ApprovedPlotsID < AtlasPublic

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---+Approved Combined Inner Detector Plots
%TOC%     <!--optional-->

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---++ Introduction

The Inner Detector commissioning and performance plots below are approved to be shown by ATLAS speakers at conferences and similar events.  

<b>Please do not add figures on your own.</b> Contact the [[mailto:pippa.wells@cern.ch][ID project leader]] in case of questions and/or suggestions.

---++Figures


---+++ Detector alignment

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee>
Unbiased residual distribution in x, integrated over all hits-on-tracks in the pixel barrel for the nominal geometry and the preliminary aligned geometry. The residual is defined as the measured hit position minus the expected hit position from the track extrapolation. Shown is the projection onto the local x coordinate, which is the precision coordinate. Tracks are selected to have pT > 2 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0). The distribution is shown for 5 cosmic runs: 91885, 91888, 91890, 91891, 91900, all have solenoid on - corresponding to ~25% of all the solenoid-on data taken in Sep/Oct 2008. New Tracking is used (in 14.5.2.1). A double Gaus fit is performed but only the mean and sigma of the narrower Gaussian are shown.
</td>
<td align="center">
<img src="%ATTACHURL%/Approved_PixBarResX.png" width="200"/><br>
[[%ATTACHURL%/Approved_PixBarResX.eps][Approved_PixBarResX.eps]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee> Unbiased residual distribution in y, integrated over all hits-on-tracks in the pixel barrel for the nominal geometry and the preliminary aligned geometry. The residual is defined as the measured hit position minus the expected hit position from the track extrapolation. Shown is the projection onto the local y coordinate, which is the non-precision coordinate. Tracks are selected to have pT > 2 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0). The distribution is shown for 5 cosmic runs: 91885, 91888, 91890, 91891, 91900, all have solenoid on - corresponding to ~25% of all the solenoid-on data taken in Sep/Oct 2008. New Tracking is used (in 14.5.2.1). A single Gaussian fit is performed.
</td>
<td align="center">
<img src="%ATTACHURL%/Approved_PixBarResY.png" width="200"/><br>
[[%ATTACHURL%/Approved_PixBarResY.eps][Approved_PixBarResY.eps]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee> Unbiased residual distribution in x, integrated over all hits-on-tracks in the SCT barrel for the nominal geometry and the preliminary aligned geometry. The residual is defined as the measured hit position minus the expected hit position from the track extrapolation. Shown is the projection onto the local x coordinate, which is the precision coordinate. Tracks are selected to have pT > 2 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0). The distribution is shown for 5 cosmic runs: 91885, 91888, 91890, 91891, 91900, all have solenoid on - corresponding to ~25% of all the solenoid-on data taken in Sep/Oct 2008. New Tracking is used (in 14.5.2.1). A single Gaussian fit is performed.
</td>
<td align="center">
<img src="%ATTACHURL%/Approved_SCTBarResX.png" width="200"/><br>
[[%ATTACHURL%/Approved_SCTBarResX.eps][Approved_SCTBarResX.eps]]
</td>
</tr>
<tr>
<td bgcolor="#eeeeee">
TRT resolution  in Fall 2008 cosmic data (Xenon) %BR%

This plots is made with combined ID tracks, with the following requirements: %BR%
- minimum  pT>2GeV %BR%
- min 2 Pixel hits %BR%
- min 9 SCT hits %BR%
- min 45 TRT hits %BR%
- Event Phase in range 5 <= EP <= 30 %BR%
- Reject tracks with endcap hits %BR%
- Reject tracks that come from events with more than one reco track (< 5 % of events, avoids pattern reco mistakes ) %BR%

The fit is a single Gaussian, where the fit was iterated until the range corresponded to +/- 1.5*sigma.  The mean and sigma of the fit are reported. 

The tracks are for five golden runs with magnetic field from Fall 2008 (runs 91885, 91888, 91890, 91891, 91900).

The reconstruction was done with Si geometry tag InDetCosmics_2008_03
The distribution is shown for both before and after (tag TRT_Comsics_2008_06) TRT L1 alignment.  The after plot includes both a TRT L1 and L2 alignment.  

<!--
TRT unbiased residual for combined tracks before and after TRT alignment. The alignment includes a global alignment with respect to the Pixel and SCT, as well as an internal module level alignment.%BR% %BR%

Description: The plot show TRT residual distribution from cosmic data with the solenoid on (run 91900).  Tracks are required to have pT >2 GeV, event phase between 5 and 30 ns, >= 45 TRT hits, >= 2 Pixel hits, >= 9 SCT hits, and no endcap hits. A single Gaussian fit to the core of the distribution (+/- 0.3 mm) is done, and the mean and sigma of the fit are reported.  The distribution is made in athena release 15 (-tag=15.0.0) and using ID alignment tags InDet_Cosmics_2008_03 and TRT_Cosmics_2008_06.   

</td>
<td align="center">  <img src="%ATTACHURLPATH%/TRT2008CosmicsCombinedIDTracks.png" width="200"  />
  !-->

</td>
<td align="center">  <img src="%ATTACHURLPATH%/TRT2008CosmicsCombinedIDTracks.png" width="200"  />
<br>
<!--  [[%ATTACHURL%/TRT2008CosmicsCombinedIDTracks.png]]   <br> !-->
See [[ApprovedPlotsTRT][ApprovedPlotsTRT]] for TRT position resolution in 2008 and 2009 data (with alignment, TRT standalone tracks).

