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special type of plastic scintillator can be used for gamma ray spectroscopy @xcite .
normal plastic scintillator detector , used for triggering particle in high energy physics experiments can also be used for gamma ray spectroscopy .
a simple and new technique has been introduced with plastic scintillator paddle for gamma ray and cosmic ray spectroscopy without using single channel analyzer ( sca ) or multi channel analyzer ( mca ) . in this technique
only a leading edge discriminator ( led ) and scaler have been used . using this technique @xmath2  -  ray spectrum
has been obtained for co@xmath0 and cs@xmath1 sources .
cosmic ray muon pulse height spectrum i.e. the spectrum for minimum ionizing particle ( mip ) has also been obtained .
the experimental technique and the data analysis technique have been described in section  [ ex_tech ] and section  [ ana_tech ] respectively , the experimental results have been described in section  [ result ] . finally in section  [ con ]
we have presented the conclusion of the study and a brief future outlook on the work .
a new technique has been developed for the gamma ray spectrum and cosmic ray pulse height spectrum without using single channel analyzer ( sca ) or multi channel analyzer ( mca ) .
only a leading edge discriminator and scaler have been used . in the measurements
two plastic scintillator paddles of dimension 7  cm @xmath3 7  cm and 10  cm @xmath3 10  cm with 1  cm thick plastic have been used .
the scintillator detectors are named as sc-01 and sc-02 respectively in this article .    for the gamma ray
spectroscopy the source ( co@xmath0 and cs@xmath1 ) has been placed on the scintillator material .
constant voltage of -  1500  v has been applied to the photo multiplier tube ( pmt ) of sc-01 for signal collection . in a separate study
we have observed that the efficiency of the detectors reaches a constant ( plateau ) value close to 100% at high voltage beyond -  1450  v. the signals from the scintillator have been fed to the discriminator .
the discriminator threshold has been increased in equal interval of 0.5  mv from an initial threshold value of 7.5  mv . for each discriminator threshold setting the count rate has been measured with the source and also without source , taking the total counts in the scaler in a particular time .    for the cosmic ray muon detection a constant voltage of -  1500
v has been applied to the photo multiplier tube ( pmt ) attached to the scintillator sc-01 but the discriminator threshold has been increased in equal interval of 2  mv from an initial threshold value of 12  mv . in this case
no source is used and the data is analyzed in a different way ( as explained in section  [ ana_tech ] ) the measurent has been started from an initial threshold value of 12  mv as lower than this value the singles count rate was very high due to noise effect . the interval is taken 2  mv as for the cosmic ray spectrum 0.5  mv is very small to get a reasonable difference betwwn two consecutive values . in this case also the count rate has been measured for each discriminator threshold settings .
data for each discriminator threshold settings has been taken for 30 minutes or more for the cosmic ray .
all the data analysis has been performed using root , a data analysis framework developed by cern @xcite . in the case of gamma ray spectrum
the difference of the count rate with and without the gamma ray source for a particular threshold setting gives the gamma ray count rate ( say c@xmath4 ) at that threshold .
likewise the gamma ray count rate ( say c@xmath5 ) has been measured for the next threshold setting .
the difference of gamma count rate for two consecutive threshold settings gives the gamma ray signal count rate ( say c = c@xmath4-c@xmath5 ) with pulse height between those consecutive threshold values .
the average of these two threshold values have been taken and the c has been said to be gamma ray count rate of pulse height at that average value .
the count rate has been plotted as a function of the discriminator threshold i.e. as a function of the pulse height ( shown in fig .
[ co60 ] and fig .
[ cs137 ] and discussed in detail later ) .
the cosmic ray muon pulse height spectrum has been obtained in the same way as described above . in this case also the difference of count rates for two consecutive threshold settings have been calculated ( say c = c@xmath4-c@xmath5 ) and assigned to pulse height with the average of these two threshold values . here
only one assumption has been taken that the noise level are same for the two consecutive threshold settings , which is not true at the lower threshold value .
this is the reason of a noise peak in the mip spectra al low pulse height region , which will be described in detail in the section  [ result ] .
co@xmath0 spectrum , a curve of count per minute as a function of pulse height . ]
cs@xmath1 spectrum , a curve of count per minute as a function of pulse height . ]
energy resolution as a function of @xmath6 . ]
calibration curve , the linear relationship between the energy and the experimentally measured pulse height . ]    for the gamma ray spectroscopy co@xmath0 and cs@xmath1 sources have been used . gamma ray spectrum for co@xmath0 source
has been plotted in figure  [ co60 ] .
the characteristic energy for co@xmath0 gamma source , 1.17  mev and 1.33  mev have been identified and the corresponding pulse heights have been measured fitting those peaks with gaussian function .
the corresponding pulse heights have been found to be 21.25  mv and 25.08  mv respectively .
the energy resolution for the detector in % defined as , @xmath7 % , has been found to be 9.3% and 7.6% for the 1.17  mev and 1.33  mev peak respectively .
here @xmath8s and the pulse heights have been found by fitting the 1.17  mev and 1.33  mev gamma ray peaks for co@xmath0 source by gaussian function . for gaussian function the @xmath8 and full width at half maxima ( fwhm )
are related by fwhm = @xmath8 @xmath3 2.355 .
