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-- Main.AmnonHarel - 12-Sep-2010

*How should we interpret the "disappearance" of the CLs limits at high lambda?*

%TOC{title="Contents:"}%

---++ CLs basics
The "modified frequentist" CLs approach is to exclude regions of phase space where %$CLs=\frac{CL_{s+b}}{CL_b} < 1-\alpha$%, where %$\alpha$% is the desired confidence level. Here, %$\alpha=0.95$%. 

---+++ Fine print
None of these really matters at the end, but for completeness:
   * When the number of pseudo datasets (PDSs) that underlie either %$CL_{s+b}$% or %$CL_b$% at the limit is below 10, we consider the determination of the limit unreliable and do not quote it.
      * For the final results, we generate enough PDFs at the crucial points in phase space to prevent this requirement from effecting the results, except where it clearly removes statistical noise (see %$\lambda=5$%TeV example below)
   * Since the test statistic is the log likelihood ratio, with or without systematics, when we define an excluded region of the LLR, it will normally be simply connected and include %$-\infty$% (the sign convention is such that this is the value most unlike the new physics scenario). We considered the possibility that when the LLR does not include systematics, this may fail to hold, in which case we would quote only the uppermost excluded LLR in the lowest exclusion region. Currently, we have no reason to believe this abnormal situation arises in our measurement.
---++ Final results
---+++ What changed
   * Found a bug that greatly reduced the shift uncertainty in all results, and another that reduced the absolute JES in the results sent to the statistic board during CWR. The three leading uncertainties were unaffected by these bugs, so the results barely change. It is only due to the finicky nature of CLs limits in the regime we're at, that these tiny effects must be resolved.
   * Better understanding of the low LLR tails, described in the next section
   * Now using the CMS LPC batch system - generating obscene amounts of pseudo-datasets has never been easier :-)
---+++ What drives the low LLR tails?
The earlier results:
   * the nuisance parameters in the tails are as one would expect from their correlations with LLR in the bulk. They are only mildly effected.
   * the plot of the ensemble broken down by the last non-empty inner bin: <br/>
     <img src="%ATTACHURLPATH%/more_ex1.png" alt="more_ex1.png" width='298' height='286' /> <br/>
both hinted that statistical effects drive the low tails.

To check this further, we took a key ensemble and filtered out PDSs where any of the nuisance parameters is more than 2 sigma away from its nominal value, and checked how this effects the LLR tails.<br />
<img src="%ATTACHURLPATH%/plot_syst_tail.png" alt="plot_syst_tail.png" width='298' height='286' /><br/>
To see the key numbers more clearly, here are the relevant table entries (tables explained below):
| |  *Lambda*  |  *N_{PDS}*  |  *At the CLs point*  ||||  *Frequentist limiting*  |  *Data*  ||||| 
| | ^ |  ^ |  *N_{S+B}*  |   *CLb*  |  *CLsb*  |  *LLR value*  |  *LLR value*  |  *LLR value*  |  *N_{S+B}*  |  *CLs*  |  *MC stat. err. on CLs*  |
| *Full systematics* |  4.00  |  151949  |  104  |  0.0007  |  0.0137  |  -3.38  |  -1.67  |  -3.57  |  40  |  0.0415  |  0.0071  |
| *Truncated systematics* |  4.00  |  192126  |  86  |  0.0004  |  0.0089  |  -3.50  |  -1.69  |  -3.57  |  55  |  0.0451  |  0.0063  |
The effect on CLs is negligible.

*We conclude* that the low LLR tails are driven entirely by the statistics, and our ability to study them is not limited by the accuracy of the systematic uncertainties.
---+++ Plots
The dashed red line in the right hand plots is the CLs=5% line.

