Presentation is loading. Please wait.

Presentation is loading. Please wait.

Sven Vahsen, CYGNUS physics meeting

Published bySonny Atmadja Modified over 5 years ago

Similar presentations

Presentation on theme: "Sven Vahsen, CYGNUS physics meeting"— Presentation transcript:

1 Sven Vahsen, CYGNUS physics meeting
Paper Status, 4/11/2018 Things still missing to complete paper Author list: Suggest we start with those who actively contributed text, material, or advice. Please send me your name, institution, and institution’s address via . (all) SI and SD reach plots with CYGNUS (Ciaran, Ngyen, Sven) Have first plots. Let’s add 10 m^3 detector. Need to agree on thresholds. Could show separate plots with reach versus threshold, or bands for possible ranges of threshold Summary of existing (James) Missing gas TPC text Missing readouts comparison table Technology comparison (Sven) Have improved electron discrimination plots. Expect further improvements. Figures still missing: Angular resolution + head/tail versus readout Directional power versus readout Cost / WIMP versus readout Update of backgrounds chapter (Warren, Neil) Update w/ Warren’s latest results: done Paper quality figures (thicker lines, high resolution): mostly done? Backgrounds from gas isotopes: still missing Higher statistics SRIM and DEGRAD MC (Cosmin, Callum) Add simulations of He/SF6 and/or He/SF6/CF4 mixtures? Suggested timescale: finish all of above by next meeting, on April 11! 5/28/2019 Sven Vahsen, CYGNUS physics meeting

2 CYGNUS SD Sensitivity Assumptions Should see solar 𝜈 events
CYGNUS 1000: 10m x 10m x 10m CYGNUS 100k: ~2 x DUNE target volume Assumptions 3 years of running time 3 keVr F threshold 1 keVr He threshold Directional mode: 20 torr SF torr 4-He Search mode: 200 torr SF torr 4-He Should see solar 𝜈 events Discoveries can be investigated in directional mode preliminary CYGNUS 1000 search mode CYGNUS 100k search mode Ciaran O’Hare Sven Vahsen UCLA DM 2018

3 CYGNUS SI Sensitivity Assumptions Should see solar 𝜈 events
3 years of running time 3 keVr F threshold 1 keVr He threshold Directional mode: 20 torr SF torr 4-He Search mode: 200 torr SF torr 4-He Should see solar 𝜈 events Discoveries can be investigated in directional mode preliminary CYGNUS 1000 search mode CYGNUS 100k search mode Ciaran O’Hare Sven Vahsen UCLA DM 2018

4 3D electron rejection (simulation) per 1keVee
limits - all electrons rejected above 4 keV limits - all electrons rejected above 7 keV No drift 25 cm drift By range versus energy signature alone, excellent electron rejection down to 3-7 keV (depending on drift length) Sven Vahsen UCLA DM 2018

Download ppt "Sven Vahsen, CYGNUS physics meeting"

Similar presentations

Advanced GAmma Tracking Array

Advanced GAmma Tracking Array
© 2012 Jenzabar, Inc. Presented by Peggy Mothershead, Registrar Systems Specialist Graceland University Friday, June 1, 201211:15 am – 12:15 pm 483 Bursting.

© 2012 Jenzabar, Inc. Presented by Peggy Mothershead, Registrar Systems Specialist Graceland University Friday, June 1, :15 am – 12:15 pm 483 Bursting.
Adding electronic noise and pedestals to the CALICE simulation LCWS 19 – 23 rd April 20041 Catherine Fry (working with D Bowerman) Imperial College London.

Adding electronic noise and pedestals to the CALICE simulation LCWS 19 – 23 rd April Catherine Fry (working with D Bowerman) Imperial College London.
LHCb PatVeloTT Performance Adam Webber. Why Upgrade?  Currently we de-focus the beams o LHCb Luminosity ~ 2x10 32 cm -2 s -1 o ~ 1 interaction per bunch.

LHCb PatVeloTT Performance Adam Webber. Why Upgrade?  Currently we de-focus the beams o LHCb Luminosity ~ 2x10 32 cm -2 s -1 o ~ 1 interaction per bunch.
Energy Reconstruction Algorithms for the ANTARES Neutrino Telescope J.D. Zornoza 1, A. Romeyer 2, R. Bruijn 3 on Behalf of the ANTARES Collaboration 1.

