text:
\section{Introduction} \label{sec:intro}
With the development of instruments and observing techniques, exoplanet science is one of the fastest developing sciences in astronomy. As more and more exoplanets are discovered, studying the detailed properties of individual exoplanets is just as important and popular as discovering more exoplanets.
For example, characterization of an exoplanet's atmosphere is vital for understanding the interior and global properties of a planet.
There are more and more studies about the atmospheres of gaseous giant planets. However, due to the lower transit depth, the atmospheres of terrestrial planets are more difficult to detect using transmission spectra than those of gas giant planets. Thus,  atmospheric studies of small rocky planets orbiting nearby bright stars are still pretty rare.

The primary atmosphere of a terrestrial planet may have been removed or replaced by a secondary atmosphere with a higher mean molecular weight \citep{2019ARA&A..57..617M}, which makes it much harder to trace where the planet was born.
During the process of establishing a secondary atmosphere, a variety of related physical and chemical processes can provide us with the opportunity to detect bio-signatures on possible habitable planets.

For now, there are only a few tentative studies about the  atmospheres of small planets using spectral data from the Hubble Space Telescope (HST)/Wide Field Camera 3 (WFC3). Some of these studies are summarized as below.
The highly irradiated super-Earth, 55 Cancri e, was found to have hydrogen cyanide (HCN, \citealt{2016ApJ...820...99T}) in its atmosphere.
TRAPPIST-1 b and c, two Earth-sized terrestrial planets discovered in
\citet{2016Natur.537...69D}, do not have a cloud-free hydrogen-dominated atmosphere.
There are no obvious absorption features in the transmission spectra of GJ 1214b ($\rm T_{eq}$ = 596 K, R = 2.742 $\rm R_\oplus$, \citealt{2021arXiv210714732C},) and HD 97658b ($\rm T_{eq}$ = 751 K, R = 2.12 $\rm R_\oplus$, \citealt{2021AJ....162..118E}), may have a cloudy atmosphere containing molecules heavier than hydrogen\citep{2014Natur.505...69K, 2014ApJ...794..155K}.
Water vapor discoveries have been reported in the atmosphere of two habitable zone super-Earths, LHS 1140 b ($\rm T_{eq}$ = 235 K, R = 1.7 $\rm R_\oplus$) and K2-18 b ($\rm M_p$ = 7.96 $\pm$ 1.91 $\rm M_\oplus$, $\rm R_p$ = 2.279 $\pm$ 0.0026 $\rm R_\oplus$) \citep{2021AJ....161...44E, 2019NatAs...3.1086T}.
However, the exact nature of the atmospheres of some of these exoplanets mentioned above is still highly debated \citep[for example]{zhang21}.
With some upcoming astronomical observing facilities (e.g., JWST and Ariel), more constraints will be put on the atmospheric properties of terrestrial exoplanets.

L~98-59 is a nearby (10.6 pc) bright (K = 7.1 mag) M3 dwarf star. Three terrestrial exoplanets have been discovered by the Transiting Exoplanet Survey Satellite (TESS) orbiting L~98-59, with a radius ranging from 0.8 to 1.6 $\rm R_\oplus$ \citep{2019AJ....158...32K, 2019A&A...629A.111C}. Their orbital periods are very short, ranging from 2.25 to 7.45 days.
As the innermost one in this multi-planet system, L~98-59~b has the lowest-mass by far measured for any exoplanet using the radial velocity technique \citep{2021A&A...653A..41D}.
\citet{2021AJ....162..169P} have evaluated the detectability of  molecular features in the planetary atmosphere with HST and JWST using simulated transmission spectra.

Here we present an atmospheric study of L~98-59~b by analyzing the transmission spectral data obtained with the G141 grism of HST/WFC3. The outline of this study is as follows. We first describe the raw data reduction process using the Iraclis pipeline in Sec~\ref{sec:analysis} and how we retrieve the atmospheric properties of L~98-59~b using the TauRex code in Sec~\ref{sec:retrieve}. Then in Sec~\ref{sec:results}, we present our main analysis results and discussion. Finally, we give our conclusion in Sec~\ref{sec:conclusion}.

\section{Data Reduction Analysis} \label{sec:analysis}

The spatially scanned transiting observations of L~98-59~b taken between February 9th, 2020 and Feb 24th, 2021 using the HST/WFC3 G141 infrared grism (1.088 - 1.68 $\mu m$), are downloaded from the public Mikulski Archive for Space Telescopes (HST proposal 15856, PI: Thomas Barclay).

There were a total of five transits observed for L 98-59 b during that period.
The observations were acquired using the 512 $\times$ 512 sub-array and the SPARS25 sample sequence with an exposure time of 69.62~s. With a scan rate of 0.496~$''$/$s$, the total scan length was 37.919~$''$.

We reduce these transit data using Iraclis, an open source pipeline designed and validated for the reduction of HST/WFC3 spatially scanning data (\citealp{2016ApJ...832..202T, 2016ApJ...820...99T} ) and available at GitHub\footnote{\url{https://github.com/ucl-exoplanets/Iraclis}}.
The following steps were used for the reduction of the raw spectroscopic data with Iraclis: zero-read subtraction, reference pixel correction, non-linearity correction, dark current subtraction, gain conversion, sky background subtraction, calibration, flat-field correction, bad pixels, and cosmic-ray correction. Please see \citet{2016ApJ...832..202T, 2016ApJ...820...99T, 2018AJ....155..156T} for more details regarding these reduction steps.

Then we extract the white and spectral light curves from the reduced spectroscopic data. The extraction region and extracted 1D spectrum are presented in Figure~\ref{extraction}. The specific geometric distortions of the spectroscopic images caused by the motion of the instrument in the scanning mode were taken into account. The position shifts are shown in Figure~\ref{diagnostics}.
In our analysis, we exclude the first orbit of each transit visit because of a stronger wavelength-dependent ramp. The limb-darkening coefficients are calculated from a non-linear limb-darkening model \citep{2000A&A...363.1081C} using the stellar parameters of L~98-59 and the Phoenix stellar model \citep{2018A&A...618A..20C}.
The stellar parameters used in the light curve fitting are taken from \citet{2021A&A...653A..41D} and are listed in Table~\ref{parameters}. We present the limb-darkening coefficients in Table~\ref{spectrum}.

\begin{figure}
\gridline{\fig{zl_forward_extraction_aperture.pdf}{0.5\textwidth}{(a)}}
\gridline{\fig{zl_forward_stellar_spectrum.pdf}{0.5\textwidth}{(b)}}
\caption{(a) The detector image of forward scan in the first visit. The zeroth order and first order can be seen, from which we extract the spectrum . Flux in the white region is estimated. The region in the white square is photometric aperture.
(b) Extracted 1D spectrum using Iraclis.}
\label{extraction}
\end{figure}

\begin{figure}
\gridline{\fig{zl_diagnostics.pdf}{0.5\textwidth}{}}
\caption{Vertical ($\Delta y$) and horizontal ($\Delta x$) shifts for each image relative to the first one, the sky ratio and raw flux of each image in the visit. Black: forward scan. Red: reverse scan. Here we take the first visit for example.}
\label{diagnostics}
\end{figure}

\begin{table}[t]
\centering
\caption{Parameters of L~98-59~b taken from \citet{2021A&A...653A..41D}, which are applied in Iraclis and TauRex.} \label{parameters}
\begin{threeparttable}
\resizebox{0.5\textwidth}{!}{
\begin{tabular}[b]{cc}
\hline\hline
\multicolumn{2}{c}{Stellar Parameters}\\
\hline
 $\rm [Fe/H](dex)$  & -0.46 $\pm$ 0.26\\
 $\rm T_{eff}(K)$ & 3415 $\pm$ 135\\
 $\rm M_*(M_{\odot})$ & 0.273 $\pm$ 0.030\\
 $\rm R_*(R_\odot)$ & 0.303 $^{+0.026}_{-0.023}$\\
 $\rm log(g_*)(cgs)$ & 4.86 $\pm$ 0.13\\
\hline\hline
\multicolumn{2}{c}{Planetary  Parameters}\\
\hline
$\rm T_{eq}(K)$ & 627 $^{+33}_{-36}$ \\
$\rm M_p(M_\oplus)$ & 0.40 $^{+0.16}_{-0.15}$\\
$\rm R_p(R_\oplus)$ & 0.85 $^{+0.061}_{-0.047}$\\
\hline\hline
\multicolumn{2}{c}{Transit  Parameters}\\
\hline
$\rm T_0(BJD)$ & 2458366.17067 $^{+0.00036}_{-0.00033}$ \\
$\rm P(days)$ & 2.2531136 $^{+0.0000012}_{-0.0000015}$\\
$\rm R_p/R_*$ & 0.02512 $^{+0.00072}_{-0.00064}$ \\
$\rm a(AU)$ & 0.02191 $^{+0.00080}_{-0.00084}$ \\
$\rm a/R_*$ & 15.0 $^{+1.4}_{-1.0}$ \\
$\rm i(deg)$ & 87.71 $^{+1.16}_{-0.44}$ \\
\hline
\hline
\end{tabular}}
\end{threeparttable}
\end{table}

