SEO is way more than just a killer marketing tool or traffic builder. The ability to insert pages into competitive searches suggests a much broader power. Because if you have the ability to focus an audience's attention onto the topic of your choosing, you hold the power of propaganda. Some of us, like Rev Sale, go so far as to say it's a potential weapon of mass destruction and that we should be concerned about how a terrorist could control the publicly posted information via the search. Bob Sakayama has even consulted with the FBI on this very matter. Our discussion today acknowledges this power and demonstrates that SEO can be a very effective enabler of justice - an equalizer bar none, because in our world, little fish can take down big dogs.
Sometimes this power is obtained serendipitously - unearned as it were. Perhaps you met that crazy person who demands an unreasonable refund and starts posting nasty reviews that start showing up for searches for your brand. If you didn't give her the money, then you will probably soon realize that those posts are hurting you, and that you're getting slammed by an SEO offensive - one that can have very bad consequences for your bottom line.
Or you may be aware of the success of businesses like reputationdefender.com - specialists who apply basic SEO to unwind bad publicity by getting better commentary ranked higher than existing bad news. Again an example of SEO justice. Or SEO justice undoing previous SEO.
Last year, our good buddy Tony paid a refundable deposit of $10,000 on a property he was considering buying. The short story is that although he was due a refund, the real estate entity refused to pay. We posted a site (no longer live) optimized for the perps trademark with the whole story spelled out in detail (vetted by our attorney). The site also solicited other victims to post their complaints. Tony got his money back within 2 weeks - just before the company declared bankruptcy.
Bob's 91 year old father in law walked into Citizens Bank in Wolfeboro NH with his nest egg, with the intent of buying very safe certificates of deposits (CDs), but was talked into a front loaded bond fund at a time of rising interest rates. Although an obvious case of unethical banking, restoring the funds was not forthcoming. After getting push back on calls to the bank, Bob posted a single page detailing the story. Money was returned within the week.
You can see where this is going. Don't let unscrupulous businesses or persons go without accountability. It's your duty as a powerful propagandist to warn the public at large of the bad citizens among us, whether you expose unethical institutions, political malfeasance, or clients who default on payments. Using a lawyer to vet your story can save you from being forced to change or remove it - you always want the law on YOUR side.
For those of us focused on enterprise optimization, this is a snap - very low level SEO skills are needed. And if you control an enterprise, you can probably push significant PR advantage to your posts and get them ranked very high, very fast. Use geo advantages and multiple documents to get as many instances into the results as high as possible. Since it's so easy I recommend you do at least 20 pages and spread it out around the names of the parties, corporations, and the significant terms surrounding the issue.
And we know this works. We have tons of great anecdotes where wrongs were righted simply because of push back from the search. Once you see how effective and easy it is to rank most of these kinds of posts, you'll never let the bad guys get away with anything.
Please send us your stories - we'll share them with our enterprise community. We know from our chats that this is a very popular topic - blog posts coming.
Everyone understands the need for recourse, sometimes known as revenge. We are often placed in an environment in which the only other real world alternative to your injustice is just not going to cut it. When that happens to you, I recommend that you use your optimization skills to set things right.
- Pick your fights - Don't bother unless the issue is significant - a major ethical violation, a lot of money, etc.
- Name names - Let your target know exactly what terms you're optimizing for. As we all know you're much more likely to rank for a brand in combination with a person's name.
- Publicize all corporate entities. This is often the weakest link. Bring investor & client nomenclature into your target terms - gets you both rank & leverage.
- Use a good number of pages, across multiple sites. I suggest 20, targeted at all the iterations. If you do it right, all 20 documents will rank appropriately.
- Use services like RipOffReport.com, which will automatically rank for the offenders company and name, and will create a permanent record on the web.
- Stay legal - don't defame. As long as you stick with the facts, you're fine. Run your copy by your lawyer just to be safe.
- Don't take your posts down without compensation for the time it took to create, post, and link.
OneInAmelia specializes in search forensics & CSS.


The following oath is a closely kept secret among the Tong. Each Associate must repeat this oath before they are accepted as a Tiger Claw. All current surveillence shows that this oath not just symbolic in meaning, but is taken literally should any member betray the "Family". There are three parts to this oath and the ceremony is administered by three Tiger Masters.
If I have supplied false particulars about myself for the purpose of joining the Tong, I shall be killed by five thunderbolts.
If I should change my mind and deny my membership of the Tong I will be killed by myriads of swords.
I shall not cause discord amongst my sworn siblings by spreading false reports about any of them or cause harm to my sworn siblings. If I do so I will be killed by myriads of swords.
After having entered the Tong I must treat the parents and relatives of my sworn siblings as my own kin. I shall suffer death by five thunderbolts if I do not keep this oath.
If I should take advantage of a sworn sibling or force unfair business deals upon him I will be killed by myriads of swords.
I must not take to myself the spouses and concubines of my sworn siblings nor commit adultery with them. If I do so I will be killed by myriads of swords.
I shall not disclose the secrets nor reveal the signs of the Tong, not even to my parents, brothers, or spouse. I will be killed by myriads of swords if I do so.
I shall never betray my sworn siblings. If, through a misunderstanding, I have caused the arrest of one of my siblings I must cause his release immediately. If I break this oath I will be killed by five thunderbolts.
After entering the Tong I must forget any previous grudges I may have borne against my sworn siblings. If I do not do so I will be killed by five thunderbolts.


text:
Q: jQuery carouFredSel li width I'm using this plugin and here is the code: http://jsfiddle.net/gm8t5/
Basically I want to increase the middle li width to look something like this:

I tried it like this:
.list_carousel li {width: 960px !important;}

But the animation is not going so smooth.
How can I fix this?

A: Set the item width in the CSS using .list_carousel li. Also, you need to set the items visible to 3 since you want 1 off to each side with 1 in the middle.
Plugin setting:
items: {
    visible: {
        min: 3,
        max: 3
    }
}

CSS
.list_carousel li {
    float: left;
    width: 300px;
    height: 60px;
}

You can play with resizing the items, as well as resizing the container. You'll want the item width to be most of the overall container width the achieve the effect you are looking for.
I made a new jsfiddle and did some serious clean up. The markup and CSS you had was actually making it impossible to achieve what you were looking for.

redpajama_set_name: RedPajamaStackExchange


text:
\section{Introduction}
An active galactic nucleus (AGN) is powered by the matter accreting onto the central
supermassive black hole (SMBH) at the center of a galaxy.
The radiation coming from the accreting AGN systems shows complex
features in their X-ray spectra. The components (e.g. hard, soft, or soft excess etc.) of the spectra come from different regions within the system.
Some fraction of the hard radiation heats up the disc and generates emission lines, while some fraction gets absorbed
by different clouds at the line of sight (LOS). The variable absorption of the continuum coming from the central inner disc  can be due to the presence of variable clouds or due to the winds from the disc.

The X-ray absorbing column density changes
dramatically by an order of magnitude over
a few years in different Seyfert galaxies \citep{Risalitietal2002}, which disfavors
the homogeneous nature of the absorbers.
Changing look (CL) AGN are those sources that show
extreme variation in the column density of the X-ray absorber, with rapid transitions between Compton-thin (N$_H < 10^{24}$ cm$^{-2}$) and Compton-thick (N$_H > 10^{24}$ cm$^{-2}$) regimes \citep[e.g.][]{Riccietal2016}.
CLAGN though first discovered serendipitously \citep{LaMassaetal2015} are now considered as a separate class of AGN that transit from type 1 to 2 and vice versa within a timescale of decades or years \citep{Veronetal1980,Maiolino1995,Denneyetal2014,Yangetal2018,Kimetal2018}. In \citet{Riccietal2020}, the CL phenomena was shown for 1ES 1927+654 can be due to rapid changes in the innermost regions of accreting SMBHs.

According to models, the timescale of CL phenomenon within months or years can be due to the variation in absorbing material that appears and disappears along the LOS, this supports the quick variation in column density \citep{Risalitietal2009}. On the contrary, many CLAGNs showed little variation in column density \citep{McElroyetal2016,NodaDone2018}, therefore CL nature could also be due to
other physical processes within the system. The weak or low optical polarization
of CLAGNs suggests that the transition from type 1 to type 2 can not be attributed to the putative dust obscuration \citep[e.g.][]{Hutsemekers2019}. The mid-infrared and optical analysis
of \citet{Shengetal2017} do not favor the obscuration scenario and support that the
CL may be caused by the intrinsic variation of accretion process. The work of \citet{NodaDone2018}
suggests CL as accretion process originated phenomenon where radiation pressure should be
more important compared to gas pressure. The radiation pressure driven instability is also
a possibility to explain the observed timescale of CL phenomenon \citep{Sniegowska2019}.

