68 & 1.41 &N  &  (f) \\
J0423$-$0120 & 08.12.04 & ST  & R & 7.00 & 13 & 0.412 & 0.1 & 0.3  & 38.52  & 1.21 &N  &  (f) \\
J0423$-$0120 & 25.10.09 & ST  & R & 4.46 & 21 & 0.128 & 0.3 & 0.6  & 76.55  & 1.48 &N  &  (f) \\
&&&&&&&&&&&&\\
J0739$+$0137 & 05.12.05 & HCT & R & 5.31 & 10 & 0.461 & 0.1 & 0.2  & 20.17  & 0.94 &N  &  (f) \\
J0739$+$0137 & 06.12.05 & HCT & R & 6.06 & 9  & 0.647 & 0.1 & 0.4  & 80.48  & 4.24 &PV &  (f) \\
J0739$+$0137 & 09.12.05 & HCT & R & 5.46 & 14 & 0.186 & 0.1 & 0.3  & 57.77  & 1.87 &N  &  (f) \\
&&&&&&&&&&&&\\
J0849$+$5108 & 30.12.98 & ST  & R & 7.08 & 39 & 0.603 & 0.8 & 1.3  & 116.19 & 1.18 &N  &  (a) \\
&&&&&&&&&&&&\\
J1058$+$0133 & 25.03.07 & ST  & R & 6.87 & 13 & 0.177 & 0.1 & 0.2  & 21.51  & 0.81 &N  &  (f) \\
J1058$+$0133 & 16.04.07 & ST  & R & 4.23 & 17 & 0.501 & 0.1 & 0.2  & 52.55  & 1.38 &N  &  (f) \\
J1058$+$0133 & 23.04.07 & ST  & R & 5.36 & 12 & 0.158 & 0.2 & 0.3  & 25.12  & 0.81 &N  &  (f) \\
&&&&&&&&&&&&\\
J1159$+$2914 & 31.03.12 & IGO & R & 5.93 & 18 & 0.134 & 0.6 & 0.7  & 34.89  & 0.53 &N  &  (f) \\
J1159$+$2914 & 01.04.12 & IGO & R & 8.40 & 26 & 0.133 & 0.8 & 0.9  & 39.13  & 0.61 &N  &  (f) \\
J1159$+$2914 & 02.04.12 & IGO & R & 7.22 & 20 & 0.144 & 1.5 & 2.9  & 69.58  & 1.59 &N  &  (f) \\
&&&&&&&&&&&&\\
J1218$-$0119 & 11.03.02 & ST  & R & 6.16 & 34 & 0.049 & 1.3 & 3.0  & 225.39 & 2.39 &PV &  (e) \\
J1218$-$0119 & 13.03.02 & ST  & R & 8.48 & 24 & 0.074 & 0.2 & 0.5  & 158.12 & 1.62 &N  &  (e) \\
J1218$-$0119 & 15.03.02 & ST  & R & 3.91 & 11 & 0.077 & 0.2 & 0.3  & 29.68  & 0.59 &N  &  (e) \\
J1218$-$0119 & 16.03.02 & ST  & R & 8.20 & 22 & 0.072 & 0.2 & 0.3  & 121.40 & 1.52 &N  &  (e) \\
&&&&&&&&&&&&\\
J1256$-$0547 & 26.01.06 & ST  & R & 4.75 & 21 & 0.596 & 0.1 & 0.2  & 65.87  & 1.38 &N  &  (f) \\
J1256$-$0547 & 28.02.06 & ST  & R & 6.51 & 42 & 0.601 & 0.1 & 0.2  & 91.54  & 0.81 &N  &  (f) \\
J1256$-$0547 & 20.04.09 & ST  & R & 5.46 & 22 & 0.601 & 0.2 & 0.3  & 43.51  & 0.75 &N  &  (f) \\
&&&&&&&&&&&&\\
J1310$+$3220 & 26.04.00 & ST  & R & 5.99 & 18 & 0.971 & 1.0 & 1.8  & 48.79  & 1.34 &N  &  (e) \\
J1310$+$3220 & 17.03.02 & ST  & R & 8.37 & 21 & 1.050 & 0.8 & 0.6  & 17.49  & 0.27 &N  &  (e) \\
J1310$+$3220 & 24.04.02 & ST  & R & 5.81 & 14 & 1.045 & 0.5 & 0.3  & 7.70   & 0.17 &N  &  (e) \\
J1310$+$3220 & 02.05.02 & ST  & R & 5.08 & 15 & 0.031 & 0.5 & 0.4  & 8.61   & 0.21 &N  &  (e) \\
&&&&&&&&&&&&\\