\begin{table*}
\centering
\caption{The transit depths in different wavelength bins. \label{spectrum}}
\begin{threeparttable}
\resizebox{\textwidth}{!}{
\begin{tabular}[b]{cccccccc}
\hline
\multicolumn{8}{c}{\multirow{2}*{$(R_p/R_*)^2 (ppm)$}} \\
& & & & & & &\\
\hline
$\lambda_1$ ($\mu m$) & $\lambda_2$ ($\mu m$) & Visit 1 & Visit 2 & Visit 3 & Visit 4 & Visit 5 & Weighted Average \\
\hline
1.1153&1.1372&645.25 $\pm$ 58&595.33 $\pm$ 53&709.06 $\pm$ 56&598.0 $\pm$ 47&684.51 $\pm$ 51&646.25 $\pm$ 22\\
1.1372&1.1583&679.39 $\pm$ 45&624.83 $\pm$ 41&689.21 $\pm$ 37&548.58 $\pm$ 46&567.37 $\pm$ 45&633.52 $\pm$ 22\\
1.1583&1.1789&751.43 $\pm$ 44&689.85 $\pm$ 44&688.7 $\pm$ 40&642.95 $\pm$ 40&627.01 $\pm$ 47&681.32 $\pm$ 22\\
1.1789&1.1987&658.37 $\pm$ 50&680.27 $\pm$ 45&724.22 $\pm$ 38&613.01 $\pm$ 41&743.39 $\pm$ 44&683.09 $\pm$ 22\\
1.1987&1.2180&683.83 $\pm$ 43&646.41 $\pm$ 44&718.05 $\pm$ 44&694.1 $\pm$ 39&739.68 $\pm$ 48&695.87 $\pm$ 22\\
1.2180&1.2370&677.88 $\pm$ 41&608.73 $\pm$ 41&731.76 $\pm$ 40&731.5 $\pm$ 40&581.93 $\pm$ 44&669.70 $\pm$ 22\\
1.2370&1.2559&629.98 $\pm$ 42&650.36 $\pm$ 44&643.78 $\pm$ 35&662.38 $\pm$ 46&761.4 $\pm$ 37&672.26 $\pm$ 22\\
1.2559&1.2751&665.05 $\pm$ 37&588.46 $\pm$ 43&674.44 $\pm$ 40&720.14 $\pm$ 34&699.16 $\pm$ 54&671.20 $\pm$ 22\\
1.2751&1.2944&765.4 $\pm$ 41&627.03 $\pm$ 39&668.02 $\pm$ 39&732.07 $\pm$ 42&694.81 $\pm$ 43&691.18 $\pm$ 22\\
1.2944&1.3132&651.22 $\pm$ 38&610.17 $\pm$ 38&689.57 $\pm$ 38&660.51 $\pm$ 41&762.37 $\pm$ 46&667.14 $\pm$ 22\\
1.3132&1.3320&688.28 $\pm$ 38&598.81 $\pm$ 45&737.05 $\pm$ 41&685.85 $\pm$ 45&724.01 $\pm$ 41&684.70 $\pm$ 22\\
1.3320&1.3509&672.42 $\pm$ 40&615.58 $\pm$ 37&705.26 $\pm$ 43&613.21 $\pm$ 41&712.07 $\pm$ 41&665.02 $\pm$ 22\\
1.3509&1.3701&662.96 $\pm$ 49&578.78 $\pm$ 43&703.64 $\pm$ 41&713.9 $\pm$ 46&707.76 $\pm$ 47&675.52 $\pm$ 22\\
1.3701&1.3900&686.03 $\pm$ 40&566.08 $\pm$ 38&748.49 $\pm$ 35&713.52 $\pm$ 41&705.19 $\pm$ 53&680.49 $\pm$ 22\\
1.3900&1.4100&714.95 $\pm$ 38&625.51 $\pm$ 44&738.81 $\pm$ 38&648.56 $\pm$ 37&741.06 $\pm$ 40&697.93 $\pm$ 22\\
1.4100&1.4303&677.26 $\pm$ 44&650.65 $\pm$ 44&775.89 $\pm$ 33&676.22 $\pm$ 39&735.16 $\pm$ 40&712.00 $\pm$ 22\\
1.4303&1.4509&624.61 $\pm$ 43&679.29 $\pm$ 38&686.32 $\pm$ 33&652.23 $\pm$ 30&681.06 $\pm$ 41&668.31 $\pm$ 22\\
1.4509&1.4721&718.08 $\pm$ 40&657.39 $\pm$ 44&674.02 $\pm$ 39&650.47 $\pm$ 39&728.44 $\pm$ 51&685.98 $\pm$ 22\\
1.4721&1.4941&702.75 $\pm$ 39&652.01 $\pm$ 39&740.52 $\pm$ 34&659.62 $\pm$ 35&672.29 $\pm$ 41&689.61 $\pm$ 22\\
1.4941&1.5165&640.03 $\pm$ 42&642.43 $\pm$ 46&754.34 $\pm$ 34&596.47 $\pm$ 40&705.65 $\pm$ 43&675.71 $\pm$ 22\\
1.5165&1.5395&703.8 $\pm$ 40&734.88 $\pm$ 48&740.23 $\pm$ 39&602.52 $\pm$ 33&680.89 $\pm$ 42&681.45 $\pm$ 22\\
1.5395&1.5636&704.98 $\pm$ 37&797.13 $\pm$ 44&710.15 $\pm$ 36&704.32 $\pm$ 35&710.06 $\pm$ 49&718.87 $\pm$ 22\\
1.5636&1.5889&735.58 $\pm$ 37&693.72 $\pm$ 41&747.85 $\pm$ 39&744.42 $\pm$ 43&680.77 $\pm$ 40&720.09 $\pm$ 22\\
1.5889&1.6153&628.66 $\pm$ 38&630.33 $\pm$ 34&710.26 $\pm$ 34&621.54 $\pm$ 34&624.5 $\pm$ 42&646.05 $\pm$ 22\\
1.6153&1.6436&632.81 $\pm$ 35&623.13 $\pm$ 36&675.7 $\pm$ 38&642.63 $\pm$ 34&686.16 $\pm$ 48&650.16 $\pm$ 22\\
\hline
\end{tabular}}
\end{threeparttable}
\end{table*}

When fitting the white light curves with a transit model, we set the mid-transit time and the ratio between the planet radius and the host star radius as free parameters, while other stellar, planetary, and orbital parameters are fixed. In the second observation, we exclude two defect points with large deviations from the whole. In panels a and b of Figure~\ref{lcs_iraclis}, we present the white light curves together with the best fitting model and residuals for the 5 transit visits.
Then we fitted spectral light curves with a fixed mid-transit time derived from white light curve fitting and set the planet and stellar radius ratio as free parameters. The spectral light curve fits are shown in Figure~\ref{all_fitting}, where an offset has been applied for clarity.

\begin{figure*}
\gridline{\fig{zl_all_fitting_b_visit1.pdf}{1.0\textwidth}{}}
\caption{Spectral light curves for the transmission spectra. Left panel: the detrended spectral light curves with best-fit model
plotted. The right panel reveals the residuals. For each spectra, we present the values of $\sigma$, chi-square ($\chi^2$) and the
AC.}
\label{all_fitting}
\end{figure*}

The spectra of 5 individual visits and the final combined spectrum are shown in the right panel of Figure~\ref{lcs_iraclis}.
The final combined transmission spectrum was obtained by calculating a weighted average of five transits spectra. Before combining the five visits into a weighted-average spectrum, we checked that the fitted transit depths in each bin are drawn from the same distribution and there are no significant outliers.
Compared with the combined spectrum, most of the data points from individual visits demonstrate $<2\sigma$ spread. And removing the outlying visit data in these spectrum bins has no appreciable effect on the final spectrum. We therefore keep all five visits when calculating the average transit depth for each wavelength bin.
The final measurement uncertainty across the WFC3/G141 bandpass was estimated by calculating the standard deviation of the residuals when subtracting the combined spectrum from spectrum of individual visit, which is $\sim$22~ppm. Therefore, we will take 22~ppm as the precision of the final combined transmission spectrum in our remaining analysis.

\begin{figure*}
\includegraphics[width=1.0\textwidth]{zl_lc_spectrum_all.pdf}
\caption{The panels (a) and (b) show the white light curves and residuals for best-fit models of 5 individual transit observations, respectively. Panel (c): transmission spectrum collected from each visit (colored data points) and the final combined transmission spectrum (black data points). Panel (d): uncertainty of each data point. Panel (e): deviation from the weighted-average spectrum, in unit of sigma, for each data point. }
\label{lcs_iraclis}
\end{figure*}

\section{Atmospheric Modeling} \label{sec:retrieve}

To retrieve the atmospheric parameters of L~98-59~b, we use the most recent version of the public available code  TauRex3\footnote{\url{https://github.com/ucl-exoplanets/TauREx3_public}} \citep{2021ApJ...917...37A, 2015ApJ...813...13W, 2015ApJ...802..107W} . Based on a Bayesian atmospheric retrieval framework, TauRex3 maps the parameter space of a planetary atmospheric model and finds the best fit to the observed spectrum using the nested sampling code MultiNest \citep{2014A&A...564A.125B}.
For our analysis, we set the live points number to 1500 and the tolerance evidence to 0.5 in the retrieval code.
Due to the narrow wavelength coverage of our observed data, we typically only probe a very restricted range of the planet's temperature–pressure profile.
Here we adopted a planetary atmosphere model with an isothermal temperature-pressure profile, a constant molecular abundance at each layer of the atmosphere, and 100 plane-parallel layers with pressure ranging from $10^{-3}$ to $10^7$~Pa. We select two uniform priors, 0.6~$\rm T_{eq}$ to 1.6~$\rm T_{eq}$ for planet temperature and 0.5~$R_p$ to 1.5~$R_p$ for planet radius, where $\rm T_{eq}=627~K$ is the planet's equilibrium temperature.

For the opacity sources, we initially assume the atmosphere is dominated by H$_2$ and $\rm He$ with the ratio fixed to $\rm He/H_2=0.17$.
Then, to model the transmission spectrum, we introduce additional active trace-gases, including $\rm HCN$ \citep{2014MNRAS.437.1828B}, $\rm CH_4$ \citep{2014MNRAS.440.1649Y}, $\rm NH_3$ \citep{2019MNRAS.490.4638C}, $\rm CO$ \citep{2015ApJS..216...15L}, $\rm CO_2$ \citep{2010JQSRT.111.2139R}, $\rm H_2O$ \citep{2018MNRAS.480.2597P}, $\rm TiO$ \citep{2019MNRAS.488.2836M}, and $\rm VO$ \citep{2016MNRAS.463..771M}. The line lists are taken from ExoMol \citep{2016JMoSp.327...73T,2021A&A...646A..21C}, HITEMP \citep{2010JQSRT.111.2139R} and HITRAN \citep{1987ApOpt..26.4058R}.
All of our models include collision-induced absorption (CIA) of $\rm H_2$-$\rm H_2$ \citep{doi:10.1021/jp109441f,2018ApJS..235...24F} and $\rm H_2$-$\rm He$ \citep{doi:10.1063/1.3676405}, Rayleigh scattering.
Clouds are modeled as gray clouds \citep{2013ApJ...778...97L}, with the cloud top pressure ranging from $10^{-2}$ to $10^7$~Pa.
$\rm  N_2$ is an inactive gas in the atmosphere over the HST/WFC3 spectral wavelength range, which only contributes to the mean molecular weight.
Thus, to evaluate whether L~98-59~b can have a heavy secondary atmosphere \citep{2021AJ....161..284M}, we will add $\rm  N_2$ \citep{2018JQSRT.219..127W} to some of the atmospheric models later.

We run two initial retrievals aiming at identifying the most likely trace gases, one in which the trace-gas abundance is set to vary from $10^{-12}$ to $10^{-1}$ in volume mixing ratios (VMR), and the other one from $10^{-12}$ to 1. This will allow a larger degree of freedom when exploring the parameter space of active trace gases abundances.
Based on the results of two initial fittings, HCN is the only actively absorbing molecule that emerges. Therefore, we choose to evaluate five atmospheric models in our second round of retrieval in Sec~\ref{sec:results}, four with HCN and one without HCN: a cloud-free atmosphere containing only HCN (model 1), a cloud-free atmosphere containing HCN and $\rm N_2$ (model 2), an atmosphere containing clouds and HCN (model 3), an atmosphere containing clouds, HCN and $\rm N_2$ (model 4), and a pure cloudy atmosphere (model 5).

