# Index of public plots and other data representations

## MicroBooNE Insignia and Logos   (#3004)

The famous 'Blue Swoosh' MicroBooNE insignia. Also available with shadow text removed.

## calibration pulse for poster   (#3461)

### calibrationPulse

calibrationPulse.png
calibrationPulse_caption.txt

Image of a 50 microsecond waveform recorded during a calibration test of the MicroBooNE Time Projection Chamber electronics.

## LArTPC Practice Talk on MicroBooNE Cryogenics   (#3571)

### Oxygen

Oxygen.png
Oxygen_caption.txt

The concentration of oxygen in the liquid argon is shown here as clean-up commences as part of Phase I of the MicroBooNE cryogenics system.

### Run_000286_00

Run_000286_00.png
Run_000286_00_caption.txt

Oscilloscope traces from the purity monitor appear here from the Phase I operation of the MicroBooNE cryogenics system. The electron drift lifetime can be determined from taking the ratio of the heights of the anode signal to that of the cathode signal.

### Water

Water.png
Water_caption.txt

The concentration of water in the liquid argon is shown here as clean-up commences as part of Phase I of the MicroBooNE cryogenics system.

## Public Plots from the SBN Physics Proposal   (#4269)

### BNB_flux_ratio_icarus_uboone

BNB_flux_ratio_icarus_uboone.pdf
BNB_flux_ratio_icarus_uboone_caption.txt

Ratio of the fluxes for each neutrino species between ICARUS and MicroBooNE. These detector locations are clearly in the $\sfrac{1}{r^2} regime with$\sfrac{470^2}{600^2} = 0.61$. ### BNB_flux_uboone BNB_flux_uboone.pdf BNB_flux_uboone_caption.txt The Booster Neutrino Beam flux at MicroBooNE. ### Dirt_ZX_nu_annotated Dirt_ZX_nu_annotated.png Dirt_ZX_nu_annotated_caption.txt Location of interaction vertices for neutrinos which deposit any energy into the MicroBooNE detector shown from above. ### Dirt_ZY_nu_annotated Dirt_ZY_nu_annotated.png Dirt_ZY_nu_annotated_caption.txt Location of interaction vertices for neutrinos which deposit any energy into the MicroBooNE detector shown from the side. ### ND_100m_uB_T600_onaxis_nue_appearance_ecalo2_nu_vePhot0_05_gap3_lessCosmics_xsec_0_flux_6_dirt_cos_sensPlot ND_100m_uB_T600_onaxis_nue_appearance_ecalo2_nu_vePhot0_05_gap3_lessCosmics_xsec_0_flux_6_dirt_cos_sensPlot.png ND_100m_uB_T600_onaxis_nue_appearance_ecalo2_nu_vePhot0_05_gap3_lessCosmics_xsec_0_flux_6_dirt_cos_sensPlot_caption.txt Sensitivity of the SBN Program to$\nu_{\mu} \rightarrow \nu_{e}$oscillation signals. All backgrounds and systematic uncertainties described in the proposal are included. The sensitivity shown corresponds to the event distributions, which includes the topological cuts on cosmic backgrounds and an additional 95% rejection factor coming from an external cosmic tagging system and internal light collection system to reject cosmic rays arriving at the detector in time with the beam. ### Nue_appearance_ecalo2_nu_vePhot0_05_gap3_470m Nue_appearance_ecalo2_nu_vePhot0_05_gap3_470m.png Nue_appearance_ecalo2_nu_vePhot0_05_gap3_470m_caption.txt Beam-related electron neutrino charged-current candidate events in MicroBooNE. Statistical uncertainties only are shown. Data exposures are indicated on the plots and assume inclusion of the full MicroBooNE, 1.32e21 proton on target, data set.$\nu_{e}$events have an assumed reconstruction efficiency of 80\%, and mis-identification from photons is taken at 6\% of events passing a topological cut. The topological cut assumes that photons with more than 50MeV of energy and a displaced vertex more than 3cm away will be reject. ### Nue_appearance_ecalo2_nu_vePhot0_05_gap3_fullCosmics_470m_globBF Nue_appearance_ecalo2_nu_vePhot0_05_gap3_fullCosmics_470m_globBF.png Nue_appearance_ecalo2_nu_vePhot0_05_gap3_fullCosmics_470m_globBF_caption.txt Electron neutrino charged-current candidate distributions in MicroBooNE shown as a function of reconstructed neutrino energy. All backgrounds are shown, only muon proximity and$\sfrac{dE}{dx}$cuts have been used to reject cosmogenic background sources. Oscillation signal events for the best-fit 3+1 oscillation parameters from Kopp et al. (JHEP 1305, 050 (2013), arXiv:1303.3011) are indicated by the white histogram on top in each distribution.