|  *Lambda*  |  *LLR distributions*  |  *CLs plot*  |
|  *2TeV*  |  <img src="%ATTACHURLPATH%/cpsdn20001I2_88.png" alt="cpsdn20001I2_88.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/v7ex1.png" alt="v7ex1.png" width='298' height='286' />  |
|  *3.6TeV*  |  <img src="%ATTACHURLPATH%/cpsdn36001I2_88.png" alt="cpsdn36001I2_88.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/v7ex8.png" alt="v7ex8.png" width='298' height='286' />  |
|  *4.0TeV*  |  <img src="%ATTACHURLPATH%/cpsdn40001I2_88.png" alt="cpsdn40001I2_88.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/v7ex6.png" alt="v7ex6.png" width='298' height='286' />  |
|  *4.05TeV*  |  <img src="%ATTACHURLPATH%/cpsdn40501I2_88.png" alt="cpsdn40501I2_88.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/v7ex5.png" alt="v7ex5.png" width='298' height='286' />  |
|  *4.1TeV*  |  <img src="%ATTACHURLPATH%/cpsdn41001I2_88.png" alt="cpsdn41001I2_88.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/v7ex7.png" alt="v7ex7.png" width='298' height='286' />  |
|  *4.15TeV*  |  <img src="%ATTACHURLPATH%/cpsdn41501I2_88.png" alt="cpsdn41501I2_88.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/v7ex9.png" alt="v7ex9.png" width='298' height='286' />  |
|  *5.0TeV*  |  <img src="%ATTACHURLPATH%/cpsdn50001I2_88.png" alt="cpsdn50001I2_88.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/v7ex2.png" alt="v7ex2.png" width='298' height='286' />  |

   * The two peak structure visible at 5.0TeV is due to having one very high mass event, which can be either inner or outer. See also the "old" plots of 4.05TeV below, with a breakdown by the last non-empty inner bin.
---+++ The table
"N_{S+B}" is the number of events in the new physics (QCD+contact interaction) ensembles whose LLR is below the relevant LLR value (CLs limiting value or observed data value).

|  *Lambda*  |  *N_{PDS}*  |  *At the CLs point*  ||||  *Frequentist limiting*  |  *Data*  ||||| 
| ^ |  ^ |  *N_{S+B}*  |   *CLb*  |  *CLsb*  |  *LLR value*  |  *LLR value*  |  *LLR value*  |  *N_{S+B}*  |  *CLs*  |  *MC stat. err. on CLs*  |
 |  1.80  |  4000  |  199  |  0.0497  |  0.9943  |  -1.09  |  -1.06  |  -27.75  |  1  |  0.0009  |  0.0009  |
 |  1.85  |  4000  |  198  |  0.0494  |  0.9888  |  -1.53  |  -1.46  |  -25.50  |  1  |  0.0010  |  0.0010  |
 |  1.90  |  4000  |  197  |  0.0493  |  0.9854  |  -2.02  |  -1.93  |  -24.14  |  1  |  0.0011  |  0.0011  |
 |  1.95  |  4000  |  196  |  0.0490  |  0.9791  |  -2.18  |  -2.08  |  -23.32  |  0  |  0.0005  |  0.0005  |
 |  2.00  |  4000  |  194  |  0.0486  |  0.9720  |  -2.38  |  -2.24  |  -21.23  |  0  |  0.0000  |  0.0000  |
 |  2.20  |  4000  |  181  |  0.0453  |  0.9069  |  -2.79  |  -2.49  |  -15.19  |  1  |  0.0019  |  0.0019  |
 |  2.40  |  4000  |  180  |  0.0449  |  0.8975  |  -2.05  |  -1.77  |  -13.98  |  0  |  0.0000  |  0.0000  |
 |  2.60  |  4000  |  155  |  0.0387  |  0.7745  |  -2.55  |  -1.99  |  -10.90  |  0  |  0.0000  |  0.0000  |
 |  2.80  |  4000  |  125  |  0.0312  |  0.6244  |  -2.80  |  -2.02  |  -8.84  |  0  |  0.0000  |  0.0000  |
 |  3.00  |  4000  |  88  |  0.0220  |  0.4395  |  -3.01  |  -2.09  |  -7.02  |  0  |  0.0013  |  0.0013  |
 |  3.20  |  4000  |  44  |  0.0110  |  0.2190  |  -3.64  |  -2.09  |  -5.99  |  1  |  0.0101  |  0.0101  |
 |  3.40  |  30000  |  179  |  0.0060  |  0.1191  |  -3.41  |  -1.79  |  -4.86  |  13  |  0.0276  |  0.0079  |
 |  3.60  |  244084  |  455  |  0.0019  |  0.0373  |  -3.50  |  -1.64  |  -4.00  |  120  |  0.0373  |  0.0035  |
 |  3.80  |  92098  |  187  |  0.0020  |  0.0406  |  -3.01  |  -1.43  |  -3.66  |  23  |  0.0321  |  0.0068  |
 |  4.00  |  402210  |  155  |  0.0004  |  0.0077  |  -3.53  |  -1.69  |  -3.57  |  125  |  0.0481  |  0.0044  |
 |  4.05  |  323618  |  ---  |  ---  |  ---  |  ---  |  -1.65  |  -3.41  |  133  |  0.0627  |  0.0056  |
 |  4.10  |  139028  |  45  |  0.0003  |  0.0065  |  -3.27  |  -1.62  |  -3.27  |  43  |  0.0491  |  0.0077  |
 |  4.15  |  152000  |  19  |  0.0001  |  0.0025  |  -3.34  |  -1.63  |  -3.18  |  49  |  0.0530  |  0.0079  |
 |  4.20  |  111028  |  3  |  0.0000  |  0.0006  |  -3.32  |  -1.55  |  -3.03  |  42  |  0.0690  |  0.0113  |
 |  5.00  |  25000  |  ---  |  ---  |  ---  |  ---  |  -1.08  |  -1.49  |  48  |  0.2426  |  0.0418  |
---+++ Conclusions
Going over the crucial lambda values one by one:
   * Though the separation at lambda=3.6TeV is low enough that it is almost power-constrained away, this lambda value is clearly excluded.
   * 3.8TeV is excluded
   * A CLs crucial value  exists at 4.0TeV. It is probably above the data so that 4.0 is excluded. Generating more PDSs...
   * 4.05TeV?
   * A CLs crucial value exists at 4.1TeV. excluded?
   * 4.15TeV? 
   * 4.2TeV?
   * If a crucial CLs value exists at 5TeV, the data value is well above it and 5TeV can not be excluded.