\section{Results and Discussion} \label{sec:results}

\begin{table*}
\centering
\caption{Statistical values of different models: Bayesian evidences, $\chi^2$, ADI and Sigma. }
\label{retrieval_results}
\begin{threeparttable}
\resizebox{\textwidth}{!}{
\begin{tabular}[b]{lllllll}
\hline
&&&&&\\
&&HST&&&\\
&&&&&\\
\hline
model & descriptions & VMR priors & $\rm log_{10}$(E) & $\chi^2$ & ADI & Sigma\\
\hline
model 1 & HCN & $10^{-12}$ $\sim$ 1 & 227.025 $\pm$ 0.071 & 18.583 & - & -\\
\hline
model 2 & HCN+$\rm N_2$ & $10^{-12}$ $\sim$ 1 & 227.925 $\pm$ 0.068 & 16.628 & - & -\\
\hline
model 3 & clouds+HCN & $10^{-12}$ $\sim$ 1 & 229.563 $\pm$ 0.065 & 14.028 & 1.023 & 2.04$\sigma$\\
\hline
model 4 & clouds+HCN+$\rm N_2$ & $10^{-12}$ $\sim$ 1 & 229.740 $\pm$ 0.064 & 14.025 & 1.2 & 2.14$\sigma$\\
\hline
model 5 & clouds & - & 228.540 $\pm$ 0.055 & 24.131 & - & -\\
\hline
\hline
&&&&&\\
&&HST+TESS&&&\\
&&&&&\\
\hline
model 4 & clouds+HCN+$\rm N_2$ & $10^{-12}$ $\sim$ 1 &  238.019 $\pm$ 0.064 & 14.345 & 1.031 & 2.04 $\sigma$\\
\hline
model 5 & clouds & - & 236.988 $\pm$ 0.055 & 24.318 & - & -\\
\hline
\hline
\end{tabular}}
\end{threeparttable}
\end{table*}

\begin{table*}
\centering
\caption{The best fit model parameters of different models.}
\label{retrieval_parameters}
\begin{threeparttable}
\resizebox{\textwidth}{!}{
\begin{tabular}[b]{llllllll}
\hline
model & descriptions & VMR priors & $\rm R_p (R_{Jup})$ & $\rm T_{equ} (K)$ & log(P)(Pa) & $\rm \mu$ (amu)\\
\hline
model 4 & clouds+HCN+$\rm N_2$ & $10^{-12}$ $\sim$ 1 & 0.06$^{+0.01}_{-0.01}$ & 593.70$^{+199.8}_{-153.92}$ & 2.02$^{+1.76}_{-1.08}$ & 11.68$^{+9.21}_{-6.04}$\\
\hline
model 5 & clouds & - & 0.06$^{+0.01}_{-0.01}$ & 441.55$^{+97.94}_{-62.51}$ & 4.87$^{+1.45}_{-1.31}$ & 2.30$^{+0.00}_{-0.00}$\\
\hline
\hline
\end{tabular}}
\end{threeparttable}
\end{table*}

To evaluate the goodness of fitting and detection significance of an atmospheric model, we use $\chi^2$ value, Bayesian evidence, and the atmospheric detectability index \citep[ADI][]{2018AJ....155..156T}, which are summarized in Table~\ref{retrieval_results}.
The ADI is a positively defined Bayes factor \citep{doi:10.1080/01621459.1995.10476572} between models with active trace molecules and a pure cloudy model, where a value of greater than 3 means a significant detection.
Table~\ref{retrieval_results} also includes the n-$\sigma$ values, where 3.0$\sigma$ indicates a moderate to strong detection \citep{2013ApJ...778..153B}. The n-$\sigma$ values are calculated with reference to Equation(10) and Equation(11) in \cite{2013ApJ...778..153B}.
The best-fit models are presented in Figure~\ref{models}, and parameter results are summarized in Table~\ref{retrieval_results} and Table~\ref{retrieval_parameters}.

\subsection{Atmospheric Models with HCN}
\label{sec:model_with_HCN}
By visually inspecting the combined spectrum, we find two weak absorption features centered near 1.40 and 1.55 $\mu m$ in the transmission spectrum of L~98-59~b shown in Figure~\ref{models}. These features can be explained by the presence of HCN in its atmosphere, which is also supported by the initial retrieval results.
For all the models with HCN included (models 1, 2, 3 and 4), the model with clouds, HCN and $\rm N_2$ (model 4) yields the highest Bayesian evidence and ADI value, which is also shown Figure~\ref{lcs_iraclis} and \ref{models}, with 1$\sigma$ (shadow regions with heavier gray) and 2$\sigma$ (shadow regions with lighter gray) uncertainties over-plotted.

Figure~\ref{taurex-posterios-best} presents the posterior distributions of the retrieved parameters from this model 4, such as planet radius, equilibrium temperature, molecular abundance mixing ratios, surface pressure of the gray cloud, and mean molecular weight.
The scale height of the atmosphere is about 49~km ($\sim12$~ppm) with $\rm T = 593.7$~K, $\mu$ = 11.68~amu, and $R_p$ = 0.06~$R_{\rm Jup}$.
The posterior distribution of the surface pressure, which is the pressure at the top of a fully opaque cloud deck, peaks around $10^{-3}$~bar.
The abundance of $\rm HCN$ is $10^{-0.63^{+0.44}_{-2.51}}$, which is much higher than the HCN abundance results from super-Earth 55 Cancri e \citep{2016ApJ...820...99T} and GJ~1132~b \citep{2021AJ....161..213S}.

To extend the wavelength coverage, we also ran atmosphere retrieval by including data from the TESS mission \citep{2021A&A...653A..41D}. The fitting results are shown in Table~\ref{retrieval_results}.
Among all the models with HCN included, model 4 still shows the highest statistical significance. However, according to \cite{2013ApJ...778..153B}, the difference in Bayesian evidence between different models is too small to give a conclusive result.

In Sec~\ref{equilibrium chemistry}, we will calculate the abundance of HCN using an equilibrium chemistry model. We will show that the high value of HCN abundance derived above cannot be explained by an equilibrium chemical model assuming a reasonable C/O ratio and metallicity, thus is likely to be nonphysical and should be discarded.

\begin{figure}
\includegraphics[width=0.5\textwidth]{zl_compare_models_22ppm.pdf}
\caption{The spectrum of different atmospheric models of HST/WFC3.}
\label{models}
\end{figure}

\begin{figure*}
\gridline{\fig{zl_output_posteriors_addcloud_hcn_n2.pdf}{1.0\textwidth}{}}
\caption{The atmospheric retrieval parameters of the best-fit model (model 4) for L~98-59~b.}
\label{taurex-posterios-best}
\end{figure*}

\begin{figure*}
\gridline{\fig{zl_output_posteriors_cloudy.pdf}{1.0\textwidth}{}}
\caption{Same as Figure~\ref{taurex-posterios-best}, but for the flat-line pure cloudy model (model 5).}
\label{taurex-posterios-cloudy}
\end{figure*}

\subsection{HCN Abundance from Equilibrium Chemistry}
\label{equilibrium chemistry}

We find the transmission spectrum of L~98-59~b is best fitted by the model with abundant HCN in a high mean molecular weight atmosphere.
HCN is a fundamental molecule in the origins of life.
In atmospheres, HCN generally forms out of the reactive radicals left over from methane and nitrogen dissociation by ultraviolet light, galactic cosmic rays, and lightning \citep{catling17, horst17, pearce22}.
The most HCN-rich atmosphere in the solar system belongs to Titan \citep[several parts per thousand in the upper atmosphere,][]{Koskinen11}.
Previously HCN has been detected in the atmosphere of the highly irradiated super-Earth 55 Cancri e \citep{2016ApJ...820...99T} and GJ~1132~b \citep{2021AJ....161..213S}.
Please also see \citet{2021AJ....161..284M} for their study on GJ~1132~b, in which no evidence was found for HCN absorption in the HST transmission spectrum.
\citet{2021AJ....161..213S} explored several scenarios in which GJ~1132~b reestablished an atmosphere with HCN and CH4 after the loss of its primary atmosphere, which included mantle outgassing, volcanic activity caused by tidal heating, and lightening.
Because L~98-59~b is located in a packed planetary system and has an orbital eccentricity of 0.1 \citep{2021A&A...653A..41D}, gravitational forces from the central star and other planets can squeeze the planet and cause strong internal tidal heating.
Thus, for L~98-59~b, it likely has lost its primary $\rm H_2$ dominated atmosphere due to photo-evaporation because of the close proximity to its central star.
Then the high–molecular weight secondary atmosphere with HCN was revived by the volcanic and mantle outgassing processes from tidal heating.

However, the HCN abundance derived in Sec~\ref{sec:model_with_HCN} seems really high.
To check if such a high HCN abundance in the atmosphere of L~98-59~b is plausible, we apply the state-of-the-art chemical equilibrium code of FastChem \citep{2018MNRAS.479..865S, 2022arXiv220608247S} to calculate the gas phase chemical composition under thermochemical equilibrium approximation for a given temperature and pressure \footnote{\url{https://github.com/exoclime/FastChem}}.

We set the temperature to 627~K and the pressure to 1~mbar. We first investigate the impact of C/O ratio on the HCN abundance by assuming solar photospheric abundances for all elements except for C and O  \citep{2009ARA&A..47..481A}.
We present the calculated molecular abundance distributions in Figure~\ref{fastchem}.
From this figure, we can see that the abundance of HCN varies between $10^{-14}$ and $10^{-12}$ when we change the C/O ratio from 0.1 to 10.
We have also explored the impact of metallicity on the abundance of HCN, and the results are shown in Figure~\ref{fastchem_metallicity}.
We can see the VMR of HCN changes from $10^{-15}$ to $10^{-9}$ when the metallicity is increased from 0.1 to 1000 solar metallicity.
Although the abundance of HCN will increase when there is more carbon available, it is still much smaller than those of other trace gases.
Therefore we cannot explain the high abundance of HCN derived in Sec~\ref{sec:model_with_HCN} for L~98-59~b using an equilibrium chemistry model with a reasonable metallicity and C/O ratio.
Therefore, we will seek an alternative model in Sec~\ref{model with cloud} to explain the transmission spectrum of L~98-59~b.

\begin{figure}[htbp]
\gridline{\fig{zl_fastchem_c_to_o_fig.pdf}{0.5\textwidth}{}}
\caption{The abundance of molecules range with different C/O ratios using equilibrium chemistry model.}
\label{fastchem}
\end{figure}

\begin{figure}[htbp]
\gridline{\fig{zl_fastchem_metallicity_fig.pdf}{0.5\textwidth}{}}
\caption{The abundance of molecules range with different metallicity (0.1 - 1000$\times$solar metallicity) using equilibrium chemistry model.}
\label{fastchem_metallicity}
\end{figure}

\subsection{Models With Clouds and Hazes
\label{model with cloud}

Here we will explore atmospheric models without the active absorber of HCN. The best retrieval result under this scenario is a flat-line (or the so called ``pure cloudy") model.
Generally, flat and featureless exoplanet transmission spectra can be attributed to three different causes: a higher mean molecular weight atmosphere (and thus smaller scale height), a high-altitude aerosol layer blocking absorption features, or no atmosphere at all.
While L~98-59~b's temperature and terrestrial nature suggest a thin atmosphere with higher mean molecular weight, the WFC3 observations alone cannot rule out the possibility of
a H/He dominated atmosphere combined with condensate clouds or organic photochemical hazes (please see also our discussion in Sec~\ref{sec:loss}).
The best fitted model parameters are shown in Table~\ref{retrieval_results}, with the model curve also shown in Figure~\ref{lcs_iraclis} and \ref{models}.

In Figure~\ref{taurex-posterios-cloudy} we present the posterior distributions of the retrieved parameters, such as planet radius, equilibrium temperature, surface pressure of the gray cloud, and mean molecular weight. The posterior distribution of the surface pressure, which is the pressure at the top of a fully opaque cloud deck, peaks around 1~bar. The mean molecular weight 2.3 is calculated using the fixed H$_2$ to He ratio.

For the pure cloudy model, the Bayesian evidence of the best fit is $\rm log(E)=228.54(0.055)$, a little lower than that of the HCN-only cloudy model, which has $\rm log(E)=229.740(0.064)$. According to \cite{2013ApJ...778..153B}, there is no statistical differences between these two models. Take the equilibrium chemical model results from Sec~\ref{equilibrium chemistry} into account, we ultimately determine that all evidence points to L~98-59~b having a featureless WFC3 spectrum, which can be explained by a thin atmosphere with high mean molecular weight, an atmosphere with highly opaque aerosol layer, or having no atmosphere. And these scenarios cannot be distinguished with the current observation data from WFC3.

It is likely that there is small non-Gaussian noise left unaccounted for in the spectral data extraction, which can cause inflation of the errors of final combined spectrum. Thus we have re-run the retrieval using inflated error bars (such as 25~ppm and 30~ppm) instead of the old 22~ppm to evaluate the robustness of the atmospheric retrieval. When using an error bar larger than 22~ppm, the Bayesian evidence of the flat-line pure cloudy model (model 5) becomes larger than the cloudy model with HCN and N$_2$ (model 4). This also supports our preference of using a flat-line pure cloudy model to explain the transmission spectrum of L~98-59~b.

