text:
\section{Introduction}

The RT-2 Experiment onboard the CORONAS-PHOTON mission (Kotov et al. 2008, Nandi et al. 2009) is
a low energy $\gamma$-ray telescope.
The experiment consists of three scientific payloads (two Phoswich detectors and
one solid-state imaging device) and one processing electronic payload. The Phoswich
detectors are RT-2/S and RT-2/G, which will work in the energy range from 15 to 150 keV,
extendable upto 1 MeV. The solid-state imaging payload RT-2/CZT, consists of
three CZT (Cadmium Zinc Telluride) detector modules and one CMOS (Complimentary Metal
Oxide Semiconductor) detector (Kotoch et al. 2010, Nandi et al. 2010).
Data from all these three detectors are processed by an electronic device, namely, RT-2/E
(Sreekumar et al. 2010), which also interfaces with the Satellite system.

All three payloads are placed outside the hermetically sealed vessel of the satellite
and co-aligned to the Sun pointing axis. The instruments have different field of view
(FOV) of $4^\circ \times 4^\circ$ for RT-2/S, $6^\circ \times 6^\circ$ for RT-2/G
and varying FOVs, from $6' \times 6'$ to $6^\circ \times 6^\circ$, for RT-2/CZT
(see Nandi et al. 2010). Though the experiment is dedicated to solar studies of high energy
phenomena, this configuration also allows the study of a large number of galactic and
extra-galactic X-ray sources (within $6^\circ$ around the ecliptic plane below 100 keV and half
the sky in the 100 keV to 1 MeV range -- the latter being due to the fact that the collimators
themselves become transparent in this range). Hard X-ray detectors on board the satellite with
different FOV will also help in the measurement of the spectrum of cosmic X-ray background
(Sarkar et al. 2010).

The paper is divided into the following Sections. In \S 2, we discuss the main scientific goals
of the RT-2 payloads. In \S 3, we describe the RT-2/S and RT-2/G instruments characteristics
as well as the signal processing methods used. In \S 4, we present the testing set-up
and the results on the test and evaluation of these instruments at the laboratory. Finally, in
\S 5, we present our concluding remarks.

\section{Goals and Scientific objectives of RT-2/S \& RT-2/G}

Being the nearest star, the Sun occupies a special place in astrophysical studies as it can be
more closely observed than any other star. Several dedicated satellites (RHESSI, SOHO, GOES etc.)
(Lin et al. 1998, Domingo et al. 1994, Harvey 2007)
have been launched to understand its behavior in a wide energy band of electromagnetic radiation.
Even though its surface temperature is only $\sim$6000 K, it emits X-rays and $\gamma$-rays up to
a few MeV. This is because of rapid magnetic reconnection which produces energetic solar
activities. Apart from the thermal electrons which obey the Maxwell-Boltzmann distribution, the
charged particles, especially electrons, are accelerated by shocks and acquire a non-thermal
(power-law) distribution. These non-thermal electrons emit energetic synchrotron emission.
The Russian satellite CORONAS-PHOTON which was launched on January 30, 2009
is the last in the CORONAS series of satellites dedicated to study these types of solar activities.
The RT-2 Experiment along with the high energy gamma-ray instrument (NATALYA-2M; Kotov et al. 2008)
and other instruments onboard CORONAS-PHOTON (Kotov et al. 2004, 2008) will cover a wide band of
energy from UV to $\sim$ 2000 MeV. One of the main goals of this mission is to understand the
energy transport processes on the solar surface. It is may be due to plasma oscillations, or
pinching or sausage instabilities in the magnetic field. Apart from this, the main objective
of the RT-2 Experiment is to study (i) the time resolved hard X-ray spectra of solar flares,
(ii) the galactic and extra-galactic sources near the ecliptic plane, (iii) the gamma ray
bursts (GRBs) and (iv) diffuse cosmic X-ray background, in a wide energy range.

Since the mission is expected to be in orbit for the next 3-5 years, it is expected to cover
the $24^\mathrm{th}$ solar cycle with the peak expected in 2012. During a peak, the number of
sunspots and flares go up drastically. The magnetic activities associated with the sunspots
which dramatically influence the UV/soft X-ray emissions are therefore expected to peak very soon.
The accompanying soft X-rays also have an impact on the Earth upper atmosphere.
As it is known extreme ultraviolet radiation and the soft X-ray photons basically
form the different layers of the ionosphere (upper atmosphere),
which consists of C, D, E and F layers based on their ion-electron densities.
During a solar flare, the electron number density and the
reflection height change on the sunlit side of the Earth and Very Low Frequency (VLF) radio waves
reflected by the upper atmosphere show a sharp rise in intensity.
From the {\it ab initio} calculation, one can find out the source
strength (solar flare) using the ion-electron density distribution in the D-layer.

Solar flares are the most powerful emission in the entire solar system. They could release
energies from $10^{32}$ to $10^{33}$ ergs over a timescale extending from $100$ to $1000$ seconds.
It is also found that during a flare, the electrons are accelerated to $10 - 100$ keV using a
significant fraction of this energy budget. From RHESSI observation, it has been established
that the particle acceleration and the energy release process (Lin et al. 2003) are linked
together. The instruments RT-2/S and RT-2/G offer a unique opportunity to investigate the
energetics of solar flares, and hence the particle acceleration, in the $15-150$ keV energy
range in `phoswich' mode (i.e., spectral data from the NaI crystal) and in the $\sim 100$~keV -- $1$~MeV
energy range in the spectroscopic mode (i.e., spectral data from CsI crystal using both G1 and G2
amplifiers) during the next solar cycle. Apart from these two `scientific' modes, RT-2/S and RT-2/G
would be operated in two other modes, namely, the Normal mode and the Event mode. Details of these
two operational modes are discussed in Section 3.4.

At the same time as the RT-2/S and RT-2/G observations will be carried about, the RT-2/CZT
instrument will enable imaging the hard X-ray solar flares with high spectral and spatial
resolution in the 20--150 keV energy range (Kotoch et al. 2010).

Other than this, RT-2 will also focus on the large-scale distribution of magnetic flux on the
Sun. The magnetic energy stored at the solar surface may be released gradually or explosively
depending on the dynamics of the magnetic field. This released energy heats up the
``quiet'' corona and also powers the solar wind. Search for nano-flares on the solar surface could
be of interesting prospect, as both RT-2/S and RT-2/G instruments can operate in high resolution
timing mode of 0.1 sec and on rare occasions (depending on the memory availability) in the
time-tagged event mode with a time resolution of 0.3 milliseconds.
The transient bursts on the solar surface for short durations with significant energy budget
($\sim 10^{24}$ ergs) are termed as `nano-flares' (Parker 1998), as compared to the largest solar
flares of energy $\sim 10^{33}$ ergs. It has been observed from several satellite data that
the time-scale variabilities of nano-flares are of $\sim 1.5 - 52$ sec
(Hudson 1991, Shimizu \& Tsuneta 1997).

It is important to study `nano-flares' for several reasons. For several decades, it was a
mystery, why the temperature of the solar corona ($>~10^6$ K), the Sun's outer atmosphere, is much
higher than the temperatures near the Sun's surface (e.g. chromosphere temperature
$\sim 2\times 10^4$ K). But observations made by Japan's Solar-A (Yohkoh) and Solar-B (Hinode)
satellites revealed that nano-flares play an important role in the coronal (active-region)
heating process (Hudson 1991, Shimizu \& Tsuneta 1997, Reale, McTiernan \& Testa 2009). Another
important aspect is to study the distribution law of energy dependence occurrence rate of
nano-flares.

The RT-2 measurements with other mission payloads' data sets will be useful to infer
the composition, flux and anisotropy of energetic ions and electrons with high spatial and
temporal resolution.

\section{Description of the RT-2/S \& RT-2/G instruments}

\subsection {Phoswich Detector}

RT-2/S and RT-2/G payloads consist of NaI(Tl) and CsI(Na) crystals mounted in a
scintillator-phoswich assembly viewed by a photomultiplier tube (PMT). This entire
assembly is procured from M/S Scionix Holland BV, The Netherlands. The
NaI crystal is $3$~mm thick and $116$~mm in diameter. The CsI crystal is tapered
to provide mechanical stability and at the top side it has a diameter of $116$~mm.
The thickness of the CsI crystal is $25$~mm. The two crystals are optically coupled
and hermetically sealed with an entrance window on the NaI(Tl) side and a viewing
glass window coupled to the PMT through an appropriate light guide on the CsI(Na) side.
The Phoswich combination of NaI and CsI crystals has good hard X-ray absorption properties
due to the relatively high effective atomic number (32 for NaI and 54 for CsI crystal) and
efficient optical light emission (415 nm wavelength emission from NaI and 420 nm wavelength
emission from CsI) (Knoll 1999). The NaI(Tl) crystal is sensitive to X-ray photons of
$15 - 150$~keV, whereas CsI(Na) is effective for high energy X-ray/$\gamma$-rays of
$30 - 1000$~keV as well as to charged particle background.

Another important use of both crystals in the Phoswich mode is for the background rejection.
The light signal from the CsI(Na) crystal has a different scintillation decay time (650 ns)
than that from the NaI(Tl) crystal (250 ns) and this distinction is used to eliminate
non X-ray background in the NaI crystal. The charge particle background will be removed by
the upper energy threshold. The Phoswich assembly is viewed by a $76.2$~mm diameter
photomultiplier through a $10$~mm thick light guide. A schematic drawing of `phoswich'
assembly of NaI(Tl) and CsI(Na) crystals with the PMT is shown in Figure 1.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=4.5cm]{fig1a.eps}
\hskip 0.5cm
\includegraphics[width=5.5cm]{fig1b.eps}}}
\caption{A Schematic drawing of Phoswich assembly (NaI and CsI crystals) along with the PMT is
shown in the left and a schematic drawing of one of the payloads (RT-2/S) is shown in the
right.}
\label{kn : fig1}
\end {figure}

The interaction of X-ray photons of energy up to 100 keV with NaI and CsI crystals is fully
dominated by the photoelectric process and thus absorbed radiation (secondary electron-hole
pair absorbed by the impurities) converts into light photons (due to the decay of the excited
impurities). These light photons eventually strike the photo-cathode of the PMT (Knoll 1999)
(gain $\sim$ 10$^6$) and converted into narrow electrical pulse whose magnitude (pulse height) is
proportional to the energy of the incident radiation.

The energy resolution (FWHM) of the scintillator Phoswich is expected to be $18\%$ at $60$~keV
and the pulse height across the crystal should be less than 3\%. The radioactive
isotopes $^{241}$Am ($59.5$~keV), $^{57}$Co ($122$~keV), $^{109}$Cd ($22$~keV and $88$~keV)
were used for laboratory calibration (energies in the parentheses correspond to the major
emission lines of the respective radio-active sources), and results are discussed in
section \S 4. The entire system will be calibrated in flight using a $100$~nano-Curie $^{57}$Co
source.