NGC\,1365 is a Seyfert 1.8 \citep{MaiolinoReike1995} galaxy at z=0.0055 with a $10^{6.5} M_\odot$ BH \citep{Risalitietal2009}. \citet{CombesEtal2019} estimated the mass of $3.98 \times 10^6 M_\odot$ from the molecular gas dynamics using ALMA data.  This spiral galaxy is intensely studied by \citet[][for a review]{Lindbladreview1999}.
The source is a CLAGN due to its Compton-thin to Compton-thick transition, that can be due to variation in the LOS absorber rather than to extreme intrinsic emission variability \citep{MattEtal2003,Risalitietal2005}.
The spectral components of NGC\,1365 in X-ray consists of several distinct features e.g. Compton hump $> 10$ keV, soft excess at low energy (below 3 keV), strong absorption features, relativistic iron and emission lines. The source also has bi-conical outflow from the nucleus \citep{Edmundsetal1988}. \citet{Sandqvistetal1995} suggested that the AGN has a weak radio jet in this source. A [O III] line is seen in the outflow \citep{Storchi-Bergmann1991,Veilleuxetal2003,SharpBlandHawthorn2010}. The emission lines observed for this source are dominated by collisionally ionized gas \citep{Guainazzietal2009}, however, it can also be hybrid \citep[photoionised+collisionally ionised;][used {\it XMM-Newton} and {\it Chandra} data]{Whewelletal2016}. NGC\,1365 has some important characteristics, when it is observed in the Compton-thin state, its X-ray spectrum  shows the presence of strong absorption lines due to Fe xxv(both the He-$\alpha$ and He-$\beta$) and Fexxvi(both the Ly$\alpha$ and Ly$\beta$ components); these lines are blue shifted by v$\sim$3000\,km s$^{-1}$ \citep{Risalitietal2005,BrennemanEtal2013}. These features can be originated due to the presence of highly ionised outflowing wind and possibly originated from the accretion disc. All these features are occasionally observed in Seyfert galaxies, however, it is unlikely to see all of them in a single source. Later, \citet{ConnolyEtal2014} examined that the long-term variability of the X-ray absorber could be originated from the changes in mass accretion rate of NGC\,1365. The analysis of {\it Suzaku} observation of the source suggested the presence of a partial covering and ionized absorber using photoionisation models \citep{GoffordEtal2013,GoffordEtal2015}. \citet{BraitoEtal2014} evidenced that two ionised absorbers were needed to fit the RGS spectra of {\it XMM-Newton} and detected a possible P-Cygni profile of the Mg\,XII Ly$\alpha$ line which is associated with mildly ionized absorber indicative of a wide angle outflowing wind. At the same time, using the {\it Chandra} data, \citet{NardiniEtal2015} estimated the location of the photoionised gas based on some evidence of broadening of the emission lines.
The central active nucleus is surrounded by a molecular torus with both narrow
and broad emission line components in the emitted spectrum and relativistic iron line \citep{Risalitietal2009}.
The variable absorbing medium along the LOS was observed by \citep{Riversetal2015} using combined {\it XMM-Newton} and {\it NuSTAR} data.
The relativistic line feature estimates the maximal spin of the BH $> 0.97$ \citep{Waltonetal2014}.
\citet{Karaetal2015} estimated soft lag due to the presence of eclipsing cloud along the line of sight using {\it NuSTAR} observations. The star formation and gas accretion to the central object were studied using near-infrared (NIR) data by \citet{Fazelietal2019} and \citet{Gaoetal2021} to check for more recent star formation activities and outflow structure of the source.

Despite the source has been studied extensively in different energy bands, the understanding of CL phenomena is still lacking due to shortcoming of physical picture in earlier studies. Most of them phenomenologically explained that the variable column density is due to the appearance/disappearance of some clouds along the LOS and  none of the previous studies self-consistently considered the accretion-ejection scenario to take into account for the CL phenomena. Therefore, in this work, we aim to address that phenomena after estimating fundamental physical quantities of accretion e.g. mass accretion rate, corona geometry etc., considering the beforehand observational characteristics such as Compton hump, jets, winds, and variable continuum in NGC\,1365 system. For that, we used joint {\it XMM-Newton} and {\it NuSTAR} data during 2012 and 2013.
This paper is organized as follows: in Section 2 we explain the observations and data reduction
procedures, in Section 3, we discuss the modelling, various analysis, and data fitting carried out using different models. A brief conclusion is given in the final Section.

\section {Observation and Data analysis}\label{sec:Observation}

We used joint {\it XMM-Newton} and {\it NuSTAR} \citep{Harrisonetal2013} observations of NGC\,1365 during 2012 and 2013. The log of observations is given in \autoref{table:observation}.

\begin{table}
\scriptsize
\centering
\caption{\label{table:observation} Log of observations. Here, X=6000204600, and Y=0692840 are the initials of the observation IDs.}
\begin{tabular}{ccccccc}
\hline
  {\it NuSTAR} &Exp. & {\it XMM-Newton} &Exp. &Epoch   & Date   & MJD\\
            &    (ks)   &          &(ks)      &    &   &   \\
\hline
X3&41 &Y201&118 &A  &2012-07-26 &56134 \\
X5&66 &Y301&108 &B  &2012-12-24 &56285 \\
X7&74 &Y401&93  &C  &2013-01-23 &56315 \\
X9&70 &Y501&116 &D  &2013-02-12 &56335 \\
\hline
\end{tabular}
\end{table}

To analyze the {\it XMM-Newton} data, we used the Science Analysis System (SAS) version 19.1.0 and followed the standard procedures given in the SAS data analysis threads\footnote{\url{https://www.cosmos.esa.int/web/xmm-newton/sas-threads}}. We first reprocessed the Observation Data Files (ODF) using the {\sc epproc} routine to generate the calibrated and concatenated event lists. We filtered the concatenated event lists to remove the periods of high background activity. We then extracted the source and background spectra using the {\sc evselect} routine. We used a circular region of radius $32^{\prime\prime}$ for both the source and the background. The background region was in the same CCD but away from the contamination of the point sources. We used {\sc rmfgen} and {\sc arfgen} tasks to generate the redistribution matrices (.rmf)  and the ancillary (.arf) files. Finally, we rebinned the spectra using the task {\sc specgroup} to have at least 25 counts in each bin.

The {\it NuSTAR} data were extracted using the standard
{\sc NUSTARDAS v1.3.1}
\footnote{\url{https://heasarc.gsfc.nasa.gov/docs/nustar/analysis/}} software. We
ran {\sc nupipeline} task to produce cleaned event lists and
{\sc nuproducts} to generate the spectra. We used a region of
$80^{\prime\prime}$  for the source and $100^{\prime\prime}$ for the background
using {\sc ds9}. The data were grouped by {\it grppha} command, with a
minimum of 30 count in each bin. For the analysis of each epoch of
observation, we used the data of joint {\it XMM-Newton} and {\it NuSTAR} in the energy range of 0.5$-$75 keV.

We used {\sc XSPEC}\footnote{\url{https://heasarc.gsfc.nasa.gov/xanadu/xspec/}} \citep{Arnaud1996} version 12.11.0 for spectral analysis.
Each epoch of observation was fitted using an accretion disc
based two component advective flow ({\fontfamily{qcr}\selectfont TCAF}~\citet{ChakrabartiTitarchuk1995}) model including jet ({\fontfamily{qcr}\selectfont JeTCAF}~\citet{MondalChakrabarti2021}). The present model takes into account the radiation processes at the base of the jet, discussed later in detail. We used the absorption model
{\fontfamily{qcr}\selectfont TBABS} \citep{Wilmsetal2000} for the Galactic absorption, keeping the hydrogen column density fixed to $1.3\times 10^{22}$cm$^{-2}$ \citep{Kalberlaetal2005} during the fitting. We used chi-square statistics for the goodness of the fitting. We employed source redshift here and left $N_H$ as a free parameter to estimate the absorbing column density responsible for the overall spectral distortion.