\subsection{Future Missions}
Future missions such as the James Webb Space Telescope (JWST) and Ariel \citep{tinetti18} will provide higher sensitivity and/or wider spectral coverage than HST/WFC3. This will have a huge impact on the detection of atmospheric features on small exoplanets, even with the presence of clouds at high altitudes \citep{Hinkley22, Constantinou22, Whittaker22}.
If there is a significant amount of HCN in the atmosphere of L~98-59~b, we should be able to detect a very strong absorption feature near 2.5~$\mu m$, which is covered by the wavelength ranges of instruments from both of JWST and Ariel.
Although we do not consider the model with abundant HCN in the atmosphere of L~98-59~b to be real, we still decide to utilize it as an example to demonstrate the power of JWST here.
The cloudy HCN+$N_2$ model (model 4) is used to simulate the spectrum from one single-transit observation of L~98-59~b using NIRISS GR700XD spectrograph (with a resolution of R~$\sim$ 50) on JWST. The simulated spectrum is presented in Figure~\ref{jwst}. Using the plot, we can demonstrate that observations from JWST can be used to place strong constraint on the HCN abundance in L~98-59~b.

\begin{figure}
\includegraphics[width=0.5\textwidth]{zl_jwst_models.pdf}
\caption{Simulated spectrum of JWST/NIRISS GR700XD. Theoretic spectral model of L 98-59 b in the wavelength range of JWST/NIRISS GR700XD for a single transit visit. If HCN is present, JWST will be able to confirm its presence.}
\label{jwst}
\end{figure}

\subsection{Stellar Contamination}

There is no evidence of strong stellar activity present on L~98-59 from the TESS data \citep{2019AJ....158...32K}, and it is likely to be a quiet M-dwarf with a weak level of XUV activity \citep{2021AJ....162..169P}.
However, since very high precision measurements are needed for this study, we still need to quantify the potential contamination to the transmission spectrum of L~98-59~b from the stellar activity of L~98-59.

We apply the stellar contamination models from \cite{2018ApJ...853..122R} to calculate the potential effect of the stellar activity (including spots and faculae) on the transmission spectrum of L~98-59~b.
Here we take four cases of stellar activity into account: giant spots, solar-like spots, giant spots with faculae, and solar-like spots with faculae.
In \cite{2018ApJ...853..122R}, they define that the radii of giant spots and solar-like spots are $ R_{spot} = 7^\circ$ and $ R_{spot} = 2^\circ$, respectively.
We compute the effect of stellar contamination on the transmission spectrum at different wavelengths using Equation (3) from \cite{2018ApJ...853..122R}. For each case, the spot and faculae covering fractions for a M3 type star are adopted from \cite{2018ApJ...853..122R}. The temperatures of photosphere, spot, and faculae are assumed to be 3200 K, 2800 K, and 3300 K, respectively, with a surface gravity of log($g$) = 5.0 and metallicity of [Fe/H] = -0.5. We use the theoretical PHOENIX BT-Settl spectra for photosphere, spot, and faculae.
The final contaminated transmission spectrum is derived by multiplying the transit model of L~98-59~b.

To check which stellar contamination model can best explain the observed transmission spectrum, we compare the observed spectrum with different stellar contamination models in Figure~\ref{stellar contamination}. In this figure, solid and dashed lines represent the transit light source effect for the maximum and mean spot or faculae filling factor, respectively \citep{2018ApJ...853..122R}.
We have also calculated the $\chi^2$ and reduced $\chi^2$ to assess the goodness of fitting for different models, which are summarized in Table~\ref{chi of stellar contaminations}.
From Figure~\ref{stellar contamination} and Table~\ref{chi of stellar contaminations}, we can see that the model of solar-like spots with the maximum spot filling factor deviates most from the observed data. Other stellar models' reduced-$\chi^2$ is $\sim$ 1, indicating that the stellar models can adequately describe the observed spectrum.

After removing the impact of stellar contamination, we also re-run the atmospheric retrieval using model 4 and model 5.
The retrieval results are shown in Table~\ref{stellar contaminations}.
We can see that for all the stellar models, the retrieval results are similar to those done in previous sections.
For one particular case, with the solar-like spots model, the pure cloudy model yields the best fitting result.
Therefore, we reach similar conclusion after including the effect of stellar contamination in our retrieval analysis.

\begin{table}[t]
\centering
\caption{The $\chi^2$ and reduced-$\chi^2$ for different stellar contamination models. \label{chi of stellar contaminations}
 }
\begin{threeparttable}
\resizebox{0.5\textwidth}{!}{
\begin{tabular}{l|l|l|c}
\hline
\multicolumn{2}{c|}{Stellar model} & $\chi^2$ & reduced-$\chi^2$ \\
\hline
\multirow{2}{*}{Giant spots} & max & 22.887 & 1.040 \\
\cline{2-4}
& mean & 23.082 & 1.049 \\
\hline
\multirow{2}{*}{Solar-like spots} & max & 33.264 & 1.512 \\
\cline{2-4}
& mean & 22.504 & 1.023 \\
\hline
\multirow{2}{*}{\shortstack{Giant spots\\+ faculae}} & max & 23.705 & 1.129 \\
\cline{2-4}
& mean & 23.314 & 1.110 \\
\hline
\multirow{2}{*}{\shortstack{Solar-like spots\\+ faculae}} & max & 22.087 & 1.052 \\
\cline{2-4}
& mean & 26.141 & 1.245 \\
\hline
\hline
\end{tabular}}
\end{threeparttable}
\end{table}

\begin{table*}
\centering
\caption{The retrieval results assuming different stellar contamination models.}
\label{stellar contaminations}
\begin{tabular}{l|l|l|l|l|l|l}
\hline
\multicolumn{2}{c|}{\multirow{2}*{Stellar model}} & \multicolumn{1}{c|}{\multirow{2}*{HCN abundance}} & \multirow{2}{*}{log(E) of model 4} & \multirow{2}{*}{log(E) of model 5} &
\multicolumn{1}{c|}{\multirow{2}{*}{\shortstack{$\Delta$ log(E)}}} & \multirow{2}{*}{\shortstack{Sigma}}\\
\multicolumn{1}{c}{} & \multicolumn{1}{c|}{} & &  &  & & \\

\hline
\multirow{2}{*}{Giant spots} & max & -0.63$^{+0.45}_{-3.42}$ & 229.799 $\pm$ 0.063 & 228.931 $\pm$ 0.055 & 0.868 & 1.940
\\
\cline{2-7}
& mean & -0.62$^{+0.45}_{-3.02}$ & 229.820 $\pm$ 0.064 & 228.700 $\pm$ 0.055 & 1.120 & 2.095\\
\hline
\multirow{2}{*}{Solar-like spots} & max & -4.01$^{+3.74}_{-5.17}$ & 228.586 $\pm$ 0.059 & 229.052 $\pm$ 0.055 & - & - \\
\cline{2-7}
& mean & -0.77$^{+0.55}_{-5.46}$ & 230.280 $\pm$ 0.061 & 229.893 $\pm$ 0.055 & 0.387 & 1.572 \\
\hline
\multirow{2}{*}{\shortstack{Giant spots\\+faculae}} & max &-0.63$^{+0.44}_{-1.96}$ & 229.672 $\pm$ 0.065 & 228.115 $\pm$ 0.055 & 1.557 & 2.331\\
\cline{2-7}
& mean & -0.57$^{+0.40}_{-2.56}$ & 229.770 $\pm$ 0.064 & 228.464 $\pm$ 0.055 & 1.306 & 2.120\\
\hline
\multirow{2}{*}{\shortstack{Solar-like spots \\+faculae}} & max & -0.70$^{+0.51}_{-3.83}$ & 230.814 $\pm$ 0.063 & 230.104 $\pm$ 0.055 & 0.71 & 1.833\\
\cline{2-7}
& mean & -0.58$^{+0.41}_{-0.68}$ & 228.999 $\pm$ 0.067 & 225.882 $\pm$ 0.056 & 3.117 & 2.993 \\
\hline
None & - & -0.63$^{+0.44}_{-2.51}$ & 229.740 $\pm$ 0.064 & 228.540 $\pm$ 0.055 & 1.2 & 2.14\\
\hline\hline
\end{tabular}
\end{table*}

\begin{figure}
\gridline{\fig{zl_plot_stellar_contanmination.pdf}{0.5\textwidth}{}}
\caption{Contamination of the transmission spectrum of L~98-59~b from different stellar activity models. Lines with the same color represent stellar contamination models with different filling factors.
The solid and dashed lines represent the transit light source effect for the maximum and mean spot or faculae filling factor,
respectively.}
\label{stellar contamination}
\end{figure}

\subsection{Primordial H/He Atmosphere and Mass Loss}
\label{sec:loss}

According to \citet{owen20}, low-mass planets similar to L~98-59~b can accrete about 1$\%$ of their total masses in H/He gases during formation.
L~98-59 is estimated to be $>$1~Gyr in age \citep{kostov19b}, which is inferred from the star's lack of spectroscopic youth indicators, slow rotation, HR diagram position, no evidence of spots, and low levels of white-light flare activity from TESS data.
According to the work of \citet{2021AJ....162..169P}, the relative size and insolation flux of L~98-59~b may have caused it to lose a significant amount of atmosphere.
Therefore, assuming no other secondary sources of hydrogen, it is very unlikely that L~98-59~b could possess a present-day cloudy primordial H/He-rich atmosphere. However, data from WFC3 alone cannot be used to rule out this possibility entirely.

\section{Conclusion \label{sec:conclusion}}
We present the HST/WFC3 transmission spectrum analysis of the rocky planet L~98-59~b in this paper.
Using the Iraclis data reduction pipeline and the TauREx3 atmospheric retrieval code, we find the transmission spectrum can be fitted either using a flat-line pure cloudy model or a cloudy HCN atmospheric model.
It is very unlikely to possess a clear and hydrogen-dominated atmosphere. The existence of other volatile molecular species can not be confirmed because of the limited precision and wavelength coverage of the WFC3 observation.
However, we cannot explain the unrealistically high HCN abundance derived using the equilibrium chemistry model. Therefore, we conclude that L~98-59~b is more likely to have a secondary thin atmosphere with a high  mean molecular weight, an atmosphere with a highly opaque aerosol layer, or effectively no atmosphere. These different scenarios cannot be distinguished using the current HST data. Future observation from JWST are needed to truly understand the existence and contents of an atmosphere around L~98-59~b.

\begin{acknowledgments}
We thank our anonymous referee for prompt and insightful comments which led to significant improvement of the manuscript. We thank professor Giovana Tinetti, whose visit has triggered this study. We thank Angelos Tsiaras, Ingo Waldmann and Ahmed Al-Refaie for their instructions on how to use Iraclis and Taurex. We acknowledge the financial support from the National Key R\&D Program of China (2020YFC2201400), China Postdoctoral Science Foundation (No.2020M672936), NSFC grant 12073092, 12103097, 12103098, 11733006, the science research grants from the China Manned Space Project (No. CMS-CSST-2021-B09), Guangdong Major Project of Basic and Applied Basic Research (Grant No. 2019B030302001), Guangzhou Basic and Applied Basic Research Program (202102080371), and the Fundamental Research Funds for the Central Universities, Sun Yat-sen University.