Electronics of both instruments (schematic drawing of one of the payloads is shown in Figure 1)
are identical, the only difference is that RT-2/G has one
thin Al sheet ($\sim$ 2 mm) above its collimator, to strongly decrease the low energy photons in the
energy range of $13$ to $20$ keV. Indeed, solar flares exhibit a wide
range in intensity and spectral shape. A bright solar flare with a
steep spectrum would produce copious amount of low energy (10 -- 20 keV) photons rendering
spectral measurements above 20 keV difficult as the instrument will be saturated. To deal with such
contingencies, we covered RT-2/G (identical in all other aspects with RT-2/S) with a filter to
decrease low energy photons.

\subsection {Electronics of RT-2/S \& RT-2/G}

Both payloads (RT-2/S \& RT-2/G) are interfaced with the satellite system (SSRNI, a Russian
acronym which means System of Collection and Registration of Scientific Information or SCRSI
in English) through the RT-2 electronic processing device (RT-2/E). RT-2/E receives necessary
commands from
the satellite system and passes them to the individual detector systems for proper functioning
of the detector units and it also acquires data from the detector systems and stores in its
memory for further processing. Detailed description of the functioning of RT-2/E and data
management scheme are discussed in Sreekumar et al. (2010).

The electronics system in the detector module consists of i) front end electronics for the
Phoswich scintillator, ii) electronics for pulse shape (PS) and pulse height (PH), iii)
FPGA (Field Programmable Gate Array) based data packaging system, iv) high voltage (HV) DC-DC
converters and distribution box and v) low voltage DC-DC converter. The block composition of
detector electronics is shown in Figure 2.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=10.0cm]{fig2.eps}}}
\vskip 0.0cm
\caption{Block diagram of electronic components of RT-2/S and RT-2/G.}
\label{kn : fig2}
\end {figure}

The electronics system receives signals from the NaI(Tl) / CsI(Na) scintillator Phoswich
detector assembly. These signals are analyzed and the details are discussed in the next section
(\S 3.3).
The data are encoded in the proper format for dispatching to the RT-2/E device. Since it is very
difficult to handle a large range of energy by a single amplifier, the entire energy range of the
Phoswich detector is covered by two different amplifiers, namely G1 and G2. This is done
electronically by comparing the detector pulse output to two analog voltages LLD (Lower Level
Discriminator) and ULD (Upper Level Discriminator) so
that pulses between LLD and ULD are deemed to be G1 and above ULD is deemed to be G2. G1 contains
information pertaining to both NaI(Tl)  and CsI(Na) crystals (which can be segregated using
the pulse shape) and G2 is presumed to be coming from the CsI(Na) crystal. The pulse shape
(PS) is measured using a 7 bit counter and the discrimination is done digitally by comparing the
pulse shape with ps$\_$cut (ps $<$ ps$\_$cut is deemed to be coming from the NaI crystal and
ps $>$ ps$\_$cut from CsI).

The pre-amplifier is designed using discrete components. It is used in an inverting operational
amplifier mode which converts the -ve input from PMT into +ve pulse with a gain factor of 1 to 2.
Two post amplifiers (G1 \& G2) with different gains and different filters are used to cover the
different energy ranges of interest. These discrete post amplifiers are of non-inverting nature
with provision of adjustable gain (during ground testing, not by command).
Amplifier G1 will cover energy range from $15 - 210$~keV (the approximate energy ranges are
15 keV - 100 keV for G1-NaI; 30 keV - 210 keV for G1-CsI) \& G2 from $40$~keV to $1$~MeV. These
ranges can be scaled by changing the HV through command and the LLD (15 keV) can be separately changed.

The NaI and CsI crystals have different decay times. The gain from these two detectors (crystals)
is a function of the time constant of the pre-amplifiers (which is common for both
detectors), resulting in a gain difference (of a factor of 1.8) of
the outputs of NaI and CsI for the same energy deposition. These energy ranges were measured
during the ground calibration. Also G1-NaI, G1-CsI \& G2 spectra and light curves are divided
into 8 different counters (4 counters for G1-NaI, 2 counters for G1-CsI and 2 counters for G2).
The channel numbers of these counters and the corresponding energy ranges are shown in Table 1,
for the default ground settings. These values can be changed by command. The electronics of both
instruments are identical and have the same working energy ranges. The basic differences of both
payloads are mentioned in Section 1 and Section 3.1.

\begin{table}[h]
\centering
\centerline {Table 1: RT-2/S \& RT-2/G channel boundary (default) and energy ranges}
\vskip 0.2cm
\begin{tabular}{|l|c|c|c|c|}
\hline
Amplifiers & Counters & Channel ranges &\multicolumn{2}{|c|}{Energy Ranges (keV)*}\\
\cline{4-5}
 & &(default)&~~~~~RT-2/S~~~~~&RT-2/G\\
\hline
        & C1 & 0 - 140   & $<$ 13  & $<$ 13 \\
        & C2 & 141 - 280 & 13 - 27 & 13 - 27\\
G1-NaI  & C3 & 281 - 560 & 27 - 55 & 27 - 56\\
        & C4 & 561 - 1023& 55 - 102& 56 - 104\\
\hline
        & C5 & 0 - 256   & $<$ 33   & $<$ 34\\
G1-CsI  & C6 & 257 - 1023& 33 - 209 & 34 - 209\\
\hline
        & C7 & 0 - 64    & $<$ 48& $<$ 246\\
G2      & C8 & 65 - 255  & 48 - 570& 246 - 1000\\
\hline
\end{tabular}

*Differences in energy boundaries of all 8 counters (C1,...,C8) of both
payloads (RT-2/S and RT-2/G) are due to different technical setting of operational
conditions (eg. HV, LLD, ULD, PS cut etc.).
\end{table}

The operational aspects of both payloads are identical. They operate with 27$^{+7}_{-3}$
Volt (Power bus of 27$^{+7}_{-3}$ V, from the satellite system, is routed through RT-2/E). The
total power consumption is limited to 4.5$\pm$0.5 Watt for each payload.
A low voltage MDI DC-DC converter is used to convert the input voltage (27 Volt) to $\pm$ 15 Volt
and +5 Volt to drive the different components of the individual payloads.
The +15 Volt is also converted separately through a voltage regulator circuit to
high voltage ($\sim$ 700 Volt) needed for biasing the PMT that is operable in a
400-900 V range. The HV can be commanded to any value in this range with an
accuracy of $\sim$ 4.5 Volt. The Pulse Shape Discriminator (PSD) of the two crystals (NaI \& CsI)
and Lower Level Discriminator (LLD) for the two amplifiers (G1 \& G2) can be also commanded.
Voltage Control Oscillator (VCO) is used to monitor the instrument health parameters, such as
+5 Volt supply, temperature (Thermistor), High Voltage (HV) \& LLD.

\subsection {Signal processing method in RT-2/S \& RT-2/G}

When an incident radiation (X-ray event) interacts with the NaI(TI) or CsI(Na) crystal, it
gives out light photons which are converted into electrical pulses by a PMT. Light outputs
from NaI and CsI crystals have decay time scales of 250 ns and 650 ns respectively. Pulses
from the detector (crystal) are amplified in a pre-amplifier and two post amplifiers (G1 and G2).
The output from the selected post amplifier (G1 or G2) is digitized using an analog to digital
converter (ADC). The ADC is 12 bits wide and has a typical conversion time of 10 $\mu$s. The block
diagram of time scale for processing of an event is shown in Figure 3 and the
events have a fixed dead time of $\sim$20 $\mu$s.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=10.0cm]{fig3.eps}}}
\vskip 0.0cm
\caption{Block diagram of the time scale for processing of an event.}
\label{kn : fig3}
\end {figure}

The peak of the pulse output from the detector is proportional to the charge deposition in the
crystal and hence the pulse height (PH) denotes the radiation energy. PH is converted into a 12 bit
digital data and sent to FPGA. PS denotes the pulse decay time,
which gives a hint of whether the event is occurring in NaI or CsI. PSD
data is directly transmitted to the FPGA in a 1 bit format. The value of this bit (i.e, based on
the PS information) is determined by the FPGA. This data is stored, by the FPGA, into a memory,
for a time determined by RT-2/E. RT-2/E will read this data every second. In the Normal mode, the
time required to send the data from RT-2/S (RT-2/G) to RT-2/E is $\sim0.21$ sec. In the Event mode,
it depends on the number of events occurred and the maximum time required is 1 sec. The maximum
number of events to be handled in event mode is 7360 events. This restriction is due to the
onboard memory size. Detail discussion of the two operational modes (Normal and Event mode) are
given in the next section.

\subsection {Data specifications and operation of RT-2/S \& RT-2/G}

As we already mentioned, there are two different modes in which RT-2/S and RT-2/G can
be operated - the Event mode and the Normal mode. In the Event mode, every event is
time-tagged with an time accuracy to 0.3 ms and in the Normal mode all the spectral data are
accumulated. Here, eight channel count rates are stored every 10 ms and are sent to RT-2/E every
second. The Normal mode data are processed in RT-2/E with a best possible time
resolution of 1 s for the full spectrum and 10 ms for the 8 channel count rates.

A `pure' event (registered X-ray event on the detector) consists of a pulse height (PH) of 12 bits,
a pulse shape (PS) of 7 bit, an amplifier identification (G1 or G2) of 1 bit and the time of
registration of the events of 12 bits. Therefore, the first 20 bits carry the spectral information
and the last 12 bits carry the time-tagged information of each event. In the Event mode, time-tagged
information is associated with the events and it is incremented after every event, whereas in the
Normal mode time-tagged information is used to count the total no. of events that are registered in
every 10 ms (calculation is done internally by the FPGA of the detector processing electronics).
Data specifications of the two different modes are given below.

\subsubsection {Event mode}

In the Event mode, each detector `event' is coded into 32 bits (4 bytes). The maximum number of
events that can be stored in the memory is 7360 events, which are sent to RT-2/E, whenever `1 sec'
command is received. The event data structure is given in the following format:

\begin{itemize}

\item[$\bullet$]{\bf Event block:} 32 bits $\times$ number of events (the number of maximum events
that can be stored in the memory is 7360). Each event consists of 32 bits {\it (D0-D11: 12 bit ADC,
D12: 1 bit G1/G2 Selection, D13-D19: 7 bit PSD and D20-D31: 12 bit Timing)} data.

\end{itemize}

The Event mode is basically used to verify the detector functionality as in this mode, the data
directly come to the processing electronic device (RT-2/E) from the detectors. For scientific
purposes, this mode could be operated to make high time resolution (0.3 ms) observations such as
the Crab Nebula. Due to the onboard memory restriction, `memory full signal' will be noticed for
an observation longer than $\sim 200$s and the system will go to the `BAD' mode
(i.e., non accumulation of scientific data). Restriction of
the operation in this mode could be done by time-tagged commands to avoid memory overflow.

\subsubsection {Normal mode}

In the Normal mode, the event data (20 bits of scientific information and 12 bits of timing data),
along with the health parameters encoded in VCO, are packaged by the FPGA and kept in a memory
page. They contain a header block including the health parameters and the counts, spectrum block, timing
block with high time resolution of the counter. The normal mode data has the following format:

\begin{itemize}

\item[{\large $\bullet$}] {\bf Header block (18 bytes):} VCO (2 bytes) and
8 counters (16 bits each) based on the PH values. The counter values are total
counts over 4 channel intervals (PH between 0 to ch1, ch1 to ch2, ch2 to ch3
and $>$ ch3) in G1-NaI; over 2 channel intervals (0 to ch5 and $>$ ch5) in G1-CsI
and over 2 channel intervals (0 to ch7 and $>$ ch7) in G2.
Header contains mode ID - 0: Normal mode and 1: Event mode.