 </td> </tr>

<tr>
<td bgcolor=#eeeeee> Cosmic tracks crossing the entire ID leave hits in both the upper and lower halves of the ID.
These tracks can be split near the interaction point and fit separately, resulting in two collision-like tracks that can then be compared. The plots shows the difference in the d0 track parameter between the two split tracks.
Tracks are selected to have pT > 2 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0). Tracks also are required to have a hit in the Pixel B layer, 3 Pixel hits and in total 7 Silicon hits.
The distribution is shown for 5 cosmic runs: 91885, 91888, 91890, 91891, 91900, all have solenoid on - corresponding to ~25% of all the solenoid-on data taken in Sep/Oct 2008. New Tracking is used (in 14.5.2.1). A single Gaussian fit is performed.
</td><td align="center">
<img src="%ATTACHURL%/Approved_DeltaD0.png" width="200"/><br>
[[%ATTACHURL%/Approved_DeltaD0.eps][Approved_DeltaD0.eps]]
</td>
</tr><tr>
<td bgcolor=#eeeeee> Cosmic tracks crossing the entire ID leave hits in both the upper and lower halves of the ID.
These tracks can be split near the interaction point and fit separately, resulting in two collision-like tracks that can then be compared. The plots shows the difference in the z0 track parameter between the two split tracks.
Tracks are selected to have pT > 2 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0). Tracks also are required to have a hit in the Pixel B layer, 3 Pixel hits and in total 7 Silicon hits.
The distribution is shown for 5 cosmic runs: 91885, 91888, 91890, 91891, 91900, all have solenoid on - corresponding to ~25% of all the solenoid-on data taken in Sep/Oct 2008. New Tracking is used (in 14.5.2.1). A single Gaussian fit is performed.
</td><td align="center">
<img src="%ATTACHURL%/Approved_DeltaZ0.png" width="200"/><br>
[[%ATTACHURL%/Approved_DeltaZ0.eps][Approved_DeltaZ0.eps]]
</td>
</tr><tr>
<td bgcolor=#eeeeee> Cosmic tracks crossing the entire ID leave hits in both the upper and lower halves of the ID.
These tracks can be split near the interaction point and fit separately, resulting in two collision-like tracks that can then be compared. The plots shows the difference in the Q/pT track parameter between the two split tracks.
Tracks are selected to have pT > 2 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0). Tracks also are required to have a hit in the Pixel B layer, 3 Pixel hits and in total 7 Silicon hits.
The distribution is shown for 5 cosmic runs: 91885, 91888, 91890, 91891, 91900, all have solenoid on - corresponding to ~25% of all the solenoid-on data taken in Sep/Oct 2008. New Tracking is used (in 14.5.2.1). A single Gaus fit is performed.
</td><td align="center">
<img src="%ATTACHURL%/Approved_DeltaQoPT.png" width="200"/><br>
[[%ATTACHURL%/Approved_DeltaQoPT.eps][Approved_DeltaQoPT.eps]]
</td>
</tr><tr>
<td bgcolor=#eeeeee> Cosmic tracks crossing the entire ID leave hits in both the upper and lower halves of the ID.
These tracks can be split near the interaction point and fit separately, resulting in two collision-like tracks that can then be compared. The plots shows the difference in the phi track parameter between the two split tracks.
Tracks are selected to have pT > 2 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0). Tracks also are required to have a hit in the Pixel B layer, 3 Pixel hits and in total 7 Silicon hits.
The distribution is shown for 5 cosmic runs: 91885, 91888, 91890, 91891, 91900, all have solenoid on - corresponding to ~25% of all the solenoid-on data taken in Sep/Oct 2008. New Tracking is used (in 14.5.2.1). A double Gaussian fit is performed but only the mean and sigma of the narrower Gaus are shown.
</td><td align="center">
<img src="%ATTACHURL%/Approved_DeltaPhi.png" width="200"/><br>
[[%ATTACHURL%/Approved_DeltaPhi.eps][Approved_DeltaPhi.eps]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee> 
Unbiased residual distribution in x, integrated over all hits-on-tracks in the pixel barrel using the 2008 aligned geometry. The residual is defined as the measured hit position minus the expected hit position from the track extrapolation. Shown is the projection onto the local x coordinate, which is the precision coordinate. Tracks are selected to have pT > 1 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0), and to have 1 B-layer, 3 Pixel, 8 SCT, and 25 TRT Hits. The distribution is shown using data taken in 2009, cosmic run: 121330, which had solenoid on. New Tracking is used (in AtlasTier0-15.2.0.7). A double Gaus fit is performed but only the mean and sigma of the narrower Gaussian are shown.  

Note: The distribution shown here is made with the new standard cuts (listed), we have verified that the results are not sensitive to the difference in track selection.
</td><td align="center">
<img src="%ATTACHURL%/ApprovedPlots2009Data_PixelX.png" width="200"/><br>
[[%ATTACHURL%/ApprovedPlots2009Data_PixelX.eps][ApprovedPlots2009Data_PixelX.eps]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee> 
Unbiased residual distribution in y, integrated over all hits-on-tracks in the pixel barrel using the 2008 aligned geometry. The residual is defined as the measured hit position minus the expected hit position from the track extrapolation. Shown is the projection onto the local y coordinate, which is the non-precision coordinate. Tracks are selected to have pT > 1 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0), and to have 1 B-layer, 3 Pixel, 8 SCT, and 25 TRT Hits. The distribution is shown using data taken in 2009, cosmic run: 121330, which had solenoid on. New Tracking is used (in AtlasTier0-15.2.0.7). A single Gaus fit is performed and the mean and sigma are shown.  

Note: The distribution shown here is made with the new standard cuts (listed), we have verified that the results are not sensitive to the difference in track selection.
</td><td align="center">
<img src="%ATTACHURL%/ApprovedPlots2009Data_PixelY.png" width="200"/><br>
[[%ATTACHURL%/ApprovedPlots2009Data_PixelY.eps][ApprovedPlots2009Data_PixelY.eps]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee> 
Unbiased residual distribution in x, integrated over all hits-on-tracks in the SCT barrel using the 2008 aligned geometry. The residual is defined as the measured hit position minus the expected hit position from the track extrapolation. Shown is the projection onto the local x coordinate. Tracks are selected to have pT > 1 GeV, |d0|<50mm, |z0|<400mm (in other words they are required to go through the pixel L0), and to have 1 B-layer, 3 Pixel, 8 SCT, and 25 TRT Hits. The distribution is shown using data taken in 2009, cosmic run: 121330, which had solenoid on. New Tracking is used (in AtlasTier0-15.2.0.7). A single Gaus fit is performed and the mean and sigma are shown.  

Note: The distribution shown here is made with the new standard cuts (listed), we have verified that the results are not sensitive to the difference in track selection.
</td><td align="center">
<img src="%ATTACHURL%/ApprovedPlots2009Data_SCTX.png" width="200"/><br>
[[%ATTACHURL%/ApprovedPlots2009Data_SCTX.eps][ApprovedPlots2009Data_SCTX.eps]]
</td>
</tr>
</table>

---+++ ID track parameter resolutions


Cosmics muons traverse the whole Inner Detector and thus leave hits in the upper and lower parts of the detector. By dividing the track to its upper and lower half according to the value of the y coordinate of hits on track and refitting both hit collections, two collision-like tracks originating from the same cosmic muon are obtained. After alignment, track parameter resolutions are studied by comparing the difference (residual) of the track parameters at the perigee point. Since both tracks have an associated error, the quoted resolution is the RMS of the residual distribution of the particular track parameter divided by square root 2. The track parameter resolutions are studied dependant on variables like the pT or the d0 of the tracks. Shifted mean values of the residual distributions can be a sign of systematic detector deformations. The following distributions show data from  runs 91885,91888,91890,91891 and 91900 taken in 2008. The tracks have been refitted using Athena release 15.0.0.7 (Tier0). 
<p>
The following cuts have ben applied per track (if not stated otherwise):

   * nPixelHits in the barrel >=2
   * nSCTHits in the barrel >=6
   * nTRTHits in the barrel >=25
   * |d0| < 40mm
   * pT >= 1 GeV

Additionally only events with an event phase between 5 and 30 ns are accepted to ensure proper timing of the sub-detectors.  The plots show comparisons of tracks using the full Inner Detector (silicon and TRT detectors, closed triangles), only the silicon sub-detecors (open triangles) together with tracks from cosmic simulation using the full Inner Detector (stars). The requirement of at least 25 TRT hits is dropped for silicon only tracks. However, the cut on the event phase is retained to ensure proper timing and the comparability of the analyzed sets of tracks. There is no cut on the event phase for simulation events since the jitter in cosmic trigger timing is not simulated.

