The Dead time correction for the light curve with millisecond time bin Liang, Jau-shian Institute of Physics, NTHU 2006/12/5.

Slides:



Advertisements
Similar presentations
Topic 8. Gamma Camera (II)
Advertisements

NUCP 2371 Radiation Measurements II
Search for Serendipitous TNO Occultation in X-rays Hsiang-Kuang Chang Institute of Astronomy National Tsing Hua University Hsinchu, Taiwan.
Prajwal Mohanmurthy, Mississippi State University with Dr. Dipangkar Dutta, Mississippi State University Medium Energy Physics Group Spin-Light Polarimeter.
E4 Cosmology. Newton’s Universe Infinite (in space and time) Static.
June 9, Tetsuro Sekiguchi, KEK BNL-E949 Collaboration The E949 experiment The analysis The results Conclusions BNL, FNAL, UNM, Stony Brook Univ.
JNM Dec Annecy, France The High Resolution Fly’s Eye John Matthews University of Utah Department of Physics and High Energy Astrophysics Institute.
Basic Principles of X-ray Source Detection Or Who Stole All Our Photons?.....
A Muon Veto for the Ultra-Cold Neutron Asymmetry Experiment Vince Bagnulo LANL Symposium 2006 Outline ● UCNA Experiment ● Muon background ● Proposed Veto.
Recent Results for Small-Scale Anisotropy with HiRes Stereo Data Chad Finley Columbia University HiRes Collaboration Rencontres de Moriond 17 March 2005.
Find period for SGR Outline SGR SGR RXTE(Rossi X-ray Timing Explorer) RXTE(Rossi X-ray Timing Explorer) Data Reduction and Analysis.
G.A.Prodi - INFN and Università di Trento, Italy International Gravitational Event Collaboration igec.lnl.infn.it ALLEGRO group:ALLEGRO (LSU)
X-ray occultation of Scorpius X-1 by small trans-neptunian objects Liang, Jau-shian Institute of Physics, NTHU 2006/04/27.
DPF Victor Pavlunin on behalf of the CLEO Collaboration DPF-2006 Results from four CLEO Y (5S) analyses:  Exclusive B s and B Reconstruction at.
A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis:
GLAST LAT ProjectI&T Meeting – Feb 12, 2003 W. Focke 1 EM timing analysis Warren Focke February 12, 2004.
Forward Detectors and Measurement of Proton-Antiproton Collision Rates by Zachary Einzig, Mentor Michele Gallinaro INTRODUCTION THE DETECTORS EXPERIMENTAL.
The Time-of-Flight system of the PAMELA experiment: in-flight performances. Rita Carbone INFN and University of Napoli RICAP ’07, Rome,
Prajwal T. Mohan Murthy Laboratory for Nuclear Science, MIT νDM Group Spin-Light Polarimeter for the Electron Ion Collider EIC Users Meeting 2014 Jun 2014.
30 Ge & Si Crystals Arranged in verticals stacks of 6 called “towers” Shielding composed of lead, poly, and a muon veto not described. 7.6 cm diameter.
Development of A Scintillation Simulation for Carleton EXO Project Rick Ueno Under supervision of Dr. Kevin Graham.
Analysis of PSI beam test R.Sawada 09/Feb/2004 MEG collaboration R.Sawada 09/Feb/2004 MEG collaboration
INTERNATIONAL STANDARDIZATION ORGANIZATION TECHNICAL SPECIFICATION Space Environment (Natural and Artificial) Probabilistic model of fluences and.
Single Electron Measurements at RHIC-PHENIX T. Hachiya Hiroshima University For the PHENIX Collaboration.
X.-X. Li, H.-H. He, F.-R. Zhu, S.-Z. Chen on behalf of the ARGO-YBJ collaboration Institute of High Energy Physics Nanjing GRB Conference,Nanjing,
Detecting GRB ν’s – an Opportunity For Observing Lorentz Invariance Violation Uri Jacob and Tsvi Piran The Hebrew University Jerusalem, Israel ν γ.
Detection of cosmic rays in the SKALTA experiment Marek Bombara (P. J. Šafárik University Košice), Kysak, August 2011.
2000/11/101 X-ray polarimetry experiment with balloon borne gas proportional counters K.Hayashida, H. Tsunemi, T. Koike, T. Horikawa (Osaka University),
Ian Ross Rose-Hulman Institute of Technology Mentor: Dr. Richard Teuscher University of Toronto ATLAS Group ATLAS Calorimetery: Cosmic Ray Commissioning.
V.L. Kashevarov. Crystal Collaboration Meeting, Mainz, September 2008 Photoproduction of    on protons ► Introduction ► Data analysis.
Ultra-low background HPGe detector at ChyeongPyung Underground Laboratory TaeYeon Kim and KIMS(Korea Invisible Mass Search) Collaboration. * Contents *