\item[{\large $\bullet$}] {\bf Spectrum block (4864 bytes):} G1-NaI (PH) :
$1024 \times 2$ bytes + G1-CsI (PH) : $1024 \times 2$ bytes + G2 (PH) : $256 \times 2$
bytes + PS : $128 \times 2$ bytes.

\item[{$\bullet$}] {\bf Timing block (1600 bytes):} 100 Timing blocks
$\times 8$ counters $\times 2$ bytes (counters in each bin will count for
10 ms).

\end{itemize}

\begin{table}[h]
\centering
\centerline {Table 2: RT-2/S and RT-2/G data specifications}
\vskip 0.2cm
\begin{tabular}{|l|c|c|c|}
\hline
\multicolumn{4}{|l|}{\bf VCO data: (2 bytes):}\\
\hline
D15 &\multicolumn{2}{|c|}{D14-D12} & D11-D0 \\
\hline
Mode Id (0/1) &\multicolumn{2}{|c|}{VCO Channel Numbers (0-7)} & VCO Counts (values) \\
\hline
\hline
\multicolumn{4}{|l|}{\bf Scientific Data in the NORMAL Mode (Id: `0') (Total 6480 bytes):}\\
\hline
         & G1-NaI & 2048 bytes & 1024 spectral ch. $\times$ 1 word*\\
\cline{2-4}
Spectrum & G1-CsI & 2048 bytes & 1024 spectral ch. $\times$ 1 word\\
\cline{2-4}
         & G2     & 512 bytes & 256 spectral ch. $\times$ 1 word\\
\cline{2-4}
         & PSD    & 256 bytes & 128 spectral ch. $\times$ 1 word\\
\hline
Timing & 800 words & 1600 bytes & 8 ch. $\times$ 100 blocks $\times$ 1 word\\
\hline
Counters & 8 words & 16 bytes & 8 counters $\times$ 1 word\\
\hline
\hline
\multicolumn{4}{|l|}{\bf Scientific Data in the EVENT Mode (Id: `1') (4 bytes/event):}\\
\hline
Time & PSD & G1/G2 & ADC \\
\hline
D31-D20 & D19-D13 & D12 & D11-D0 \\
\hline
\end{tabular}

*1 word = 2 bytes = 16 bits.
\end{table}

The data structure of stored (scientific) data of RT-2/S and RT-2/G are summarized in Table 2.
On the receipt of a `1 sec' command from RT-2/E (issued every second), the stored data are sent
to RT-2/E for further processing in specific formats (Sreekumar et al. 2010).
The header, the spectral and the timing blocks are sent in the Normal mode and
the header and the event block are sent in the Event mode. These modes of operation could be
decided by ground commands (Sreekumar et al. 2010).

\section{Tests and Evaluation of the RT-2/S \& RT-2/G payloads}

It is essential to carry out extensive space qualification tests (on ground)
of the scientific payloads in order to ensure that they can sustain and perform
according to expectations during their in-flight lifetime.
An instrument's proper functionality (scientific performance) is based on
High Voltage (HV) and LLD/ULD operation, stability of Pulse shape (PS) and Pulse height (PH),
health parameters, quality of spectral (scientific) data etc. Both payloads (RT-2/S and
RT-2/G) were space qualified independently.
The space qualification tests we performed include:

\begin{itemize}

\item[{$\bullet$}] {\bf Vacuum Test:} Payloads were kept in Vacuum chamber of pressure
$\sim$10$^{-6}$ mm of Hg at 23$^\circ$C. During this test, the instrument's functionality was
verified. Major test result of HV variation is summarized in Section 4.3.

\item[{$\bullet$}] {\bf Thermal Test:} Both payloads were tested at various temperature
conditions ranging from -10$^\circ$C to 40$^\circ$C. In this condition, the functional tests
results are summarized in Section 4.4 and 4.5.

\item[{$\bullet$}] {\bf Vibration Test:} Vibration test is essential to check the resonance effect
on the detector structure as well as electrical card systems of the payloads. Before and after
this test, instruments functionality were verified and we did not find any malfunction in both
instruments.

\item[{$\bullet$}] {\bf EMI Test:} The electro-magnetic interference (EMI) test is important for the
RT-2 instruments. Radiation from the other devices (such as radio transmitting device on the
spacecraft) may affect the normal behavior of the RT-2 payloads. While doing this test,
functionality of both detectors were verified.

\item [{$\bullet$}] {\bf SRC Test:} The standard room condition (SRC) test was carried to check
the normal functionality of both detectors. This test was carried out after each space
environment test. This test includes the verification of total power consumption, health
parameter, HV and LLD/ULD operation, scientific data etc.

\end{itemize}

During these laboratory tests, the complete functioning of both RT-2/S and
RT-2/G payloads were investigated and we calibrated HV, LLD, PS and PH
variation with temperature, energy spectra etc. Testing
of both payloads were carried out for a period of three months.
The results are discussed in the following sections. In the next section, the lab testing set-up
is described.

\subsection{Testing set-up of RT-2/S and RT-2/G}

The overall testing of RT-2/S, RT-2/G, RT-2/CZT \& RT-2/E were carried out with Ground Check-Out
system (KIA, a Russian acronym). In reality, KIA mimics the total functionality of the Satellite
system (SSRNI) for the RT-2 system. We used the check-out software written in LabVIEW platform
to test the individual and complete packages (payloads).
Details of the overall set-up schemes are discussed in Sreekumar et al. (2010).

We tested the instruments by directly interfacing it with a PC via the OPTO device, the SCB-68
connector box and the NI data acquisition card (PCI 6534). The OPTO device was used to
isolate the payloads electrically from the PC system using a buffer and an opto-isolator. The
LabVIEW based software along with the OPTO device mimics the functioning of the processing
electronic device (RT-2/E). Figure 4 shows the schematic block diagram of the testing set-up used.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=7.0cm,angle=270]{fig4.ps}}}
\vskip 0.0cm
\caption{Schematic block diagram of laboratory set-up for testing of payloads.}
\label{kn : fig4}
\end {figure}

The complete control of the instrument operation was done by executing series of commands
setting the channel boundary, the HV, the PS cut and the LLD value of each payload. The
command structure used to set the different instrument parameters is given in Table 3.

RT-2/S \& RT-2/G are normally operated with a high voltage (HV) of $\sim$ 710 Volt (command:
hx07A6 for S, hx27A6 for G), a LLD threshold of 0.86 V (command: hx0628 for S, hx2628 for G)
and a PS cut value equal to channel 26 (command: hx051A for S) and channel 28 (command: hx251C
for G).

\begin{table}[h]
\centering
\centerline {Table 3: RT-2/S \& RT-2/G detector commands}
\vskip 0.2cm
\begin{tabular}{|c|c|c|l|}
\hline
{\bf Command Type}&\multicolumn{2}{|c|}{\bf HEX Command of}&{\bf Description}\\
\cline{2-3}
 & RT-2/S & RT-2/G & \\
\hline
`1 sec' & 0800 & 2800 & Set detector in normal mode\\
\cline{2-4}
command & 0801 & 2801 & Set detector in event mode\\
\cline{2-4}
 & 0802 & 2802 & Corona override*\\
\hline
Range setting & 00xx & 20xx & Set ch. boundary for G1-NaI (ch1)\\
\cline{2-4}
command**  & 01xx & 21xx & Set ch. boundary for G1-NaI (ch2)\\
\cline{2-4}
(value = `xx' times 4, & 02xx & 22xx & Set ch. boundary for G1-NaI (ch3)\\
\cline{2-4}
except ch7 boundary) & 03xx & 23xx & Set ch. boundary for G1-CsI (ch5)\\
\cline{2-4}
	 & 04xx & 24xx & Set ch. boundary for G2 (ch7)\\
\hline
PS cut value &05xx & 25xx& Set PS cut value (ps$\_$cut) to separate\\
(7bit value) &     &     & G1-NaI \& G1-CsI spectra\\
\hline
DAC setting & 06xx & 26xx & Set LLD value from DAC\\
\cline{2-4}
(8bit value)& 07xx & 27xx & Set HV value from DAC\\
\hline
RAM select & 0c00 & 2c00 & Select section 1 (256 Kbytes) of RAM\\
\cline{2-4}
command & 0e00 & 2e00 & Select section 2 (256 Kbytes) of RAM\\
\hline
\end{tabular}

*A facility is also kept to suppress the automatic corona sensing and this can be activated by
the `corona-override' command.

**Range setting command: `xx' refers to HEX value. The actual channel boundary is given by four
times of the `xx' value for ch1, ch2, ch3 and ch5, whereas for ch7 the value is just `xx'. For
example, if channel boundary of `ch1' is to be set at 140 channel, then `xx' value should be hx23
(as hx23 = dx35 and original channel value is 35 x 4 = 140 channel).

\end{table}

\subsection{Health parameters of the RT-2/S \& RT-2/G instruments}

There are eight VCO channels giving health information on each instrument.
Six over the eight channels were configured to certain voltage levels, which are given in
Table 4. Each VCO channel shows some count values that can be related to a physical or
instrumental parameter thanks to a dedicated calibration. As an example, the variation of VCO
counts for HV variation is shown in Figure 5.
The different health parameters to be monitored during various space environmental tests are
given in Table 4.
The channels 3 \& 7 were kept unused.

\begin{table}[h]
\centering
\centerline {Table 4: RT-2/S \& RT-2/G health parameters (VCO channels)}
\vskip 0.2cm
\begin{tabular}{|c|c|c|}
\hline
{\bf Channel No.}&{\bf Description}&{\bf Operating Voltage}\\
 & & {\bf Level}\\
\hline
0 & Supply Voltage & 5.0 $\pm$ 0.5 V\\
\hline
1 & Thermistor & 1.5 - 5.5 V\\
\hline
2 & Supply Analog & 5.0 $\pm$ 0.5 V\\
\hline
3 & NC* &  0 V\\
\hline
4 & HV Feedback & 1.5 - 5.0 V\\
\hline
5 & HV Reference & 1.5 - 5.0 V\\
\hline
6 & LLD & 0.5 -1.6 V\\
\hline
7 & NC* &  0 V\\
\hline
\end{tabular}

*NC: not configured
\end{table}

\subsection{High Voltage (HV) calibration of RT-2/S}

The normal operation of HV in space environment is an important issue, as the present detectors
functionality depends on HV operation. So, we calibrated the HV of both instruments during the
Vacuum test, which mimics the space environment conditions.
The high voltage (HV) calibration of the RT-2/S payload was done by changing input digital to analog
converter (DAC)
values by steps through commands. Each DAC value corresponds to different HV and so different
VCO counts. DAC values were varied from 134 to 208 and corresponding VCO counts (channel 5) were
found to be varying from 4976 to 11280. The HV calibration result is shown in Figure 5. It is
found that the instrument is operable in the linear regime of HV variation from 565 to 900 Volt
(within the specified operating range of PMT).
During each step of HV variation, we checked the Pulse height (PH) variation, as it is important
for calibration of the energy spectrum.
We also found similar behavior of HV variation of the RT-2/G payload.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=5.0cm,angle=270]{fig5.ps}}}
\vskip 0.0cm
\caption{High Voltage (HV) calibration with DAC value (commands).}
\label{kn : fig5}
\end {figure}

\subsection{Thermistor calibration of RT-2/S}

The thermistor is the temperature sensor placed inside each instrument to monitor its
temperature variation. The sensor (resistor-type) is the same on both instruments. The thermistor
resistance, which changes with temperature, is measured as VCO counts. Through the
monitoring of the VCO counts (channel 1), we can calibrate the temperature of the payload.
The instrument is operable in the temperature range from -10$^\circ$C to +40$^\circ$C.
Therefore, we measured the temperature variation of the thermistor in the same temperature
range. The VCO count variation with temperature is shown in Figure 6. The plot is not a
linear function, because the in-built resistance of the thermistor varies non-linearly
with temperature. The thermistor resistance is coupled to the VCO circuit to measure the
voltage change (see Table 4) and hence the VCO counts. Looking at the VCO counts
(channel 1) from the scientific data, one can estimate the onboard payload temperature.