gamma ray spectrum for the cs@xmath1 source has been obtained by the same method as described above and plotted in figure  [ cs137 ] .
the characteristic 662  kev peak has been fitted with gaussian curve and the peak pulse height has been determined . the peak pulse height for the cs@xmath1 gamma source
has been found to be 12.45  mv . in this case
the energy resolution value has been found to be 10.2% .
energy resolution obtained for the two peaks of co@xmath0 and one peak of cs@xmath1 , as a function of @xmath6 is plotted in figure  [ reso ] .
the points are fitted with a straight line .
an energy calibration curve has been drawn for sc-01 at -  1500  v operating voltage , taking two points obtained from co@xmath0 spectrum and one point obtained from cs@xmath1 spectrum @xcite .
the calibration curve has been fitted with a straight line .
the calibration curve has been shown in figure  [ calib ] . from the fit parameters it is clear that the curve nearly passes through the origin and the calibration factor
is 0.054  mev / mv .
the linear relationship between the energy and the experimentally measured pulse height has been observed .
cosmic ray ( mip ) spectrum fitted with landau function from detector sc-01 . ]
mpv as a function of the applied voltage detector sc-01 . ]    cosmic ray muon pulse height spectrum has also been obtained in this set - up as described in section  [ ex_tech ] and section  [ ana_tech ] .
the the cosmic ray induced pulse height spectra have been obtained for two detectors sc-01 and sc-02 and is shown in figure  [ mip1 ] for sc-01 .
same type of spectrum has also been observed for sc-02 .
the plot has been fitted with landau distribution ; as for the cosmic ray there is a large fluctuation of energy deposition in the detector material as revealed from the @xmath9 per degrees of freedom .
this plot has been obtained keeping the pmt voltage constant at -  1500  v. mip peak seems to have developed around @xmath10  30  mv but large noise peak ( below 20  mv ) masks it .
this peak come due to our assumption that the noise level are nearly same for the two consecutive threshold settings , which is not true for the very low threshold . from the cosmic ray spectra obtained from sc-01 and sc-02 it is also clear that at most probable value ( mpv ) of the count rate is nearly double for the sc-02 relative to sc-01 as the area of the sc-02 ( area 100 @xmath11 ) which is nearly double of that of the sc-01 ( area 49 @xmath11 ) .
as the calibration curve has been drawn for the sc-01 at -  1500  v and the sc-01 has been operated at -  1500  v during the cosmic ray study it is seen from figure  [ mip1 ] that the most probable energy deposition in 1  cm thick plastic scintillator is @xmath10  1.4  mev .
the cosmic ray spectra for these two scintillators have also been obtained varying the applied voltage and the mpvs are plotted as a function of the applied voltage in figure  [ mpv1 ] for sc-01 .
similar plot has also been obtained for sc-02 .
both the plots are fitted with the exponential function mpv = @xmath12 , where the parameters are @xmath13 and @xmath14 .
@xmath14 for both the scintillators have been found to be @xmath10  0.004@xmath150.0008 .
a simple and new technique has been developed for gamma ray and cosmic ray muon pulse height spectroscopy without using sca or mca . only scintillator detector , a leading edge discriminator and a nim scaler have been used in this technique .
gamma ray spectrum has been obtained for co@xmath0 and cs@xmath1 sources .
proportionality in energy and pulse height has been observed .
the energy resolution for the detector has been found to be 9.3% and 7.6% for the co@xmath0 1.17  mev and 1.33  mev peak respectively and 10.2% for 662  kev peak of cs@xmath1 .
cosmic ray muon pulse height spectrum has been obtained for two scintillators and fitted with landau distribution .
the most probable energy deposition in 1  cm thick plastic material has been found to be @xmath10 1.4  mev .
although the energy resolution is not so good but still using plastic scintillator detector gamma spectroscopy and cosmic ray muon pulse height spectroscopy can be done .
main drawback of this technique is that this process is time consumable and may not be useful for real experiment ; however , this process is very useful and can be applied for laboratory measurement where mca or sca are not available .
we acknowledge mr . subasha rout of utkal university , dr .
sudakshina prusty , dr . gunda santosh babu , dr . lokesh kumar and mr .
rudranarayan mohanty of niser for helping during this study .
s. biswas acknowledges the support of dst - serb ramanujan fellowship ( d.o .
sr / s2/rjn-02/2012 ) . xii@xmath16 plan dae project experimental high energy physics at niser - alice
is also acknowledged .
a new and simple technique has been developed using plastic scintillator detectors for gamma ray and cosmic ray spectroscopy without single channel analyzer ( sca ) or multichannel analyzer ( mca ) . in these experiments 
 only a leading edge discriminator ( led ) and nim scalers have been used . 
 energy calibration of gamma spectra in plastic scintillators has been done using co@xmath0 and cs@xmath1 sources . 
 the details experimental technique , analysis procedure and experimental results has been presented in this article .    
 plastic scintillator , gamma ray , cosmic ray , spectroscopy , energy resolution