J1512$-$0906 & 14.06.05 & ST  & R & 4.93 & 11 & 0.347 & 0.1 & 0.1  & 9.33   & 0.39 &N  &  (f) \\
J1512$-$0906 & 01.05.09 & ST  & R & 6.02 & 25 & 0.557 & 0.3 & 0.5  & 58.70  & 1.02 &N  &  (f) \\
J1512$-$0906 & 20.05.09 & ST  & R & 5.16 & 25 & 0.580 & 0.5 & 0.7  & 55.86  & 0.67 &N  &  (f) \\
&&&&&&&&&&&&\\
J2222$-$0457 & 08.10.10 & ST  & R & 5.72 & 18 & 0.044 & 0.4 & 0.9  & 69.00  & 1.59 &N  &  (g) \\
&&&&&&&&&&&&\\\hline
\multicolumn{13}{l}{\small TeV detected BL Lac objects (TeV-BLs)[13 sources; 54 DLCs]}\\ \hline
J0112$+$2244 & 29.10.05 & ST  & R & 7.14 & 36 & 0.250 & 0.1 & 0.2  & 71.03  & 0.85 &N  &  (h) \\
&&&&&&&&&&&&\\
J0222$+$4302 & 13.11.99 & ST  & R & 5.92 & 123 & 0.051 & 0.1& 0.2  & 416.3  & 1.43 &PV &  (i) \\
J0222$+$4302 & 24.10.00 & ST  & R & 9.15 & 73  & 0.050 & 0.1& 0.3  & 310.17 & 1.95 &V  &  (i) \\
J0222$+$4302 & 01.11.00 & ST  & R & 9.02 & 103 & 0.363 & 0.2& 0.3  & 218.47 & 0.86 &N  &  (i) \\
&&&&&&&&&&&&\\
J0721$+$7120 & 01.02.05 & ST  & R & 1.68 & 26 & 0.159 & 0.2 & 0.3  & 62.62  & 0.86 &N  &  (g) \\
&&&&&&&&&&&&\\
J0738$+$1742 & 26.12.98 & ST  & R & 7.79 & 49 & 0.122 & 0.4 & 0.6  & 89.48  & 0.75 &N  &  (j) \\
J0738$+$1742 & 30.12.99 & ST  & R & 7.44 & 64 & 0.066 & 0.4 & 0.5  & 96.90  & 0.64 &N  &  (j) \\
J0738$+$1742 & 25.12.00 & ST  & R & 6.01 & 42 & 0.061 & 0.4 & 0.5  & 69.02  & 0.69 &N  &  (j) \\
J0738$+$1742 & 24.12.01 & ST  & R & 7.30 & 38 & 0.190 & 0.3 & 0.4  & 47.70  & 0.52 &N  &  (j) \\
J0738$+$1742 & 20.12.03 & HCT & R & 6.00 & 38 & 0.818 & 0.2 & 0.3  & 71.02  & 0.80 &N  &  (j) \\
J0738$+$1742 & 10.12.04 & ST  & R & 6.23 & 30 & 0.512 & 0.2 & 0.3  & 98.67  & 1.17 &N  &  (j) \\
J0738$+$1742 & 23.12.04 & ST  & R & 5.88 & 13 & 0.505 & 0.1 & 0.2  & 36.57  & 1.15 &N  &  (j) \\
J0738$+$1742 & 02.01.05 & ST  & R & 4.87 & 22 & 0.522 & 0.2 & 0.2  & 29.93  & 0.81 &N  &  (j) \\
J0738$+$1742 & 05.01.05 & ST  & R & 5.23 & 26 & 0.158 & 0.1 & 0.2  & 64.56  & 1.08 &N  &  (j) \\
J0738$+$1742 & 09.01.05 & ST  & R & 7.13 & 30 & 0.152 & 0.1 & 0.2  & 64.47  & 0.90 &N  &  (j) \\
J0738$+$1742 & 09.11.05 & ST  & R & 4.27 & 19 & 0.624 & 0.1 & 0.2  & 48.34  & 1.13 &N  &  (j) \\
J0738$+$1742 & 16.11.06 & ST  & R & 4.97 & 21 & 0.033 & 0.2 & 0.3  & 64.94  & 1.10 &N  &  (j) \\
J0738$+$1742 & 29.11.06 & ST  & R & 6.49 & 28 & 0.516 & 0.2 & 0.3  & 66.83  & 1.00 &N  &  (j) \\
J0738$+$1742 & 17.12.06 & ST  & R & 6.54 & 28 & 0.507 & 0.1 & 0.3  & 118.30 & 1.45 &N  &  (j) \\