A taste of statistics Normal error (Gaussian) distribution  most important in statistical analysis of data, describes the distribution of random observations.
Gus Sinnis Asilomar Meeting 11/16/2003 The Next Generation All-Sky VHE Gamma-Ray Telescope.
Measurement of J/  -> e + e - and  C -> J/  +   in dAu collisions at PHENIX/RHIC A. Lebedev, ISU 1 Fall 2003 DNP Meeting Alexandre Lebedev, Iowa State.
Photon Flux Control Liping Gan UNCW. Outline PrimEx-  experiment requirement Tagged photon Procedure to obtain the number of tagged photons Relative.
Hadronic interaction studies with the ARGO-YBJ experiment (5,800 m 2 ) 10 Pads (56 x 62 cm 2 ) for each RPC 8 Strips (6.5 x 62 cm 2 ) for each Pad ( 
A search for strange tribaryonic states in the reaction Heejoong Yim Seoul National University For KEK-PS E549 collaboration.
Hybrid measurement of CR light component spectrum by using ARGO-YBJ and WFCTA Shoushan Zhang on behalf of LHAASO collaboration and ARGO-YBJ collaboration.
K. Jahoda, 6 Aug 2007 X-ray School, GWU Proportional Counters Some of what you should know in order to use proportional counters for Spectroscopy, Timing,
Villa Olmo Search for neutrino bursts from gravitational collapse of stars at the Baksan Underground Scintillation Telescope Yu.F. Novoseltsev,
Russian Aviation and Space Agency Institute for Space Research NASA 2001 Mars Odyssey page 1 Workshop HEND Radiation environment on Odyssey and.
High-energy gammas from the giant flare of SGR of December 2004 in AMANDA Juande D. Zornoza on behalf of the IceCube.
Reconstructing energy from HERD beam test data Zheng QUAN IHEP 3 rd HERD work shop Xi’an, 20 Jan
Update on Rolling Cascade Search Brennan Hughey UW-Madison
Ursula Bassler convenors meeting, August 28th, Tower 2 problem For about 30 BLS boards tower 0 is read out instead of tower 2  the information.
A search for neutrinos from long-duration GRBs with the ANTARES underwater neutrino telescope arxiv C.W. James for the ANTARES collaboration.
1 The IBEX-HI SensorVoyagers in the Heliosheath Conference, January 12, 2009 January 12, 2009 Voyagers in the Heliosheath Kauai, Hawaii. The IBEX Hi Sensor:
1 A two-phase Ar avalanche detector with CsI photocathode: first results A. Bondar, A. Buzulutskov, A. Grebenuk, D. Pavlyuchenko, R. Snopkov, Y. Tikhonov.
15 cm Plots of missing mass spectrum and 90% interval for width of 0.5 and 10 MeV. Color lines show upper limit, lower limit and sensitivity. Search for.
Feb. 21st, 2011YongPyong20121 B AYESIAN S TUDY OF UHECR S Wooram Cho Institute of Physics and Applied Physics Yonsei University, Seoul, Korea
Jet + Isolated Photon Triple Differential Cross Section Nikolay Skachkov: “Photon2007”, Paris, 9-13 July 2007 DO Measurement of Triple Differential Photon.
Belle General meeting Measurement of spectral function in the decay 1. Motivation 2. Event selection 3. mass spectrum (unfolding) 4. Evaluation.
PoGOLiteMC_ ppt 1 Updated MC Study of PoGOLite Trigger Rate/BG January 30, 2007 Tsunefumi Mizuno (Hiroshima Univ.)
2001/9/111 X-ray polarimetry with balloon borne gas proportional counters K.Hayashida, H. Tsunemi, T. Horikawa, Y. Nakashima (Osaka University, Japan),
Development of UV-sensitive MPPC for upgrade of liquid xenon detector in MEG experiment Daisuke Kaneko, on behalf of the MEG Collaboration µ γ Liquid xenon.
PCA Energy Calibration – Lessons for the future Remember to be alert: the data might answer questions you didn’t ask Keith Jahoda 29 March 2012.
ICARUS T600: low energy electrons
Daniel Mazin and Nadia Tonello Max-Planck-Institut für Physik München
IceCube: Multiwavelength Approach to
Measurement of SM V+gamma by ATLAS
Ioannis Manthos Laboratory of Nuclear & Particle Physics
General Properties of Radiation
p0 life time analysis: general method, updates and preliminary result
Discrete Event Simulation - 4
1. Introduction Secondary Heavy charged particle (fragment) production
Status of Neutron flux Analysis in KIMS experiment
Study of e+e- pp process using initial state radiation with BaBar
p0 ALL analysis in PHENIX
Status of the cross section analysis in e! e
Presentation transcript:

The Dead time correction for the light curve with millisecond time bin Liang, Jau-shian Institute of Physics, NTHU 2006/12/5

Reference K. Jahoda, J. H. Swank, et al., 1996 Proc. SPIE 2808, p. 59 K. Jahoda, M. J. Stark, et al., 1999, Nucl. Phys. B (Proc. Suppl.), 69, 210 Dennis Wei, Senior Thesis submitted to the MIT Dept. of Physics K. Jahoda, C. B. Markwardt, et al., 2006, ApJS, 163, 401

Outline Introduction Recovery method Discussion Summary

Proportional counter A proportional counter is a measurement device to count particles and photons of ionizing radiation and measure their energy.

Cross section view of one PCA detector collimators propane layer xenon layer 1 xenon layer 2 xenon layer 3 xenon veto layer

The propane layer is principally intended to act as a veto layer to reduce the background rate but could be used as a lower energy detector.

The “good” events that trigger only a single xenon chain. Coincident events are likely particle events and thus are not included among the good events. X-ray Good event q 5LLD event

If the source is very bright, there is a non- negligible probability that two photons will arrive within the anti-coincidence window of each other, causing the PCA to mistakenly disqualify both photons.

Good and Coincidence rates observed from a burst of J (5 pcu)

Remaining rate vs Good rate for a burst from J

The distribution of time intervals between adjacent events Dead time ~ 9  s

L1 + R1 L1R1 L1 R1 14 incident photons L1 + R1 L1R1 6 good event

Dead time correction

the incident rate on each signal chain R j where the index j runs from 1 to 7 and corresponds to L1, R1, L2, R2, L3, R3, and VP. Dead time model (K. Jahoda, et. al. 1999) Predicting the coincidence rate

1 Coincidence timing window

There is not enough information to do dead time correction with millisecond time resolution. The missed coincidence photons should be added in. An available way is to construct a recovery method which needs only good rate. Recovery method

Blank sky #2 (Counts/s/PCU) Good VP Remaining LLD LLD LLD VX44025 VLE10090

assumptions The 7 anodes are simplified into 3 anodes (VP, L1 and R1). The background of VP, L1 and R1 can be neglected. The VP rate is proportional to the incident xenon rate. VP=2  Xe L1=XeR1=Xe

:: 0 photon:1 photon:2 photons The Poisson probability distribution should be considered.

L1R1VP L1R1 R1L1 R1VP L1VP VPR1 VPL1 0LLD(R1) 0LLD(L1) 0LLD(VP) The probability of that the photon does not exist should also be considered.

The prediction of the coincidence rate The parameters provided by K. Jahoda et al. are pressumed correct.

5s5s 9s9s 4s4s The first event of a coincident set will appear to be a good event (or a propane event) and will trigger the ADC before being labelled “bad” upon the arrival of the second event of the coincident set. The ADC is nonetheless busy for a time (~9  s) following the first event of the coincident set. ( D. Wei, 2006 ) The dead time window is accounted for 4  s.

Good Remaining L1&R1 Output rates vs. incident rates

Estimate and subtract VP, 2LLD, 0LLD Caculate dead time X’ out = X out ? Adjust X in Output X in Yes No X in

Prediction rates compare with slew data Good Remaining(data) Remaining(prediction) VP(data) VP(prediction)

Prediction rates compare with data Remaining(data) Remaining(prediction) VP(data) VP(prediction)

Light curve Corrected light curve Some results

Light curve Corrected light curve

Discussion the advantages and weaknesses Are the dips possibly caused by bursts? particle bursts within milliseconds?

the advantages and weaknesses The prediction rates agree with the data well. The light curve can be corrected with only the observed good rate even blow the time scale 1/8s. the advantages

the weaknesses Particle background is still unknown. The fluctuation is enlarged. Incident propane rate to incident xenon rate ratio is not constant. The parameters may be depend on the spectrum.

Are the dips possibly caused by bursts? It can be expected that the busts will cause the L1R1 coincidence rates increasing dramatically. The hypothesis should be rejected, since the L1R1 coincidence rates increasing are not be observed.

particle bursts within milliseconds? If the particles come in densely, that will also make the detector blind. Good counts particles

T. A. Jones inferred that these energetic events may be the consequence of particle showers produced in the RXTE spacecraft by cosmic rays.

There are some indications that the events may caused by high energy particles.

Summary The light curve can be corrected with only the observed good rate even blow the time scale 1/8s. The burst hypothesis has been rejected, since the L1R1 coincidence rates increasing are not be observed. The millisecond dips may caused by high energy particles.