We did the temperature related test of both instruments for long duration. We kept the
instruments inside a thermal chamber for at least 3-4 hrs to attain a particular temperature,
such that each part of the instrument get heated uniformly. Once the thermal equilibrium is
reached, we verified the normal functionality (health parameter, temperature, spectral
information etc.) of each instrument.
We also found similar behavior in temperature variation for the RT-2/G payload.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=5.0cm,angle=270]{fig6.ps}}}
\vskip 0.0cm
\caption{Thermistor calibration: Variation of VCO values with temperature for RT-2/S payload.}
\label{kn : fig6}
\end {figure}

The nominal operating temperature of both instruments is $\sim$23$^\circ$C.
Initial results from the onboard data showed that the temperature of both payloads are
maintained at comfortable operating range of +18$^\circ$C to +25$^\circ$C (Nandi et al. 2009).

\subsection{Pulse shape (PS) \& Pulse height (PH) variation with temperature of RT-2/S}

The study of PS and PH variation is important as both change with temperature
and therefore this may have some consequences on the operation of the
instruments. Indeed, PS denotes whether an event is occurring in the NaI or
CsI crystal in the PSD spectrum. Therefore, the stability of PS is crucial to
ensure the reability of the spectral information coming from both crystals.
So, if there is any change in the PS cut value due to a temperature change, we
can adjust the change in PS cut through commands. PH gives some information
on the energy of an event. As an example, PH has a value of around channel 600
for $^{241}$Am 59.5 keV photons in the NaI crystal. From channel-energy
calibration (discussed in the next section), we can derive the energy
resolution as well as the gain (keV/Chan) of both instruments.  If
there is any change in gain, we can adjust the gain through a HV command.

We made a systematic study of PS and PH variation with temperature over the
in-flight operating temperature range (from -10$^\circ$C to +40$^\circ$C). In Figure 7(a), the
PS variation with temperature is shown. PS appears to be almost stable over
the operating temperature range with a maximum variation of 7\% with respect to
the average PS value.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=4.5cm,angle=270]{fig7a.ps}
\hskip 0.02 cm
\includegraphics[width=4.5cm,angle=270]{fig7b.ps}}}
\vskip 0.0cm
\caption{(a) Pulse shape (PS) variation as a function of temperature and (b) Pulse Height (PH)
variation ($^{241}$Am source peak @ 59.5 keV) of G1-NaI spectrum with temperature.}
\label{kn : fig7(a-b)}
\end {figure}

In Figure 7(b), we plotted the pulse height (PH) variation of G1-NaI spectra with temperature
varying from -10$^\circ$C to 40$^\circ$C. To study the temperature effect on PH, we used the
$^{241}$Am 59.5 keV line as a reference. At the room temperature (+$25^\circ$C), PH is stable at
around channel 600. The PH variation is observed to be less than 6\% over the entire temperature
range.

We also performed the same PH measurement for G1-CsI spectrum and found similar PH variation
using a $^{57}$Co 122 keV line in the G1-CsI spectrum. But, we did not measure the PH
variation of G2 spectra. PS measurement is not applicable to G2 spectrum, as G2 spectral data
directly come from the CsI crystal.

We also thoroughly studied the PS and PH variation of RT-2/G detector with temperature and we
found similar results for PS and PH variation of RT-2/G.

\subsection{Calibration of the G1-NaI spectral response of both RT-2/S and RT-2/G}

To calibrate the G1-NaI spectrum (of both instruments), which covers 1024 channels, we used
two strong radio-active sources ($^{241}$Am \& $^{109}$Cd). The main emission line energies of
$^{241}$Am are at 13.95 (13.3\%), 17.74 (19.4\%), 20.8 (4.9\%), 26.35 (2.4\%) \& 59.54 (35.8\%) keV
and for $^{109}$Cd are at 22.16 (84\%) \& 88.04 (4\%) keV (in the parenthesis, the source strength of
respective emission lines is mentioned. See for reference, http://ie.lbl.gov/education/isotopes.htm).
For the calibration purpose, we used only three emission peaks
(59.54 keV of $^{241}$Am and 22.16, 88.04 keV of $^{109}$Cd) of these two sources, as all of
the three lines are well separated in energies (no chance of blending with one another). The low
energy emission lines (13.95 and 17.74 keV) are not used for calibration, as both lines are
not resolved completely in RT-2/S and suppressed in RT-2/G due to the
Al filter and too weak when compared to the 22 keV emission line of $^{109}$Cd emission.
The energy spectra of G1-NaI of both instruments are shown in Figures 8(a,b) and 9(a,b). Both
spectra are taken in identical operational condition with the same exposure time of 200 sec. The
standard emission lines of $^{241}$Am and $^{109}$Cd are detected in the NaI spectra along with
a weak background continuum. The difference in peak amplitude of $^{241}$Am (or $^{109}$Cd)
emission feature in RT-2/S and RT-2/G is mostly due to the difference in operational
setting conditions, such as HV and LLD setting, PS cut value etc. of both instruments. The
significant amplitude difference could not be due to Quantum Efficiency (QE) difference (although
we did not perform any QE test for both instruments) as both the crystals (detectors) are
completely identical in nature.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=4.5cm,height=5.0cm,angle=270]{fig8a.ps}
\hskip 0.01cm
\includegraphics[width=4.5cm,height=5.0cm,angle=270]{fig8b.ps}
\vskip 0.1cm
\includegraphics[width=5.5cm,height=5.0cm,angle=0]{fig8c.ps}}}
\hskip 0.01cm
\caption{Energy calibration of RT-2/S. (a) The top left panel shows the G1-NaI
spectrum obtained using a $^{241}$Am source. Note that the 13.94 \& 17.74 keV lines and 20.8 \&
26.35 keV lines are blended; (b) the right panel shows the G1-NaI spectrum obtained using
$^{109}$Cd (emission peaks: 22 keV, \& 88 keV); (c) bottom panel: the channel-energy
calibration curve is plotted with the mark of identification (diamond point) of the
$^{121}$I decay peak at 57.19 keV (see text for details).}
\label{kn : fig8(a-c)}
\end {figure}

We fitted each peak profile (marked with solid black line) using a Gaussian in order to find their
centroid values (channel
numbers). Importantly, it is noted that the $^{241}$Am (59.5 keV) line is asymmetrical in nature
towards the low energy (Figures 8(a) and 9(a)), while other emission lines are almost symmetrical
in nature. The asymmetry is due to the superposition of the background line ($^{121}$I decay peak,
channel values are close to the $^{241}$Am @ 59.5 keV line, see Table 5). This line is clearly
seen in Figures 8(b) and 9(b).
The centroid values of all the emission lines are measured in channel number
using the background subtracted data.
The characteristics of the background spectrum are discussed in the next section.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=4.5cm,height=5.0cm,angle=270]{fig9a.ps}
\hskip 0.01cm
\includegraphics[width=4.5cm,height=5.0cm,angle=270]{fig9b.ps}
\vskip 0.1cm
\includegraphics[width=5.5cm,height=5.0cm,angle=0]{fig9c.ps}}}
\hskip 0.01cm
\caption{Energy calibration of RT-2/G. (a) The top left panel shows the G1-NaI
spectrum obtained using a $^{241}$Am source. Note that the 20.80 keV and 26.35 keV
lines are blended; (b) the right panel shows the G1-NaI spectrum obtained using
$^{109}$Cd (emission peaks: 22 keV, \& 88 keV); (c) bottom panel: the channel-energy
calibration curve is plotted with the mark of identification (diamond point) of the
$^{121}$I decay peak at 56.05 keV (see text for details).}
\label{kn : fig9(a-c)}
\end {figure}

Knowing the channel values of the line centroids, we are able to compute the energy scale.
Since the detector spectral response
should be linear, we fitted a linear function to our measurements using the least square
fit technique. The G1-NaI channel-energy calibration plots are shown in Figure 8(c) and in
Figure 9(c) for both instruments. The derived relation is useful to calibrate the first
four channel boundaries (see Table 1) of both instruments. The lower and upper energy
thresholds of the G1-NaI energy scale are around 13 keV and 100 keV with a gain factor
of 0.101 keV/Chan for RT-2/S and of 0.104 keV/Chan for RT-2/G, respectively. The differences
in energy boundaries of all four channels between both instruments (see Table 1) are due to
the different technical settings of the operational conditions (e.g. the HV setting, LLD/ULD
setting and PS cut values etc.).