This work is based on observations with the NASA/ESA Hubble Space Telescope,  obtained at the Space Telescope Science Institute (STScI) operated by AURA, Inc. The publicly available HST observations presented here were taken as part of proposal 15856, led by Thomas Barclay. These were obtained
from the Hubble Archive, which is part of the Mikulski Archive
for Space Telescopes. This paper also includes data collected by the TESS mission,
which is funded by the NASA Explorer Program. TESS data is
also publicly available via the Mikulski Archive for Space
Telescopes (MAST).
\end{acknowledgments}

	{	\small
		\bibliographystyle{apj}

redpajama_set_name: RedPajamaArXiv


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Defining the main social media platforms, including audience demographics and methods of engagement.
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How to prioritize your activities by targeting audiences.
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This workshop will be presented by Arabella Meyer, Principal at ACMeyer Strategic Communications LLC.
Level: General Prior Knowledge (201 level): Attendees will be familiar with the topic, but only assumed to have general knowledge.
Please Note: This meeting is open to current NPCC nonprofit members and non-member organizations, and may be limited to ONE person per organization due to space constraints. If your organization is not a current nonprofit member of NPCC, you can visit http://www.npccny.org/membership/how-to-join/ for more information on joining NPCC.


In the last post How and When to adjust the Oscillators such as RSI or Stochastics with market momentum, we adjusted our Oscillator settings at this point in the circle after market rhythm changed. Working with new adjusted settings of 34,13, 20, 5 we would have captured the upmove around 8315 and got exited at 8340 a profit of 25 points with very low risk of 10 points as the stop was at 8305 a bit below the first swing low so that we don't get stopped out at fake break out.
While, we were entering in this position we might not be aware of Risk: Reward Ratio (if would have been using Elliott wave or Fibonacci we would have known our targets in advance and hence Risk Reward) still we knew one thing how much money could we loose in this trade and that is sufficient to consider if we will enter in the trade or not? Knowing the Stop in advance is a very essential part of trading because knowing this helps us to plan better and do proper money management, so that our capital is preserved, which will help us to trade in many other profitable setups and if you don't put and decide the stop in advance and remain in a losing position you will be kicked out by market, so the option is within you, weather to get out with the stop hit voluntarily or the market will kick you out brutally.
There is a difference in you getting out yourself than the market kicking you out. When we come out voluntarily we have sufficient capital to again earn profits because opportunities are always there in one stock or the other, but when you fight with the market and keep on holding a losing trade it spoils your capital which could have been otherwise used to reenter into 100s of other new trades and would have helped you gain experience in the market and not letting you say bye bye to markets forever.
The trade that started at 2 pm and you would have kept revising your stops at every Reversal in the oscillator and would have stopped out either at a Fibonacci target or got out voluntarily since, a 1 minute trader should never carry his position next day.
Now lets see the second Chart. You can see that Oscillator overbought at 10 am did not matched the actual top, here is when you should open another chart and start adjusting the settings so that they can correlate with actual tops and bottoms as well as reach the Oversold and Overbought zones properly.
Next top at 11 am correlated exactly with the oscillator reversal but did not read overbought zone, which can create a doubt in taking a position. Which, is why in order to not miss out on such chances one needs to adjust the settings. I am talking a 1 minute example, so it has to be done quickly and shows that one is a day trader, his trading is his living and if he delays to adjust oscillator he will miss out moves or get in wrong moves.
The top at 12 noon again not catch-able as the oscillator did not reached the overbought zone properly, adjusting the setting is the key. Now, if these were say 15 minutes or higher time frame charts you could have taken your time.
In the third and last chart you will note that settings have been changed to 73, 8, 8, 4. You need to play around it and you will be able to do it, if you aren't write me a mail at ruchirgupta2000@gmail.com.
1. You would have noticed that once you change the setting it is works for 3-4 moves in future, this could be a great insight on starting to realize that may be the oscillator setting is due and I should look for change in market Rhythm.
2. Remember the old settings, when ever market changes the rhythm first apply the old settings that have successfully pointed tops and bottoms. If they don't work this time then only use the new setting.
3. Every stock, commodity, currency has its own temperament or rhythm. The setting that is working on Nifty may not work on BankNifty and visa versa.
We, have been given certain default settings and we never bothered to alter these. The change in the settings is one of the keys to identify the trends.
1. Nifty took support on blue channel lower trendline.
2. The downfall was slower in terms of momentum compared to 5-7 May fall and 12 may fall.
3. Visual Squaring of time and price from 5-7 May fall was applied to recent fall of 22-28 may. This concept is derived from Gann's work and I have mixed my trick and made it visually applicable without any trendline or scale measurement.
Now, going forward we should project the C waves into the future. Confirmation will be received once we break the b of B wave at 8368. In my view, Nifty must reach atleast till odd color channel, 8546 to 8640, many fib Ratios lie here, 62% of the A of (B) will land here, while A of (B) = C of (B) will lie in upper channel. Both the possibilities are alive nifty has shown the signs of reversal. Lets see how new waves unfold, I still in a view of C on upside is left then only the downside 1100 points will get balanced correction, we are still left with few hours to complete the 38% time retracement that was discussed last time.
Mercury Retrograde period 19 May – 11 June 2015- Why you should not trade in the times of Mercury retrogrades?
Mercury retrogrades have been famous for their uncertainty, even the best of the best traders struggle to trade this period. If you are trading in this period high chances are targets will be reached but first they will hit your stops or may be the prices will reverse few points before your target gets achieved. The profits that were earned previously were given away. This period is not good for any kind of financial decision making. If someone still wants to trade in this period he/she should trade with very light position. Its like a Storm, a powerful wind the trees who are too stubborn and high with egos tend to fall in this wind. Trade safe.
Elliott Wave and Fibonacci Analysis of Nifty- as Discussed in the earlier update on Nifty Elliott Wave and Fibonacci analysis,the abc on the downside till 8000 was a 3 wave abc subdivision (to read the Previous Report, click here). Which was making a case for a Flat or a Triangle, and suggesting the upmove till 8680 in 3 waves, the present upmove till 8490 which we have seen till now could only be the wave 'a' of the larger (B)wave on the upside. Now, it seems that wave A is over on the upside, wave B in 3 waves must unfold on the downside, which can get supports at 8240 and 8185 areas. After, which a final C wave must follow completing the (B) wave.
As per the structure unfolding till now, possibility of a Flat or Triangle are open, (low of 8000 must hold for that), and if it holds and we reverse from the above mentioned fib support zones we may reach the completion of (B) wave discussed above (which has high likelihood of reaching 8680).
Now, Lets try to assess the ending of the Wave B on the downside, which is in action. More levels may unfold if these are broken and entire wave count might have to be changed in the low of 8000 is broken and get it adjusted to a leading diagonal pattern. But for right now we must assess the levels for the wave B.
Nifty Support Levels: What is making the 8240-45 as the immediate support? What is making the 8240-45 as the immediate support?
– Fibonacci levels are overlapping on each other.
– Many other levels also lie there, which are not being displayed.
– Channel is also coming to support that level.
– The angle of the decline in also very favorable to reach this level.
Nifty may stop here, if not then, next level of 8185, will again give strong support coz of the reasons mentioned for 8240-45 level.
Nifty Time Analysis: The full abc correction on the downside from 9100 till 8000 took 39 trading days and this must be countered by the upside move for atleast 38% of the time. Ideal time would be 50% to 62%. The upside so far has not met the ideal minimum requirement of 38%, which also suggests more upside or after this wave B on the downside in over.
1) the ABC wave decline is a Wave 'a' of larger degree and is over (from 9100 to 8000) and the 'b' wave of the Flat is going on, which should be again 3 waves, this up move could be 62% to 138% of the 1100 points fall. After this we may see the final C wave, a 5 wave decline.
Since, in a flat wave must be atleast 62% of Wave 'a' ,Nifty must atleast reach till 62%, which is 8680. The Present upmove which has started seems to be the A of b wave on upside, It is very weak, as is correction to the correction. You can see in the channel, prices are not able to cross the middle line.
2) Complex corrections in wave 4s could be very easily be Triangles and that scene is also open and that still requires 62% retracement of the upside.
So both the cases may taking us towards 62% retracements.
3) There is also a possibility of double and triple threes in wave 4. Which may imply we may face complex correction for months.
Please refer both the charts. Hourly as well as Daily and take your own decisions.
State Bank of India may test the these fibonacci levels in the near future. This is just my view and a recommendation or a tip. No Elliott Waves analysis has been used in it. Fibonacci in itself is a very strong tool, these fibonacci levels are different from what we use for particular waves to waves for future projection.
This update on Tata Steel is in continuation to the previous 2 updates. I have analysed the multiple time charts with Elliott waves principle and tried to explain what to expect in future.
Hourly Chart: If this was C wave, and correction was to end with this (read previous post) , this volume spike which is even bigger than any of the the impulse waves should not have happened. The Volumes at ending c wave corrections become low and not increase like it happened here. Refer to next 2 higher time frame charts with this post.
Weekly Chart: The Large decline on a larger time frame tempted to assess what was happening here. The Upmove clearly shows 3 subdivisions. 3 waves up suggesting, that present downside may not be over. Which forces to analyse even a longer time frame chart.
Monthly Chart: On Larger time frame I found Triangle in action. Its E wave on the down side is going on. This the picture much clear, on the larger time frame this is a 4th wave correction in form of triangle from 2007 to present and since its in the last phase of correction E wave it must start moving up. also C wave = 62% of A, and D wave = 62% of B. Ideally, E wave must be 62% of C which may bring it to 248 levels in coming 5 – 9 months. To me it seems a time to accumulate at every 20-25 Rs fall for long term investors. Again, its just my view. I felt to update this as a responsibility to bring the larger picture coz in earlier post it seemed a set up for going long is getting ready, it may or may not go up but coz of the risk and reward comparison, I will stay away from it as I am a swing trader.
Tata Steel Elliott Waves Analysis Update: After writing the review yesterday on Tata Steel, Wave C actually Started subdividing, it formed the Wave 1 of C with the upmove and now its opened gap down. It has clearly broken the first support level of 50% and reached 62%. Here the support is at 343-338 area (ideally prices should not god below this area), which is holding, yet we should ideally see the 5th wave on the downside (sometimes the C waves are only 3 waves), still since the 62% retracement is over and time wise we have reached 50% of the full Impulsive move.
As already said in the wave 2 the corrections are shorter in duration than wave 4 and structures are sharper than 4. This is general observation. Which means we should start seeing an upmove in the form of wave 3 once the correction ends.
Second, scene is that this completed abc (though 5th wave still may be remaining), is just the wave a of the entire correction, if that's the case we may still go up as a wave B.
So, both cases suggesting the case of upmove. (we may be able to gauge the if its B wave or 3 wave with the strength of the move). I, must tell you that even though both cases may be suggesting the upmove, I don't take my entry just based on this, I have a proper system from entering till exiting, which is very lengthy to explain here.
To learn Elliott waves, Fibonacci and Gann in detail please contact and message me in Inbox. My Email address is Ruchirgupta2000@gmail.com. Please like and follow my page and also share my post , made it for teaching Elliott wave and Gann.https://www.facebook.com/pages/Learn-Elliott-Waves-Gann/299034886964403 You can get many updates such as this on my page.
Elliott Waves Analysis of Tata Steel: The upmove was a 9 wave in which 5th wave subdivided in sub waves. Wave 1 on the upside is complete and we in a wave 2 correction. A and B of the ABC are over while C is going on. Since A and B were subdivided in 3 waves each which suggests the formation of a flat (3-3-5). So, the C wave ideally be subdivided into 5 waves, though I have not seen any subdivision, which could mean C wave completion without any subdivision. First support, I see at 347 which is at 50% internal and 127% external retracement.
While the possibility of correction to reach 62% is still open, the correction in waves are majority steep decline and short term, so the complex correction though possibility is open, probability is low.