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee>Transverse impact parameter resolution as a function of pT. In the low pT region, the resolution is dominated by multiple scattering effects. At higher values, the resolution is flat. Taking into account the TRT information improves the resolution. The difference to the MC curve indicates the remaining mislaignment.
</td><td align="center">
<img src="%ATTACHURL%/delta_d0_vs_pT.png" width="200"/><br>
[[%ATTACHURL%/delta_d0_vs_pT.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Transverse impact parameter resolution as a function of d0 itself. For this plot the d0 cut is released to 120 mm and the minum number of Pixel hits is set to one. In general the resolution for full ID tracks is better. The resolution is better in the central d0 region due to more Pixel layers crossed and less spread clusters in the Pixel detector. Dips are seen if the d0 of the tracks equal the radii of the pixel layers (indicated by dashed lines). Since the d0 is in these cases very close to a hit on a Pixel layer, the extrapolation to the perigee point is very small and the resolution improves. The MC distributions confirms the observed behaviour. 
</td><td align="center">
<img src="%ATTACHURL%/delta_d0_vs_d0.png" width="200"/><br>
[[%ATTACHURL%/delta_d0_vs_d0.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Mean of the transverse impact parameter distribution as a function of pT.  The expected value of the mean is 0 as confirmed by the MC distribution. In data a shift is seen for full ID and silicon only tracks. The shift increases with higher pT. 
</td><td align="center">
<img src="%ATTACHURL%/mean_delta_d0_vs_pT.png" width="200"/><br>
[[%ATTACHURL%/mean_delta_d0_vs_pT.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Mean of the transverse impact parameter distribution as a function of d0 itself. For this plot the d0 cut is released to 120 mm and the minum number of Pixel hits is set to one. The expected value of the mean is 0 as confirmed by the MC distribution. In data a shift is seen for full ID and silicon only tracks. The shift is biggest in the central d0 region.
</td><td align="center">
<img src="%ATTACHURL%/mean_delta_d0_vs_d0.png" width="200"/><br>
[[%ATTACHURL%/mean_delta_d0_vs_d0.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Relative momentum resolution as a function of pT. The relative momentum resolution increases with higher pT due to stiffer tracks and a more difficult measurement of the sagitta. Including information from the TRT extends the lever arm and helps improving the resolution especially at high pT values. The difference to the MC curve indicates the remaining misalignment. 
</td><td align="center">
<img src="%ATTACHURL%/delta_QoverP_vs_pT.png" width="200"/><br>
[[%ATTACHURL%/delta_QoverP_vs_pT.eps][eps figure]]
</td>
</tr>


<tr>
<td bgcolor=#eeeeee>Mean of the relative momentum distribution as a function of pT. The expected value of the mean is 0 as confirmed by the MC distribution. In data a shift is seen for full ID and silicon only tracks. The shift increases with higher pT. 
</td><td align="center">
<img src="%ATTACHURL%/mean_delta_QoverP_vs_pT.png" width="200"/><br>
[[%ATTACHURL%/mean_delta_QoverP_vs_pT.eps][eps figure]]
</td>
</tr>


<tr>
<td bgcolor=#eeeeee>Resolution of the azimuthal angle as a function of pT. In the low pT region, the resolution is dominated by multiple scattering effects. At higher values, the resolution is flat. Taking into account the TRT information improves the resolution. The difference to the MC curve indicates the remaining mislaignment.
</td><td align="center">
<img src="%ATTACHURL%/delta_phi0_vs_pT.png" width="200"/><br>
[[%ATTACHURL%/delta_phi0_vs_pT.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Resolution of the polar angle as a function of eta. The resolution of the polar angle theta improves at larger eta due to broader pixel clusters that allow a more precise position measurement. Since the TRT effectively does not measure the z coordinate in the barrel region, the resolutions are equal for silicon only and full ID tracks. The difference to the MC curve indicates the remaining misalignment.
</td><td align="center">
<img src="%ATTACHURL%/delta_theta_vs_eta.png" width="200"/><br>
[[%ATTACHURL%/delta_theta_vs_eta.eps][eps figure]]
</td>
</tr>
</table>

---+++ Distributions from cosmic ray tracks 

Warning: Cosmic ray spectra including comparisons with MC which appeared before on this page are not approved for external use at this stage.
The MC does not model some details of the special cosmic trigger configuration and timing. It includes the two main access shafts, but not
the two lift shafts. Until these effects are taken into account, the MC-data comparison is not useful. 
<p>
Cosmic muons crossing the entire ATLAS detector leave hits in the Inner Detector (ID) and so
tracks can be reconstructed. Two different tracking algorithms are in use for the 
reconstruction: the CTB (Cosmics and Test Beam) tracking and the New Tracking. The results
below show the performance of the CTB.
<p>
Tracks are characterized by 5 parameters. These are defined in a reference point, the perigee,
which is the point of closest approach to the z/beam axis. d0 is the signed distance to the
z-axis, z0 is the z-coordinate of the perigee, phi0 is the angle in the x-y plane at the
perigee, theta0 is the angle with the z-axis and q/p is the charge of the cosmic muon divided
by its momentum.
<p>
In the next plots, the parameters of these cosmic muon tracks (reconstructed with CTB tracking
and release 14.5.0.5, AtlasProduction) from the ATLAS combined cosmic run 91890 (Autumn 2008)
are shown. Both toroid and solenoid were on during this run.
<p>
For the theta0 and z0 distributions, tracks are required to have Silicon hits (since these
parameters are not measured by the TRT barrel).

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee>
Cosmic spectra (d0 distribution) as seen in run 91890.
</td><td align="center">
<img src="%ATTACHURL%/trackpar_d0.png" width="200"/><br>
[[%ATTACHURL%/trackpar_d0.eps][eps figure]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee>Cosmic spectra (z0 distribution) as seen in run 91890.
</td><td align="center">
<img src="%ATTACHURL%/trackpar_z0.png" width="200"/><br>
[[%ATTACHURL%/trackpar_z0.eps][eps figure]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee>Cosmic spectra (phi0 distribution) as seen in run 91890.
</td><td align="center">
<img src="%ATTACHURL%/trackpar_phi0.png" width="200"/><br>
[[%ATTACHURL%/trackpar_phi0.eps][eps figure]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee>Cosmic spectra (theta0 distribution) as seen in run 91890.
</td><td align="center">
<img src="%ATTACHURL%/trackpar_theta0.png" width="200"/><br>
[[%ATTACHURL%/trackpar_theta0.eps][eps figure]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee>Cosmic spectra (!QoverP distribution) as seen in run 91890.
</td><td align="center">
<img src="%ATTACHURL%/trackpar_QoverP.png" width="200"/><br>
[[%ATTACHURL%/trackpar_QoverP.eps][eps figure]]
</td>
</tr>
</table>