Figure 8(a) shows two emission lines at low energy. The two features
correspond to two blended lines: i) 13.95 keV and 17.74 keV; ii) 20.8 keV and
26.35 keV. Because it is impossible to resolve these lines, we used a single
Gaussian line profile to fit these blended lines and to derive their mean line
centroid. Note that for RT-2/G only the second blended line (20.8 keV and
26.35 keV) is seen due to the Al filter. The fitted channel numbers and
calibrated energy values of all the different emission lines are shown in
Table 5 along with their corresponding 1 sigma errors.
From Figures 8(a) and 9(a), it is evident that though the lower energy threshold of both instruments
are at $\sim$13 keV (see Table 1), there is a significant difference in amplitude at lower
energies due to the presence of the Al filter.

\begin{table}[h]
\centering
\centerline {Table 5: Identification of emission lines and their channel-energy calibration}
\vskip 0.2cm
\begin{tabular}{|l|c|c|c|c|}
\hline
{\bf Energy Peaks}&\multicolumn{2}{|c|}{\bf RT-2/S}&\multicolumn{2}{|c|}{\bf RT-2/G}\\
 \cline{2-5}
(keV) &{\bf Channel No.}&{\bf Energy (keV)}&{\bf Channel No.}&{\bf Energy (keV)}\\
\hline
\multicolumn{5}{|l|}{\it Emission lines used for calibration:}\\
\hline
& & & & \\
{\bf 22.00 }& $228.22_{-0.32}^{+0.28}$ & $21.796_{-1.033}^{+1.058}$ & $230.95_{-0.35}^{+0.35}$ & $21.779_{-1.118}^{+1.148}$ \\
& & & & \\
\hline
& & & & \\
{\bf 59.50 }& $605.41_{-0.91}^{+0.89}$ & $59.971_{-1.499}^{+1.537}$ & $597.22_{-0.92}^{+0.88}$ & $60.011_{-1.624}^{+1.668}$ \\
& & & & \\
\hline
& & & & \\
{\bf 88.00 }& $879.69_{-8.69}^{+8.21}$ & $87.732_{-1.839}^{+1.885}$ & $862.57_{-3.97}^{+3.13}$ & $87.709_{-1.991}^{+2.045}$ \\
& & & & \\
\hline
\multicolumn{5}{|l|}{\it Calibrated emission lines:}\\
\hline
& & & & \\
{\bf 13.94 \& 17.74}& $183.63_{-0.93}^{+0.87}$ & $17.283_{-0.977}^{+1.002}$ & - - - & - - - \\
{\bf (blended peak)}& & & & \\
\hline
& & & & \\
{\bf 20.8 \& 26.35 }& $274.06_{-3.46}^{+2.94}$ & $26.435_{-1.089}^{+1.116}$ & $282.79_{-1.49}^{+1.81}$ & $27.190_{-1.189}^{+1.221}$ \\
{\bf (blended peak)}& & & & \\
\hline
& & & & \\
{\bf $^{121}$I decay peak }& $577.92_{-4.02}^{+4.08}$ & $57.189_{-1.465}^{+1.502}$ & $559.31_{-2.01}^{+1.89}$ & $56.054_{-1.572}^{+1.614}$ \\
{\bf ($\sim$58.00 keV)}& & & & \\
\hline
\end{tabular}
\end{table}

As mentioned earlier, there is a prominent background line observed at around
58 keV (see Figs. 8(b) \& 9(b)).
This line is due to activation of the Iodine in the NaI/CsI crystal via
inelastic scattering of $^{57}$Co gamma-rays producing a $^{121}$I decay peak (see
Gruber et al. 1996, Rothshild et al. 1998, Nandi et al. 2009).
As the exact energy of this emission line is `unknown', we could not use it in the calibration
of the energy scale even if its intensity is larger than the 88 keV $^{109}$Cd line. Using the
derived channel-energy relation, the $^{121}$I decay peak line is found to be
at 57.19 keV and 56.05 keV for RT-2/S and RT-2/G respectively (see Table 5).
However, once the energy of this particular line is known, it becomes an useful tool for
onboard calibration of G1-NaI spectra for both instruments.

The scintillator crystals are low to medium energy resolution ($\Delta E/E$, where $\Delta E$ is
the FWHM of the Gaussian at the particular energy E) detectors with
energy resolution of about 18\% at 60 keV. The energy calibration need to be a factor of 10
better than the basic energy resolution, hence we have targeted an energy calibration accuracy
of about 1 - 2 keV. The measured G1-NaI energy resolution is around 17.54\%$\pm 0.55$
and 17.68\%$\pm 0.27$ at 59.5 keV for the RT-2/S and RT-2/G instruments, respectively.
We performed similar energy resolution measurements with other sources to study the behavior
of energy resolution {\it vs.} energy (Figures
10(a) and 10(b)). The results are quite satisfactory and both the plots (i.e.,
energy resolution vs energy) are fitted with a simple power-law of
index -0.123 and -0.127 for NaI spectra of S and G respectively.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=5.2cm,height=4.8cm,angle=0]{fig10a.ps}
\hskip 0.01cm
\includegraphics[width=5.2cm,height=4.8cm,angle=0]{fig10b.ps}}}
\hskip 0.01cm
\caption{The variation of energy resolution of NaI spectrum as a function of energy for both
instruments (left panel for RT-2/S and right panel for RT-2/G).}
\label{kn : fig10(ab)}
\end {figure}

In the next section, we discuss the G1-CsI and G2 energy calibration procedure.

\subsection{Laboratory Calibration of RT-2/S \& RT-2/G Spectra}

As already discussed, both instruments have three separate energy spectra: G1-NaI, G1-CsI
and G2 with different characteristics. The G1-NaI and G1-CsI spectra cover 1024 channels, whereas
G2 spectrum covers only 256 channels. PSD technique is used to discriminate the events that are
detected in NaI and CsI crystals for G1 amplifier only. The PSD spectrum of both instruments are
shown in Figures 11(a) and 12(a) (corresponding PS cut values are marked in the respective
Figures). A high gain amplifier G2 is also used to register the high energy events in CsI
crystal to have G2 spectrum.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=4.3cm,angle=270]{fig11a.ps}
\hskip 0.01cm
\includegraphics[width=4.3cm,angle=270]{fig11b.ps}}
\vskip 0.02cm
\centering{
\includegraphics[width=4.3cm,angle=270]{fig11c.ps}
\hskip 0.01cm
\includegraphics[width=4.3cm,angle=270]{fig11d.ps}}}
\vskip 0.06cm
\caption{Four spectra of RT-2/S payload: (a) PSD spectrum, (b) G1-NaI(Tl) spectrum, (c) G1-CsI(Na)
spectrum and (d) G2 spectrum. Calibration source peak of $^{57}$Co (122 keV) is detected at G1-CsI
and G2 spectra.}
\label{kn : fig10(a-d)}
\end{figure}

In order to calibrate the G1-CsI and G2 energy scale, we used a 122 keV $^{57}$Co
line. During the laboratory tests, the G1-CsI and G2 gains were changed by
varying the HV, LLD and ULD voltages in order to: i) identify the PH
values of the 122 keV line in channel number and ii) study the G1-CsI and G2 gain
stability.

The measured G1-CsI and G2 gain values are 0.2289 keV/Chan and 2.732 keV/Chan
for RT-2/S and 0.2279 keV/Chan and 3.948 keV/Chan for RT-2/G, respectively.
The G1-CsI and G2 energy converted spectra are used to measure the energy
resolution of the 122 keV emission line for both instruments. The measured
G1-CsI and G2 values, which are consistent with previous experiments (such as
BeppoSAX, and RXTE using similar detectors), are 19.79\% and 25.73\% for RT-2/S
and 20.69\% and 18.65\% for RT-2/G, respectively.

Apart from the energy scale calibration, it is also essential to have
the G1-CsI and G2 background for both instruments. The
in-flight background calibration is carried out using a $^{57}$Co radio-active
source (122 keV) placed in one of the slats of the collimator.

The energy calibrated background spectra of G1-NaI, G1-CsI and G2 for both instruments are shown
in Figure 11(b,c,d) and in Figure 12(b,c,d). The G1-NaI spectrum shows the signature of
$^{121}$I decay peak (due to $^{57}$Co, discussed in the previous section) at 57.19 keV and at
56.05 keV for RT-2/S and RT-2/G respectively. The background spectra G1-CsI and G2 are dominated
by the line emission of 122 keV of $^{57}$Co over the background continuum. The large `continuum'
in G1-CsI spectrum is due to high energy background photons that are detected in CsI crystal
in wider energy range of $\sim$30 keV to 210 keV along with the broad emission feature of 122
keV line (energy resolution 19.79\% for RT-2/S and 20.69\% for RT-2/G).
The G2 spectra of both instruments are from extremely high energy photons (as detected in the
laboratory). The 122 keV line intensity is strong enough as compared to the high energy background photons, which
causes the G2 spectra a `tail' like continuum.

\begin {figure}[h]
\vbox{
\vskip 0.0 cm
\centering{
\includegraphics[width=4.3cm,angle=270]{fig12a.ps}
\hskip 0.01cm
\includegraphics[width=4.3cm,angle=270]{fig12b.ps}}
\vskip 0.02cm
\centering{
\includegraphics[width=4.3cm,angle=270]{fig12c.ps}
\hskip 0.01cm
\includegraphics[width=4.3cm,angle=270]{fig12d.ps}}}
\vskip 0.06cm
\caption{Four spectra of RT-2/G payload: (a) PSD spectrum, (b) G1-NaI(Tl) spectrum, (c) G1-CsI(Na)
spectrum and (d) G2 spectrum. Calibration source peak of $^{57}$Co (122 keV) is detected at G1-CsI
and G2 spectra.}
\label{kn : fig11(a-d)}
\end{figure}

Although the `phoswich' technique (discussed in \S 3) is useful
for background rejection for charge particles, but we could not perform any specific test in
the ground (laboratory test) with charged particles in order to test the particle background
rejection process.

\section{Concluding remarks}

In this paper, we described the complete functionality (e.g., HV calibration, Thermistor
calibration, stability of PS and PH variation, validity of spectral data, health parameters
etc.) during various environmental tests of RT-2 payloads (RT-2/S \& RT-2/G) of RT-2 Experiment
onboard the CORONAS-PHOTON mission which has been launched on January 30, 2009. Laboratory results,
which include the space environmental tests (e.g., vibration, thermal, vacuum, emi, src tests etc.)
and the functionality tests
suggest that both instruments are qualified for space use. All these tests were carried out
in a period of three months. We found that the scientific results based on functionality
test are stable for the entire period of the testing phase.
In fact, both instruments (RT-2/S and RT-2/G) are identical (except their FOV and in low energy
working range) as far as the configuration details are concerned. However, the
basic differences in their spectral characteristics
(e.g., amplitude, shape, energy ranges etc.) are due to the
difference in technical settings of the operational conditions (e.g., HV, LLD/ULD variation, PSD
setting etc.). The energy ranges (channel boundary) of the
amplifiers (G1 and G2) of both instruments are
very wide and would be quite useful. During the onboard operation, different
channel boundaries (energy ranges) would be set
to understand the background rejection effect for both instruments (payloads).

To study the particle background rejection process, a `robust' logic
was implemented inside the FPGA to process any `event' that is detected
in the crystals. PSD technique was used to separate out the event registered in NaI or CsI
crystal. The photons with higher energy ($\ge$ 100 keV) are mostly detected in CsI crystal. Apart
from the PSD technique, the in-built logic inside the FPGA also can separate out the
high energy photons ($\ge$ 40 keV) which are detected in CsI crystal of G2 amplifier (G2 spectrum).

During the commissioning phase of both instruments, we found that the initial results (Nandi et
al. 2009) are in agreement with the results obtained in the ground condition.
In its lifetime ($\sim$ 3-5 years), RT-2 will cover the peak of the $24^{th}$ solar cycle. So
far, the solar activity has not really taken off. Only a few weak flares which occurred have been
successfully detected by RT-2/S and RT-2/G, and the results will be reported elsewhere.