J0738$+$1742 & 15.12.07 & ST  & R & 7.05 & 29 & 0.162 & 0.1 & 0.2  & 89.88  & 1.35 &N  &  (j) \\
J0738$+$1742 & 16.12.07 & ST  & R & 7.29 & 30 & 0.508 & 0.2 & 0.2  & 30.66  & 0.42 &N  &  (j) \\
J0738$+$1742 & 22.11.08 & ST  & R & 5.98 & 29 & 0.128 & 0.2 & 0.2  & 48.35  & 0.53 &N  &  (j) \\
J0738$+$1742 & 08.12.09 & ST  & R & 6.94 & 31 & 0.128 & 0.3 & 0.5  & 80.87  & 0.91 &N  &  (h) \\
J0738$+$1742 & 05.01.11 & ST  & R & 6.80 & 32 & 0.330 & 0.3 & 0.4  & 43.17  & 0.51 &N  &  (h) \\
J0738$+$1742 & 29.11.11 & ST  & R & 6.11 & 29 & 0.499 & 0.2 & 0.3  & 34.25  & 0.51 &N  &  (h) \\
&&&&&&&&&&&&\\
J0809$+$3122 & 28.12.98 & ST  & R & 7.29 & 36 & 0.844 & 0.3 & 0.6  & 153.04 & 1.69 &N  &  (a) \\
&&&&&&&&&&&&\\
J0809$+$5218 & 04.02.05 & HCT & R & 7.24 & 29 & 0.885 & 0.1 & 0.3  & 97.92  & 1.43 &N  &  (g) \\
J0809$+$5218 & 05.12.05 & HCT & R & 5.85 & 10 & 0.892 & 0.1 & 0.3  & 31.21  & 1.26 &N  &  (g) \\
J0809$+$5218 & 08.12.05 & HCT & R & 5.77 & 16 & 0.894 & 0.2 & 0.2  & 18.25  & 0.40 &N  &  (g) \\
J0809$+$5218 & 09.12.05 & HCT & R & 5.46 & 14 & 0.892 & 0.2 & 0.2  & 17.38  & 0.56 &N  &  (g) \\
&&&&&&&&&&&&\\
J0854$+$2006 & 29.12.98 & ST  & R & 6.77 & 19 & 0.014 & 1.0 & 0.5  & 4.27   & 0.10 &N  &   (i)\\
J0854$+$2006 & 31.12.99 & ST  & R & 5.61 & 29 & 0.471 & 0.2 & 0.4  & 98.30  & 1.48 &N  &   (i)\\
J0854$+$2006 & 28.03.00 & ST  & R & 4.24 & 22 & 0.462 & 0.4 & 0.5  & 29.78  & 0.64 &N  &   (i)\\
J0854$+$2006 & 17.02.01 & ST  & R & 6.92 & 47 & 0.467 & 0.4 & 0.4  & 46.55  & 0.42 &N  &   (i)\\
J0854$+$2006 & 05.02.05 & HCT & R & 7.82 & 42 & 1.739 & 0.1 & 0.2  & 127.8  & 1.05 &N  &   (g)\\
J0854$+$2006 & 12.04.05 & ST  & R & 4.77 & 56 & 0.907 & 0.3 & 0.4  & 65.20  & 0.45 &N  &   (g)\\
&&&&&&&&&&&&\\
J1015$+$4926 & 06.02.10 & ST  & R & 5.93 & 26 & 0.248 & 0.1 & 0.2  & 84.52  & 1.42 &N  &  (g) \\
J1015$+$4926 & 19.02.10 & ST  & R & 6.05 & 43 & 0.252 & 0.2 & 0.3  & 171.66 & 1.26 &N  &  (g) \\
J1015$+$4926 & 07.03.10 & ST  & R & 5.50 & 36 & 0.180 & 0.2 & 0.4  & 132.23 & 1.14 &N  &  (g) \\
&&&&&&&&&&&&\\
J1221$+$2813 & 19.03.04 & ST  & R & 6.20 & 60 & 2.324 & 0.3 & 0.5  & 159.14 & 1.14 &N  &  (g) \\
J1221$+$2813 & 20.03.04 & ST  & R & 6.29 & 67 & 2.322 & 0.4 & 0.7  & 196.68 & 1.08 &N  &  (g) \\
J1221$+$2813 & 18.03.05 & ST  & R & 4.18 & 28 & 1.301 & 0.2 & 0.5  & 116.81 & 2.22 &PV &  (g) \\