\section{Modelling}\label{sec:Modelling}

For the spectral fitting, we used the accretion-ejection based {\fontfamily{qcr}\selectfont JeTCAF}~model \citep{MondalChakrabarti2021} along with
multiplicative models e.g. partial covering fraction absorption ({\fontfamily{qcr}\selectfont ZPCFABS}), and Gaussian absorption line ({\fontfamily{qcr}\selectfont GABS}). The {\fontfamily{qcr}\selectfont JeTCAF}\, model geometry and flow configuration is illustrated in \autoref{fig:modelCartoon}.
In this model, the accretion disc has two components, one is a Keplerian disc sitting at the equatorial plane which is the source of soft photons, and a sub-Keplerian
halo (hot component) sitting above and below the Keplerian disc. The second component forms the shock in accretion disc \citep{Chakrabarti1989} after satisfying Rankine-Hugoniot conditions.
This shocked region behaves as the centrifugal pressure supported boundary layer (CENBOL) of the corona. The same region is also producing thermally driven jets. Matter falling onto the black hole, piles up inside the shocked (post-shock) region. The {\fontfamily{qcr}\selectfont JeTCAF}\, model takes into account the radiation mechanisms at the base of the jet and the bulk motion effect by the outflowing jet on the emitted spectra. This model requires six parameters (if the mass is considered as a free parameter) which are (i) mass of the BH ($M_{\rm BH}$), (ii) disc accretion rate
($\dot m_{\rm d}$), (iii) halo accretion rate ($\dot m_{\rm h}$), (iv) size of the dynamic corona or the location of the shock ($X_{\rm s}$ in $r_g=2GM_{\rm BH}/c^2$ unit), (v) shock compression ratio ($R$), and (vi) ratio of the solid angle subtended by the outflow to the inflow ($f_{\rm col}=\Theta_o/\Theta_{\rm in}$).

The emergent spectrum from {\fontfamily{qcr}\selectfont JeTCAF}\,has four components, (1) multicolour blackbody spectrum which is coming from the disc, (2) the hard radiation; from the upscattering of the soft photons from the disc by the hot corona, (3) the second hard component at the shoulder of the black body bump is due to scattering of soft photons from the disc by the base of the jet, (4) downscattering of hard radiation from the corona by the bulk motion of the jet produces excess above 10\,keV \citep{TitarchukShrader2005,MondalChakrabarti2021}. This component also fits the Compton hump that are observed in reflection models. The current {\fontfamily{qcr}\selectfont JeTCAF}\, model is an updated version (including jet) of {\fontfamily{qcr}\selectfont TCAF}\, model, which has been successfully applied to low mass black hole X-ray binaries \citep[][and references therein]{Debnathetal2014,Mondaletal2014,MondalChakrabarti2019} and to AGNs  \citep[e.g.][]{Nandietal2019,MondalStalin2021} to fit their spectra and to infer the underlying accretion dynamics. In this model the same corona, which is producing hard radiation, also launching jet at its base. The jet/mass outflow rate is coming after solving a series of coupled hydrodynamic equations, thus, it naturally connects disc and jet. As NGC\,1365 evidenced the presence of both accretion discs, jets/outflows and Compton hump $> 10$keV, therefore, it is worth applying {\fontfamily{qcr}\selectfont JeTCAF}\, model to study the CL phenomena. For the first time, we are applying {\fontfamily{qcr}\selectfont JeTCAF}\, model as a physical model to understand the CL phenomena, and we believe it has the potential to explore the observed accretion-ejection features in NGC\,1365. We note that, the present model does not include detailed line emission/absorption properties.

The spectrum of NGC\,1365 showed complex features including distortions between 3-7 keV, which can be due to varying absorber covering the source, that substantially changes the shape of the spectrum below 10\, keV \citep{Risalitietal2009}. It also showed broadening of Fe line $\sim$6\,keV in combined {\it XMM-Newton} and {\it NuSTAR} data due to relativistic effects near the inner region of the disc \citep{Risalitietal2013}. Below $\sim 3$\,keV energy, the {\it XMM-Newton} data showed diffuse thermal contribution and significant excess below $\sim$2\,keV, the origin of which is not clear yet. However, it can be originated by the up-scattering of seed photons from the disc by some warm, optically thick medium \citep[see for recent study][and references therein]{MehdipourEtal2021}. As the current {\fontfamily{qcr}\selectfont JeTCAF}\,model does not include relativistic effects, therefore for the skewing and broadening of the Fe line shapes near the innermost region of the disc, we used {\fontfamily{qcr}\selectfont GAUSS}~model to take into account those effects. Furthermore, we focus on the accretion parameters and the geometrical configuration of the corona that generate variable emission, which can be successfully obtained by analyzing the combined {\it XMM-Newton} and {\it NuSTAR} data in the range of 0.4-75\,keV. In this range all spectra showed both emission and absorption features, those are taken into account by {\fontfamily{qcr}\selectfont GAUSS}~and {\fontfamily{qcr}\selectfont GABS}~models. One Gaussian component is used at $\sim 6.4$\,keV for FeK line and the second one is used at $\sim 0.8$\,keV to fit the broad line feature at low energy. The other two/three Gaussian components are applied at different energy regions throughout the spectra, however, all are used below 6\,keV. The origin of (Soft) Gaussian components below 2\,keV is not clear yet, however, it can be originated from distant reflection \citep{MislavEtal2018}.  {\fontfamily{qcr}\selectfont ZPCFABS}\,model is used for addressing the source intrinsic absorption, partial covering and to estimate the column density along the LOS.
The complete model reads in  {\it XSPEC} as
\\
{\fontfamily{qcr}\selectfont TBABS}*{\fontfamily{qcr}\selectfont ZPCFABS}*{\fontfamily{qcr}\selectfont GABS}[2]*({\fontfamily{qcr}\selectfont GAUSS}[4-5]+{\fontfamily{qcr}\selectfont JeTCAF}).

The {\fontfamily{qcr}\selectfont ZPCFABS}\, model is not a good representation for an ionizing medium, as it does not include the effects of ionization, to generate the emission/absorption lines. For the ionization rate estimation, freely available photoionization software (e.g. {\sc cloudy} or {\sc xstar} etc.) can be appropriate, as extensively discussed in the literature \citep[see][and references therein]{GoffordEtal2013,BraitoEtal2014,GoffordEtal2015}. However, the current paper aims to quantify the accretion-ejection parameters assuming that accretion rate and corona properties might be triggering CL phenomena, therefore the detailed ionization modelling is beyond the scope of the paper.

\begin{figure}
\centering{
\hspace{-1.2cm}
\includegraphics[height=6.0truecm]{Figures/skc-cartoon-fig.pdf}}
\caption{Illustration of the {\fontfamily{qcr}\selectfont JeTCAF}~model. The zig-zag arrows show the scattering of photons from the disc and jet. The $\Theta_o$ and $\Theta_{\rm in}$ are the solid angle subtended by the outflow and inflow. The figure is adopted from \citet{MondalChakrabarti2021}.
}
\label{fig:modelCartoon}
\end{figure}

\section{Results and Discussions} \label{sec:Results}
\autoref{fig:SpecFits} shows the spectral fitting to the data for four epochs. In all the spectra, we found complex features including absorption lines, skewing of FeK line, soft excess, and some excess at high energies, which can be due to the bulk motion of the outflowing
material from the central region or can be due to reflection \citep[as reported by][and references therein]{Riversetal2015}. The model fitted parameters are given in \autoref{table:JetcafResults}. The variation of the {\fontfamily{qcr}\selectfont JeTCAF}\,model fitted parameters are shown in \autoref{fig:FittedPars}. The top panel shows the variation of mass which is constant during the observation period, as expected, however, other parameters changed significantly from second top to bottom panel. The disc or Keplerian accretion rate was $\leq$ 1\% of the Eddington rate, however, changed significantly between epochs A to D (second panel). \citet{BraitoEtal2014} estimated the mass accretion rate for this source, which is a factor few higher than our estimates. It can be due to either strong dependence of their estimates on the ionized winds and the covering factor they used in their model or due to using higher mass of the BH ($10^7 M_\odot$) and a different accretion efficiency (0.06).
The low-angular momentum, hot flow rate was always higher than the Keplerian one. We also noticed that the size of the dynamic corona shrunk from 28 to 10 $r_g$. As the size of the corona was changed significantly, and the disc accretion rate
was low compared to the halo accretion rate, these are the indication of hard/intermediate spectral state, if the spectra of AGN allow a similar classification as in low mass black hole binaries.
Our model fitted shock compression ratio ($R$) varies between 3.9 to 6.2. As the presence of jet was confirmed from [{\sc OIII}]
line that the source has bi-conical outflows \citep{Edmundsetal1988}, we therefore estimated the mass outflow/inflow rate (dimensionless quantity) using  the relation, $R_{\dot m}=\frac{\dot M_{\rm out}}{\dot M_{\rm tot}}=f_{\rm col}f_0^{3/2}\frac{R}{4} exp\left[\frac{3}{2} -f_0\right]$,
where, $f_{\rm 0}=\frac{R^2}{R-1}$ \citep{Chakrabarti1999}, $\dot M_{\rm tot}=(\dot m_d+R\times \dot m_h)$ \citep{MondalEtal2014ApSS}, and $\dot M_{\rm out}$ is the mass outflow rate in $M_\odot yr^{-1}$ respectively. The $f_{\rm col}$ value varied between 0.22 to 0.4 (column 7 in \autoref{table:JetcafResults}. Our calculated values lie in the range between $0.019\pm0.006$ to $0.12\pm0.04$. This gives the mass outflow rate $\sim 0.047$ M$_\odot$ yr$^{-1}$,  which is in agreement ($\sim 0.067$ M$_\odot$ yr$^{-1}$) to the independent optical and {\it Chandra} imaging studies\citep{Venturietal2018} and the {\it XMM-Newton}-RGS data analysis \citep{BraitoEtal2014}.