$\nu_{e}$events have an assumed reconstruction efficiency of 80\%, and mis-identification from photons is taken at 6\% of events passing a topological cut. The topological cut assumes that photons with more than 50MeV of energy and a displaced vertex more than 3cm away will be reject. ### Nue_appearance_ecalo2_nu_vePhot0_05_gap3_lessCosmics_470m_globBF Nue_appearance_ecalo2_nu_vePhot0_05_gap3_lessCosmics_470m_globBF.png Nue_appearance_ecalo2_nu_vePhot0_05_gap3_lessCosmics_470m_globBF_caption.txt Electron neutrino charged-current candidate distributions in MicroBooNE shown as a function of reconstructed neutrino energy. All backgrounds are shown. For cosmicgenically induced events muon proximity,$\sfrac{dE}{dx}$cuts, and a combination of the internal light collection systems and external cosmic tagger systems at each detector are assumed to conservatively identify 95% of the triggers with a cosmic muon in the beam spill time and those events are used to reject events. Oscillation signal events for the best-fit 3+1 oscillation parameters from Kopp et al. (JHEP 1305, 050 (2013), arXiv:1303.3011) are indicated by the white histogram on top in each distribution.$\nu_{e}$events have an assumed reconstruction efficiency of 80\%, and mis-identification from photons is taken at 6\% of events passing a topological cut. The topological cut assumes that photons with more than 50MeV of energy and a displaced vertex more than 3cm away will be reject. ### Nue_sensitivity_compare_program Nue_sensitivity_compare_program.pdf Nue_sensitivity_compare_program_caption.txt Sensitivity comparisons for$\nu_{\mu} \rightarrow \nu_e$oscillations including all backgrounds and systematic uncertainties described in the proposal assuming 6.6e20 protons on target in LAr1-ND and the ICARUS-T600 and 13.2e20 protons on target in MicroBooNE. The three curves present the significance of coverage of the LSND 99% allowed region (above) for the three different possible combinations of SBN detectors: LAr1-ND and MicroBooNE only (blue), LAr1-ND and ICARUS only (black), and all three detectors (red). ### Numu_Evt_Dis_470m_1 Numu_Evt_Dis_470m_1.png Numu_Evt_Dis_470m_1_caption.txt Examples of$\nu_{\mu}$disappearance signals in MicroBooNE for$\Delta m^{2} = 1 \text{eV}^2$with 13.2e20 protons on target. ### Numu_Evt_Dis_470m_44 Numu_Evt_Dis_470m_44.png Numu_Evt_Dis_470m_44_caption.txt Examples of$\nu_{\mu}$disappearance signals in MicroBooNE for$\Delta m^{2} = 0.44 \text{eV}^2$with 13.2e20 protons on target. ### Numu_MicroBooNE_TrackLengthCut Numu_MicroBooNE_TrackLengthCut.pdf Numu_MicroBooNE_TrackLengthCut_caption.txt Selected muon neutrino charged-current inclusive candidate events MicroBooNE (center). Final state muon tracks that are fully contained in the TPC volume are required to travel greater than 50 cm. Muons which exit the active detectors are required to travel >1 m before exiting. Statistical uncertainties only are shown. Data exposures are indicated on the plots and assume inclusion of the full MicroBooNE, 1.32e21 proton on target, data set. ### Numu_dis_sensitivity Numu_dis_sensitivity.pdf Numu_dis_sensitivity_caption.txt Sensitivity prediction for the SBN program to$\nu_{\mu} \rightarrow \nu_{x}$oscillations including all backgrounds and systematic uncertainties described in the proposal. SBN can extend the search for muon neutrino disappearance an order of magnitude beyond the combined analysis of SciBooNE and MiniBooNE. ## General cross section public plots and tables (#4331) ### cFS cFS.eps cFS.png cFS_caption.txt Energy distribution of BNB muon neutrino event rates in MicroBooNE for different event signatures for an 87 ton active volume. Selection efficiencies are not considered. ### c c.eps c.png c_caption.txt Energy distribution of BNB muon neutrino event rates in MicroBooNE for different interaction channels for an 87 ton active volume and 6.6e20 POT. Selection efficiencies are not considered. Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ### ccc ccc.eps ccc.png ccc_caption.txt Energy distribution of BNB muon neutrino CC interaction event rates in MicroBooNE for different interaction channels for an 87 ton active volume and 6.6e20 POT. Selection efficiencies are not considered. Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ### cnc cnc.eps cnc.png cnc_caption.txt Energy distribution of BNB muon neutrino NC interaction event rates in MicroBooNE for different interaction channels for an 87 ton active volume and 6.6e20 POT. Selection efficiencies are not considered. Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ### cnue cnue.eps cnue.png cnue_caption.txt Energy distribution of BNB electron and antielectron neutrino events in MicroBooNE for different interaction channels for an 87 ton active volume. Selection efficiencies are not considered. Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ### cpotFS cpotFS.eps cpotFS.png cpotFS_caption.txt Cumulative event rates of BNB muon neutrinos in MicroBooNE for different event signatures as a function of protons on target for an 87 ton active volume. Selection efficiencies are not considered. ### cpot cpot.eps cpot.png cpot_caption.txt Cumulative event rates of BNB muon neutrinos in MicroBooNE for different interaction channels as a function of protons on target for an 87 ton active volume. Selection efficiencies are not considered. Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ### cpotcc cpotcc.eps cpotcc.png cpotcc_caption.txt Energy distribution of BNB muon neutrino CC interaction event rates in MicroBooNE for different interaction channels for an 87 ton active volume. Selection efficiencies are not considered. Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ### cpotnc cpotnc.eps cpotnc.png cpotnc_caption.txt Energy distribution of BNB muon neutrino NC interaction event rates in MicroBooNE for different interaction channels for an 87 ton active volume. Selection efficiencies are not considered. (Note: the DIS curve is hidden underneath the coherent). Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ### cpotnue cpotnue.eps cpotnue.png cpotnue_caption.txt Cumulative event rates of BNB electron and antielectron neutrinos in MicroBooNE for different interaction channels as a function of protons on target for an 87 ton active volume. Selection efficiencies are not considered. Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ### eventrates1e20FS eventrates1e20FS.png eventrates1e20FS_caption.txt Neutrino interactions expected in the MicroBooNE detector for 1e20 POT and 87 tons active volume. Selection efficiencies are not considered. ### eventrates1e20 eventrates1e20.png eventrates1e20_caption.txt Expected event rates of BNB neutrinos in MicroBooNE for different interaction channels for an 87 ton active volume and 1e20 POT. Selection efficiencies are not considered. Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ### eventrates6.6e20 eventrates6.6e20.png eventrates6.6e20_caption.txt Expected event rates of BNB neutrinos in MicroBooNE for different interaction channels for an 87 ton active volume and 1e20 POT. Selection efficiencies are not considered. Separation between RES and DIS channels is based on a cut on the hadronic mass W < 2 GeV (RES) and W > 2 GeV (DIS) rather than GENIE interaction mode. ## Cryostat Cool-Down and Purge Plots (#4411) ### AveCryostatTemp AveCryostatTemp.pdf AveCryostatTemp.png AveCryostatTemp_caption.txt Average temperature of the MicroBooNE cryostat during the cool-down of the gaseous argon. ### O2Purge O2Purge.pdf O2Purge.png O2Purge_caption.txt The oxygen contamination of the gaseous argon while purging air. The sensor for this oxygen concentration was turned on after 10:00 AM April 21, 2015, and it reached its sensitivity limit during the evening of April 23, 2015. ## MicroBooNE First Images (#4658) ### run1147_ev00 run1147_ev00.jpeg run1147_ev00.pdf run1147_ev00.png run1147_ev00_caption.txt First cosmic event from MicroBooNE ### run1147_ev00_full run1147_ev00_full.jpeg run1147_ev00_full.pdf run1147_ev00_full.png run1147_ev00_full_caption.txt First cosmic event from MicroBooNE ### run1147_ev00_full_zoomin run1147_ev00_full_zoomin.jpeg run1147_ev00_full_zoomin.pdf run1147_ev00_full_zoomin.png run1147_ev00_full_zoomin_caption.txt First cosmic event from MicroBooNE ### run1148_ev1016 run1148_ev1016.jpeg run1148_ev1016.pdf run1148_ev1016.png run1148_ev1016_caption.txt First cosmic events from MicroBooNE ### run1148_ev778 run1148_ev778.jpeg run1148_ev778.pdf run1148_ev778.png run1148_ev778_caption.txt First cosmic events from MicroBooNE ### run1149_ev158 run1149_ev158.jpg run1149_ev158.pdf run1149_ev158.png run1149_ev158_caption.txt First cosmic events from MicroBooNE ### run1153_ev10 run1153_ev10.jpg run1153_ev10.pdf run1153_ev10.png run1153_ev10_caption.txt First cosmic events from MicroBooNE ### run1153_ev13 run1153_ev13.jpg run1153_ev13.pdf run1153_ev13.png run1153_ev13_caption.txt First cosmic events from MicroBooNE ### run1153_ev40 run1153_ev40.jpeg run1153_ev40.pdf run1153_ev40.png run1153_ev40_caption.txt First cosmic events from MicroBooNE ## UV laser event display (#4687) ### run1306_ev134 run1306_ev134.png run1306_ev134_caption.txt Caption: Display of the collection view of an event with a UV laser induced track at 58 kV drift voltage. The laser track can be identified by the endpoint on the cathode (larger charge visible at the top of the image) and the absence of charge fluctuations along the track. Additional information: - The charge released at the cathode comes photo-electric effect. - The short track where the laser beam enters the TPC (bottom right in the figure) is from a cosmic muon ## Noise Dependence on Temperature and LAr Fill Level in the uBooNE Time Projection Chamber (#4717) ### fill_vs_time fill_vs_time.png fill_vs_time_caption.txt LAr fill level over the several weeks during which the filling process occurred. LAr level measurements were calculated using the fill-levels recorded on the slow-control monitors. The fill-level measurement is performed by calculating a liquid level based on a pressure measurement. 