\noindent {\bf Acknowledgments:}
DD thanks CSIR/NET scholarship and TBK thanks RT-2/SRF fellowship which supported their research
work. The authors are thankful to scientists, engineers and technical staffs from
TIFR/ICSP/VSSC/ISRO-HQ for various supports during RT-2 related experiments. The authors also
thank the anonymous referee for the very detailed comments to improve the quality of the manuscript.

redpajama_set_name: RedPajamaArXiv


text:
Stanford's Baccalaureate Speaker Tells Class of 2013 to Enter the Whirlwind of Life with Their Whole Heart
|In Blog, Millennials, Press
|By Valarie Kaur
Stanford's Baccalaureate Speaker Tells Class of 2013 to Enter the Whirlwind of Life with Their Whole Heart
By Kathleen J. Sullivan
Published by Stanford News.
When facing the dangers of a courageous life, have faith, alumna Valarie Kaur told the graduates at Baccalaureate, a multi-faith celebration of thanksgiving and inspiration. "Faith in God or faith in goodness, faith that love can conquer death and darkness and despair, faith in yourself, faith in each other."
Speaking to the Class of 2013, alumna Valarie Kaur said graduates don't need to be superhuman, super-smart, super fuzzy or super techie to stand up for what they believe in, but need only to keep alive the desire to do good, and to keep their faith when the world becomes a whirlwind.
"If you think of your life as a great journey, filled with splendors and dangers and chances to make the world a better place – and you hold fast to the friends you have made here – then there will be only one thing left to do when a whirlwind comes calling," Kaur said. "Enter it with your whole heart."
Kaur told the audience she entered the whirlwind as a 20-year-old Stanford junior. She was a religious studies major with no filmmaking experience who grabbed a camera and left campus to crisscross the country, filming hundreds of stories of hate crimes committed after 9/11 against "people who looked like us – Sikh, Muslim and Arab Americans, chased, beaten, gunned down."
A man she knew as an uncle was killed in a hate crime in Arizona. His murder "barely made the evening news," she said.
Speaking Saturday morning in the Main Quad at Baccalaureate, a festive celebration of thanksgiving and inspiration, Kaur said it was her maternal grandfather who urged her to act.
"My grandfather was the most fearless man I knew," she said. "He was a soldier in World War II, so when he taught me a Sikh prayer – Tati vao na lagi, par brahm sharnai. The hot winds cannot touch me, I am sheltered by the Divine – I took it as the secret to his fearlessness. With his prayer on my heart, I wrote my professor, Linda Hess, with my idea, and she said, 'You're in a position to enter this unique moment in history … and catch the life of it. It's like entering the whirlwind.'"
But Kaur also faced down danger. She was arrested while filming anti-war protesters in New York City, injured by a police officer who badly twisted her arm, and detained in a makeshift detention center known as "Guantanamo on the Hudson." She later finished that film, Divided We Fall: Americans in the Aftermath, supported by longtime Stanford friends who reached out to care for her.
"And it was Dean Tommy Lee Woon who taught me the greatest lesson that changed my life," Kaur said. "He said: If we drive ourselves into the ground, if we pretend that we are perfect, if we hide our pain and imperfection, then we are embodying the very dysfunction and neglect we seek to heal out in the world. The way we make change is just as important as the change we make.'"
Jonathan York offers the student reflection during Baccalaureate.
Kaur, who grew up in Clovis, Calif., is an award-winning filmmaker, civil rights advocate and interfaith organizer. She was the featured speaker at the hour-long ceremony, which is led by students under the auspices of the Office for Religious Life. Ten years ago, as a graduating senior, she gave the student reflection at Baccalaureate. After graduation from Stanford she earned a master's degree in theological studies from Harvard Divinity School and a law degree from Yale.
She is the founding director of Groundswell, a nonprofit initiative at Auburn Theological Seminary in New York City that mobilizes people of faith in social action. Currently a fellow at Yale Law School, Kaur is the founding director of the Yale Visual Law Project, where she makes documentary films and trains students in the art of visual advocacy.
"Whatever you do, wherever you go after tomorrow, whether it's in public service or academia, or a corporate office or an NGO or an urban farm, you will find that courage is dangerous business," Kaur said.
"You may be broken and bleeding. You may find yourself awake at night with a ghost in your throat. You may find your arm twisted, your heart broken in two. But the hot winds cannot touch you if you have faith – faith in God or faith in goodness, faith that love can conquer death and darkness and despair, faith in yourself, faith in each other."
The Baccalaureate celebration opened with a solemn Buddhist call to prayer performed on a singing bowl and ended with a dramatic drumming blessing, Tatsumaki (Whirlwind), performed by Stanford Taiko.
In between there was an invocation, A Prayer of the Ojibway Nation, which the audience, primarily soon-to-be graduates and their families, recited. The Baccalaureate readings were Be a Gardener, by Julian of Norwich, and Courage and Vision, by Mohandas Gandhi.
Stanford Talisman, a student a cappella group, performed two songs, Wanting Memories, a song of the African Diaspora, and One by One, a song sung in Xhosa that was inspired by the South African anti-apartheid movement and expresses solidarity in the struggle against oppression.
Jonathan York, who offered the student reflection, described himself as the "unlikely combination" of an Iranian mother whose family fled Ayatollah Ruhollah Khomeini's revolution and settled in Akron, Ohio, and an Iranian father, the son of a great rabbi, who changed his name to York – from Yadegaran – when he arrived in America in 1970.
York, whose family lives in Los Angeles, Tel Aviv and Tehran, said he is Jewish, Iranian, American and Israeli.
"I didn't know just how much of a contradiction I was growing up, surrounded by those who looked and sounded like me," said York, a graduating senior who majored in international relations and minored in human biology. "It never seemed a conflict to celebrate Norouz and Passover within days of each other."
Until he arrived at Stanford, that is.
"Until I went to Shabbat services at Hillel and heard Ashkenazi melodies foreign to my Sephardic ears," he said. "Until I studied abroad in Madrid and had to answer time and again the same follow-up question, 'But where are you really from?' Until I participated in Stanford in Washington and the Farsi and Hebrew skills I learned at home became strategic assets."
Yet through it all, Stanford remained the one place where, for all his contradictions, he was still just "Jonathan," York said.
At Stanford, York said, students shared their contradictions – and with them, their fears and histories – in the hope of finding understanding and support.
"Today we look around, at our friends and colleagues, our parents and professors," he said. "We look around and see in them all those who made our unlikely contradictions possible and their synergies beautiful."
York urged the graduates to savor the moment.
"And with the strength of our common experience, let us walk forward together, tested but not weary, to a future where from our many contradictions, we may derive but inspiration and light."

redpajama_set_name: RedPajamaCommonCrawl


Below are the nutrition facts and Weight Watchers points for White Cheddar Bagel Twist from Dunkin Donuts .
There are 390 calories in a White Cheddar Bagel Twist from Dunkin Donuts. Most of those calories come from carbohydrates (66%).
Is the White Cheddar Bagel Twist good for you?
Does the White Cheddar Bagel Twist taste good?


text:
Resist anti-union laws
December 12, 2022 Patrick Harrington News Leave a comment
Rishi Sunak has confirmed the government is ready to ram through new anti-strike laws.
The government has already started the process to pass a new law implementing minimum service levels during transport strikes, which would gut the right to strike.
The prime minister's official spokesperson said on Wednesday that work was "ongoing" on other options for mitigating future industrial action, including a ban on walkouts by ambulance staff and other emergency workers, and extension of proposed minimum service level legislation to cover the whole public sector.
Unions, including Solidarity, have condemned the proposals.
"[The government] changes the law every time it loses an argument," Mr Lynch of the RMT union told reporters.
"If people want to protest against them, they say you're not allowed to do that anymore. If people want to take industrial action, they say it's illegal.
"All of the opinion polls show it. They are losing the argument [on wages]. So, they are trying to get rid of the argument by suppressing trade union rights."
Mr Lynch said that the trade union movement needs a co-ordinated and robust response to the attacks.
He said: "I fully expect [the government] to press ahead because they need a diversion for all their incompetence, so it's a handy thing for them.
"Trade unions have no choice. When your members are being impoverished, you have to respond."
Other union leaders have also spoken out against the plans.
Pat Harrington, general secretary of Solidarity said:
"Attacks on the right to strike are assaults on democracy. Strikes, or the threat of strikes, are a way for ordinary workers to bring about change in their pay and conditions. Sometimes a strike is the only way to get bad bosses to listen to their workers. No one wants to go on strike but sometimes it's necessary. If passed this legislation will be fiercely resisted and will further divide our society."
Fire Brigades Union (FBU) general secretary Matt Wrack said any attempt to ban workers from taking strike action would be an "outrage to so-called democracy.
"To further restrict the right to take industrial action would be a highly authoritarian move, and more in keeping with the actions of a dictatorial regime," he said.
"The Tories are badly misjudging the public mood with these attacks.
"Any attempt to limit the right to strike will be fiercely resisted by the FBU."
Unison general secretary Christina McAnea said that the government should instead be concentrating efforts to meeting with unions to solve the disputes.
"This threatens to backfire spectacularly on the government," she said.
"The public has immense sympathy for ambulance workers and their NHS colleagues.
"Ministers could do well to remember that union members are voters too."
When asked what action they would take on strike laws, a Labour spokesperson said only that they would repeal the "archaic" 2016 laws brought in under previous Tory administration, but offered no specifics beyond that.
anti-unionAnti-union lawsFBUlawsnewsresistRishi SunakRMTUnison
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An ideal snowfields adventure for families, Lake Mountain is also the most easily reached peak from Melbourne.
Setting out for snow, your Acacia guide will first transport you through the glorious Yarra Valley and mountain ash forests of the Yarra ranges to the postcard-perfect Alpine foothill village of Marysville, a lush green spot in which to grab a morning coffee.
Once everyone has had their freezing fun, we'll transport you back to Melbourne but not before stopping at your choice of the Yarra Valley's finest gourmet offerings, from handcrafted chocolatiers to cheesemongers.
As for the grown-ups, they can opt for a wine tasting or perhaps sample beer and cider at Napoleone Brewery.