Treating BH mass as a free parameter in {\fontfamily{qcr}\selectfont JeTCAF}~we found BH mass is constant (see \autoref{fig:FittedPars}) during the combined {\it XMM} and {\it NuSTAR} data fitting, that comes out to be $4.38\pm0.34 - 4.51\pm0.29 \times10^{6} M_\odot$, closely matches ($4.47 \times 10^6 M_\odot$) with the estimation by \cite{Onorietal2017} and from the molecular gas dynamics ($3.98 \times 10^6 M_\odot$) using ALMA data by \citet{CombesEtal2019}.

In addition to accretion disc parameters, the {\fontfamily{qcr}\selectfont ZPCFABS}~model fitted $N_{\rm H}$ varied (in column 8 of \autoref{table:JetcafResults}) by more than an order of magnitude between epochs A to C, and the partial covering fraction ($c_f$) was relatively high (see column 9) in all four epochs, however, constant within the error bar.
The variation of $N_{\rm H}$ with {\fontfamily{qcr}\selectfont JeTCAF}\,model parameters are shown in \autoref{fig:correlation}. The left panel shows its variation with $\dot m_{\rm d}$. A similar variation is observed with the halo rate and accretion rate ration (ARR=disc rate/halo rate). This relative ratio of accretion rates is an indicator of the ratio of disc and corona flux contribution. As the ratio is always $<1$, implies dominant contribution of hot flow rate; thus the radiation coming from the corona is hard. It is quite certain that changing the geometry and accretion flow properties can change the intensity of the radiation emitting from the corona, since it reprocesses photons from the underlying accretion flow. This radiation when falling onto the disc can also influence the disc mass outflow, thus the column density, which can be seen from other panels in \autoref{fig:correlation}. The confidence contours of $N_H$ with {\fontfamily{qcr}\selectfont JeTCAF}\,model parameters are shown in \autoref{fig:ConfCont} in \autoref{sec:Contour}, which show that the parameters are non-degenerate and robust.

\begin{table*}
\centering
\caption{\label{table:JetcafResults} Best fitted model parameters are provided in this table. Here, N$_H$ and c$_f$ are hydrogen column density and dimensionless covering fraction.
$E_a$ and $\sigma_a$ are the absorption line energy and width. The superscripts 1 and 2 correspond to the absorption line 1 and 2. }
\resizebox{\textwidth}{!}{\begin{tabular}{cccccccccccccc}
\hline
Epoch       &$M_{\rm BH}$ &$\dot m_{\rm d}$ & $\dot m_{\rm h}$ & $X_{\rm s}$ & R &$f_{\rm col}$&$N_H$&c$_f$&$E_a^1$&$\sigma_a^1$&$E_a^2$&$\sigma_a^2$&$\chi_{\rm r}^2/dof$ \\
	        & $\times 10^6 M_\odot$&$\dot M_{\rm Edd}$&$\dot M_{\rm Edd}$&$r_{\rm g}$& & &$\times 10^{22}$ cm$^{-2}$& &keV &keV &keV &keV & \\
\hline
A &$4.45\pm0.21$&$0.003\pm0.001$&$0.381\pm0.028$&$27.8\pm3.1$&$4.80\pm0.52$&$0.39\pm0.08$   &$19.72\pm2.27$&$0.79\pm0.17$ &$2.04\pm0.12$&$0.91\pm0.13$&$6.71\pm0.08$&$0.17\pm0.06$&641/506 \\
B &$4.38\pm0.34$&$0.007\pm0.001$&$0.643\pm0.034$&$14.3\pm1.9$&$6.21\pm0.51$&$0.22\pm0.03$     &$2.38\pm0.15$ &$0.77\pm0.03$ &$2.50\pm0.02$&$0.11\pm0.03$&$6.78\pm0.02$&$0.19\pm0.02$&1101/704 \\
C &$4.48\pm0.52$&$0.009\pm0.002$&$0.609\pm0.022$&$9.8\pm1.2$&$3.91\pm0.42$&$0.38\pm0.11$      &$0.80\pm0.18$ &$0.89\pm0.08$ &$1.87\pm0.06$&$1.74\pm0.07$&$6.76\pm0.02$&$0.21\pm0.03$&1214/707 \\
D &$4.51\pm0.29$&$0.006\pm0.001$&$0.484\pm0.024$&$12.7\pm1.6$&$4.67\pm0.38$&$0.40\pm0.09$     &$4.13\pm0.67$ &$0.87\pm0.04$ &$2.26\pm0.15$&$0.75\pm0.10$&$6.62\pm0.15$&$0.12\pm0.19$&959/688 \\
\hline
\end{tabular} }
\end{table*}

\begin{figure*}
\centering{
\includegraphics[height=9truecm,angle=270]{Figures/x03-jetcaf-combined-NOapec-V2-eps-converted-to.pdf}
\hspace{-0.5cm}
\includegraphics[height=9truecm,angle=270]{Figures/x05-jetcaf-combined-NOapec-eps-converted-to.pdf}} \\
\centering{
\includegraphics[height=9truecm,angle=270]{Figures/x07-jetcaf-combined-NOapec-V2-eps-converted-to.pdf}
\hspace{-0.5cm}
\includegraphics[height=9truecm,angle=270]{Figures/x09-jetcaf-combined-NOapec-eps-converted-to.pdf}}
\caption {{\fontfamily{qcr}\selectfont JeTCAF}~model fitted 0.4$-$75.0 keV spectra for all four epochs of NGC\,1365 during {\it XMM-Newton} and {\it NuSTAR} era. Here, (a-d) corresponds to
epochs A to D. The different Gaussian lines are used for emission/excess at different energy range including at $\sim$6.4 keV. The model fits show the absorption line and spectral shape change in each epoch, along with a PCygni profile in the FeK band.}
\label{fig:SpecFits}
\end{figure*}

\subsection{Robustness of model parameters} \label{sec:Contour}
\autoref{fig:ConfCont} shows the confidence contours of $N_{H}$ with other {\fontfamily{qcr}\selectfont JeTCAF}\, model parameters. We have used {\it steppar} command in {\it XSPEC} to generate these plots. Different model parameters are labelled in x-axis. Three different contour colors (red, green, and blue) correspond to one, two, and three sigma confidence level. It is also the same as $\Delta \chi^2$ fit statistics of 2.3, 4.61, and 9.21. The correlation of $N_H$ with model parameters are clearly visible from the contour plots.
The uncertainty of $N_H$ fits within 0.6 dex for 2 sigma confidence level. The other parameters assess better precision. The correlations are clear, which show that there is no obvious degeneracy between parameters and the solution is robust.

The top panel shows direct correlation of $N_H$, with M$_{BH}$, $\dot m_d$, and $\dot m_h$, implies that if these parameters value increase, continuum luminosity will also increase, therefore continuum driven wind will also contain more material along the LOS. However, in the case of $X_s$ is opposite, as it anti-correlates with the disc accretion rate. In the case of R \citep[up to the strong shock condition value, which is 4; see][]{Chakrabarti1999} and $f_{col}$, increase in both the parameters, increase the luminosity contribution from the jet, therefore the wind material launching along the LOS will increase. This gives a positive correlation. We note that in the case of, $f_{col}$ the contour is not closed at its higher value side (the upper limit of the grid value for this parameter is 0.5), this can be an artefact. Our continuum driven wind launching correlation study agrees with the work by \citet[][and references therein]{GoffordEtal2015}, where authors studied (anti)correlation of continuum luminosity with different physical quantities of the wind applicable for a large sample.