---+++ Cosmic ray track statistics

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee>Collected track statistics in autumn 2008:
| |  *field off*  |  *field on*  |  *total*  |
|  All tracks  |   4940000  |   2670000  |   7610000  |
|  SCT hit  |   1150000  |   880000  |   2030000  |
|  Pixel hit  |   230000  |   190000  |   420000  | 
</td><td align="center">
<img src="%ATTACHURL%/IDCosmic08_statistics.gif" width="200"/><br>
[[%ATTACHURL%/IDCosmic08_statistics.pdf][pdf figure]]
</td>
</tr>
</table>

---+++ Event displays

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee >Inner detector event display for event 757427 of the cosmic run 90270 with field ON.
</td><td align="center">
[[https://twiki.cern.ch/twiki/bin/viewfile/Atlas/ApprovedPlotsED?rev=1;filename=curvedcosmic6.png][<img src="https://twiki.cern.ch/twiki/bin/viewfile/Atlas/ApprovedPlotsED?rev=1;filename=curvedcosmic6.png" alt="curvedcosmic6.png" width='200' />]]
</td>
</tr>
<tr>
<td bgcolor=#eeeeee >Inner detector event display for event 62340 of the cosmic run 90731 (no Solenoid). Showing hits on track for both TRT endcaps, as well as SCT and pixel barrel and endcap hits.
</td><td align="center">
[[https://twiki.cern.ch/twiki/bin/viewfile/Atlas/ApprovedPlotsED?rev=1;filename=barrel_endcaptrack.png][<img src="https://twiki.cern.ch/twiki/bin/viewfile/Atlas/ApprovedPlotsED?rev=1;filename=barrel_endcaptrack.png" alt="barrel_endcaptrack.png" width='200' />]]
</td>
</tr>
</table>

---+++ Beam Conditions Monitor (BCM) timing distributions

During the combined Inner Detector running in November 2008, out of 50 million triggers, over 100 events with signals in the BCM were observed. The BCM reads out 31 consecutive bunch crossings for each trigger, and the initial timing calibration from measured cable and fibre lengths puts the signal around bin 19. The timing distribution is narrower for events triggered by the TRT than for events triggered by the RPC muon chambers.

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee>BCM timing distribution for RPC triggered events
</td><td align="center">
<img src="%ATTACHURL%/bcm_rpc.png" width="200"/><br>
[[%ATTACHURL%/bcm_rpc.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>BCM timing distribution for TRT triggered events
</td><td align="center">
<img src="%ATTACHURL%/bcm_trt.png" width="200"/><br>
[[%ATTACHURL%/bcm_trt.eps][eps figure]]
</td>
</tr>
</table>

---+++ Beam Conditions Monitor (BCM) beam aborts

Beam aborts from aperture scans. These plots were approved on 16 February 2010.

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee> Total number of BCM high and low gain channel hits integrated over 40 us versus time during a Beam 2 IR1 horizontal aperture scan with LHC fill 923. The post mortem buffer covers 1177 LHC revolutions (105 ms). It is frozen 9 ms (~100 orbits) after an abort. An increase of the number of BCM hits is visible during a step of the aperture scan starting at -26 ms before the end of the buffer. A beam abort initiated by BCM occurred at -9.8 ms before the end of the buffer and the BCM hit activity returns to zero after the beam is dumped.

</td><td align="center">
<img src="%ATTACHURL%/Aperture_Scan_Abort_40us.png" width="200"/><br>
[[%ATTACHURL%/Aperture_Scan_Abort_40us.eps][eps figure]]
</td>
</tr>



<tr>
<td bgcolor=#eeeeee> 

Timelines of all 16 BCM readout channels in full 390 ps sampling resolution covering 3 25 ns bunch crossings. The are recorded with the BCM post mortem buffer during a Beam 2 IR1 horizontal aperture scan with LHC fill 923 in the moment of a BCM initiated beam abort. The left timelines are recorded by one, the right by another ROD. High gain (HG) channel timelines have a green, low gain (LG) ones a yellow background. The top four timelines are from A side detectors, the bottom four from C side detectors. The 3 HG + 3 LG beam abort condition was reached for both RODs and the HG channel show, as expected, longer pulse widths. The pulses of the C side detectors are about 12.5 ns before the A side detector pulses as expected for beam background from Beam 2 (C->A).

</td><td align="center">
<img src="%ATTACHURL%/Aperture_Scan_Abort.png" width="200"/><br>
[[%ATTACHURL%/Aperture_Scan_Abort.eps][eps figure]]
</td>
</tr>
<!--  Plot in preparation to show cooling performance 
<tr>
<td bgcolor=#eeeeee > Inner detector number of Cooling Loops ON as a function of time.
</td><td align="center">
<img src="%ATTACHURL%/SCTLoopsTime.gif" width="200"/><br>
</td>
</tr>
end of commented out row of the table with the cooling plot !--> 
</table>




---+++ Comparison of !NewTracking and CTBTracking


Comparison of NewTracking versus CTB Tracking for real data from the IDCosmic stream of run 91885 (field ON) reconstructed in the first reprocessing in December 2008. (These are technical plots, comparing the results of two different tracking algorithms).
<p>
The following cuts have ben applied:
   * 2*nPixelHits+nSCTHits>=8
   * number of TRT hits >=40
   * pT >= 5 GeV

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee>Distribution of pt for NewTracking and CTB Tracking.
</td><td align="center">
<img src="%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecPt.png" width="200"/><br>
[[%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecPt.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Distribution of q/p for NewTracking and CTB Tracking.
</td><td align="center">
<img src="%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecQoverP.png" width="200"/><br>
[[%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecQoverP.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Number of Hits (nPixel+nSCT+nTRT) on the track.
</td><td align="center">
<img src="%ATTACHURL%/91885_IDCosmic_NewTVsCTB_nHits.png" width="200"/><br>
[[%ATTACHURL%/91885_IDCosmic_NewTVsCTB_nHits.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Distribution of d0 for NewTracking and CTB Tracking.
</td><td align="center">
<img src="%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecD0.png" width="200"/><br>
[[%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecD0.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Distribution of phi0 for NewTracking and CTB Tracking.
</td><td align="center">
<img src="%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecPhi0.png" width="200"/><br>
[[%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecPhi0.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Distribution of z0 for NewTracking and CTB Tracking.
</td><td align="center">
<img src="%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecZ0.png" width="200"/><br>
[[%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecZ0.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Distribution of &#951; for NewTracking and CTB Tracking.
The double-peak structure at 
&#951; &#8776; -0.4 und &#951; &#8776; 0.3 is due to the construction shafts through which the ATLAS detector was lowered into the cavern.

</td><td align="center">
<img src="%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecEta.png" width="200"/><br>
[[%ATTACHURL%/91885_IDCosmic_NewTVsCTB_RecEta.eps][eps figure]]
</td>
</tr>
</table>


---+++ Impact of Random Misalignments

The figures below are taken from the ATLAS PUB note [[http://cdsweb.cern.ch/record/1178860/files/ATL-PHYS-PUB-2009-080.pdf][The Impact of Inner Detector Misalignments on Selected Physics Processes]]. Shown here is the impact of the Day-1 and Day-100 random ID misalignments on reconstructed Zmumu, Jpsi and Bd masses in Monte Carlo simulated samples of these processes.