text:
package io.quarkus.kubernetes.spi;

import io.quarkus.builder.item.MultiBuildItem;

public final class KubernetesAnnotationBuildItem extends MultiBuildItem {

    private final String key;
    private final String value;
    private final String target;

    public KubernetesAnnotationBuildItem(String key, String value, String target) {
        this.key = key;
        this.value = value;
        this.target = target;
    }

    public String getKey() {
        return key;
    }

    public String getValue() {
        return value;
    }

    public String getTarget() {
        return target;
    }

}

redpajama_set_name: RedPajamaGithub


← A unanimous decision from the supreme court today!
Early Neutral Evaluation comes to Denver!
Family law cases are complicated, and they are often better resolved if the parties can reach an agreement outside of the courtroom. Alternate Dispute Resolution allows parties to craft more personalized and flexible solutions that are tailored to the circumstances facing their families. Usually, ADR in family law cases takes the form of mediation, in which a neutral third-party helps the parties to discuss and reach agreement on their issues.
The Colorado Dispute Resolution Act also provides for Early Neutral Evaluation (ENE) as an ADR mechanism. C.R.S. §13-22-302(2). The idea behind ENE is to involve a court-appointed evaluator early in the process to assist the parties in case management by identifying, simplifying, and eliminating some issues when possible. Essentially, the evaluator listens to the parties' positions and offers feedback on the likely outcome of the issue in front of the court. This is different from mediation because the purpose of the ENE meeting is not necessarily to get either side to compromise; rather, the goal is to provide the parties with realistic feedback about their changes in court.
In May of this year, Denver County announced that it has initiated an Early Neutral Assessment pilot project allowing parties to opt in to the project. The project will cost $400 per party (though the Office of the Child Representative has agreed to fund ENA for indigent parties). If parties opt in to the program, they will work with a two-person team consisting of a mental health professional and a retired judge.
The biggest advantage of ENE in family law cases seems to be the ability to get feedback regarding potential outcomes earlier in the process than would otherwise be typical. I will be very curious to see how this process works throughout Colorado and hope that it can help parties move through the process more quickly and inexpensively.
This entry was posted in Alternate Dispute Resolution, Best interests of the child. Bookmark the permalink.


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Home » Joseph Boyden
The Orenda
Joseph Boyden
In the remote winter landscape a brutal massacre and the kidnapping of a young Iroquois girl violently re-ignites a deep rift between two tribes. The girl's captor, Bird, is one of the Huron Nation's great warriors and statesmen. Years have passed since the murder of his family, and yet they are never far from his mind. In the girl, Snow Falls, he recognizes the ghost of his lost daughter, but as he fights for her heart and allegiance, small battles erupt into bigger wars as both tribes face a new, more dangerous threat from afar.
Traveling with the Huron is Christophe, a charismatic missionary who has found his calling among the tribe and devotes himself to learning and understanding their customs and language. An emissary from distant lands, he brings much more than his faith to this new world, with its natural beauty and riches.
As these three souls dance with each other through intricately woven acts of duplicity, their social, political and spiritual worlds collide - and a new nation rises from a world in flux.
History & Fiction / Romance & Love
Kwe: Standing With Our Sisters
Driven by deep frustration, anger, and sorrow in the wake of yet another violent assault upon a First Nations woman in November 2014, dozens of acclaimed writers and artists have come together to add their voices to a call for action addressing the deep-rooted and horrific crimes that continue to fester in our country.
Kwe means woman in Ojibwe. More specifically, kwe means life-giver or life-carrier in Anishinaabemowin, the Ojibwe language. It is a pure word, one that speaks powerfully of women's place at the heart of all our First Nations.
These women who bring light and life to our world are in peril. Aboriginal women in our country are three times more likely to face violent attack and murder than any other of their gender. We must take concrete steps to stop this and we must do it now.
A nation is only as good, is only as strong, as how it treats its most vulnerable and those of us in danger. This book is a call to action. It's sometimes a whisper, sometimes a scream, but we speak our words as one when we demand justice for our more than 1200 murdered and missing Indigenous women. After all, they are our mothers, our daughters, our nieces, our aunties, our sisters, our friends.
Kikwaakew
"Niska is trying to tell him something from far away, something important. She's done this before, working her shake tent, filling his head deep at night with images he can't quite make out through the mist. She warned him about kikwaakew." 25 years after the war of Three Day Road, Joseph Boyden revisits Xavier Bird, who looks to his sons to help defeat an old foe on the trap lines. Kikwaakew first appeared in the July/August 2012 issue of The Walrus magazine. Three Day Road is winner of the Amazon/Books in Canada First Novel Award and the Roger's Writers Trust Fiction Prize.
Through Black Spruce
A haunting novel about identity, love, and loss by the author of *Three Day Road*
Will Bird is a legendary Cree bush pilot, now lying in a coma in a hospital in his hometown of Moose Factory, Ontario. His niece Annie Bird, beautiful and self-reliant, has returned from her own perilous journey to sit beside his bed. Broken in different ways, the two take silent communion in their unspoken kinship, and the story that unfolds is rife with heartbreak, fierce love, ancient blood feuds, mysterious disappearances, fires, plane crashes, murders, and the bonds that hold a family, and a people, together. As Will and Annie reveal their secrets-the tragic betrayal that cost Will his family, Annie's desperate search for her missing sister, the famous model Suzanne-a remarkable saga of resilience and destiny takes shape. From the dangerous bush country of upper Canada to the drug-fueled glamour of the Manhattan club scene, Joseph Boyden tracks his characters with a keen eye for the telling detail and a rare empathy for the empty places concealed within the heart. Sure to appeal to readers of Louise Erdrich and Jim Harrison, Through Black Spruce establishes Boyden as a writer of startling originality and uncommon power.
Born With a Tooth
Almost a decade after its original publication, award winner and Governor General Literary Award nominee Joseph Boyden's classic book of short stories is finally being reissued. Born With A Tooth, Boyden's debut work of fiction, is a collection of thirteen beautifully written stories about aboriginal life in Ontario. They are stories of love, unexpected triumph, and a passionate belief in dreams. They are also stories of anger and longing, of struggling to adapt, of searching but remaining unfulfilled. The collection includes 'Bearwalker', a story that introduces a character who appears again in Boyden's novel Three Day Road. By taking on a new voice in each story, Joseph Boyden explores aboriginal stereotypes and traditions in a most unexpected way. Whether told by a woman trying to forget her past or by a drunken man trying to preserve his culture, each story paints an unforgettable and varied image of modern aboriginal culture in Ontario. An extraordinary first book, Born With A Tooth reveals why Joseph Boyden is a writer worth reading.
Three Day Road
Set in Canada and the battlefields of France and Belgium, Three-Day Road is a mesmerizing novel told through the eyes of Niska—a Canadian Oji-Cree woman living off the land who is the last of a line of healers and diviners—and her nephew Xavier.
At the urging of his friend Elijah, a Cree boy raised in reserve schools, Xavier joins the war effort. Shipped off to Europe when they are nineteen, the boys are marginalized from the Canadian soldiers not only by their native appearance but also by the fine marksmanship that years of hunting in the bush has taught them. Both become snipers renowned for their uncanny accuracy. But while Xavier struggles to understand the purpose of the war and to come to terms with his conscience for the many lives he has ended, Elijah becomes obsessed with killing, taking great risks to become the most accomplished sniper in the army. Eventually the harrowing and bloody truth of war takes its toll on the two friends in different, profound ways. Intertwined with this account is the story of Niska, who herself has borne witness to a lifetime of death—the death of her people.
In part inspired by the legend of Francis Pegahmagabow, the great Indian sniper of World War I, Three-Day Road is an impeccably researched and beautifully written story that offers a searing reminder about the cost of war.
Wenjack
Shortlisted for the 2017 OLSN Northern Lit Award
An Ojibwe boy runs away from a North Ontario Indian School, not realizing just how far away home is. Along the way he's followed by Manitous, spirits of the forest who comment on his plight, cajoling, taunting, and ultimately offering him a type of comfort on his difficult journey back to the place he was so brutally removed from.
Written by Scotiabank Giller Prize-winning author Joseph Boyden and beautifully illustrated by acclaimed artist Kent Monkman, Wenjack is a powerful and poignant look into the world of a residential school runaway trying to find his way home.