---++ Updated results during CWR
Generated an obscene amount of additional PDSs...

---+++ Tools
   * Added statistical uncertainties on the CLs values.
      * Since the # of PDS (%$N$%) is predetermined, the uncertainties on CLb and CLsb are (independent) binomial efficiency problems. I use the usual approximation of putting in the observed efficiency (%$p=A/N$%, where %$A$% is the number of PDSs below the LLR value). This gives an uncertainty on the relevant fraction (%$f$%, either CLb or CLsb) of %$\sigma_f = f \sqrt{ \frac{1}{A}-\frac{1}{N}}$%.
      * Then the two numbers are combined with standard error propagation, which implies the Gaussian approximation.
   * Added more diagnostic columns to the tables: N_{S+B} (explained below), CLs at data with its uncertainty due to MC statistics.
   * Plots now available for all relevant lambda values
---+++ Plots
The dashed red line in the right hand plots is the CLs=5% line.

|  *Lambda*  |  *LLR distributions*  |  *CLs plot*  |
|  *2TeV*  |  <img src="%ATTACHURLPATH%/cpsdn20001I2_88_v4.png" alt="cpsdn20001I2_88_v4.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/n8ex1.png" alt="n8ex1.png" width='298' height='286' />  |
|  *3.6TeV*  |  <img src="%ATTACHURLPATH%/cpsdn36001I2_88_v4.png" alt="cpsdn36001I2_88_v4.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/n8ex8.png" alt="n8ex8.png" width='298' height='286' />  |
|  *4.0TeV*  |  <img src="%ATTACHURLPATH%/cpsdn40001I2_88_v4.png" alt="cpsdn40001I2_88_v4.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/n8ex6.png" alt="n8ex6.png" width='298' height='286' />  |
|  *4.05TeV*  |  <img src="%ATTACHURLPATH%/cpsdn40501I2_88_v4.png" alt="cpsdn40501I2_88_v4.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/n8ex5.png" alt="n8ex5.png" width='298' height='286' />  |
|  *4.1TeV*  |  <img src="%ATTACHURLPATH%/cpsdn41001I2_88_v4.png" alt="cpsdn41001I2_88_v4.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/n8ex7.png" alt="n8ex7.png" width='298' height='286' />  |
|  *4.15TeV*  |  <img src="%ATTACHURLPATH%/cpsdn41501I2_88_v4.png" alt="cpsdn41501I2_88_v4.png" width='298' height='286' />  |  <img src="%ATTACHURLPATH%/n8ex9.png" alt="n8ex9.png" width='298' height='286' />  |
|  *5.0TeV*  |  <img src="%ATTACHURLPATH%/cpsdn50001I2_88_v4.png" alt="cpsdn50001I2_88_v4.png" width='398' height='226' />  |  <img src="%ATTACHURLPATH%/n8ex2.png" alt="n8ex2.png" width='298' height='286' />  |
   * The two peak structure visible at 5.0TeV is due to having one very high mass event, which can be either inner or outer. See also the "old" plots of 4.05TeV below, with a breakdown by the last non-empty inner bin.
---+++ The table
"N_{S+B}" is the number of events in the new physics (QCD+contact interaction) ensembles whose LLR is below the relevant LLR value (CLs limiting value or observed data value).