text:
Call Us 24/7 - Toll Free Hotline
Helping Victims of Sexual Abuse
Anyone who was inappropriately touched by anyone of authority from the Catholic church may now qualify for a significant cash settlement. Time to file for compensation is limited! Complete the form below to check eligibility.
Over the last year, Catholic Dioceses from across the United States have released lists of known clergy sexual abusers. There's no greater breach of trust than when someone in a position of power and authority sexually abuses someone. These acts have devastating effects on victims. Already, more than 3,000 civil lawsuits have been filed on behalf of victims of clergy abuse. If you have suffered sexual abuse by a member of the clergy or a person of authority please fill out the form. We offer free consultations to help you access compensation and help with your recovery. We stand ready to assist you, and we stand ready to hold these institutions to accountable.
Even if this abuse happened decades ago it does not matter, Diocese officials said the fund will be open to all clergy sex abuse victims, including people living in the country illegally and those who are barred from filing lawsuits because the abuse occurred long ago and is beyond the statute of limitations.
CONFIDENTIAL FREE CASE REVIEW
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If you were abused by a member of the clergy, you have rights, and we protect those rights and fight to ensure you get the justice and compensation you deserve.
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Submitting this form and the information contained therein does not establish an attorney client relationship. The information submitted may be reviewed by more than one attorney and/or law firm. By submitting this form, you understand any information received in response to this questionnaire is general information for which there will be no charge. You further acknowledge that the law for each state may vary, and therefore, you will not rely upon this information as legal advice. Since this matter may require advice regarding your home state, local counsel may be contacted for referral of this matter. By clicking NEXT, you acknowledge that the information viewed is advertising and you agree to receive future advertisements from LS5 and/or its partners.
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text:
Dennis Amiss
Dennis Leslie Amiss
(1943-04-07) 7 April 1943 (age 77)
Harborne, Birmingham, Warwickshire, England
Sacker
Left arm medium
Slow left arm orthodox
National side
Test debut (cap 434)
18 August 1966 v West Indies
Last Test
12 July 1977 v Australia
ODI debut (cap 12)
24 August 1972 v Australia
Last ODI
6 June 1977 v Australia
Domestic team information
Runs scored
3,612 859 43,423 12,519
100s/50s
11/11 4/1 102/212 15/77
262* 137 262* 137
Balls bowled
– – 1,153 129
– – 18 2
Bowling average
– – 39.88 62.50
5 wickets in innings
10 wickets in match
Best bowling
– – 3/21 1/15
Catches/stumpings
24/– 2/– 417/– 105/–
Source: Cricinfo, 28 October 2009
Dennis Leslie Amiss MBE (born 7 April 1943)[1] is a former English cricketer and cricket administrator. He played for both Warwickshire and England. A right-handed batsman, Amiss was a stroke maker particularly through extra cover and midwicket – his two favourite areas to score runs. He was an accomplished batsman in all forms of the game. He averaged 42.86 in first-class, 35.06 in List-A, 46.30 in Tests and 47.72 in One Day Internationals. In first-class cricket he scored 102 centuries, and his England record amassed over 50 Tests ranks him with the best England has produced.[1]
After retiring as a player in 1987, he served Warwickshire as Chairman of the Cricket Committee, and he followed David Heath as chief executive from 1994 until 2006.[2] In 1992 he was selected as an England selector.[1] In November 2007 he became the deputy chairman of the England and Wales Cricket Board; in August 2011, The Daily Telegraph described his role on the board as providing "cricketing knowledge and expertise [that] complemented Clarke's business skills."[3]
1 Early years
2 England career
Early years[edit]
Amiss was born at Harborne in Birmingham. He suffered a serious back injury whilst playing football in his teenage years, which entailed him starting each day of his sporting life undergoing stretching routines to loosen up.[1]
England career[edit]
Amiss made his Test debut for England in the fifth Test of the 1966 series with West Indies, and he proved an accomplished Test match batsman. He was one of the first batsmen to use a protective helmet.[4][1] In scoring 3,612 Test runs, Amiss made eleven half-centuries and eleven centuries, including two double centuries against the West Indies. His highest Test match score, also his highest first-class score, was 262 not out against the West Indies in the 1973–74 Kingston Test, an innings that saved the Test match for England after they conceded a first innings lead of 230. The next highest score in England's innings was 38. After being dropped by England in 1975, he made a successful return against the West Indies at the Oval in the final Test of 1976, although his 203 in the first innings did not prevent England losing the match. Amiss's last Test came in 1977 when he was left out to make way for Geoff Boycott's return from self-imposed exile.
His former Warwickshire teammate, Jack Bannister, stated "Dennis was always tinkering with his game, he was a bigger perfectionist than Colin Cowdrey".[1]
Amiss was also a handy One Day International batsman scoring 859 runs, including four centuries and one half-century, with a top score of 137 against India which is still England's fourth highest individual score in the Cricket World Cup, behind the 158 scored by Andrew Strauss against India in 2011, Jason Roy's 153 against Bangladesh in 2019, and Eoin Morgan's 148 against Afghanistan at the same tournament.[5] He has the distinction of scoring the first ever One Day International century (103 in only the second One Day International on 24 August 1972) which is also the first instance of a debutant scoring a century in ODI. Amiss along with Keith Fletcher is also credited to have shared the first ever partnership of hundred runs in the same match.[6][7] He ended with an ODI batting average of 47.72, which excepting those players to have played fewer than five times, remains the highest of any England batsman who has completed his career. The still-active Kevin Pietersen averaged over 50 throughout the first 60 matches of his ODI career up until September 2007, but that figure had fallen to under 41 by June 2011.
Amiss played World Series Cricket in the late 1970s in Australia; during the 1978 World Series Cricket tournament, he became the first player to wear a batting helmet regularly.[4][8]
Amiss was banned from Test cricket for three years for taking part in the first 'rebel' tour of South Africa in 1982.[citation needed]
Honours[edit]
Amiss was selected as one of the five Wisden Cricketers of the Year in 1975.[9]
Amiss was awarded an MBE in 1988; in 2007 he received a Doctor of the University from the University of Birmingham.[2]
A graph of Dennis Amiss's Test performances.
Records[edit]
Dennis Amiss is the first player in ODI cricket to have scored a century on both his debut and in his last match, the only other being Desmond Haynes.[10] On 7 June 1975 at Lord's in the first match of the Prudential World Cup (which was also the very first Cricket World Cup to have been held) Amiss smashed 137 runs in just 147 balls against India powered by 18 boundaries. His innings provided enough leverage for England to post a very imposing and improbable target of 335 for India to be chased down within a span of 60 overs. It was also the first time that a team would score 300 or more runs in an ODI match. The match also featured the infamous and notorious ODI innings of Sunil Gavaskar who in reply to the nearly unreachable target set by England scored an unbeaten 36 in 174 balls with just one boundary to adorn his innings.[11]
^ a b c d e f Bateman, Colin (1993). If The Cap Fits. Tony Williams Publications. pp. 12–13. ISBN 1-869833-21-X.
^ a b "University of Birmingham Honorary Graduands for July 2007". 10 July 2007. Retrieved 26 November 2014. Dennis Amiss has had a career in professional cricket spanning more than 40 years at both domestic and international levels. He gained 51 England caps between 1966 and 1977, scoring a total of 3,612 runs. He was the Chief Executive of Warwickshire County Cricket Club between 1994 and 2006 and is now Director of the England and Wales Cricket Board. He was awarded an MBE in 1988.
^ Bolton, Paul (11 August 2011). "Dennis Amiss set to stand down as ECB deputy chairman and retire from cricket administration". The Daily Telegraph. Retrieved 26 November 2014. Amiss narrowly beat former Lancashire chairman Jack Simmons in a ballot in November 2007 to become right-hand man to ECB chairman Giles Clarke but he was re-elected unopposed in January last year.
^ a b "The bravery of the batsman". The Economist. 26 November 2014. Retrieved 26 November 2014. until the late 1970s helmets were unheard of; batsmen wore nothing to protect their noggins except a cloth cap. When they began to creep into the game—Dennis Amiss, an English batsman, is usually cited as the first to wear one regularly during the 1978 World Series Cricket tournament—they were essentially adapted motorcycle helmets. Batsmen who donned them were sometimes mocked as cowards.
^ "Cricket Records – Records – World Cup – High scores – ESPN Cricinfo". Cricinfo. Archived from the original on 24 October 2012.
^ "1st ODI: England v Australia at Manchester, Aug 24, 1972 – Cricket Scorecard – ESPN Cricinfo". Cricinfo.
^ Frindall, Bill (2009). Ask Bearders. BBC Books. pp. 153–154. ISBN 978-1-84607-880-4.
^ Briggs, Simon. "Amiss unearths helmet that changed the game". telegraph.co.uk. Retrieved 15 January 2013.
^ "Dennis Amiss". Cricket Archive. Retrieved 31 January 2017.
^ "Records – One-Day Internationals – Batting records – Hundred in last match – ESPN Cricinfo". Cricinfo.
^ "1st Match: England v India at Lord's, 7 June 1975 – Cricket Scorecard – ESPN Cricinfo". Cricinfo.
Dennis Amiss at ESPNcricinfo
England squad – 1975 Cricket World Cup semi-finalists
1 Denness (c)
2 Amiss
3 Arnold
4 Fletcher
5 Greig
6 Hayes
7 Jameson
8 Knott (wk)
9 Lever
11 Snow
12 Underwood
13 Wood
World XI squad – World Series Cricket
1 Greig (c)
3 Asif Iqbal
4 Barlow
5 Hadlee
6 Imran Khan
7 Javed Miandad
9 Le Roux
10 Haroon Rashid
11 Majid Khan
12 Mushtaq Mohammed
13 Procter
14 Rice
15 Richards
16 Sarfraz Nawaz
18 Taslim Arif (wk)
20 Woolmer
21 Zaheer Abbas
Batsmen who have scored 100 first-class centuries
Hobbs (199)
Hendren (170)
Mead (153)
Boycott (151)
Sutcliffe (149)
Woolley (145)
Hick (136)
Hutton (129)
Gooch (128)
Compton (123)
Graveney (122)
Bradman (117)
Richards (114)
Ramprakash (114)
Abbas (108)
Sandham (107)
Cowdrey (107)
Hayward (104)
Turner (103)
Edrich (103)
Ames (102)
Tyldesley (102)
Amiss (102)
Retrieved from "https://en.wikipedia.org/w/index.php?title=Dennis_Amiss&oldid=985783291"
Cricketers at the 1975 Cricket World Cup
English cricket administrators
English cricketers
English cricketers of 1969 to 2000
England One Day International cricketers
England Test cricketers
International Cavaliers cricketers
Marylebone Cricket Club cricketers
Secretaries of Warwickshire County Cricket Club
Cricketers from Birmingham, West Midlands
Warwickshire cricketers
Wisden Cricketers of the Year
World Series Cricket players
Cricketers who made a century on One Day International debut
People from Harborne
D. H. Robins' XI cricketers
T. N. Pearce's XI cricketers
EngvarB from August 2013
Pages using Template:Post-nominals with missing parameters


If you want to study BBA in Hospital Management in Kolkata, then get admitted to the best Graduate Course in Hospital Management offered by NIMS. Nopany Institute of Management Sciences located in Girish Park in Central Kolkata offers Hospital Management Course in Kolkata. Popularly known as NIMS they have state of the art infrastructure and facilities and is by far the best Hospital Management College in West Bengal. Visit us at www.nims.ac.in or call us at 7044175206 / 033-25332869 for details about course information and admission. NIMS offers 100% placement to all its students.