\begin{figure*}[h!]
\centering{
\includegraphics[height=6.5truecm,angle=270]{Figures/A-contour-mbh-Nh-label-off-eps-converted-to.pdf}
\hspace{-1.0cm}
\includegraphics[height=6.5truecm,angle=270]{Figures/A-contour-md-Nh-label-off-eps-converted-to.pdf}
\hspace{-1.0cm}
\includegraphics[height=6.5truecm,angle=270]{Figures/A-contour-mh-Nh-label-off-eps-converted-to.pdf}}\\
\centering{
\includegraphics[height=6.5truecm,angle=270]{Figures/A-contour-xs-Nh-label-off-eps-converted-to.pdf}
\hspace{-1.0cm}
\includegraphics[height=6.5truecm,angle=270]{Figures/A-contour-R-Nh-label-off-eps-converted-to.pdf}\hspace{-1.0cm}
\includegraphics[height=6.5truecm,angle=270]{Figures/A-contour-fcol-Nh-label-off-eps-converted-to.pdf}}
\caption{Confidence contour of $N_{H}$ with different continuum model parameters for the epoch A. Three different contour colors show the confidence level of one (red), two (green), and three sigma (blue). Here, x-labels follow the parameter notations used in \autoref{table:JetcafResults}, e.g. mdotd, mdoth, and fcol represents $\dot m_d$, $\dot m_h$, and $f_{col}$ respectively.}
\label{fig:ConfCont}
\end{figure*}

As an additional test, we used photoionization simulation to predict absorption and emission line spectra for the modeled intrinsic spectral energy distributions (SEDs) shown in \autoref{fig:Incid}. The SED includes both disc (UV/optical photons), corona, and the jet component (hard X-ray) as discussed in \autoref{sec:Modelling}. In JeTCAF model, we compute the EUV photons considering the disc to be multi-temperature at each radius. At the zeroth iteration, the flux emitted from the disc is purely Keplerian \citep{Shakura1973}. These seed photons are getting upscattered by the hot corona. As the iterations go on, the interception of corona photons by the disc is taken into consideration, which modifies the original disc temperature.
In order to estimate the transmitted spectrum that an observer can measure along the LOS, we performed the numerical simulation of radiation transfer using the photoionization code {\sc cloudy}17.02 \citep{Ferland2017}. The essential parameters: the spectral energy distribution (SED), gas density $n_{\rm H}$, column density $N_{\rm H}$ are adopted in such a way that satisfies the spectral fitting from Table~\ref{table:JetcafResults}. The illuminating SEDs used in {\sc cloudy} are the {\fontfamily{qcr}\selectfont JeTCAF} ~model component from Fig.~\ref{fig:SpecFits} fitted for each epoch (excluding the other components). The gas density values $n_{\rm H}=2.65 \times 10^{10}$, $1.73 \times 10^{11}$,$1.47 \times 10^{11}$ and $1.01 \times 10^{11}$ cm$^{-3}$ are taken for the epochs A to D respectively.

Likewise, the column density values, $N_{\rm H}$= $1.97\times10^{23}$, $2.38\times10^{22}$, $0.8\times10^{22}$ and $4.13 \times 10^{22}$ cm$^{-2}$ are adopted from Column 8 of the Table~\ref{table:JetcafResults} for the epochs A to D respectively. The models are computed for the two representative cases of ionization parameter $\xi$=$10^{2}$ and $10^{3}$ erg cm s$^{-1}$ respectively. The $N_H$ and $\xi$ values fall within the range estimated in the literature \citep[][and references therein]{GoffordEtal2013,Waltonetal2014,BraitoEtal2014}. The $N_H$ values presently obtained are approximated values, as the fit does not consider ionization effects to the continuum. In all of these simulations, we considered the {\it Solar} values of the chemical composition, default in {\sc cloudy} adopted from \citet{Grevesse1998}. In order to account for the effects of micro-turbulence in absorption-emission lines, typical turbulent velocity $v_{\rm turb}=1000$ kms$^{-1}$ is used. Here we are not estimating or quantifying the turbulent velocity rather considering a typical value as a test case to generate the observed lines, however, for a detailed study for this effect we refer the work by \citet{GoffordEtal2013}. Note that, only the classical approach of one dimensional radiation transfer with plane-parallel open geometry without the inclusion of relativistic effects are considered. For the details of {\sc cloudy} applications in various AGN environments and generic definitions of parameters used, we refer the reader to the relevant literature \citep [for e.g.][]{Adhikari2015,Adhikari2019,Adhikari2019b} and cloudy documentation {\it Hazy} files\footnote{https://gitlab.nublado.org/cloudy/cloudy/-/wikis/home}.

 The transmitted spectra zoomed in the band $6-9$ keV
 are presented in the Fig.~\ref{fig:cloudy_spec}. The results from {\sc cloudy} simulations show absorption in the region around 6.4\,keV, which is similar to that seen in the observed spectra
 shown in Fig.~\ref{fig:SpecFits}. The change in the spectral shapes, reflected in the illuminating SEDs in {\sc cloudy}, during the transition from epoch A to epoch D also changes the extent of Fe absorption. For the lowest value of mass accretion rate (0.003 $\dot M_{\rm Edd}$) in epoch A, there is a considerable amount of Fe absorption, and it becomes weak as the accretion rate becomes maximum (0.009 $\dot M_{\rm Edd}$) in epoch C. This result from basic simulations in {\sc cloudy} nicely corroborates with the observed features of absorption presented in Fig.~\ref{fig:SpecFits}. However, the emission lines observed are somehow skewed or broadened by the general relativistic (GR) effects of the highly spinning source. These effects are not included in {\sc cloudy} spectra and thus several components of narrow emission lines are present in Fig.~\ref{fig:cloudy_spec}.
 We noticed that the energy at which the absorption is significant depends on the adopted value of the $\xi$ in the photoionization models. The increase in $\xi$ allows for the ionization of the Fe to higher levels and as a result significant absorption towards the higher energy bands are seen. We note that the current CLOUDY modelling is to check whether the model SEDs for a given ionization parameter and turbulent velocity can generate emission and absorption lines similar to what is observed for NGC\, 1365 or not. However, the current approach does not measure the $\xi$ parameter robustly, it requires a detailed study. We plan to address this issue with grid of photoionization simulations with variations in ionization parameter in the future work.

\begin{figure}
\centering{
\includegraphics[height=9.0truecm,trim={0.4cm, 0.9cm, 1.5cm, 2.0cm}, clip]{Figures/Jetcaf-parameters.pdf}}
\caption{Variation of {\fontfamily{qcr}\selectfont JeTCAF}~model fitted parameters with observational epochs.
}
\label{fig:FittedPars}
\end{figure}

\begin{figure}
\centering{
\includegraphics[height=4.5truecm,trim={2.0cm, 0.0cm, 0.0cm, 1.5cm}, clip]{Figures/jetcaf-correlation-NGC1365.pdf}}
\caption{$N_{\rm H}$ decreases with increasing accretion rates, and an opposite profile is observed with the geometry of the corona.
}
\label{fig:correlation}
\end{figure}

\begin{figure}
\includegraphics[height=6truecm]{Figures/Incident_seds.pdf}
\caption {The incident SEDs used in {\sc cloudy} models for the four epochs considered here. The SEDs are computed using the {\fontfamily{qcr}\selectfont JeTCAF}\,model which includes relevant physical processes in the accretion disc. The EUV flux is computed assuming the disc is emitting modified multi-color blackbody photons from each radius of the disc.}
\label{fig:Incid}
\end{figure}

\begin{figure}
\includegraphics[scale=0.6]{Figures/CL_absorption_turb1000_combined.pdf}
\caption {The simulated spectra zoomed between $6$ to $9$ keV for four different epochs using {\sc cloudy} photoionization code. The evolution of the absorption properties with the change in the disc mass accretion rates (as seen from the fitted data) are plotted in each panel. The red and blue lines correspond to $\xi=$ 100 and 1000 respectively. The micro-turbulence of $v_{\rm turb}=1000$ km s$^{-1}$ is used in the simulations for all epochs.}
\label{fig:cloudy_spec}
\end{figure}

\subsection{Failed wind scenario}
We consider here the case of the absorber is being associated with the outflowing matter. One of the most prominent outflowing region within AGNs is the broad line region (BLR), it is also one of the candidate to host intervening matter. Studies of warm absorbers (WA) observed at X-rays consider disc outflow or BLR as a source of absorption \citep[][]{Maiolino2010,Risaliti2011} or at least one of its component \citep[like NGC 5548 case described by][]{Kaastraetal2014}. Also, torus can be responsible for part of absorption \citep[Mrk 509 study by][]{Kaastraetal2012}. The expected ionization parameter value suggested here, ${\rm log}\ \xi \sim 2-3$, agrees with the values expected at the BLR position. Thus, we give here theoretical consideration of the BLR-like outflow. One of the possible outflow scenario is the failed radiatively driven outflow (FRADO) model, which clearly connects the BLR with the underlying accretion disc \citep{CzernyHryniewicz2011}.