|  *Lambda*  |  *N_{PDS}*  |  *At the CLs point*  ||||  *Frequentist limiting*  |  *Data*  ||||| 
| ^ |  ^ |  *N_{S+B}*  |   *CLb*  |  *CLsb*  |  *LLR value*  |  *LLR value*  |  *LLR value*  |  *N_{S+B}*  |  *CLs*  |  *MC stat. err. on CLs*  |
 |  1.80  |  4000  |  199  |  0.0498  |  0.9963  |  -1.01  |  -0.99  |  -27.75  |  0  |  0.0000  |  0.0000  |
 |  1.85  |  4000  |  199  |  0.0497  |  0.9939  |  -0.82  |  -0.78  |  -25.50  |  0  |  0.0000  |  0.0000  |
 |  1.90  |  4000  |  197  |  0.0494  |  0.9875  |  -1.49  |  -1.41  |  -24.14  |  0  |  0.0005  |  0.0005  |
 |  1.95  |  4000  |  198  |  0.0495  |  0.9906  |  -0.78  |  -0.73  |  -23.32  |  1  |  0.0015  |  0.0015  |
 |  2.00  |  4000  |  196  |  0.0489  |  0.9787  |  -2.04  |  -1.92  |  -21.23  |  0  |  0.0002  |  0.0002  |
 |  2.20  |  4000  |  185  |  0.0462  |  0.9238  |  -2.24  |  -2.03  |  -15.19  |  0  |  0.0000  |  0.0000  |
 |  2.40  |  4000  |  177  |  0.0443  |  0.8856  |  -2.17  |  -1.83  |  -13.98  |  0  |  0.0000  |  0.0000  |
 |  2.60  |  4000  |  184  |  0.0460  |  0.9194  |  -0.29  |  -0.12  |  -10.90  |  0  |  0.0000  |  0.0000  |
 |  2.80  |  4000  |  166  |  0.0414  |  0.8276  |  -0.94  |  -0.71  |  -8.84  |  0  |  0.0000  |  0.0000  |
 |  3.00  |  4000  |  84  |  0.0209  |  0.4188  |  -3.10  |  -1.95  |  -7.02  |  2  |  0.0211  |  0.0162  |
 |  3.20  |  4000  |  63  |  0.0157  |  0.3132  |  -2.99  |  -1.81  |  -5.99  |  2  |  0.0181  |  0.0148  |
 |  3.40  |  4000  |  19  |  0.0047  |  0.0933  |  -3.46  |  -1.67  |  -4.86  |  1  |  0.0265  |  0.0268  |
 |  3.60  |  21000  |  121  |  0.0058  |  0.1153  |  -2.74  |  -1.46  |  -4.00  |  10  |  0.0389  |  0.0123  |
 |  3.80  |  12000  |  28  |  0.0023  |  0.0466  |  -2.90  |  -1.38  |  -3.66  |  2  |  0.0261  |  0.0187  |
 |  4.00  |  16000  |  32  |  0.0020  |  0.0395  |  -3.02  |  -1.47  |  -3.57  |  1  |  0.0057  |  0.0057  |
 |  4.05  |  181000  |  346  |  0.0019  |  0.0382  |  -2.89  |  -1.47  |  -3.41  |  44  |  0.0403  |  0.0063  |
 |  4.10  |  146000  |  178  |  0.0012  |  0.0244  |  -2.91  |  -1.46  |  -3.27  |  35  |  0.0434  |  0.0076  |
 |  4.15  |  35000  |  ---  |  ---  |  ---  |  ---  |  -1.46  |  -3.18  |  15  |  0.0793  |  0.0216  |
 |  4.20  |  4000  |  ---  |  ---  |  ---  |  ---  |  -1.61  |  -3.03  |  4  |  0.1469  |  0.0859  |
 |  5.00  |  4000  |  ---  |  ---  |  ---  |  ---  |  -1.07  |  -1.49  |  11  |  0.4184  |  0.1493  |

