Directionsensitive dark matter detection with gaseous tracking detectors

Direction-sensitive dark matter detection with gaseous tracking detectors (new proposal / D_RD_21) Kentaro Miuchi　 (KOBE University) CoｰPI: Daniel Santos (LPSC/IN 2 P 3) @ 2019 Joint workshop of FKPPL and TYL/FJPPL 0

Physics case : dark matter ～ 1/4 of the universe (can be) unknown particle beyond standard model direct search: DM-nucleus interaction the universe (energy pie chart) Our GALAXY （dark matter “HALO”） GC constellation “CYGNUS” @ lab (direct search) DM SUN nucleus SIGNAL ER<～ 100 ke. V 1

DM direct search DM nucleus SIGNAL ER<～ 100 ke. V expected direct DM signals • ① observed * events ② energy spectrum • ③ seasonal modulation • ④ material dependence • ⑤ direction-sensitive 2

“direction-sensitive” dark matter direct search detect the direction of the recoil nuclei Our GALAXY GC constellation “CYGNUS” [count/3 m 3/year/bin] SUN 40 directionality (expected) M=80 Ge. V σ=0. 1 pb @ lab DM nucleus θ SIGNAL ER<～ 100 ke. V 20 0 -1 0 cosθ 1 forward recoil would be a “smoking-gun” evidence 3

proposal overview Title：Direction-sensitive dark matter detection with gaseous tracking detectors Plan: 2019 -2020 detector calibration @ Grenoble 　　 2020 - Dark matter search @ Kamioka Member：Japan　Kentaro Miuchi（Kobe）（PI）　 　　　　　 Kiseki Nakamura, Tomonori Ikeda, Hirohisa Ishiura, Takuma Nakamura, Takuya Shimada （Kobe） 　　　　　 France　Daniel Santos (LPSC/IN 2 P 3) (PI)　　　　　 Charling Tao (CPPM/IN 2 P 3), Fabrice Naraghi, Olivier Guillaudin, Jean-François Muraz (LPSC/IN 2 P 3) Funding request (2019 -2020)：　 Japan 1700 k France 5 k € 4

Background Miuchi and Santos are leading two major direction-sensitive experiments: 　NEWAGE and MIMAC Both use MPGD (micro-patterned gaseous detectors) No co-working before NEWAGE Kamioka underground 30 cm MIMAC Moderne underground 40 cm • m-PIC (400 mm pitch) • direction-sensitive limit • Underground PTEP (2015) 043 F 01 s 25 cm 10 cm 5

We are in the same “CYGNUS” community. Bi-annnual workshop 20076 This TYL/FJPPL would be a good kick-off for a important collaborative work.

pre-works 2×review papers 7

NEWAGE: 3 D-tracking New general WIMP search with an Advanced Gaseous tracker Experiment μ-PIC(MPGD) based TPC 3 -D tracks SKYMAP 30 cm 40 cm CF 4 gas for SD search Proposal PLB 578 (2004) 241 First direction-sensitive limits 　PLB 654 (2007) 58 Underground results SKYMAP (measured DATA) PLB 686 (2010) 11, PTEP (2015) 043 F 01 s Phase for “low BG detector” 8

Expertise of MIMAC: COMIMAC J. F. Muraz, J. Médard, D. Santos et al. , NIMA 832 (2016), 214 9

COMIMAC measures Quenching Factor (nuclear tracks ionize less effectively than electron tracks)　 　　⇒important as a “calibration ” for a DM detector QF=0. 25 QF=0. 36 10

Ionization Quenching Factor for Fluorine in pure CF 4 at 50 mbar and for 4 He in helium (D. Santos et al. ) 0. 900 0. 800 Quenching Factor 0. 700 Fluorine in CF 4 at 50 mbar 0. 600 0. 500 0. 400 He in He + 5% C 4 H 10 at 350 mbar 0. 300 0. 200 0. 100 0. 000 0 10 20 30 40 Recoil Energy (ke. V) 50 60 11

Expertise of NEWAGE: Negative-Ion TPC original study by New Mexico group readout electronics development by NEWAGE intensive SF 6 gas study several species of ions with 2017 JINST 12 P 02012 averaged waveform (Tomonori Ikeda) different velocities NEWAGE Background schematics z-fidutialzation　→　Background killer! 12

NEWAGE electronics for SF 6 2019 J. Inst. 14 T 01008 Kobe-KEK(Liq Ar group) ASIC development first-ever detected 3 D tracks in SF 6 gas 13

This proposal ① (2019 -2020): averaged waveform (Tomonori Ikeda) ＋ 19 F quenching factor measurement @ LPSC Grenoble low energies (1 -50 ke. V) low pressure SF 6 gas 14

This proposal ② (2020 -) : MIMAC low background MIcromegas CYGNUS/NEWAGE multi-window chamber ＋ direction-sensitive dark matter search @ Kamioka 15

Summary New Proposal: Direction-sensitive dark matter detection with gaseous tracking detectors By Miuchi (NEWAGE leader) and Santos (MIMAC leader) QF measurement (2019 -2020) Dark Matter Search (2020 -) 16

BACKUPS 17

low pressure gas TPCs DRIFT [UK+US] NEWAGE [Kobe+] 30 cm • MWPC (2 mm pitch) • First started directionsensitive method • Underground • Low background • Large size (1 m 3) 1 m 40 cm • m-PIC (400 mm pitch) • direction-sensitive limit • Underground 50 cm D 3 [Hawaii] MIMAC [France] 10 cm 2 cm NITEC/CYGNO [Italy] • Pixel readout (ATLAS FE-I 4) chip • R&D in the surface lab 10 cm • pixel/optical 25 cm • Micromegas (~400 mm pitch) • quenching factor measurement 18 • Underground

T. Ikeda JPS Sep ２０１７ 19

“CYGNUS” physics after discovery Test the DM motion ex. Sagittarius stream Our GALAXY expected GC Sagitt ar stream ius standard HALO SUN constellation “CYGNUS” standard HALO + stream galactic coordinate 21 streams, halo model…

“CYGNUS” physics after discovery Test the interaction by scattering angle SI SD some operators are distinguishable 22

“CYGNUS” physics after discovery Test the interaction by scattering angle ② i. DM (inelastic scatterings dark matter) and normal darkmatter ( FFe. DM (form factor elastic dark matter)) show different angular DISTRIBUTION 23