J1221$+$2813 & 05.04.05 & ST  & R & 7.28 & 41 & 1.280 & 0.2 & 0.4  & 170.26 & 1.75 &PV &  (g) \\
&&&&&&&&&&&&\\
J1221$+$3010 & 08.03.10 & IGO & R & 6.54 & 17 & 0.004 & 0.1 & 0.4  & 123.33 & 2.84 &PV &  (g) \\
J1221$+$3010 & 18.03.10 & ST  & R & 5.87 & 27 & 1.016 & 0.3 & 0.4  & 41.95  & 0.70 &N  &  (g) \\
J1221$+$3010 & 22.05.10 & ST  & R & 4.21 & 21 & 0.009 & 1.3 & 1.4  & 25.99  & 0.50 &N  &  (g) \\
&&&&&&&&&&&&\\
J1419$+$5423 & 28.03.99 & ST  & R & 5.65 & 33 & 0.142 & 0.3 & 0.5  & 68.98  & 0.82 &N  &  (a) \\
&&&&&&&&&&&&\\
J1428$+$4240 & 21.04.04 & HCT & R & 6.12 & 35 & 0.865 & 0.4 & 0.8  & 165.94 & 1.54 &N  &  (g) \\
J1428$+$4240 & 22.04.09 & ST  & R & 4.48 & 19 & 0.306 & 0.6 & 0.8  & 28.34  & 0.72 &N  &  (g) \\
J1428$+$4240 & 29.04.09 & ST  & R & 6.81 & 29 & 0.856 & 0.6 & 0.9  & 78.27  & 0.86 &N  &  (g) \\
&&&&&&&&&&&&\\
J1555$+$1111 & 05.05.99 & ST  & R & 4.15 & 23 & 1.170 & 0.3 & 0.5  & 65.67  & 1.26 &N  &   (a)\\
J1555$+$1111 & 24.06.09 & ST  & R & 4.22 & 26 & 0.137 & 0.1 & 0.3  & 108.25 & 1.77 &N  &   (g)\\
J1555$+$1111 & 15.05.10 & ST  & R & 6.50 & 22 & 0.041 & 0.1 & 0.3  & 112.32 & 1.98 &N  &   (g)\\
J1555$+$1111 & 16.05.10 & ST  & R & 6.27 & 33 & 0.101 & 0.2 & 0.3  & 164.16 & 1.53 &N  &   (g)\\
&&&&&&&&&&&&\\
\enddata

{\small
Columns :- (1) source name; (2) date of observation; (3) telescope used; (4) filter used; (5) duration of
monitoring; (6) number of data points in the DLC; (7) mean apparent magnitude difference of the steady star-star pair;
(8) quadratic mean of the $\sc IRAF$ errors for the steady star-star DLC;
(9) standard deviation of the steady star-star DLC;
(10) $\chi^2$-value for the star-star DLC; (10) $F$-value for the star-star DLC;
(12) variability status for the star-star DLC;
(13) reference for the INOV data.\\

{$^\P$} ST - Sampurnanand Telescope (ARIES); HCT - Himalayan Chandra Telescope (IIA);
IGO - IUCAA Girawali Observatory; VBT - Vainu Bappu Telescope (IIA);  GSO - Gurushikhar telecsope (PRL). \\
$^\dag$ V = Variable; N = Non-variable; PV = Probable Variable; \\
{$^\pounds$}References for the INOV data:
(a) \citet{2005MNRAS.356..607Stalin}; (b) \citet{2007BASI...35..141AG};
(c) \citet{2004MNRAS.350..175Stalin}; (d) \citet{2010MNRAS.401.2622AG};
(e) \citet{2004MNRAS.348..176Sagar}; (f) \citet{2012A&A...544A..37AG};
(g) \citet{2011MNRAS.416..101GK}; (h) AGs unpublished data;
(i) \citet{2004JApA...25....1Stalin}; (j) \citet{2009MNRAS.399.1622AG}.