We assume that the wind moves away from the disc with constant speed $v_{\rm w}$,
in the form of a partial thin spherical shell at a distance $R_{\rm BLR}$ from the central source, the amount of mass per unit time carried out by the wind is:
\begin{equation}
    \dot M_{\rm w}=\mu m_p N_{\rm H} v_{\rm w} R_{\rm BLR} \Omega,
\end{equation}
where, $\mu=1.4$, $m_p=1.67\times 10^{-24}$~gm, $\Omega=\pi/2$ \citep{Maiolino1995}, and
$R_{\rm BLR}$ are the mean atomic mass per proton, proton mass, typical value of the solid angle subtended by the outflow, and the radius of the BLR respectively. From our spectral fitting, we found that
$N_{\rm H}$ decreases with increasing $\dot m_{\rm d}$, follows the relation $\mathcal{N} \dot m_{\rm d}^{-\beta}$. For NGC\,1365, $\mathcal{N} \sim 1.5 \times 10^{17}$ cm$^{-2}$ and $\beta$, $2.43\pm0.15$.

To estimate the radial position of the outflowing matter we used an empirical relation based on reverberation mapping results for nearby AGNs \citep[ie.][]{Bentzetal2009} which is supported and explained by the FRADO model.
The BLR radius can be estimated from \citet{CzernyHryniewicz2011},

\begin{equation} \label{eq:rblrVsL}
    \log R_{\rm BLR}=1.538\pm0.027 + 0.5\log L_{44, 5100}
\end{equation}

where $R_{\rm BLR}$ is in light days and $L_{44,5100}$ is the monochromatic luminosity at 5100 \AA ~($\lambda L_{\lambda}$) measured in units of $10^{44}$ erg s$^{-1}$.
We can translate $L_{44,5100}$ to the bolometric luminosity using the relation
 $L_{\rm bol}=10.33 L_{\rm 5100}$ \citep{Richardsetal2006}. The $L_{\rm bol}$ is calculated using the relation $\eta \dot m_d c^2$, where, $\eta=0.1$ is considered. Our estimated values for $R_{\rm BLR}$ (in cm) using \autoref{eq:rblrVsL} are, \{$3.61\times10^{15}$, $5.47\times10^{15}$, $6.27\times10^{15}$, and $5.14\times10^{15}$\} for the epochs A to D are consistent with the literature.

As the radiation from the central region falls onto the wind,
and considering that on average each emitted photon scatters about
once before escaping to infinity, this suggests that the total
wind momentum must be of the order of the photon momentum
\citep{King2010}
can be written as
\begin{equation}
    \dot M_{\rm w} v_{\rm w} \simeq \frac{L_{\rm bol}}{c},
\end{equation}
here $c$ is the speed of light.

After solving few steps, we find the equation for the wind velocity as,

\begin{equation}
    v_{\rm w}=\frac{L_{\rm bol}^{0.5}\dot m_{\rm d}^{\beta/2}}{(\mathcal{N} c m_p R_{\rm BLR} \mu \Omega)^{1/2}}=30 \left(\frac{L_{\rm bol}\dot m_{\rm d}^\beta}{\mathcal{N} R_{\rm BLR}}\right)^{1/2} ~~\text{km}~~\text{s}^{-1} .
\end{equation}

Our estimated wind velocities for all four epochs from A to D are: 1445, 4978, 7235, and 4001 km s$^{-1}$ respectively. The estimated wind velocities fall in the range reported in earlier studies on continuum driven wind launching \citep[see][and references therein]{GoffordEtal2013,BraitoEtal2014,GoffordEtal2015}.
In epochs A and D, the velocity values are less than the wind terminal velocity attained maximum (5748 and 4839 km~~s$^{-1}$ estimated using $\sqrt{2 G M_{\rm BH}/R_{\rm BLR}}$, here, G = Gravitational constant). For the epoch B, wind velocity is comparable with its terminal velocity (4623 km~~s$^{-1}$) of the wind. This failed wind behaves as a cloud shielding the central emission. However, in epoch C wind velocity higher than the terminal velocity (4365 km~~s$^{-1}$) can help to drive the material away from the disc, therefore, much less column density was observed. A similar scenario was studied earlier for a low mass black hole binaries \citep{Milleretal2020}.

From the model fits, the high absorption; variable column density along the LOS, which we argue could be due to the
failed wind above the disc surface. The disc accretion rate was low, implies the radiative pressure was also low, therefore the
wind launched from the disc could stay in place and the matter was not pushed by the radiation to outer radii. In addition, strong ionizing radiation or outflows (which often is observed in the hard or intermediate spectral states, when accretion rate is low) from the central region of the disc itself can over ionize the wind from the disc, that can prevent the wind being driven away from the disc, therefore its velocity decreases \citep[for an extensive study in][]{Progaetal2004}. On the other hand, the failed wind BLR model suggests that the outflow velocity scales with the accretion rate. This happens because of its strong connection with the underlying accretion disc. As the dusty matter is pushed away from the disc atmosphere by the radiation from the underlying disc and later is exposed to the central radiation, which breaks its driving force or  pushes it away stronger to the outer radii \citep[][]{Naddaf-Bozena2021}. There are other physical mechanisms that can produce different emission/absorption lines in AGN environment, recently discussed in \citet[][for a review]{Lahaetal2021}.

\section{Conclusions} \label{sec:Conclusion}

In this paper, we study the changing look active galactic nucleus NGC\,1365 using accretion-ejection model including absorption and line emission in order to understand the maximum possible underlying physical processes behind this changing look
phenomenon. From our analysis, we conclude that:
\begin{itemize}
\item The accretion rates and their ratio, and the size of the dynamic corona varied significantly during the observation period.
\item The compression ratio of the shock at the boundary layer of the dynamic corona lies between 3.9 to 6.2, which is used to estimate the mass outflow rate from the dynamic corona. The maximum outflow rate estimated is $\sim 12\%$ of the inflow rate. This confirms the previous findings that the outflows are present in the system.
\item The geometry/size of the dynamic corona is also responsible for variable luminosity, that correlates with the hydrogen column density along the line of sight.
\item The accretion-ejection model fitted mass is placed within a range between $4.38\pm0.34 - 4.51\pm 0.29 \times 10^{6} M_\odot$, remarkably matches with the estimation by \citet{Onorietal2017}.
\item The presence of prominent absorption line and high hydrogen column density is due to low mass accretion rate. The low accretion rate is not able to generate enough pressure to push the matter farther out from the disc \citep[consistent with recent simulation by][]{Naddaf-Bozena2021}, therefore, it blocks the radiation coming from the inner region. This is also evidenced from the {\sc cloudy} simulations, where absorption features are stronger (at the highest $N_{\rm H}$) for the low mass accretion state. This explains the ``failed wind" scenario due to low wind velocity.
\item We studied the correlation between $N_H$ with other model fitted continuum parameters (see \autoref{sec:Contour}) and found that they are consistent with the physical picture of the model and agree with the earlier works on continuum driven wind launching \citep[][and references therein]{GoffordEtal2015}.
\item Therefore, CLAGNs can show significant variability if the accretion rate and the corona geometry change substantially.

\end{itemize}

\begin{acknowledgements}
We thank the referee for helpful comments and suggestions that improved the quality of the manuscript. SM acknowledges funding from Ramanujan Fellowship grant (\# RJF/2020/000113) by SERB-DST, Govt. of India. T. P. A gratefully  acknowledges the Inter-University Center for Astronomy and Astrophysics (IUCAA), Pune, India for providing the access to the Computational Cluster, where the numerical simulations used in this paper are performed.
This research has made use of the {\it NuSTAR} Data Analysis Software ({\sc nustardas}) jointly developed by the ASI Science Data Center (ASDC), Italy and the California Institute of Technology (Caltech), USA. This research has also made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by NASA/Goddard Space Flight Center.

\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


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text:
Lifestyle | Health and Fitness
Fitness review: HIIT group class
Pack rat
Text: Sarah Lian
Sarah Lian breaks a real sweat with this killer workout
The lowdown: Having a GuavaPass means that I get to choose from a buffet of classes offered at various gyms and studios across Singapore. This time around, I made my way to a little studio in the quaint neighbourhood of Bugis to check out another GuavaPass-partnered studio, Fitness Bravo.
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Try it out here: Fitness Bravo
Duration of session: 60 minutes
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About Sarah Lian
Sarah Lian is a fitness enthusiast who works out as much as she can to compensate for her appetite during the durian harvest. During the 10 month off-season, she believes in releasing endorphins with an active lifestyle and inspires others to do the same with the help of a GuavaPass membership. You can follow her journey on her Instagram (@imSarahLian) and her other day job on www.sarahlian.com.
Source:http://www.buro247.sg/lifestyle/health-fitness/fitness-review-power-plates-at-croyez-studio.html

redpajama_set_name: RedPajamaCommonCrawl


Below you will find a list of the department stores & malls in Roseville, CA. These 128 department stores & malls are organized by their distance from Roseville. The closest businesses to Roseville are Folsom Premium Outlets on Folsom Blvd (Folsom) and Washington Square Shopping Center on Washington Blvd (Roseville) in the category Shopping Centers & Malls, Susie's Deals on Roseville Sq (Roseville) in the category Department Stores, Catherines Roseville Square on Roseville Sq (Roseville) in the category Clothing and Big Lots on Harding Blvd (Roseville) in the category Variety Stores.