redpajama_set_name: RedPajamaCommonCrawl


text:
Brian Finnegan
www.brianfinnegan.ie
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The Not So Beautiful Game
Cinnamon Toast and the End of the World: A Review
Posted by Brian Finnegan
At the beginning of Janet E. Cameron's book, Cinnamon Toast and The End of the World, Stephen Shulevitz's world as he knows it comes to an end. He's reached the sudden realisation that he's in love with his best buddy, Mark, and that he desperately wants to kiss him.
This is a 'coming out' novel. You know from the opening scene that Stephen will have to overcome a series of emotional obstacles before eventually coming to terms with his sexuality; that towards the end he's going to tell Mark that he fancies him, for better or worse; and that there's going to be some deep issues with Stephen's parents that he's going to have to sort out along the way. There'll probably be a story arc featuring Stephen's close female friend too. As with any romance novel, where the two paramours are introduced in the opening chapter and you know that on the very last page they will get together, the table is set for a three-course meal you've consumed several versions of before.
The desire to keep reading a novel in such a well-trodden genre is founded in questions about how the journey will unfold, and the mark of success is whether it keeps the reader questioning.
Luckily Cameron knows how to keep the questions popping up. She's a talented writer, and the journey she takes us on is always pleasurable, sometimes moving, and has a lyrical literary style that separates it from the masses of 'coming out' fiction that litter the queer cannon. It also dares, at times, to jumble up the equation and come up with different answers, as in a later reunion scene between Stephen and his absent, drop-out Dad, Stanley, in which a lesser novelist would have given her readers warm, fuzzy emotional resolution.
Before any conclusion is reached, Stanley says: "I think this conversation has run its course." Stephen, instead of getting his father to say he loves him, is left in confusion, and Cameron resists any urge to move Stanley centre stage again for the tying up of loose ends.
The tale is set in 1987, mostly in the small Canadian town of Riverside, where boredom rather than outright prejudice drives the violent motivations of its teenage population. Cameron clearly loves the eighties. The book is filled with playful cultural references to the era. When Stephen contemplates suicide, he does so through the filter of watching an umpteenth Friday The 13th sequel. At the inevitably excruciating prom, he dances with rebellious abandonment to Aha's The Sun Always Shines on TV.
He may be surrounded by stalwarts of the genre – the best girlfriend (Lana) who secretly fancies him, the ambivalent but unavailable love interest, the school bullies – but its in her depiction of supporting characters, like Lana's immigrant father, Mr. Kovalenko ("a look on his face like he'd been chewing old sardines"), and Stephen's fleeting, sexually gluttonous girlfriend, Tina Thompson, with her "muscular tongue", that Cameron really lights up. Stephen himself is a sharply drawn protagonist, his teenage view of the world suitably cynical, but underlined with almost poetic, acute observation.
Towards the end the inevitable happens, and as Stephen's orientation becomes known to his peers, he becomes more and more vulnerable. Cameron isn't afraid to shift the lighthearted tone of the first half of the novel into much darker territory, and during the penultimate, chaotic scene between Stephen and Mark, you begin to think this might not turn out the way all 'coming out' novels turn out, after all.
You'll have to read the book to find out if it does, but in the meantime I'm taking bets that Cameron's second novel will leave the 'coming out' genre behind. She's simply a writer, a good one, who likes to tell a cracking story. That this story is about a gay boy finding himself is incidental.
Posted in Bits 'n' Pieces
Tags: author, Books, coming out, gay, novel, Review, teenager, Writing
How The President Got ABBA Tickets
There's another story doing the rounds about Abba reuniting, with Agnetha rowing in to say she wouldn't be adverse to doing a charity concert. In Knowing Me Knowing You, they reunite to do a concert for Unicef, and my characters all go to Stockholm for the concert of a lifetime. Writing it was like writing a dream come true for me. When I was a kid, all I wanted to do was see ABBA in concert. The nearest I ever got was going to ABBA: The Movie in the Savoy Cinema in Sligo, Ireland on a rainy summer's night, but even then my excitement was so much, I could hardly eat the whole day beforehand. (I guess that's called the ABBA diet.)
ABBA came to Ireland in 1979, when I wasn't nearly old enough to go to a concert, so my parents wouldn't hear of it. And anyway, the tickets sold out instantly and then became like gold dust. On the day they played, the then President of Ireland, Patrick Hillery, went on the most popular radio show of the time, The Gay Byrne Show, and appealed for tickets so his daughter could go to the show. She had a pair by 5pm.
My friend, John, who lived in Limerick (I didn't know him at the time, we only met as adults) remembers this, and remembers how disgusted he was, that the President would be able to use his power to get tickets like that, and when you think about it, Mr Hillery was being very cheeky indeed.
I hope his daughter enjoyed the show. And maybe, if Bjorn, Benny Agnetha and Frida ever get back on a stage together, myself and John can go and see them play!
Tags: Abba, Agnetha, Books, culture, Music, pop
Gone Tabloid: The Shock of My Name in the Headlines
I thought I knew a fair bit about the media industry. After all, I've been magazine editing for 13 years now, and I know a good story when I see one. Over those years I've often been asked to go on TV, radio and in print to talk about gay rights issues, and the one proviso I always gave was that I don't talk about my personal life. The reason for this is I have a son, and I felt a responsibility to keep his life out of it, since he had no choice in the matter.
My son's grown up now, and he lives abroad, plus he's totally comfortable with me talking about him, so when The John Murray Show on RTE Radio One asked me to come on and talk about my new novel, Knowing Me Knowing You, and at the same time tell the nation what it's like being a gay dad, how it all happened, and what my relationships with my son and his mother were like, I said yes. I was reluctant – my book is mainstream commercial fiction featuring heterosexual characters, and no gay dads, but i understand that personal stories are interesting to listeners, and I felt ready to tell my story.
The show was broadcast on Monday, and right after it the RTE press office contacted me to say The Daily Mirror were interested in running a story, based on the interview. Then The Irish Sun called me and said they'd like to run a story too. I said yes, although again with trepidation. There was little I could do about it – my interview was public property. I asked both the Mirror and The Sun to print a photo of my book cover with their pieces and left them to it.
The stories appeared yesterday. The copy stuck to the tone of my interview, which was an honest account of how I came to have a child, the process of coming out as gay, how my child's mother took the news, and how we have managed to bring our son up together but apart, the very best we could.
But the headlines were a different story.
'I TOLD HER I WAS GAY BUT WE HAD A BABY ANYWAY' shouted The Mirror.
'GAY DAD PACT HIS BAGS DAY SON TURNED 1' said The Sun – http://tinyurl.com/c7c2kz8
I know a headline is there to make a reader read the story, but still I was shocked at the negative slant in the headlines about my own life. They don't reflect the truth of the story at all, and there's a kind of homophobia to them, a suggestion of irresponsibility coupled with the word 'gay' that, for all my knowledge of the tabloid papers and their sexually prurient slant, I was not expecting. I guess, when it's your life, you can't imagine it framed in any other way.
God only knows what it must be like to be famous and see this kind of stuff every day!
Anyway, my publishers are delighted. Both papers printed the book's cover so it should help sales. And that's what it's all about, isn't it, folks?
Tags: Abba, gay, Media, publishing, radio, Writing
Review of The Red House by Mark Haddon
Although I wasn't a huge fan of The Curious Incident, I loved Mark Haddon's second adult novel, A Spot of Bother. I think he is brilliant at writing the dynamics of family, the mixture of love, resentment, competition, annoyance and friendship that comes with having parents and siblings. While A Spot of Bother was quite comedic, and very moving, in its exploration of the breakdown of a parent and its effect on his wife and children, The Red House is a much darker take on family dynamics. But it's nonetheless gripping and beautifully written.
An estranged brother and sister, Angela and Richard, go on holidays together in rural Wales with their respective families after the death of their mother, and the story unfolds over a week staying in The Red House.
The younger characters come across as the most interesting, particularly the 16 year-old self-serving, calculating bully Melissa, and catastrophically confused Jesus-freak Daisy, who is the same age. The relationship that develops between the two, who have only met each other for the first time is much more the excruciating heart of this book than the one between Angela and Richard.
Whereas A Spot of Bother ended with a sense of resolution, by the time the book ends, the two families go their separate ways and few conclusions have been come to, except maybe for Daisy who has come to a moment of self-realisation.
Hovering over this book is the imagined ghost of Angela's stillborn first child, Karen, and she makes for a genuinely creepy presence, even if she ends up being the glue that just may hold this disparate group of people together.
A fine read, full of wonderful literary tricks and quirks, but I'm a sucker for resolution, so it left me feeling a little frustrated. But then again, family is like that. The relationships go on, and while there may be moments of clarity, there is rarely resolution.
Tags: A Spot of Bother, Books, Mark Haddon, The Red House, Writing
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Live Matrix for What's When on the Web™
This post won't change your life, but Live Matrix might. Created by a former SVP at TV Guide and a pioneer in semantic web technology, Live Matrix promises to keep you updated on What's When on the Web™. In a nutshell, it's a grid of all the live upcoming events scheduled to happen anywhere on the internet, so you'll never miss a beat—or a Gilt sale.
Like everything else these days, users create a custom profile and "follow" content channels that interest them. I signed up yesterday, and currently, I'm following Wired for Wine, Mingle Media TV, G4 TV, The Indy Radio Factor, Gilt Women, and FORA.tv. There have been some hiccups in this Beta version, such as unreasonable "account suspension" and the profile photo upload appears not to be working. Little things like that are expected, though, so I'm not holding it against them. However, as of right now, the whole site seems to be a little bit of an over glorified QVC timetable, as the majority of happenings revolve around product sales, reviews, and web infomercials. That, too, I'm willing to let slide for awhile because, honestly, this whole idea is a beautiful step forward for the future of intelligent content streaming, channeling, and scheduling on the internet.
It's refreshing that someone is wrangling up what's useful on the web and organizing it in a practical way. And as content improves, which it undoubtedly will, Live Matrix stands to become really, really important to daily life. My best-of content scenario includes intelligent news hubs, niche lifestyle channels, and maybe even the return of music videos. I know that all of these things do exist out there on the web, but to have them aggregated, scheduled, and frequently updated is something truly advantageous.


NICE has in first draft guidance rejected Bristol-Myers Squibb's cancer immunotherapy, Opdivo (nivolumab), for use in advanced kidney cancer.
NICE said it rejected Opdivo because it cost more than £60,000 per quality-adjusted life year gained in advanced renal cell carcinoma whose disease has progressed following previous treatment.
This is above NICE's normal £30,000 threshold and extra leeway given for drugs used at the end of life.
Further details in the guidance document show NICE's committee thought the drug cost around £74,000 per QALY compared with Pfizer's Inlyta (axitinib) and almost £92,000 more per QALY than Novartis' Afinitor (everolimus).
NICE added that there were uncertainties in clinical evidence from the CheckMate 025 trial as data were immature, and that survival benefits were unclear.
The committee added that there was no statistically significant benefit for patients who had received two previous treatments.
BMS has yet to offer a discount as often happens in situations such as this. It noted in a statement that Opdivo has been recommended for NHS patients with advanced skin cancer, yet patients with advanced lung and kidney cancer do not have access.
The company pointed out that the Medicines and Healthcare Products Regulatory Agency had earmarked Opdivo as a Promising Innovative Medicine.
BMS gave no indication in the statement about whether it would offer a discount.
Nick Turkentine, CEO of the charity Kidney Cancer UK, said the decision is a "serious blow" for patients with advanced kidney cancer.
"This drug could potentially extend their lives and today's outcome clearly shows the need for urgent fundamental reform of how medicines are made available on the NHS," said Turkentine.
Rose Woodward, from the Kidney Cancer Support Network, said the news is "deeply distressing" for kidney cancer patients.
NICE will consult on the guidance for four weeks, which will be followed by a second draft later this year.


text:
Rhyscotoides silvestrii is een pissebed uit de familie Rhyscotidae. De wetenschappelijke naam van de soort is voor het eerst geldig gepubliceerd in 1950 door Alceste Arcangeli.

Rhyscotidae

redpajama_set_name: RedPajamaWikipedia


text:
The Silencing of Jesuit Figurist Joseph de Prémare in Eighteenth-Century China
D. E. Mungello
The image of a voice in the wilderness evokes an outcast who has been condemned and banished by society. That image fits the scholar-priest Joseph de Prémare who spent the last thirty-eight years of his life (1698-1736) mainly in remote areas of China. He was condemned to silence by not only his religious superiors, but also by intellectuals in Europe. He was silenced because his Figurist theories were regarded as dangerous and implausible. And yet the irony of this silencing is that Father Prémare was one of the most knowledgeable Sinologists of all time. As a missionary in towns in the southern province of Jiangxi, he was freed from many pastoral duties by an assisting catechist and able to devote himself to intensive study of Chinese texts. He was practically a scholar-hermit who left the urban, politicized atmosphere of Beijing after only two years to return to Jiangxi province. There he cultivated Chinese literati who helped him assemble a remarkable collection of classical texts. He was prolific in producing a wide body of works in philology, history, philosophy, religion and drama.
Faced by critics who were claiming that Chinese culture was alien to Christianity, Prémare joined the effort led by his fellow Jesuit Joachim Bouvet to save the Christian mission in China from destruction. The Figurists were radical in arguing that the ancient Chinese texts, like the Old Testament, anticipated the coming of Christ long before his birth. They claimed that Chinese commentators erred in viewing these ancient texts as records of history when in fact they were works of metaphorical and figurative meaning. Influenced by a Chinese scholar, Prémare made a philological analysis of Chinese characters to explain his theory. When Figurism was condemned by his religious superiors, Prémare attempted to circumvent their prohibition by sending his manuscripts to the proto-Sinologist Etienne Fourmont in Paris, asking that they be published anonymously. Fourmont criticized Prémare's theories and failed to publish them. By the time of his death, Prémare had sent most of his manuscripts to Paris where they remained buried for many years.
978-1-4985-9564-3 • Hardback • June 2019 • $85.00 • (£54.95)
978-1-4985-9565-0 • eBook • June 2019 • $80.50 • (£54.95)
Subjects: History / Asia / China
D. E. Mungello is professor emeritus of history at Baylor University.
Chapter I: Water
Chapter II: Drama versus History
Chapter III: The Vestigia
Chapter IV: Daoism and Hieroglyphics in the Vestigia
Chapter V: Earth to Earth, Dust to Dust
This book is a major contribution to a fascinating aspect of the Jesuit mission in China. Prémare's is a tragic story, and it is well told here, with compelling examples of his 'discovery' in the Chinese classics of prefigurations of Christian Revelation. However ultimately misguided his claims may have been, the author establishes beyond any possible doubt Prémare's encyclopedic knowledge of Chinese language and culture, and his devoted sincerity of purpose.
— Jonathan Chaves, professor of Chinese, The George Washington University
Never before has interest in the Jesuit enterprise in China been been more acute, and D. E. Mungello's study of the Jesuit Figurist, Joseph de Prémare, is among the most insightful and informed studies now available. This remarkable work on one of the progenitors of modern Sinology will receive wide acclaim.
— Anthony E. Clark, Whitworth University