text:
1979–80 Primeira Divisão
Title: 1979–80 Primeira Divisão
Subject: U.D. Leiria, Primeira Liga, 1969–70 Primeira Divisão, 1979 European Super Cup, 1999–2000 Primeira Liga
Collection: 1979 in Association Football, 1979 in Portuguese Sport, 1979–80 Domestic Association Football Leagues, 1979–80 in European Association Football Leagues, 1979–80 in Portuguese Football, 1980 in Association Football, 1980 in Portuguese Sport, Primeira Liga, Primeira Liga Seasons
600 (2.5 per match)
← 1978–79
1980–81 →
Statistics of Portuguese Liga in the 1979–80 season.
League standings 2
Footnotes 3
It was contested by 16 teams, and Sporting Clube de Portugal won the championship.
1 Sporting Clube de Portugal (C) 30 24 4 2 67 17 52 European Cup
2 F.C. Porto 30 22 6 2 59 9 50 UEFA Cup
3 S.L. Benfica 30 19 7 4 79 21 45 UEFA Cup Winners' Cup
4 Boavista F.C. 30 15 7 8 44 30 37 UEFA Cup
5 C.F. Os Belenenses 30 13 8 9 33 38 34
6 Vitória S.C. 30 11 10 9 42 38 32
7 S.C. Espinho 30 11 6 13 29 42 28
8 Portimonense S.C. 30 10 6 14 32 49 26
9 S.C. Braga 30 10 6 14 34 40 26
10 Varzim S.C. 30 8 10 12 37 45 26
11 C.S. Marítimo 30 9 8 13 25 37 26
12 Vitória F.C. 30 9 5 16 29 41 23
13 U.D. Leiria (R) 30 6 9 15 26 49 21 Relegation to Segunda Divisão
14 G.D. Estoril-Praia (R) 30 5 11 14 18 37 21 Relegation to Segunda Divisão
15 S.C. Beira-Mar (R) 30 5 10 15 24 46 20 Relegation to Segunda Divisão
16 Rio Ave F.C. (R) 30 5 3 22 22 61 13 Relegation to Segunda Divisão
Portugal 1979-80 - RSSSF (Jorge Miguel Teixeira)
Portuguese League 1979/80 - footballzz.co.uk
Portugal - Table of Honor - Soccer Library
Portuguese WorldHeritage - Campeonato Português de Futebol - I Divisão 1979/1980
Top-level football seasons in Portugal
Experimental Primeira Liga
1979–80 in European football (UEFA)
Denmark '79 '80
Estonia '79 '80
Faroe Islands '79 '80
Finland '79 '80
Iceland '79 '80
Latvia '79 '80
Lithuania '79 '80
Norway '79 '80
Soviet Union '79 '80
Sweden '79 '80
League cups
European Cup (Final)
Cup Winners' Cup (Final)
UEFA Cup (Final)
Primeira Liga seasons
1979–80 in Portuguese football
1979–80 in European association football leagues
Portugal, Brazil, Italy, Spain, England
Spain, Portuguese language, Lisbon, Porto, Madeira
S.L. Benfica, Sporting Clube de Portugal, FC Porto, C.F. Os Belenenses, Boavista F.C.
Sporting Clube de Portugal, S.L. Benfica, Vitória F.C., Vitória S.C., C.F. Os Belenenses
1979 European Super Cup
FC Barcelona, Nottingham Forest F.C., England, Spain, UEFA Super Cup
1999–2000 Primeira Liga
Portugal, Vitória F.C., Rio Ave F.C., S.L. Benfica, Boavista F.C.


34) A new commandment I give unto you, That ye love one another; as I have loved you, that ye also love one another.
35) By this shall all men know that ye are my disciples, if ye have love one to another.
5) Likewise, ye younger, submit yourselves unto the elder. Yea, all of you be subject one to another, and be clothed with humility: for God resisteth the proud, and giveth grace to the humble.


Apple iPhone 4's video calling application Facetime Beta is now coming for your Mac operating system as well. It's about time!
Facetime is the video calling feature in Apple iPhone 4 that allows its users with a Wi-Fi network to use this application on both ends having an iPhone 4, making communication possible and exciting using iPhone camera. This Apple application, originally dedicated to Apple iPhone 4, was not featured in Apple Mac, which no doubt was somewhat an unpleasant experience for users who owned both an Apple iPhone and Mac. But the wait is over and it`s all one again. Now you can receive and call anyone using Facetime on his iPhone 4 using your Mac. But this Facetime Beta application is only available for Mac Version 10.4.8 or newer. But according to me this limitation can be taken as the only down side of this offer. Everything else is a treat!
Apple`s Facetime is really easy to set up on your Mac. Just get yourself an Apple ID and an email address. And you are done.
iPad 2 FaceTime, Camera & PhotoBooth Apps!


text:
SYNONYM

#### According to
The Catalogue of Life, 3rd January 2011

#### Published in
null

#### Original name
Lecanora massalongiana Gyeln.

### Remarks
null

redpajama_set_name: RedPajamaGithub


Las Falles is a traditional celebration held in commemoration of saint Joseph in the city of Valencia, Spain. Within the city, each neighborhood is assigned a group, the Casal Faller, that will hold fundraising dinners, events, and parties in order to fund the construction of a falla. Mostly constructed of cardboard and paper-mache, the Fallas are filled with fireworks and firecrackers. On the final night of this 5 day celebration, the fallas go up in flames. The entire city is engulfed with thousands of humans celebrating in the streets as they watch the fallas burn. The term Falles refers to both the celebration and the monuments burnt during the celebration.


Marriage can be so hard. J was recently studying the tower of Babel for school and it just reminded me so much of marriage some days. Being in sync with your spouse is almost a magical feeling. You're on the same page and headed in the same direction - such an enormous blessing for everyone involved, especially the kiddos. But there are times when it is as if you've been struck like the people building the tower were and no matter what you try to communicate, it just seems to come out as gibberish to the other. It can just be so hard. Don't let that be discouraging if you hope to get married some day, but just make sure your expectations are realistic. Even in your best hard reality flick, you don't see how much work has to go into every relationship that is worth its salt. See those smiles down there? They are real, but not long after the picture was taken the wind picked up and sand was flying everywhere. I freaked out and thought he was crazy for wanting to stay any longer. He LOVES adventure and I panic at new things. Marriage can be really complicated.
Earlier this week, Mr. Butler and I found ourselves continuing to argue about things. Arguments aren't unusual (we're polar opposites in so many ways) but not seeming to ever get resolved wasn't our norm. After multiple attempts, the resolution was only achieved after realizing our entire issue was based on the different ways we were communicating things. Don't you hate when that happens? :) Sometimes we get into ruts where we just expect the person we're arguing with to be against us and not good-willed when really the language has gotten lost in translation somewhere.
It's December now and no matter who you are and what your life choices are, this will be one of your busiest and potentially most stressful months of the year. Let's work on our language (and I'm not exactly talking about bad words) and bridging the gap between our frustrations and the appreciation we want others to feel. It's easy to attack others for what we think they think about us, but simplifying our communication might just clear everything up and help us feel a whole lot better.


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Superintendent's Meeting Schedule
Mr. Kenneth Dyer
Office: School Administration Building, 200 Pine Ave.
E-mail: kenneth.dyer@docoschools.org
About the Superintendent:
Mr. Kenneth Dyer was selected in February 2017 by the Dougherty County Board of Education to become the district's superintendent after having served as Associate Superintendent and Chief Financial Officer.
Dyer earned his Bachelors and Master's degrees in the areas of accounting and business administration (finance), respectively, from Albany State University. Dyer's 23-year professional career includes experience in municipal government, commercial construction and as a small business owner; but, he is most known for his experience as an educational leader.
Serving over 18 years in leadership roles at the secondary and post-secondary education levels, Dyer served as the vice president and chief financial and operations officer at three colleges/universities prior to joining the DCSS in 2011. Dyer has provided stellar leadership since he came to the DCSS and is largely credited with leading the school system out of difficult financial times. In addition, it has been his effective stewardship that enabled the school system to invest in several initiatives aimed at improving student achievement.
It is Dyer's visionary and capable leadership, as well as his passion for improving the lives of the students and families of the DCSS that led the Dougherty County Board of Education to promote him to the superintendency. Dyer understands the tremendous responsibility of the superintendency and looks forward to the opportunity to build upon recent accomplishments of the school system, while creating an environment for the DCSS to ascend to even greater heights.
A 2012 graduate of Leadership Albany, Dyer is active in the Albany/Dougherty community by serving as a Deacon at Mt. Zion Baptist Church, a life member of the Alpha Phi Alpha Fraternity, Inc., a member of the Government Relations Committee of the Boys and Girls Club of Albany, and a member of the Board of Directors of Albany Technical College. He previously served on the Board of Directors for Leadership Albany.
Dyer is the son of Bobby and Lillie G. Patrick. He is married to Dr. Stephanie H. Dyer and they have two beautiful daughters, Kenadi and Kendyl.
Lowanna Johnson
Executive Administrative Assistant
ljohnson@docoschools.org


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Archive for the 'Military casualties' Category
Military Deaths in Afghanistan and the Middle East — 2016 Update
Summary: 2016 annual report (with 2017 updates) of U.S. military deaths in the Afghanistan war (Operation Enduring Freedom; Operation Freedom's Sentinel) and the war against ISIS / ISIL / Islamic State in Syria and Iraq (Operation Inherent Resolve) and in Libya ( Operation Odyssey Lightning), compiled from U.S. Department of Defense news releases and iCasualties.org. Updates on U.S. military deaths in 2017.
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Summary: 2015 annual report (with 2016 updates) of U.S. military deaths in the Afghanistan war (Operation Enduring Freedom; Operation Freedom's Sentinel) and the war against ISIS / ISIL / Islamic State in Syria and Iraq (Operation Inherent Resolve), compiled from U.S. Department of Defense news releases and iCasualties.org. Updates on U.S. military deaths in 2016.
Military Deaths in Afghanistan Update — December 2014
Summary: December 2014 monthly report of U.S. military deaths in the Afghanistan war (Operation Enduring Freedom; Operation Freedom's Sentinel) and the war against ISIS / ISIL / Islamic State in Syria and Iraq (Operation Inherent Resolve), compiled from U.S. Department of Defense news releases and iCasualties.org. Updates on U.S. military deaths in 2015.
Military Deaths in Afghanistan Update — November 2014
Summary: November 2014 monthly report of U.S. military deaths in the Afghanistan war (Operation Enduring Freedom) and the war against ISIS / ISIL / Islamic State in Syria and Iraq (Operation Inherent Resolve), compiled from U.S. Department of Defense news releases and iCasualties.org.
Military Deaths in Afghanistan Update — October 2014
Summary: October 2014 monthly report of U.S. military deaths in the Afghanistan war (Operation Enduring Freedom) and the war against ISIS / ISIL / Islamic State in Syria and Iraq (Operation Inherent Resolve), compiled from U.S. Department of Defense news releases and iCasualties.org.
Military Deaths in Afghanistan Update — September 2014
Oct 1st, 2014
Summary: September 2014 monthly report of U.S. military deaths in the Afghanistan war, compiled from U.S. Department of Defense news releases and iCasualties.org.
Military Deaths in Afghanistan Update — August 2014
Summary: August 2014 monthly report of U.S. military deaths in the Afghanistan war, compiled from U.S. Department of Defense news releases and iCasualties.org.
Military Deaths in Afghanistan Update — July 2014
Summary: July 2014 monthly report of U.S. military deaths in the Afghanistan war, compiled from U.S. Department of Defense news releases and iCasualties.org.
Military Deaths in Afghanistan Update — June 2014
Summary: June 2014 monthly report of U.S. military deaths in the Afghanistan war, compiled from U.S. Department of Defense news releases and iCasualties.org.
Military Deaths in Afghanistan Update — May 2014
Summary: May 2014 monthly report of U.S. military deaths in the Afghanistan war, compiled from U.S. Department of Defense news releases and iCasualties.org.


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