Even with the force of a "classic" behind it, remake fever can't hold up the hollowness of this style-drenched Omen.
The prophecy from the Book of Revelation provides a map to a terrifying future. The passage specifically points to the arrival of the Anti-Christ and the beginning of Armageddon. Robert Thorn, a senior American diplomat, has other things on his mind. His wife, Katherine, who had suffered two previous miscarriages, has endured yet another unsuccessful delivery, but she's unaware their newborn child has died. The hospital priest, Father Spiletto, presents Thorn with another child born that night, whose mother died in childbirth. The priest compels Thorn to take the infant boy as his own. Katherine will never know the truth. Katherine embraces the child as her own, blossoming in motherhood. Thorn's career ascends. He becomes the U.S. ambassador to Great Britain, and the family settles into an estate outside London. But certain disturbing events seem to revolve around the now five-year-old Damien. The boy's nanny hangs herself at his birthday party; a strange priest brings dire warnings to Thorn; a children's trip to the zoo results in a panicked frenzy; Damien becomes hysterical during a drive to church; and blurred movements in a series of photographs portend shocking deaths. Then tragedy strikes closer to home. It's apparent that Damien is the long-prophesized Anti-Christ. Now, Thorn must make the ultimate sacrifice to prevent the unspeakable terror that awaits the world.
A disastrously miscast remake of the 1976 horror classic, which retains the apocalyptic themes of David Seltzer's original script but renders them dull and fright-free.
This new version is an almost scene-for-scene remake, which is good news in the first half and bad news in the torpid second.
Not since Gus Van Sant inexplicably directed a shot-by-shot remake of Hitchcock's Psycho has a thriller been copied with so little point or impact.
This is one of those movies that profits from very low expectations. If you go in expecting something dreadful, be assured: It's only near dreadful.
John Moore's remake of The Omen rivals Gus Van Sant's Psycho both for its fidelity to the source material and for its utter pointlessness.
The film doesn't leave you with bad dreams. It just makes you wonder: what's the point watching this remake when DVDs of the original are at hand?
It's a highly entertaining comedy, and the best thing about it is - you don't have to watch any football.
Certainly, it's not the worst remake of all time, but it really is one of the more ridiculous, unnecessary, and gimmicky of them.
While not a shot-for-shot copy of Richard Donner's far superior 1976 original "Omen," David Seltzer --the screenwriter of both films%u2014barely updates his original script for this gratuitous remake.
Unnecessary remake of a classic, this version of Richard Donner's The Omen is almost exactly like the original horror classic. The only difference is, is that everything is up to date, style wise, technology wise and so forth. This remake is worthless, and what's surprising is the impressive cast here. Not even a cast like this can save a dull film like this. If you've seen the far superior original directed by Richard Donner, skip this film. I'm actually surprised that with the talent involved, the filmmakers couldn't create a more effective remake. Instead this is a shot for shot clone and it's boring, dull, and above all lacks any real horror because, well it's predictable. There are some remakes that are good, unfortunately this updated version of The Omen isn't one of them. The film is very much like Gus Van Sant's version of Psycho. The reason that this film is terrible is that the film doesn't do anything, besides copying the original. For what it is, this is a mediocre horror film that is somewhat entertaining, but lacks the fire of the classic. The film simply misses the mark, and this the type of film that really puts an emphasis on unoriginality. Despite the cast, this film simply lacked the fire of the original, it's exactly the same film, except it's updated for modern times. The reason the film fails is that we know right from the start what happens, and the payoff just isn't like the original film. If you do watch this, you're watching the same film, minus the original jolts that the classic Omen delivered so well.
I've not seen the original to be honest, so I can't compare them. I have to say though this was quite slow moving, more creepy than scary. The original has quite a reputation, which might be a little dated now. This just didn't deliver any scares, jumps or action for me, shame as it has a very good cast!
Didn't think it was 26% bad, but it could have been alot better. It has its fair share of good scares though.
Pointless remake which did nothing to add anything original and different except to jazz up the death scenes with a bit of blood. The 1976 original was superior in every way and not once did this remake come close to challenging it. Wasn't really scary, a few cheap frights were thrown in here and there and, like I mentioned before, a couple of the death scenes have been over-sylized which admittedly do look impressive, but it takes away any scare appeal. Marco Beltrami did a very good job with the musical score, but stil, it's not a match for Jerry Goldsmiths Oscar winning original. This one will probably be enjoyed more by people who have not seen the excellent original version.
Damien: Did I scare you, Mommy? I didn't mean to.
Father Brennan: When the Jews return to Zion, and a comet fills the sky, and the holy Roman Empire rises, then you and I must die. From the eternal sea he rises, creating armies on either shore, turning man against his brother, until man exists no more.
Katherine Thorn: Don't let him kill me.


text:
Q: How to Set Multiple Cursors in VSCode at Each Find Result Today I wanted to edit all stops in a SQL INSERT that followed a Regex pattern. I realized that if I could use the multi cursor feature in Visual Studio Code I could make a ton of changes all at one time.
For instance, in the following SQL
INSERT INTO [dbo].[Location] (key, longName, shortName, oldRegion, contactId, email, city, state, zip, isActive)
VALUES
('GEORG','Georgian College','GEORG','1A','1271','globalint@school.edu','Barrie','ON','L4M 3X9','1'),
('LOYAL','Loyalist College','LOYAL','2A','1271','globalint@school.edu','Belleville','ON','K8N 5B9','0')
-- etc.

the contactId and isActive weren't really varchars, and I could find them with a regex of '\d+', but I couldn't figure out how to set the cursors to each spot with keyboard commands or shortcuts. How would you do this?

A: How to Place Multiple Cursors at the End of All Your RegEx Finds
ALT + ENTER is what you're after (Thanks to Mark).
To find this or similar keybindings open the Keyboard Shortcuts and search for findWidget for commands used with CTRL + F, or searchViewlet for commands used with CTRL + SHIFT + F.
These keybinding are useful for both VSCode and Azure Data Studio and can be customized.
Full Example for Your Case
For your example, you could do this through the following keyboard commands:

*

*CTRL + F (Find)

*ALT + R (toggleFindRegex command)

*'\d+' (what to look for)

*ALT + ENTER (add cursors; editor.action.selectAllMatches command)

-OR-

*CTRL + SHIFT + L (add cursors; editor.action.selectHighlights command)

*ESC (closeFindWidget command)

Now the following text should have four blinking cursors (at the daggers ), where you can edit to your s content!
INSERT INTO [dbo].[Location] (key, longName, shortName, oldRegion, contactId, email, city, state, zip, isActive)
VALUES
('GEORG','Georgian College','GEORG','1A','1271','globalint@school.edu','Barrie','ON','L4M 3X9','1'),
('LOYAL','Loyalist College','LOYAL','2A','1271','globalint@school.edu','Belleville','ON','K8N 5B9','0')
-- etc.


text:
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redpajama_set_name: RedPajamaGithub