The correct selling price of a Long Beach Island or Manahawkin NJ area home is the highest price that the market will bear. To assist you in determining the correct asking price I will be happy to provide you with a comprehensive market analysis of comparable properties sold and offered for sale in your neighborhood.
Simply enter your criteria below, and I will provide you with a speedy response. The more information you provide, the more accurate the evaluation. All information you provide is secure and will be kept strictly confidential. There is no obligation. Please indicate when you are thinking of selling and if you are moving to the area or out of the area.
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text:
Penn State class captures soldiers' rare stories from Iraq
GENARO C. ARMAS
STATE COLLEGE — U.S. Marines veteran Matt Poth looked into the video camera and told a story about his time in Iraq that, until that point, only a few fellow soldiers had heard.
It's hard for him to talk about watching a soldier die at the hands of a suicide bomber, and harder still to relay it to people who have never worn a uniform.
A first-of-its kind class at Penn State documented the recollections of war and military life from Poth and other student veterans home from Iraq. Students like Poth also say it has made it easier to talk about a sensitive subject.
"I've gotten what I think I should have gotten, which is the ability to talk about this stuff, and get it out there, air it out," Poth, 24, of Coatesville, said about his nine-minute video, part of an online exhibit recently posted by WPSU in State College called "Back from Iraq: The Veterans' Stories Project."
"What I hope veterans get out of this, is that they can talk about it," Poth said. "It opens the door and says, 'Hey, all you got to do is talk.'"
Eight students completed last year's course entitled "Narrative, Oral History, New Media Technologies" designed to teach veterans video and web applications to chronicle stories about war and the military.
They learned documentary film-making and oral history interviewing techniques, posted blogs and created videos. The class itself was also documented, with portions posted online late last year.
Nathan Tobey, a coordinating producer at WPSU and one of the course instructors, said he thinks it was the first project of its kind dedicated to documenting Iraq war veterans' stories.
"Some of the topics are not easy to talk about, but they're so important," he said. "We hope this serves as the starting point for conversations going forward."
Poth, a sophomore and former machine gunner who was deployed to Iraq twice, especially took risks in choosing to make himself the subject of his documentary. His film starts describing his time as a wide-eyed teenager seeking a "John Wayne-type lifestyle" to talking about his experiences as a Marine in colorful but expletive-laced descriptions.
Poth said he felt it was important to leave the expletives in his piece since it was such a part of life in combat.
"I think it's a sense of being hard-wired. It's hard-wired as an outlet," Poth said in an interview. "You have to have that raw-less emotion. It's just tapping into that pure rage."
He talks enthusiastically until speaking about watching a fellow Marine shoot at a suicide bomber driving a car toward their patrol.
The car swerved off the road, but ran into a wall and exploded, sending shrapnel through the air and killing Poth's buddy. Talking about the death of a fellow service member is rare outside the military fraternity, Poth and another classmate, Mike Bressler, said.
"People don't realize how hard it is watching a buddy die," Poth said in the film, choking up and slouching forward in his chair. "To watch your friend run in front of danger without giving it a second thought to save your life, that's rough."
Bressler, 27, a senior from Wilkes-Barre, said he took part in the class in part to connect with other veterans. He ended up becoming good friends with Poth and served as the interviewer for his film.
"A lot of people ask, 'What was it like' and this and that," Bressler said. "I can tell him all day the story, and he's going to know what I'm talking about, and that's what I hoped to gain, friendship and reconnecting with veterans. It's a brotherhood."
Dave Walker, 28, of Danville, recently graduated with degrees in biochemistry and molecular biology. An Army veteran who enlisted as a combat demolition engineer after the Sept. 11, 2001, terrorist attacks, Walker said he took the class more out of curiosity than a need to connect with veterans.
Walker's stylishly-produced film tracks the contrasts in attitudes and experiences between an enthusiastic ROTC student looking forward to military service, to that of one of Walker's friends who served in Iraq.
"I was kind of mean for a long time when I got back from Iraq, I'm not like that now," Danny Gardner, 29, of Scranton, said in a solemn voice on film. "I still won't be that carefree, happy-go-lucky guy I was when I left, and I don't think I'll ever be again."
Like Poth, Walker said the class helped him open up about his experiences. He said it also made him realize the importance of offering truthful answers to civilians curious about Iraq, including critics.
"They get angry and all they see is the negative side instead of looking at it as a whole," Walker said. "They see that one thing and automatically want to put that one thing on everything."
Poth said he isn't sure how much civilians may get from his film, in part because of his more brusque persona. At the least, Poth said he hopes civilians, especially those more wary of war, have a better understanding of veterans.
"Sometimes it's easy to take for granted the liberties that a lot of guys went and fought for, and maybe before they cast veterans off as disgruntled, tattooed, drinking, cussing whatevers, let's maybe look a little deeper and figure that out," Poth said.
Funding limited the class to just the spring 2009 semester, though Tobey said he hopes other schools or organizations may try similar projects for Iraq war veterans.
Back from Iraq site:
http://wpsu.org/backfromiraq/index


Could you please guide me about how to setup budgeting and analyse budget vs actual in MSD NAV 2016.
Easiest is to export the budget to excel and edit.
After that you can import the file.
Is there any default report for Budget VS Actual analysis?
Yes - you have two options.
How this possible to prevent posting to the particular G/L Account whenever the defined budget amount is exceeded for the period?
Thank You very much for your previous inputs, it was very helpful for me to do the budget setup, import and analysis.
That is not possible out-of-the-box. You will need a customisation which matches your needs to implement a requirement like this.


Yesterday, all over the world the media were trumpeting the arrival of a new web browser called Chrome. Google, whose little baby it is, claimed they weren't trying to mount a full frontal assault on Internet explorer and I for one believe them.
Why? Well, withing minutes of launch the bloggers started asking one pretty salient question. Where's the Google Toolbar? The answer is there isn't one!!!!
This has to be one of the most hilarious oversights this year. If Google want the early adopting tecchie community to try out Chrome then they need to spend some serious time understanding their user. Haven't they ever heard of interaction design or usability testing?
The reason people love Google is it makes their world easier. I am addicted to the Google Toolbar because it gives me easy access to my life – emails, calendar and I have been trying out the documents as well. Without this toolbar I don't have access to the bookmarks I have been collecting for a specific project, I can't check my emails easily etc etc.
I think Google are telling the truth. They aren't even close to mounting a challenge on IE, even though it pains me to say so. I fear they have gone into battle unarmed.


text:
Top new stories and national headlines
Madras High Court gets a New Chief Justice
Justice Vijaya Kamlesh Tahilramani was appointed as the Chief Justice of the Madras High Court on August 11, 2018. She has replaced Justice Indira Banerjee who has been now appointed as a Supreme Court judge.
First Woman Chief Justice of J&K High Court
Justice Gita Mittal became the first-ever woman Chief Justice of Jammu and Kashmir High Court on August 11. She succeeds Ramalingam Sudhakar and the oath was administered by Governor N.N. Vohra in Srinagar.
Chief Justice of Delhi High Court Sworn in
On August 11, Justice Rajendra Menon was sworn in as the Chief Justice of Delhi High Court. He was earlier the Chief Justice of Patna High Court and has also served as a judge in the Gwalior Bench of the Madhya Pradesh High Court. The oath was administered by the Lt Governor of Delhi, Anil Baijal.
National Handloom Day Celebrated
National Handloom Day (NHD-2018) was launched in 2015 and is celebrated all over India on August 7. It marks the day of launch of the Swadeshi Movement which started on August 7, 1905. Artisans and weavers are awarded 'Sant Kabir' awards to encourage their handiwork and Indian crafts.
Rekha Sharma, Chairperson of National Commission for Women (NCW)
Rekha Sharma has been appointed the chairperson of NCW. She has been holding the additional charge of chairperson after Lalitha Kumaramangalam stepped down from the position in September 2017.
Lok Sabha passes Arbitration and Conciliation Bill (Amendment) 2018
The Bill passed by the Lok Sabha on August 10, was introduced by the Minister for Law and Justice, P.P. Chaudhary on July 18, seeking to amend the Arbitration and Conciliation Act, 1996. A High Level Committee (HLC) with retired SC Judge, Justice B.H. Srikrishna as the chairperson, was constituted by the Central Government to facilitate achieving the goal of improving institutional arbitration.
Amendment Bill for Commercial Disputes
The Lok Sabha passed the Commercial Courts, Commercial Division and Commercial Appellate Division of High Courts (Amendment) Bill, 2018 on July 31 with the Rajya Sabha following suit on August 10. The bill which will now be sent to the President for his consent, seeks to amend the law for prompt elimination of commercial disputes and to reduce the fiscal jurisdiction of commercial courts from Rs 1 crore to Rs 3 lakh.
Parliament passes Bill which is a Boon for Homebuyers
The Insolvency and Bankruptcy Code (Second Amendment) Bill, 2018, was passed by the Rajya Sabha on August 10. The bill had been passed by the Lok Sabha on July 31. In June 2018, The Bill is a relief to homebuyers who invested in housing projects of companies gone bankrupt.
Amendments in Instant Triple Talaq Bill Approved by Cabinet
Amendments in the instant triple talaq bill were approved by the Union Cabinet on August 9 and it will be presented in the Rajya Sabha on August 10, for approval. It not only makes instant triple talaq or talaq-e-biddat illegal and void in any form, but also makes the declaration of talaq a cognizable and non-bailable offence.
NITI Aayog, CII Partnership for Sustainable Development
NITI Aayog and the Confederation of Indian Industries (CII) partnered for meeting the Sustainable Development Goals (SDGs) of India on August 8.
A recent report by the CII on Indian Solutions for the World to Achieve SDGs, covers individual SDG, targets and business implications.
Defence Industrial Corridor Launched in Aligarh
Defence Minister Nirmala Sitharaman and Uttar Pradesh Chief Minister Yogi Adityanath inaugurated the first phase of UP Deference Corridor in Aligarh, Uttar Pradesh on August 11.
Pradhan Mantri Gram Sadak Yojana to Continue
The Cabinet Committee on Economic Affairs, chaired by the Prime Minister approved the continuation of Pradhan Mantri Gram Sadak Yojana (PMGSY) beyond the 12th five year plan period on August 11. It was launched on December 25, 2000, with the objective to provide all-weather road connectivity of unconnected habitations.
India Science Technology and Innovation Portal Launched
Vigyan Prasar, the communication wing of the Union Science Ministry, launched the India Science Technology and Innovation portal on August 11 which will reach out to students, researchers, scholars and scientists, in India and abroad. This comes in the footsteps of the launch of India Science, an internet based science channel which will showcase India's developments in science and technology.
Southern Naval Command Launches Operation 'Madad'
The Southern Naval Command (SNC) at Kochi, Kerala launched operation 'Madad' on August 9, to carry out disaster relief operations in Kerala. Naval helicopters are providing relief material to the flooded areas.
Gurugram's Air Quality Index Hazardous
On August 5, 2018, Gurugram was declared India's most polluted city out of 62 cities in the country by the Central Pollution Control Board (CPCB) on August 5 with an AQI of 321.
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