74.5 cm were subtracted from that measurement to account for the distance between the bottom of the TPC and the bottom of the cryostat. Fill levels are relative to the bottom of the crostat. The shaded grey area marks the tine in which the LAr level fell between the bottom and top of the TPC frame. Each step in this plot marks the approximate time of a fill. ### noise_vs_fill noise_vs_fill.png noise_vs_fill_caption.txt Noise on collection plane wires vs. LAr submersion level of the μBooNE Time Projection Chamber. This plot shows one data point for each fill level at which the liquid-argon level was above the bottom, and below the top of the TPC frame. How was each data-point calculated? Fig. 7 in the Tech-Note (DocDB 4717) shows the runs considered in this analysis grouped by each fill. For each fill-level, a data-point is plotted. For each fill-level, noise measurements from all runs taken at that fill-level are averaged. The averages of these measurements are the data-points plotted on this figure. How was the error-bar calculated? Likewise, for each fill-level the standard deviation of the noise-measurements for all runs at a given fill-level was calculated. Because some fill-levels have very few data-points, the value of the standard-deviation calculated at some fill-levels was very small. Therefore, we decided to take as a measure of the error the largest standard-deviation measured for any fill-level. This corresponds to the one measured for the fill of June 27th. The relative error on the data-point for that fill was calculated, and this error was then applied to all data-points. ENC is measured in number of electrons by taking the ADC noise measured at a 14 mV/fC ASIC gain and multiplying it by [ 1.6E-4 (fC/e-) X 1.935 (ADC/mV) X 14 (mV/fC)]^-1. LAr level measurements were calculated using the fill-levels recorded on the slow-control monitors. The fill-level measurement is performed by calculating a liquid level based on a pressure measurement. 74.5 cm were subtracted from that measurement to account for the distance between the bottom of the TPC and the bottom of the cryostat. ### noise_vs_temp noise_vs_temp.png noise_vs_temp_caption.txt Noise measured on collection plane wires as a function of temperature in the MicroBooNE TPC. Each data point corresponds to the measured noise level for a given run. The times shown are the times at which each run was taken. For each run, a list of channels was selected such that 1) it was a collection plane wire, 2) it had noise values within a certain range. The average and standard deviation of the distribution of RMS noise values for channels passing the cut was calculated. Data points represent the average RMS, and error-bars show the standard deviation of these distributions. Error bars are meant to show how the change in temperature affects noise levels compared to the intrinsic variability of noise in the detector due to channel-to-channel gain variations. ENC values are measured in number of electrons by taking the ADC noise measured at a 14 mV/fC ASIC gain and multiplying it by [ 1.6E-4 (fC/e-) X 1.935 (ADC/mV) X 14 (mV/fC)]^-1. Noise values drop with the gasseous argon temperature. This is expected behavior due mainly to the properties of the CMOS ASIC chips. Temperature measurements were performed by reading the temperature values on sensors TE192 and TE196, placed on the top and bottom of the TPC frame respectively. These temperatures were recorded several times per minute. We use the average of the two temperatures as a measure of the average temperature in the cryostat. Erorr bars on the temperature measurements are equal to half the difference in temperature between the two sensors. A noise measurement performed at a given run was matched to a temperature measurement by looking for the temperature measurement performed nearest in time to the run start time. The large population of data-points close to 100 K is due to the fact that by that point the temperature in the cryostat had stabilized, and many runs were being taken at a stable temperature. ### noise_vs_time noise_vs_time.png noise_vs_time_caption.txt