---+++ Conclusions
---++++ Why did we see fake rises?
   * the main problem is that we evaluated the significance using the number of PDS in the low-end rise region. The right way to think of it is by analogy to a bump hunt - is there a signficant excess over background? Just using the number of PDS is looking at S+B. In particular, a high B is a reason to distrust an excess, not to trust it :-(
      * it also hurt that the S+N numbers weren't readily available. They are in the tables now (they mostyle help answer other questions).
   * also a mild "look elsewhere" effect
---++++ Which CLs limits should we use?
It is not safe to use CLs limits which are based on small tail probabilities. How small?
   * From these results, anything below ~0.001 is suspect
   * *proved irrelevant - see above!* Our description of systematic uncertainties wasn't meant to cover such extreme cases. It's probably good enough till at least 3 sigma --> ~0.0015. It's certainly not good enough at 4 sigma (truncated there) --> ~0.00003. Also the choice of the prior for the JES wasn't checked below ~0.001 (see AmnonHarelStatusReportForStatisticsBoard#New_prior_shapes_for_nuisance_pa)

Going over the crucial lambda values one by one:
   * Though the separation at lambda=3.6TeV is low enough that it is almost power-constrained away, it is certain that a CLs limit exists and the data lies below it, so this value is excluded.
   * 4.0TeV is excluded
   * A CLs limit exists at 4.05TeV. It is probably above the data, so that 4.05 is excluded. I'd guestimate the significance of the previous statement, in terms of MC statistics, at around 2 sigma.
   * A CLs limit exists at 4.1TeV. There is a hint that it is above the data, so that 4.1 is excluded. I'd guestimate the significance of the previous statement, in terms of MC statistics, at around 0.5 sigma.
   * There is a hint that no CLs limit exists at 4.15TeV. If a crucial CLs value exists, the data value can easily (~50%?) lie above it.

So the best choice is to stick with the limits presented in the CWR, and add one more item to the discussion of the difficulties with CLs: 

"CLs sometimes requires estimating extreme tails which stresses the validity of the systematic variations and is difficult using brute force ensemble testing."

*the above may be true, but we now (after CWR) realize it is irrelevant to this measurement* 

Need to decide on the right presentation though...