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee>The ID reconstructed Z mass distribution for a Zmumu Monte Carlo sample reconstructed using the Day-1 
and Day-100 ID misalignments and the perfect ID alignment. The ID reconstructed Z mass is the invariant mass 
formed from the two highest pT Inner Detector tracks, with both tracks satisfying pT>15 GeV and having opposite charge. One can see 
that the random smearing of module positions in the Day-1 and Day-100 alignment constants clearly impact the Z mass resolution.
</td><td align="center">
<img src="%ATTACHURL%/CSC_DayX_Zmumu.png" width="200"/><br>
[[%ATTACHURL%/CSC_DayX_Zmumu.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>The difference between the ID reconstructed Z mass and the true Z mass for a Zmumu Monte Carlo sample reconstructed using the Day-1 and Day-100 ID misalignments and the perfect ID alignment. The ID reconstructed Z mass is the invariant mass 
formed from the two highest pT Inner Detector tracks, with both tracks satisfying pT>15 GeV  and having opposite charge. The true Z mass is the invariant 
mass of the two true particles can be associated to the ID tracks used in the Z reconstruction. A Gaussian is fitted in the range [mu-RMS,mu+RMS], 
and the mean and width of this Gaussian stated in the plot. 
The random module position smearing of the The Day-1 misalignments, at the level of 20microns, produces a  Z mass resolution degraded 
by ~50% when compared to the perfect alignment case.  The Day-100 geometry uses a reduced random smearing of the module positions,  
at the level of 10microns, and consequently the impact on the Z mass resolution is smaller, a ~13% degradation.
</td><td align="center">
<img src="%ATTACHURL%/CSC_DayX_Delta_Zmumu.png" width="200"/><br>
[[%ATTACHURL%/CSC_DayX_Delta_Zmumu.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>The difference between the ID reconstructed Z mass and the true Z mass for a Zmumu Monte Carlo sample reconstructed using the Day-1 and Day-100 ID misalignments and the perfect ID alignment, where the tracks have been restricted to |eta|<1.0 (barrel region).
</td><td align="center">
<img src="%ATTACHURL%/CSC_DayX_Delta_Zmumu_barrel.png" width="200"/><br>
[[%ATTACHURL%/CSC_DayX_Delta_Zmumu_barrel.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>The results of a Gaussian fit to the JPsi mass for events in a Bd Monte Carlo sample that have been 
reconstructed with Day-1 and Day-100 ID alignment constants and perfect ID alignment. The JPsi candidates are selected 
by looking for opposite charged track pairs which originate from a common vertex and have a mass within 3 sigma of the nominal JPsi mass. 
One can see that the impact of random misalignments on the JPsi mass resolution is not significant.
</td><td align="center">
<img src="%ATTACHURL%/JpsiMass-DayX-UML.png" width="200"/><br>
[[%ATTACHURL%/JpsiMass-DayX-UML.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>The distribution of the event-by-event difference between the JPsi mass when reconstructed with the ideal ID alignment, to 
the mass when the same event is reconstructed using the Day-1 or Day-100 ID random misalignments. 
The mean and width of a Gaussian fit made to the core of the distribution is reported in the plot. The Day-1 and Day-100 misalignments 
degrade the JPsi mass resolution relative to the ideal alignment case by only 
~23MeV and ~12MeV respectively. This effect is not significant when added in quadrature to the ideal alignment JPsi resolution of 48MeV (see plot above). 
</td><td align="center">
<img src="%ATTACHURL%/JpsiMass-DayX-MisalgMinusIdeal.png" width="200"/><br>
[[%ATTACHURL%/JpsiMass-DayX-MisalgMinusIdeal.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>The results of a Gaussian fit to the Bd mass for events in a Bd Monte Carlo sample that have been 
reconstructed with Day-1 and Day-100 ID alignment constants and perfect ID alignment. For details of the Bd mass reconstruction see the [[http://cdsweb.cern.ch/record/1125884][CSC book]] pages 1124-1126. 
One can see that the impact of random misalignments on the Bd mass resolution is not significant.
</td><td align="center">
<img src="%ATTACHURL%/BdMass-DayX-UML.png" width="200"/><br>
[[%ATTACHURL%/BdMass-DayX-UML.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>The distribution of the event-by-event difference between the Bd mass when reconstructed with the ideal ID alignment, to 
the mass when the same event is reconstructed using the Day-1 or Day-100 ID random misalignments. 
The mean and width of a Gaussian fit made to the core of the distribution is reported in the plot. The Day-1 and Day-100 misalignments 
degrade the Bd mass resolution relative to the ideal alignment case by only 
~32MeV and ~16MeV respectively. This effect is not significant when added in quadrature to the ideal alignment Bd resolution of 77MeV (see plot above). 
</td><td align="center">
<img src="%ATTACHURL%/BdMass-DayX-MisalgMinusIdeal.png" width="200"/><br>
[[%ATTACHURL%/BdMass-DayX-MisalgMinusIdeal.eps][eps figure]]
</td>
</tr>
</table>

---+++ Impact of Global Systematic Misalignments

The figures below are taken from the ATLAS PUB note [[http://cdsweb.cern.ch/record/1178860/files/ATL-PHYS-PUB-2009-080.pdf][The Impact of Inner Detector Misalignments on Selected Physics Processes]]. Shown here is the impact of the Curl, Twist, Elliptical and Telescope global systematic ID misalignments on combined ID track reconstruction and on reconstructed Zmumu, Jpsi and Bd masses.