Noise measured on collection plane wires as a function of time. Each data point corresponds to the measured noise level for a given run. The times shown are the times at which each run was taken. For each run, a list of channels was selected such that 1) it was a collection plane wire, 2) it had noise values within a certain range. The average and standard deviation of the distribution of RMS noise values for channels passing the cut was calculated. Data points represent the average RMS, and error-bars show the standard deviation of these distributions. Error bars are meant to show how the change in temperature affects noise levels compared to the intrinsic variability of noise in the detector due to channel-to-channel gain variations. ENC values are measured in number of electrons by taking the ADC noise measured at a 14 mV/fC ASIC gain and multiplying it by [ 1.6E-4 (fC/e-) X 1.935 (ADC/mV) X 14 (mV/fC)]^-1. Noise values drop with the gasseous argon temperature. This is expected behavior due mainly to the properties of the CMOS ASIC chips. The red vertical line in this plot represents the time at which the LAr filling-process began. After this point noise levels begin to rise. This behavior is explained in the Tech-Note in DocDB 4717 in Sec. 5. Sporadicity of the data-points is due to irregular run-taking patterns in the very early weeks of the commissioning phase. Noise levels fluctuate slightly upwards in early and mid June. This is because the cryostat cooling was temporarily interrupted for a brief period, allowing the temperature, and thus the noise values, to rise. ## Aproved Plots at Sept. 4th Plot Approval Meeting (#4787) ### R1532E1_black_grid_axis R1532E1_black_grid_axis.png R1532E1_black_grid_axis_caption.txt A snapshot from LArSoft based 3D event display showing cosmic tracks entering the MicroBooNE detector. The three boxes show the full readout window of the MicroBooNE detector which corresponds to 4.8 ms or equivalently the total effective drift volume for running at full field strength (-128 kV to cathode or 500 V/cm). The red highlighted box shows the physical volume of the TPC. The Colored lines shown in the boxes are 3D reconstructed tracks, different colors represent different tracks. Tracks are drawn along with their trajectory points. The data shown corresponds to cosmic run 1532, event 1 taken on 17th of August, 2015 at 4:03 PM at -70kV (or equivalently 273 V/cm) Electric field. ### R1532E1_white_nogrid_axis R1532E1_white_nogrid_axis.png R1532E1_white_nogrid_axis_caption.txt A snapshot from LArSoft based 3D event display showing cosmic tracks entering the MicroBooNE detector. The three boxes show the full readout window of the MicroBooNE detector which corresponds to 4.8 ms or equivalently the total effective drift volume for running at full field strength (-128 kV to cathode or 500 V/cm). The red highlighted box shows the physical volume of the TPC. The Colored lines shown in the boxes are 3D reconstructed tracks, different colors represent different tracks. Tracks are drawn along with their trajectory points. The data shown corresponds to cosmic run 1532, event 1 taken on 17th of August, 2015 at 4:03 PM at -70kV (or equivalently 273 V/cm) Electric field. ## Updated Neutrino Beam Timing Plots (#5390) ### BNB BNB.pdf BNB.png BNB_caption.txt The measured distribution of flash times (requiring flashes greater than 50PE) with respect to the trigger time for BNB-triggered events, shown as a ratio to the expected cosmic rate from off-beam data. The blue band denoting the cosmic rate was centered at one, with a width corresponding to the measured uncertainty in the cosmic rate. A clear excess can be seen due to neutrinos between 3 and 5$\mu$s after the trigger. This is where the neutrinos were expected based on the RWM signal arrival time. A total of 1.92E6 BNB triggered events (unbiased trigger) were used to produce this plot. ### NUMI NUMI.pdf NUMI.png NUMI_caption.txt The measured distribution of flash times (requiring flashes greater than 50PE) with respect to the trigger time for NuMI-triggered events, shown as a ratio to the expected cosmic rate from off-beam data. The blue band denoting the cosmic rate was centered at one, with a width corresponding to the measured uncertainty in the cosmic rate. A clear excess can be seen due to neutrinos between 6 and 15$\mu\$s after the trigger. A total of 3.67E5 NuMI triggered events (unbiased trigger) were used to produce this plot.

Questions? Click on the document numbers for notes and authors, or contact us. Page last updated: Tue Mar 15 11:52:59 2016