---++ Improved plots with ensembles as of a bit before CWR (early 21st of September)
The plots on this section use systematics which are slightly lower than the final ones. There are not qualitative differences, in particular, the sensitivity runs out at 4TeV either way, and quantitative differences are likely to be tiny.
---+++ The simple cases
To understand how the CLs limits go away, we'll look at plots of CLs as a function of LLR (for a given new physics model, here contact interactions).
---++++ Easy exclusion
|  *LLR distributions*  |  *CLs plot*  |
|   <img src="%ATTACHURLPATH%/cpsdn20001I2_88_v2.png" alt="cpsdn20001I2_88_v2.png" width='298' height='286' />   |  <img src="%ATTACHURLPATH%/ex1.png" alt="ex1.png" width='298' height='286' />  |
---++++ No exclusion
|  *With systematics (as usual)*  ||  *Only statistical variations*  ||  
|  *LLR distributions*  |  *CLs plot*  |  *LLR distributions*  |  *CLs plot*  |
|   <img src="%ATTACHURLPATH%/cpsdn50001I2_88_v2.png" alt="cpsdn50001I2_88_v2.png" width='298' height='286' />   |  <img src="%ATTACHURLPATH%/ex2.png" alt="ex2.png" width='298' height='286' />  |   <img src="%ATTACHURLPATH%/cpsdn50002I2_88.png" alt="cpsdn50002I2_88.png" width='298' height='286' />   |  <img src="%ATTACHURLPATH%/cls_wo_syst_5TeV.png" alt="cls_wo_syst_5TeV.png" width='298' height='286' />  |
The leftmost "0" is real, but due to a single point from the SM ensemble. The 0,0 points (quite a few, actually) are an artifact that does not effect the code (these plots were meant to be internal to the code...).
---+++ CLs with borderline sensitivity
More than one behavior near the edge of the experimental sensitivity is possible. Here are two simple scenarios. In both scenarios, under both hypotheses (i.e. in both ensembles), the LLR is distributed as a Gaussian and the two distributions are displaced by an amount that descreases as we run out of experimental sensitivity.
   * *1* - the Gaussians have the same width
      * in this scenario, the lower the LLR (below the SM peak), the more the SM is prefered.
      * thus, as %$\lambda$% increases and we run out of experimental sensitivity, the CLs limit exists, and will rapidly drop to %$-\infty$%. However, our ability to determine its correct value will detriorate quickly - brute force ensemble testing is not a suitable tool for learning about the tails of distributions.
      * this is the behavior that was observed in the ICHEP results, where increasing the ensemble size by an order of magnitude extended the limit
   * *2* - the new physics distribution is wider
      * in this scenario, for very low LLR values (well below the SM peak), the SM is no longer prefered.
      * thus, as %$\lambda$% increases and we run out of experimental sensitivity, the CLs limit no longer exists as the plot is always above 0.05
      * this is the behavior observed in the current results - increasing the ensemble size does not extended the limit
---+++ The current borderline sensitivity region
|  *LLR distributions*  |  *CLs plot*  || |
| ^ |  *from 0 to 1*  |  *zoomed in*  | |
|   <img src="%ATTACHURLPATH%/cpsdn40001I2_88_v2.png" alt="cpsdn40001I2_88_v2.png" width='298' height='286' />   |  <img src="%ATTACHURLPATH%/ex3.png" alt="ex3.png" width='298' height='286' />  |  <img src="%ATTACHURLPATH%/ex6.png" alt="ex6.png" width='298' height='286' />  |
|  *LLR distributions*  |  *CLs plot*  ||  *LLR breakdown*  |
| ^ |  *from 0 to 1*  |  *zoomed in*  |  *by highest non-zero inner bin*  |
|   <img src="%ATTACHURLPATH%/cpsdn40501I2_88_v2.png" alt="cpsdn40501I2_88_v2.png" width='298' height='286' />   |  <img src="%ATTACHURLPATH%/ex4.png" alt="ex4.png" width='298' height='286' />  |  <img src="%ATTACHURLPATH%/ex5.png" alt="ex5.png" width='298' height='286' />  |  <img src="%ATTACHURLPATH%/more_ex1.png" alt="more_ex1.png" width='298' height='286' />  |
|  *LLR distributions*  |  *CLs plot*  || |
| ^ |  *from 0 to 1*  |  *zoomed in*  |  |
|   <img src="%ATTACHURLPATH%/cpsdn41001I2_88_v2.png" alt="cpsdn41001I2_88_v2.png" width='298' height='286' />   |  ---  |  <img src="%ATTACHURLPATH%/ex7.png" alt="ex7.png" width='298' height='286' />  |  |