<table class="twikiTable" width="100%" bgcolor=#f5f5fa  border=1 cellpadding=10 cellspacing=10>
<tr>
<td bgcolor=#eeeeee> The \chisquareddof~distributions of Inner Detector tracks when reconstructed with each of the Curl, Twist, Elliptical and Telescope weak mode ID misalignments compared to the ideal ID alignment case. A Zmumu Monte Carlo sample is used, and all tracks with reconstructed pT>2GeV are shown. 
</td><td align="center">
<img src="%ATTACHURL%/Curl_chi2dof.png" width="200"/><br>
[[%ATTACHURL%/Curl_chi2dof.eps][Curl eps figure]]
[[%ATTACHURL%/Twist_chi2dof.eps][Twist eps figure]]
[[%ATTACHURL%/Elliptical_chi2dof.eps][Elliptical eps figure]]
[[%ATTACHURL%/Telescope_chi2dof.eps][Telescope eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee> The difference between the reconstructed Inner Detector track Q/pT and the associated truth particle Q/pT when tracks are reconstructed 
with the Curl-Large and Curl-Small ID misalignments compared to the ideal ID alignment case.  A Zmumu Monte Carlo sample is used, and all tracks with 
reconstructed pT>2GeV are shown. The different plots cover different track eta regions. 
</td><td align="center">
<img src="%ATTACHURL%/Curl_dqopt_barrel.png" width="200"/><br>
[[%ATTACHURL%/Curl_dqopt_barrel.eps][Barrel eps figure]]
[[%ATTACHURL%/Curl_dqopt_eca.eps][ECA eps figure]]
[[%ATTACHURL%/Curl_dqopt_ecc.eps][ECC eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee> Ratio of the reconstructed Inner Detector track pT to the associated truth particle pT as a function of the truth particle 
Q*pT for track |eta|<1.0. Tracks from a Zmumu Monte Carlo sample are reconstructed with the Curl-Large and Curl-Small ID misalignments and the ideal 
alignment case. Each point represents the mean of the pT^{reco}/pT^{truth} distribution in that bin, with the error bars representing the error on the mean. 
The plot is made separately for positively and negatively charged tracks. 
</td><td align="center">
<img src="%ATTACHURL%/Curl_dPtvsTruthPt_barrel_positive.png" width="200"/><br>
[[%ATTACHURL%/Curl_dPtvsTruthPt_barrel_positive.eps][Positive eps figure]]
[[%ATTACHURL%/Curl_dPtvsTruthPt_barrel_negative.eps][Negative eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee> The ID reconstructed Z mass distribution for a \zmumu~Monte Carlo sample reconstructed using the Curl misalignments, compared with 
the ideal ID alignment. The ID reconstructed Z mass is the invariant mass 
formed from the two highest pT Inner Detector tracks, with both tracks satisfying pT>15GeV and having opposite charge. An impact on the 
Z mass resolution is clearly produced by the Curl misalignment. The magnitude of this impact is better seen in the figure below.
</td><td align="center">
<img src="%ATTACHURL%/Curl_Zmumu.png" width="200"/><br>
[[%ATTACHURL%/Curl_Zmumu.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee> The difference between the ID reconstructed Z mass and the truth Z mass, for a Zmumu Monte Carlo sample 
reconstructed using the Curl-Large and Curl-Small ID misalignments and the ideal ID alignment. The two plots differ in the Eta restrictions 
applied to the tracks used to reconstruct the Z boson (either no restriction or requiring both legs |eta|<1.0). A Gaussian is fitted in the range [mu-RMS,mu+RMS], 
and the mean and width of this Gaussian stated in the plot.
</td><td align="center">
<img src="%ATTACHURL%/Curl_Delta_Zmumu.png" width="200"/><br>
[[%ATTACHURL%/Curl_Delta_Zmumu.eps][eps figure]]
[[%ATTACHURL%/Curl_Delta_Zmumu_barrel.eps][Barrel eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>The distribution of the event-by-event difference between the JPsi mass when reconstructed with the ideal ID alignment, to 
the mass when the same event is reconstructed using the Curl-Large and Curl-Small ID misalignments. A Bd simulated Monte Carlo sample is used.
The mean and width of a Gaussian fit made to the core of the distribution is reported in the plot. 
</td><td align="center">
<img src="%ATTACHURL%/JpsiMass-Curl-MisalgMinusIdeal.png" width="200"/><br>
[[%ATTACHURL%/JpsiMass-Curl-MisalgMinusIdeal.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>The distribution of the event-by-event difference between the Bd mass when reconstructed with the ideal ID alignment, to 
the mass when the same event is reconstructed using the Curl-Large and Curl-Small ID misalignments. A Bd simulated Monte Carlo sample is used.
The mean and width of a Gaussian fit made to the core of the distribution is reported in the plot. 
</td><td align="center">
<img src="%ATTACHURL%/BdMass-Curl-MisalgMinusIdeal.png" width="200"/><br>
[[%ATTACHURL%/BdMass-Curl-MisalgMinusIdeal.eps][eps figure]]
</td>
</tr>

<tr>
<td bgcolor=#eeeeee>Figure description ...
</td><td align="center">
figure
</td>
</tr>

</table>

---++Links

   * [[InDetTrackingPerformance][Inner Detector tracking performance Wiki]]
   * [[InnerDetectorSoftware][Inner Detector software Wiki]]
   * [[https://twiki.cern.ch/twiki/bin/view/Atlas/IDAlignPlotsApproveWorkshop][Plots prepared and approved for the LHC Detector Alignment Workshop in June 2009]]. For presentations with more technical ID alignment information. Please contact the [[mailto:jochen.schieck@cern.ch][ ID Alignment convener]] before using them.


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%RESPONSIBLE% %REVINFO{Main.PippaWells}% %BR%
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%REVIEW% *Never reviewed*


<!--
   * Atlas_ID_Loops_ON_cy_2008.gif: <br />
     <img src="%ATTACHURLPATH%/Atlas_ID_Loops_ON_cy_2008.gif" alt="Atlas_ID_Loops_ON_cy_2008.gif" width='504' height='720' />
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   * BCM timing for RPC triggers: <br />
     <img src="%ATTACHURLPATH%/bcm_rpc.png" alt="bcm_rpc.png" width='1134' height='768' />

   * BCM timing for TRT triggers: <br />
     <img src="%ATTACHURLPATH%/bcm_trt.png" alt="bcm_trt.png" width='1134' height='768' />