}

\end{deluxetable}
\section*{Acknowledgements}
AG would like to thank Dr. Santosh Joshi (ARIES) for carrring out
optical observations on a few occasions. The authors are thankful
to the anonymous referee for the critical and constructive
suggestions.
\\
\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


I accidentally tapped "new group" on whatapp…..how do I delete?
Also how do I change my status on latest whatapp.
Really battling on this updated version.
If I clear a group chat as admin, does it clear on other phones too? I don't want to delete the group, just clear the chat and start a fresh.
you can scroll up to the "To delete a group in WhatsApp on iPhone" section, make sure to select 'clear chat' other than 'delete group' as shown in the screenshot above.
deletegroupp is using Hatena Blog. Would you like to try it too?


text:
AiG: Kristian Stratton new & first WA State Manager
The Australian Industry Group (AiG), is ramping up its Western Australia (WA) presence with the appointment of a new WA State Manager.
Ai Group provides support and representation to employers in a broad range of industries across the economy including manufacturing, construction, mining equipment manufacturers and suppliers, defense, labor hire, and technology and communications.
Ai Group Chief Executive, Innes Willox, said: "I'm delighted to confirm that Kristian Stratton has been appointed as Ai Group's new and first WA State Manager."
"We are fortunate to have found someone who has such deep connections within the WA business community and insights into their issues as well as a long term, strong understanding of Ai Group and all that we do and stand for."
"Kristian will head our Perth-based operations in providing advice and support to local industry and representation with Government in support of policies that are good for business, good for the community and that help the local and national economy grow."
"Ai Group has provided support to local WA businesses and national companies with a WA presence for many years but this is the first time we have appointed such a senior manager with state-wide responsibilities."
Kristian Stratton added: "I'm looking forward to the opportunity to engage with business throughout WA. Ai Group operations in WA will give business an additional channel to add their voice to important national issues."
Kristian Stratton: LinkedIn http://au.linkedin.com/in/kristianstratton
Source: Ai Group
Topics: Ai Group-Australian Industry Group, Change of Guard


Buy on Bandcamp for the moment.
The Hula Honeys are proud to present two remixes of Walter S. Baumann's dusty material that he released on Lalamusik in the end of 2010.
The digital album "Dust Sparkling in the Sun" was a collection of 8 tracks with material that had its origin over 30 years ago. For the beautiful release on the Swiss netlabel Lalamusik, Walter S. Baumann brought his music up to date, still preserving its original grains.
Nik! takes a shot at What You Get: his Bear the Eagle Refix slows down the tempo and finds his groove around 130bpm. Standing on a heavy dubwise bassline at the lower end, Nik! works out the crackling sounds and noises and squeezes them into a shuffled techno track with a mental twist.
Soult's Wounded Rock Remix of Lick tells the story of the rock that feels no pain. It starts out as a spaced-out half time stepper, only to turn into a beautifully cut up pop song, opening hearts on the fly.


Hair issue: Our favourite mid-length haircuts!
Fitness motivation: Spring gym clothes!
Mini backpacks: The bag trend we love!
Camisole: The most flattering top ever!
Simple ways to update your spring outfit with accessories!
Quote of the week: Listen with the intent to understand.
The perfect smile: How to!
Coachella 2018: The best street style outfits!
Hot pink: how to wear our favourite colour!


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