Though we are small the CF community is showing itself to be mighty!
When Chester was diagnosed and I became a CF mum, I became part of a much bigger family, a family of strangers forged together by a common enemy, Cystic Fibrosis.
We are a family that for the most will never meet and our children will never play together. We may be a relatively small community in the scheme of things, but this does not deter us, though we may be small we are proving to have a huge voice!
As a family we know the highs and lows, we live them too, we know the heartbreak and sadness that each of us has gone through and continue to go through daily. We know the pain, the torment and the guilt, we've probably all felt it at one time or another.
We are there for each other no matter what the time of day or night, we standby each other ready to pick up those who fall, with kind words, optimism and advice, always virtual counsellor ready at the press of a key. We are there for each other when our children are sick, to offer comfort, sometimes in the darkest of hours and we are there to rejoice in others good fortune, because that's what this family does!
We have determination like no other, taking on challenge after challenge in our children's names, finding strength each time to continue because we know our children have no choice than to get on with it. We dig deep to find the strength to take on the biggest of battles and we have the will, to want, to win and we do all this side by side, together every step of the way.
This community has been waiting for something special, for something to change CF, some have already waited too long already, so to be told that something is "Too expensive" and "Not cost effective" just isn't going to work, you won't be surprised to hear that we aren't prepared to take that as an answer.
We have united in our fight for access to Orkambi, and we won't rest until the negotiations start and a deal is struck, we are shouting louder than we ever have before and we are going to be heard!
Seeing this amazing team ethos and concerted effort by all those affected by CF and their friends and families has made me proud to be a CF mum and has restored my faith in humankind, that even when people are at their busiest in life, they can take two minutes out of their day to support our quest to get Orkambi for our children.
Like Chester there are many people in the CF community that possibly won't benefit from Orkambi, but to us that doesn't matter, we are family and we fight for all our children, one in all in!
It's a fact that Orkambi is been proven to slow lung function decline and reduce exacerbations and is the first drug to actually treat the root cause of CF instead of treating the symptoms, this is a huge breakthrough and has bought much hope for people throughout this family. It's approval also paves the way for future pipeline deals for other medications compatible for other mutations which essentially means one day Chester could get his cure.
All we want is for our children to get what they need, they didn't ask for CF and fighting for them is all we can do. These beautiful children deserve to live their lives free from hospital admissions and from hours of physiotherapy and they sure as hell deserve to be heard and we will make sure they are!
Becoming a CF mum was never my choice, given the option I would never want to be a CF mum, but I am and for now I can't change that.
One thing is for sure, that for a condition that can at times be isolating and lonely, I've never felt so surrounded by such wonderful people.
To me, diagnosis day and hospital admissions aside, this period has to be one of the most testing for me as the parent of a small child with CF, not only does he want to eat everything in sight except what I actually make for him (which I guess isn't all bad) but I find he is now much more independent, headstrong and a lot more mobile, I am forever moving things higher out of reach, a change from my first child who must have just been incredibly lazy because he hardly moved.
I don't doubt I am dealing with all the same problems any other parent would face, from the toddler tantrums, watching my once quiet and reserved baby boy become almost monster like, throwing himself around on the floor screaming in a rage, this coupled with the fact he has quite recently learned to say "No" mean I am hearing "No" pretty much all the time.
The typical food games toddlers like to play have started, refusing to eat anything I put in front of him, with a shake of his head he pushes every meal away. Now in an ideal world I would not be quite so pushy, but having lost a large amount of weight recently, I know how important it is to put some fat back on him. I find myself going back to the old tricks of adding cream, butter and cheese to everything I possibly can in the hope he eats something, even just a little. I even find myself buying him a cheeky McDonalds when his older brother isn't around and desperately trying to fill him up on fast food snacks before going to clinic to be weighed just to be able to add a few grams on.
Despite refusing my culinary delights, I often find that while my back is turned he has raided the fridge and can often be found in the front room with the odd block of butter or a chocolate bar he has stolen. I know to most this would be of concern, however, I find myself looking to see just how much butter or chocolate he has eaten, feeling slight nauseous at the thought of him chewing on butter like he would a choc ice and a little worried about working out how much Creon I should give him.
Luckily this time I caught him before he ate it!
Talking about Creon, anyone know how many Creon you need for a worm and some additional soil? No, me neither! This is why Chester is not left unsupervised in the garden……ever!
As we all know, physical activities are fantastic for people with CF but I am beginning to wonder if all the activities he takes part in, such as bouncing on his trampoline, running games and "play fighting" with his brother have given him extra strength, I swear he's almost superhuman, it never ceases to amaze me how physically strong this boy is. Which is fantastic until it comes to him becoming the toddler that doesn't want to go where you are going.
The majority of outings end the same way, me carrying a screaming toddler under one arm. He has simply taken to lying down on the floor and refusing to move. Let's face it, any CF parent's worst nightmare right there, all I can think about are the germs on the floor, never quite knowing who or what has trodden that path before. But any parent of a toddler or older will know how difficult it is trying to pick up a child that has started lifting up their arms to make getting a grip on them impossible and with having mastered making himself extra heavy it just adds to the embarrassment of being a fully grown adult, physically incapable of lifting up the little person on the floor.
Just a few of our wonderful trips out!
Then with CF comes the pill taking, and refusal to do so. I find everything becomes this game of "How many times in one day can I say No?" and to be honest, I have lost count by the end of breakfast most days. Up until Christmas Chester couldn't say a single word, Christmas day started with Mamma, which was music to my ears, but soon overshadowed by him saying No to everything.
Anyway I digress; Chester has around 30 tablets a day, vitamins, antibiotics, antacids and enzymes, all with their specific purpose, the majority he has to take with food. But being this power crazy, stubborn little being, on occasions he doesn't want to, so I find myself using the good old trick of parent bribery, and this see's Chester looking smug in the knowledge that he will get that milkybar dessert after his dinner because it is already on the table!
My mother in law often says she thinks Chester has been on this earth before because he just seems to know, and I am starting to think she is on to something. Needless to say, Chester takes his tablets and will have at least one high fat mouthful of food which is a win for me, even though the smug toddler thinks he has won!
So with toddlers comes potty training, what a delight! After "Poogate" last week which saw Chester trying to change his own dirty nappy, by smearing poo all over the floor, his teddy bears, his bed and in around 15 nappies which he had used to try and clean it up, I can't say I am looking forward to this stage. We have still yet to get his movements to an acceptable level per day, and he currently goes to the toilet, a lot, and although he is showing signs of wanting to use the toilet. This area of parenting is the one I am dreading the most, especially with a beige carpet, let's just say it won't be little nuggets of poop we are cleaning up!
To me, CF is just a part of who Chester is, I wouldn't say I have come to terms with it, because I don't think I ever will, and whilst CF throws other factors into things we do, and sometimes shapes how we deal with things, I am keen to remember CF or not, he is a toddler first and I have to try and step back and let him learn for himself.
New Year, blank page, same CF.
As the year ends and the blank pages of the story book for this year opens, I find myself full of mixed emotions, for most it's a fresh start, for me, it's still the same CF. That said, I feel that glimmer of hope that this could be the year technological advances take us one step closer to finally being able to say our child used to have CF. Sadly I find it somewhat overshadowed by a deep sadness that has come from seeing far too many little ones pass away this past year, their fight cut short too soon and the feeling of helplessness at the apparent lack of progress to get them the precision medications they need.
I struggle when I think about the heartbreaking pain and the sadness of the parents who have lost their beautiful children and I cannot begin to comprehend the grief they face now. I only know the awful pain I feel in my dreams when CF takes over causing tragedy in my sleep, a reoccurring nightmare I have and even though only a dream it often feels too real, waking me up in tears and an awful sickly feeling.
I have spent the past few weeks struggling with a heavy mood often deep in thought about CF, something which hasn't happened to me in a long time and something I find myself incredibly uncomfortable with. I found I was withdrawing from all CF related conversations because I felt I just couldn't cope talking or hearing about it. I just tried to focus on the here and now, and get into the Christmas Spirit.
I began thinking about how CF affects so much, I sat watching a mother feeding her beautiful new baby without a thought for things like creon or having to rush home to fit in Physio and treatments, thinking about all the things my children miss out on because of CF. For the first time in a long time I couldn't help but think about what my life would be like without CF in it.
I was becoming so negative in my own thoughts that I knew I had to snap out of it and I started to turn it around to try and think about some of the positive things I have found since having CF in my life.
Let's face it, no one wants CF in their life, but we have it and there's no changing that right now and when I actually snapped out of my mood I realised having CF in my life has taught me a great deal of positive things.
CF has taught me about strength, not only a strength in myself I never knew I had but also the huge strength in those around me, more often than not, small children. People with CF have this incredible ability to see the positive in everything, they are so incredibly resilient and I have come to realise that I have often been inspired by these amazing people that whilst fighting their own private battle are always there for each other sharing their highs and lows, picking each other up when they are down.
Having CF in my life has taught me to come to terms with the fact that it's not possible to remain strong all the time and crying, getting angry and feeling down is perfectly normal and definitely allowed, that to be strong you will often get knocked back with difficult times, but with each time being able to reappear stronger and more knowledgeable than before.
If I didn't have CF in my life I wouldn't have the appreciation for time like I do now. Time is incredibly precious, CF or not, no one ever knows how long they have, so I have learned to make the most of what time we do have, doing all the things we want to do, enjoying every moment whilst making lifelong memories.
Without CF I would never know the kindness and humility I have seen from the wonderful CF community I have become part of, the people who drop everything for those in the same situation, each parent going through their own individual heartache but always there no matter what, with words of kindness and wisdom.
I have seen kindness and thoughtfulness from parents have lost their own children and even in their own immense grief, it doesn't stop them from carrying out acts of kindness for others. I will never stop being amazed at the kindness and generosity of this wonderfully selfless community.
So whilst I hate CF and have moments where everything feels so miserable and heavy, I have to look at all the positives it has bought to my life, I have a beautiful little boy who is fighting hard and probably wouldn't be the boy he is without CF and I can honestly say that without CF in my life I wouldn't be the person you see today.