---+++ The table
|  *Lambda*  |  *N_{PDS}*  |  *At the CLs point*  ||||  *Frequentist limiting*  |  *Data*  ||||| 
| ^ |  ^ |  *N_{S+B}*  |   *CLb*  |  *CLsb*  |  *LLR value*  |  *LLR value*  |  *LLR value*  |  *N_{S+B}*  |  *CLs*  |  *MC stat. err. on CLs*  |
 |  1.80  |  4000  |  199  |  0.0498  |  0.9963  |  -1.01  |  -0.99  |  -27.75  |  0  |  0.0000  |  0.0000  |
 |  1.85  |  4000  |  199  |  0.0497  |  0.9939  |  -0.82  |  -0.78  |  -25.50  |  0  |  0.0000  |  0.0000  |
 |  1.90  |  4000  |  197  |  0.0494  |  0.9875  |  -1.49  |  -1.41  |  -24.14  |  0  |  0.0005  |  0.0005  |
 |  1.95  |  4000  |  198  |  0.0495  |  0.9906  |  -0.78  |  -0.73  |  -23.32  |  1  |  0.0015  |  0.0015  |
 |  2.00  |  4000  |  196  |  0.0489  |  0.9787  |  -2.04  |  -1.92  |  -21.23  |  0  |  0.0002  |  0.0002  |
 |  2.20  |  4000  |  185  |  0.0462  |  0.9238  |  -2.24  |  -2.03  |  -15.19  |  0  |  0.0000  |  0.0000  |
 |  2.40  |  4000  |  177  |  0.0443  |  0.8856  |  -2.17  |  -1.83  |  -13.98  |  0  |  0.0000  |  0.0000  |
 |  2.60  |  4000  |  184  |  0.0460  |  0.9194  |  -0.29  |  -0.12  |  -10.90  |  0  |  0.0000  |  0.0000  |
 |  2.80  |  4000  |  166  |  0.0414  |  0.8276  |  -0.94  |  -0.71  |  -8.84  |  0  |  0.0000  |  0.0000  |
 |  3.00  |  4000  |  84  |  0.0209  |  0.4188  |  -3.10  |  -1.95  |  -7.02  |  2  |  0.0211  |  0.0162  |
 |  3.20  |  4000  |  63  |  0.0157  |  0.3132  |  -2.99  |  -1.81  |  -5.99  |  2  |  0.0181  |  0.0148  |
 |  3.40  |  4000  |  19  |  0.0047  |  0.0933  |  -3.46  |  -1.67  |  -4.86  |  1  |  0.0265  |  0.0268  |
 |  3.60  |  8000  |  ---  |  ---  |  ---  |  ---  |  -1.59  |  -4.00  |  7  |  0.0803  |  0.0307  |
 |  3.80  |  12000  |  28  |  0.0023  |  0.0466  |  -2.90  |  -1.38  |  -3.66  |  2  |  0.0261  |  0.0187  |
 |  4.00  |  16000  |  32  |  0.0020  |  0.0395  |  -3.02  |  -1.47  |  -3.57  |  1  |  0.0057  |  0.0057  |
 |  4.05  |  12000  |  ---  |  ---  |  ---  |  ---  |  -1.66  |  -3.41  |  6  |  0.0992  |  0.0440  |
 |  4.10  |  8000  |  ---  |  ---  |  ---  |  ---  |  -1.57  |  -3.27  |  5  |  0.1350  |  0.0641  |
 |  4.15  |  4000  |  ---  |  ---  |  ---  |  ---  |  -1.60  |  -3.18  |  4  |  0.2368  |  0.1259  |
 |  4.20  |  4000  |  ---  |  ---  |  ---  |  ---  |  -1.61  |  -3.03  |  4  |  0.1469  |  0.0859  |
 |  5.00  |  4000  |  ---  |  ---  |  ---  |  ---  |  -1.07  |  -1.49  |  11  |  0.4184  |  0.1493  |
---+++ Assorted attachments