   * [[%ATTACHURL%/bcm_trt.eps][bcm_trt.eps]]: BCM timing for TRT triggers


%STOPINCLUDE%

Attachments

Topic attachments
I	Attachment	History	Action	Size	Date	Who	Comment
eps	91885_IDCosmic_NewTVsCTB_RecD0.eps	r1	manage	14.6 K	2009-03-20 - 18:26	ChristianSchmitt
png	91885_IDCosmic_NewTVsCTB_RecD0.png	r1	manage	7.8 K	2009-03-20 - 18:26	ChristianSchmitt
eps	91885_IDCosmic_NewTVsCTB_RecEta.eps	r1	manage	13.4 K	2009-03-20 - 18:25	ChristianSchmitt
png	91885_IDCosmic_NewTVsCTB_RecEta.png	r1	manage	6.9 K	2009-03-20 - 18:25	ChristianSchmitt
eps	91885_IDCosmic_NewTVsCTB_RecPhi0.eps	r1	manage	13.9 K	2009-03-20 - 18:25	ChristianSchmitt
png	91885_IDCosmic_NewTVsCTB_RecPhi0.png	r1	manage	7.2 K	2009-03-20 - 18:25	ChristianSchmitt
eps	91885_IDCosmic_NewTVsCTB_RecPt.eps	r1	manage	16.0 K	2009-03-20 - 18:25	ChristianSchmitt
png	91885_IDCosmic_NewTVsCTB_RecPt.png	r1	manage	7.7 K	2009-03-20 - 18:24	ChristianSchmitt
eps	91885_IDCosmic_NewTVsCTB_RecQoverP.eps	r1	manage	11.2 K	2009-03-20 - 18:24	ChristianSchmitt
png	91885_IDCosmic_NewTVsCTB_RecQoverP.png	r1	manage	7.1 K	2009-03-20 - 18:24	ChristianSchmitt
eps	91885_IDCosmic_NewTVsCTB_RecZ0.eps	r1	manage	16.9 K	2009-03-20 - 18:23	ChristianSchmitt
png	91885_IDCosmic_NewTVsCTB_RecZ0.png	r1	manage	8.2 K	2009-03-20 - 18:23	ChristianSchmitt
eps	91885_IDCosmic_NewTVsCTB_nHits.eps	r1	manage	15.3 K	2009-03-20 - 18:24	ChristianSchmitt
png	91885_IDCosmic_NewTVsCTB_nHits.png	r1	manage	7.7 K	2009-03-20 - 18:23	ChristianSchmitt
eps	Aperture_Scan_Abort.eps	r1	manage	7388.8 K	2010-02-19 - 09:51	PippaWells
png	Aperture_Scan_Abort.png	r1	manage	94.2 K	2010-02-19 - 09:51	PippaWells
eps	Aperture_Scan_Abort_40us.eps	r1	manage	2620.4 K	2010-02-19 - 09:51	PippaWells
png	Aperture_Scan_Abort_40us.png	r1	manage	74.4 K	2010-02-19 - 09:51	PippaWells
eps	ApprovedPlots2009Data_PixelX.eps	r1	manage	19.1 K	2009-07-27 - 11:56	UnknownUser
png	ApprovedPlots2009Data_PixelX.png	r1	manage	14.9 K	2009-07-27 - 11:56	UnknownUser
eps	ApprovedPlots2009Data_PixelY.eps	r1	manage	25.9 K	2009-07-27 - 11:56	UnknownUser
png	ApprovedPlots2009Data_PixelY.png	r1	manage	16.5 K	2009-07-27 - 11:57	UnknownUser
eps	ApprovedPlots2009Data_SCTX.eps	r1	manage	17.8 K	2009-07-27 - 11:57	UnknownUser
png	ApprovedPlots2009Data_SCTX.png	r1	manage	15.4 K	2009-07-27 - 11:57	UnknownUser
eps	Approved_DeltaD0.eps	r1	manage	32.0 K	2009-03-05 - 14:19	TobiasGolling	Delta D0 from cosmic tracks broken down in 2 legs
png	Approved_DeltaD0.png	r1	manage	30.6 K	2009-03-05 - 14:19	TobiasGolling	Delta D0 from cosmic tracks broken down in 2 legs
eps	Approved_DeltaPhi.eps	r1	manage	49.1 K	2009-03-05 - 14:20	TobiasGolling	Delta Phi from cosmic tracks broken down in 2 legs
png	Approved_DeltaPhi.png	r1	manage	31.4 K	2009-03-05 - 14:21	TobiasGolling	Delta Phi from cosmic tracks broken down in 2 legs
eps	Approved_DeltaQoPT.eps	r1	manage	17.6 K	2009-03-05 - 14:21	TobiasGolling	Delta QopT from cosmic tracks broken down in 2 legs
png	Approved_DeltaQoPT.png	r1	manage	29.8 K	2009-03-05 - 14:21	TobiasGolling	Delta QopT from cosmic tracks broken down in 2 legs
eps	Approved_DeltaZ0.eps	r1	manage	26.0 K	2009-03-05 - 14:21	TobiasGolling	Delta Z0 from cosmic tracks broken down in 2 legs
png	Approved_DeltaZ0.png	r1	manage	32.7 K	2009-03-05 - 14:22	TobiasGolling	Delta Z0 from cosmic tracks broken down in 2 legs
eps	Approved_PixBarResX.eps	r1	manage	28.5 K	2009-03-05 - 14:22	TobiasGolling	Pixel x residuals
png	Approved_PixBarResX.png	r1	manage	32.8 K	2009-03-05 - 14:23	TobiasGolling	Pixel x residuals
eps	Approved_PixBarResY.eps	r1	manage	38.8 K	2009-03-05 - 14:23	TobiasGolling	Pixel y residuals
png	Approved_PixBarResY.png	r1	manage	39.7 K	2009-03-05 - 14:23	TobiasGolling	Pixel y residuals
eps	Approved_SCTBarResX.eps	r1	manage	27.5 K	2009-03-05 - 14:24	TobiasGolling	SCT x residuals
png	Approved_SCTBarResX.png	r1	manage	31.5 K	2009-03-05 - 14:24	TobiasGolling	SCT x residuals
gif	Atlas_ID_Loops_ON_cy_2008.gif	r1	manage	20.9 K	2009-03-09 - 14:19	SaverioDAuria	Number of ID Cooling Loops ON as a function of time
eps	BdMass-Curl-MisalgMinusIdeal.eps	r1	manage	24.6 K	2009-07-29 - 15:41	BenCooper
png	BdMass-Curl-MisalgMinusIdeal.png	r1	manage	43.8 K	2009-07-29 - 15:41	BenCooper
eps	BdMass-DayX-MisalgMinusIdeal.eps	r1	manage	24.1 K	2009-07-29 - 13:19	BenCooper
png	BdMass-DayX-MisalgMinusIdeal.png	r1	manage	46.4 K	2009-07-29 - 13:40	BenCooper
eps	BdMass-DayX-UML.eps	r1	manage	17.5 K	2009-07-29 - 13:18	BenCooper
png	BdMass-DayX-UML.png	r1	manage	37.4 K	2009-07-29 - 13:17	BenCooper
eps	CSC_DayX_Delta_Zmumu.eps	r1	manage	34.8 K	2009-07-29 - 13:05	BenCooper
png	CSC_DayX_Delta_Zmumu.png	r1	manage	47.2 K	2009-07-29 - 13:05	BenCooper
eps	CSC_DayX_Delta_Zmumu_barrel.eps	r1	manage	31.3 K	2009-07-29 - 13:05	BenCooper
png	CSC_DayX_Delta_Zmumu_barrel.png	r1	manage	44.7 K	2009-07-29 - 13:05	BenCooper
eps	CSC_DayX_Zmumu.eps	r1	manage	30.8 K	2009-07-29 - 12:53	BenCooper	The ID reconstructed $Z$ mass distribution for a \zmumu~Monte Carlo sample reconstructed