Energy Reconstruction Algorithms for the ANTARES Neutrino Telescope J.D. Zornoza 1, A. Romeyer 2, R. Bruijn 3 on Behalf of the ANTARES Collaboration 1.
PFA Development – Definitions and Preparation 0) Generate some events w/G4 in proper format 1)Check Sampling Fractions ECAL, HCAL separately How? Photons,

PFA Development – Definitions and Preparation 0) Generate some events w/G4 in proper format 1)Check Sampling Fractions ECAL, HCAL separately How? Photons,
PANDAX Results and Outlook

PANDAX Results and Outlook
Recent Progress on D3 - The Directional Dark Matter Detector

Recent Progress on D3 - The Directional Dark Matter Detector
Potassium Geo-neutrino Detection Mark Chen Queen’s University Neutrino Geophysics, Honolulu, Hawaii December 15, 2005.

Potassium Geo-neutrino Detection Mark Chen Queen’s University Neutrino Geophysics, Honolulu, Hawaii December 15, 2005.
GLAST LAT Project Test Beam Meeting, June 6, 2006 S. Funk 1/6 PS Positron Simulations Stefan Funk June 6, 2006.

GLAST LAT Project Test Beam Meeting, June 6, 2006 S. Funk 1/6 PS Positron Simulations Stefan Funk June 6, 2006.
1 TEV PA Meeting July 2009 Preliminary Fermi-LAT Limits on High Energy Gamma Lines from WIMP Annihilation Yvonne Edmonds representing the Fermi-LAT Collaboration.

1 TEV PA Meeting July 2009 Preliminary Fermi-LAT Limits on High Energy Gamma Lines from WIMP Annihilation Yvonne Edmonds representing the Fermi-LAT Collaboration.
LBNE R&D Briefing May 12, 2014 LBNE R&D Briefing May 12, 2014 LArIAT and LBNE Jim Stewart LArIAT EPAG Chair BNL LBNE LARIAT-EPAG J. Stewart BNL T. Junk.

LBNE R&D Briefing May 12, 2014 LBNE R&D Briefing May 12, 2014 LArIAT and LBNE Jim Stewart LArIAT EPAG Chair BNL LBNE LARIAT-EPAG J. Stewart BNL T. Junk.
Atmospheric Neutrino Oscillations in Soudan 2

Atmospheric Neutrino Oscillations in Soudan 2
I. Giomataris NOSTOS Neutrino studies with a tritium source Neutrino Oscillations with triton neutrinos The concept of a spherical TPC Measurement of.

I. Giomataris NOSTOS Neutrino studies with a tritium source Neutrino Oscillations with triton neutrinos The concept of a spherical TPC Measurement of.
T.C. Jude D.I. Glazier, D.P. Watts The University of Edinburgh Strangeness Photoproduction At Threshold Energies.

T.C. Jude D.I. Glazier, D.P. Watts The University of Edinburgh Strangeness Photoproduction At Threshold Energies.
Status of DRIFT II Ed Daw representing the DRIFT collaboration: Univ. of Sheffield, Univ. of Edinburgh, Occidental College, Univ. of New Mexico Overview.

Status of DRIFT II Ed Daw representing the DRIFT collaboration: Univ. of Sheffield, Univ. of Edinburgh, Occidental College, Univ. of New Mexico Overview.
Status of COBRA 6 th SNOLAB Workshop, 22.8.2007 Picture courtesy

Status of COBRA 6 th SNOLAB Workshop, Picture courtesy
Irakli Chakaberia Final Examination April 28, 2014.

Irakli Chakaberia Final Examination April 28, 2014.
Applications of Micro-TPC to Dark Matter Search 1. WIMP signatures 2. Performance of the Micro-TPC 3. WIMP-wind measurement 4. Future works 5. Conclusions.

Applications of Micro-TPC to Dark Matter Search 1. WIMP signatures 2. Performance of the Micro-TPC 3. WIMP-wind measurement 4. Future works 5. Conclusions.
EAS Reconstruction with Cerenkov Photons Shower Simulation Reconstruction Algorithm Toy MC Study Two Detector Configuration Summary M.Z. Wang and C.C.

EAS Reconstruction with Cerenkov Photons Shower Simulation Reconstruction Algorithm Toy MC Study Two Detector Configuration Summary M.Z. Wang and C.C.

Similar presentations

Ads by Google