Attachments

Topic attachments
I	Attachment	History	Action	Size	Date	Who
png	cls_wo_syst_5TeV.png	r1	manage	8.2 K	2010-09-27 - 21:08	AmnonHarel
png	cpsdn20001I2_88.png	r3 r2 r1	manage	15.9 K	2010-10-07 - 17:03	AmnonHarel
png	cpsdn20001I2_88_v2.png	r1	manage	16.2 K	2010-09-30 - 20:30	AmnonHarel
png	cpsdn20001I2_88_v4.png	r1	manage	16.2 K	2010-10-07 - 16:31	AmnonHarel
png	cpsdn36001I2_88.png	r2 r1	manage	14.8 K	2010-10-07 - 17:03	AmnonHarel
png	cpsdn36001I2_88_v4.png	r1	manage	17.5 K	2010-10-07 - 16:31	AmnonHarel
png	cpsdn40001I2_88.png	r3 r2 r1	manage	15.8 K	2010-10-07 - 17:04	AmnonHarel
png	cpsdn40001I2_88_v2.png	r1	manage	16.7 K	2010-09-30 - 20:31	AmnonHarel
png	cpsdn40001I2_88_v4.png	r1	manage	15.9 K	2010-10-07 - 16:30	AmnonHarel
png	cpsdn40501I2_88.png	r4 r3 r2 r1	manage	15.1 K	2010-10-07 - 17:04	AmnonHarel
png	cpsdn40501I2_88_v2.png	r1	manage	18.0 K	2010-09-30 - 20:33	AmnonHarel
png	cpsdn40501I2_88_v4.png	r1	manage	15.5 K	2010-10-07 - 16:29	AmnonHarel
png	cpsdn41001I2_88.png	r3 r2 r1	manage	14.6 K	2010-10-07 - 17:04	AmnonHarel
png	cpsdn41001I2_88_v2.png	r1	manage	17.9 K	2010-09-30 - 20:31	AmnonHarel
png	cpsdn41001I2_88_v4.png	r1	manage	14.8 K	2010-10-07 - 16:32	AmnonHarel
png	cpsdn41501I2_88.png	r2 r1	manage	14.7 K	2010-10-07 - 17:05	AmnonHarel
png	cpsdn41501I2_88_v4.png	r1	manage	17.7 K	2010-10-07 - 16:29	AmnonHarel
png	cpsdn50001I2_88.png	r2 r1	manage	17.1 K	2010-09-30 - 20:44	AmnonHarel
png	cpsdn50001I2_88_v2.png	r1	manage	17.1 K	2010-09-30 - 20:30	AmnonHarel
png	cpsdn50001I2_88_v4.png	r1	manage	17.1 K	2010-10-07 - 16:30	AmnonHarel
png	cpsdn50002I2_88.png	r1	manage	16.6 K	2010-10-07 - 17:06	AmnonHarel
png	ex1.png	r3 r2 r1	manage	10.9 K	2010-09-30 - 19:00	AmnonHarel
png	ex2.png	r3 r2 r1	manage	12.9 K	2010-09-30 - 19:00	AmnonHarel
png	ex3.png	r3 r2 r1	manage	12.1 K	2010-09-30 - 19:03	AmnonHarel
png	ex4.png	r2 r1	manage	12.7 K	2010-09-30 - 19:01	AmnonHarel
png	ex5.png	r2 r1	manage	14.1 K	2010-09-30 - 19:01	AmnonHarel
png	ex6.png	r2 r1	manage	11.4 K	2010-09-30 - 19:01	AmnonHarel
png	ex7.png	r1	manage	11.3 K	2010-09-30 - 19:02	AmnonHarel
png	more_ex1.png	r1	manage	20.9 K	2010-09-28 - 17:21	AmnonHarel
png	n8ex1.png	r1	manage	10.9 K	2010-09-30 - 19:20	AmnonHarel
png	n8ex2.png	r1	manage	12.9 K	2010-09-30 - 19:20	AmnonHarel
png	n8ex3.png	r1	manage	12.1 K	2010-09-30 - 19:20	AmnonHarel
png	n8ex4.png	r1	manage	12.4 K	2010-09-30 - 19:20	AmnonHarel
png	n8ex5.png	r1	manage	13.9 K	2010-09-30 - 19:21	AmnonHarel
png	n8ex6.png	r1	manage	11.4 K	2010-09-30 - 19:21	AmnonHarel
png	n8ex7.png	r1	manage	10.6 K	2010-09-30 - 19:21	AmnonHarel
png	n8ex8.png	r1	manage	10.6 K	2010-09-30 - 19:35	AmnonHarel
png	n8ex9.png	r1	manage	13.8 K	2010-09-30 - 20:50	AmnonHarel
png	plot_syst_tail.png	r1	manage	21.1 K	2010-10-07 - 12:59	AmnonHarel
png	v7ex1.png	r1	manage	10.9 K	2010-10-07 - 16:54	AmnonHarel
png	v7ex2.png	r1	manage	12.5 K	2010-10-07 - 16:54	AmnonHarel
png	v7ex5.png	r1	manage	13.6 K	2010-10-07 - 16:53	AmnonHarel
png	v7ex6.png	r2 r1	manage	13.5 K	2010-10-07 - 17:15	AmnonHarel
png	v7ex7.png	r2 r1	manage	11.9 K	2010-10-07 - 17:14	AmnonHarel
png	v7ex8.png	r2 r1	manage	11.5 K	2010-10-07 - 17:15	AmnonHarel
png	v7ex9.png	r1	manage	13.5 K	2010-10-07 - 16:50	AmnonHarel

Topic revision: r10 - 2010-10-07 - AmnonHarel

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