png	CSC_DayX_Zmumu.png	r1	manage	38.8 K	2009-07-29 - 12:57	BenCooper
eps	Curl_Delta_Zmumu.eps	r1	manage	34.8 K	2009-07-29 - 15:23	BenCooper
png	Curl_Delta_Zmumu.png	r1	manage	46.5 K	2009-07-29 - 15:24	BenCooper
eps	Curl_Delta_Zmumu_barrel.eps	r1	manage	31.5 K	2009-07-29 - 15:24	BenCooper
eps	Curl_Zmumu.eps	r1	manage	30.7 K	2009-07-29 - 15:22	BenCooper
png	Curl_Zmumu.png	r1	manage	38.5 K	2009-07-29 - 15:23	BenCooper
eps	Curl_chi2dof.eps	r1	manage	27.7 K	2009-07-29 - 15:07	BenCooper
png	Curl_chi2dof.png	r1	manage	34.4 K	2009-07-29 - 15:07	BenCooper
eps	Curl_dPtvsTruthPt_barrel_negative.eps	r1	manage	26.5 K	2009-07-29 - 15:19	BenCooper
eps	Curl_dPtvsTruthPt_barrel_positive.eps	r1	manage	26.9 K	2009-07-29 - 15:19	BenCooper
png	Curl_dPtvsTruthPt_barrel_positive.png	r1	manage	30.5 K	2009-07-29 - 15:19	BenCooper
eps	Curl_dqopt_barrel.eps	r1	manage	98.4 K	2009-07-29 - 15:20	BenCooper
png	Curl_dqopt_barrel.png	r1	manage	41.8 K	2009-07-29 - 15:20	BenCooper
eps	Curl_dqopt_eca.eps	r1	manage	102.5 K	2009-07-29 - 15:20	BenCooper
eps	Curl_dqopt_ecc.eps	r1	manage	104.6 K	2009-07-29 - 15:20	BenCooper
eps	Elliptical_chi2dof.eps	r1	manage	27.7 K	2009-07-29 - 15:07	BenCooper
gif	IDCosmic08_statistics.gif	r1	manage	60.4 K	2009-02-13 - 09:33	ChristianSchmitt
pdf	IDCosmic08_statistics.pdf	r1	manage	18.0 K	2009-02-13 - 09:33	ChristianSchmitt
eps	JpsiMass-Curl-MisalgMinusIdeal.eps	r1	manage	23.4 K	2009-07-29 - 15:41	BenCooper
png	JpsiMass-Curl-MisalgMinusIdeal.png	r1	manage	42.2 K	2009-07-29 - 15:40	BenCooper
eps	JpsiMass-DayX-MisalgMinusIdeal.eps	r1	manage	24.6 K	2009-07-29 - 13:18	BenCooper
png	JpsiMass-DayX-MisalgMinusIdeal.png	r1	manage	45.8 K	2009-07-29 - 13:17	BenCooper
eps	JpsiMass-DayX-UML.eps	r1	manage	16.7 K	2009-07-29 - 13:18	BenCooper
png	JpsiMass-DayX-UML.png	r1	manage	35.0 K	2009-07-29 - 13:17	BenCooper
png	PixResX_NewT_D0Z0cut_Mat_vsNominal.png	r2 r1	manage	33.4 K	2008-12-11 - 19:11	TobiasGolling	Pixel x residuals
png	PixResY_NewT_D0Z0cut.png	r2 r1	manage	40.6 K	2008-12-11 - 19:12	TobiasGolling	Pixel y residuals
png	SCTResX_NewT_D0Z0cut.png	r2 r1	manage	31.8 K	2008-12-11 - 19:13	TobiasGolling	SCT x residuals
eps	TRT2008CosmicsCombinedIDTracks.eps	r1	manage	56.6 K	2009-09-17 - 09:08	JohnAlison
png	TRT2008CosmicsCombinedIDTracks.png	r1	manage	28.3 K	2009-09-17 - 09:08	JohnAlison
eps	Telescope_chi2dof.eps	r1	manage	27.7 K	2009-07-29 - 15:08	BenCooper
eps	Twist_chi2dof.eps	r1	manage	27.7 K	2009-07-29 - 15:08	BenCooper
eps	bcm_rpc.eps	r1	manage	10.5 K	2009-06-18 - 11:34	PippaWells	BCM timing for RPC triggers
png	bcm_rpc.png	r1	manage	76.7 K	2009-06-18 - 11:33	PippaWells	BCM timing for RPC triggers
eps	bcm_trt.eps	r1	manage	10.6 K	2009-06-18 - 11:35	PippaWells	BCM timing for TRT triggers
png	bcm_trt.png	r1	manage	76.3 K	2009-06-18 - 11:34	PippaWells	BCM timing for TRT triggers
eps	delta_QoverP_vs_pT.eps	r1	manage	10.2 K	2009-06-16 - 15:30	ManuelKayl
png	delta_QoverP_vs_pT.png	r1	manage	13.2 K	2009-06-16 - 15:30	ManuelKayl
eps	delta_d0_vs_d0.eps	r1	manage	15.4 K	2009-06-16 - 15:14	ManuelKayl
png	delta_d0_vs_d0.png	r1	manage	19.8 K	2009-06-16 - 15:34	ManuelKayl
eps	delta_d0_vs_pT.eps	r1	manage	11.8 K	2009-06-16 - 15:13	ManuelKayl
png	delta_d0_vs_pT.png	r1	manage	15.4 K	2009-06-16 - 15:13	ManuelKayl
eps	delta_phi0_vs_pT.eps	r1	manage	11.0 K	2009-06-16 - 15:30	ManuelKayl
png	delta_phi0_vs_pT.png	r1	manage	14.1 K	2009-06-16 - 15:30	ManuelKayl
eps	delta_theta_vs_eta.eps	r1	manage	11.3 K	2009-06-16 - 15:31	ManuelKayl
png	delta_theta_vs_eta.png	r1	manage	12.5 K	2009-06-16 - 15:31	ManuelKayl
eps	mean_delta_QoverP_vs_pT.eps	r2 r1	manage	11.3 K	2009-06-16 - 15:46	ManuelKayl
png	mean_delta_QoverP_vs_pT.png	r2 r1	manage	15.4 K	2009-06-16 - 15:46	ManuelKayl
eps	mean_delta_d0_vs_d0.eps	r1	manage	15.6 K	2009-06-16 - 15:32	ManuelKayl
png	mean_delta_d0_vs_d0.png	r1	manage	16.4 K	2009-06-16 - 15:32	ManuelKayl
eps	mean_delta_d0_vs_pT.eps	r1	manage	11.7 K	2009-06-16 - 15:33	ManuelKayl
png	mean_delta_d0_vs_pT.png	r1	manage	14.8 K	2009-06-16 - 15:33	ManuelKayl
eps	trackpar_QoverP.eps	r1	manage	12.9 K	2009-03-09 - 14:16	PippaWells
png	trackpar_QoverP.png	r1	manage	8.1 K	2009-03-09 - 14:15	PippaWells
eps	trackpar_d0.eps	r1	manage	11.3 K	2009-03-09 - 14:18	PippaWells
png	trackpar_d0.png	r1	manage	7.8 K	2009-03-09 - 14:18	PippaWells
eps	trackpar_eta.eps	r1	manage	9.5 K	2009-03-09 - 14:17	PippaWells
png	trackpar_eta.png	r1	manage	6.1 K	2009-03-09 - 14:17	PippaWells
eps	trackpar_phi0.eps	r1	manage	12.5 K	2009-03-09 - 14:17	PippaWells
png	trackpar_phi0.png	r1	manage	8.3 K	2009-03-09 - 14:17	PippaWells
eps	trackpar_theta0.eps	r1	manage	10.4 K	2009-03-09 - 14:15	PippaWells
png	trackpar_theta0.png	r1	manage	6.9 K	2009-03-09 - 14:14	PippaWells
eps	trackpar_z0.eps	r1	manage	12.3 K	2009-03-09 - 14:14	PippaWells
png	trackpar_z0.png	r1	manage	8.5 K	2009-03-09 - 14:13	PippaWells

This topic: AtlasPublic > ApprovedDetectorPlots > ApprovedPlotsID
Topic revision: r38 - 2010-03-11 - PatrickJussel

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