MADMAX: A new road to axion dark matter detection OUTLINE:

Transcription

1 MADMAX: A new road to axion dark matter detection Béla Majorovits MPI für Physik, München, Germany for the MADMAX interest group OUTLINE: Axions as dark matter: The post inflationary scenario Experimental idea First proof of prinicple measurements Outlook 1

2 MADMAX: A new road to axion dark matter detection Béla Majorovits MPI für Physik, München, Germany for the MADMAX interest group CEA IRFU, Saclay DESY Hamburg MPI für Radioastronomie, Bonn MPI für Physik, München University of Hamburg University of Zaragoza 2

3 Axion DM: Scenario PQ Inflation 3

4 MADMAX MAgnetized Disc and Mirror Axion experiment Mirror 10 T dipole magnet Horn antenna (+ receiver) 80 adjustable dielectric discs : ~1m Parabolic Mirror Seperate cryogenic volume 4

5 Experimental idea Chose dielectric material: High dielectric constant ε (for large boost & conversion) Low loss low tan δ (reduce photon losses) Stable Cheap Sapphire (Al 2 O 3 300K, 10 GHz: ε~10; tan δ ~ few 10 5 Lanthanide Aluminate (LaAlO 3 77K ε~24; tan δ~ Titanium dioxide Rutil (TiO 2 ) ε~100; tan δ~0.001(?) 5

6 Experimental idea Heterodyne detection: -10 db 12GHz - 18 GHz 35 db T N = 75 K 10 GHz 19 db GHz 25 MHz Signal analyzer G G f LO1 1. Local oscillator 11.7GHz - 70GHz f LO2 2. Local oscillator 1.7GHz Signal analyzer (3 samplers) 2. local oscillator 1. local oscillator Rubidium time standard (oscillator and sampler synchronization) 1. Amplifier + high pass Research Seminar at MPP, 2 June

7 First measurements: Low noise preamp: Inject fake 18GHz axion signal with W power Measurement for 28 hours (integrate signal): Receiver at LHe temp. Cross correlation analysis (8kHz Lorentz shaped) found > 6σ signal succesfully For 1 week measurement: expect Sensitivity at the level of ~ few W (t.b.c.) 7

8 First measurements: Low noise preamp: s: Signal T: Testfunction (Lorentz, Gauss, ) Inject fake 18GHz axion signal with W power Measurement for 28 hours (integrate signal): Receiver at LHe temp. Cross correlation analysis (8kHz Lorentz shaped) found > 6σ signal succesfully For 1 week measurement: expect Sensitivity at the level of ~ few W (t.b.c.) 8

9 First prototype booster setup: Transmissivity measurement: 9

10 First prototype booster setup: Transmissivity measurement: 10

11 Removable copper mirror First prototype booster setup: Reflectivity measurement: Dielectric discs (Saphire) Wave guide Horn antenna Mirror 11

12 First prototype booster setup: Reflectivity measurement: 12

13 First prototype booster setup: Reflectivity measurement: 13

14 First prototype booster setup: Position reproducibility: 14

15 Prototype booster Upgrade: 20 disc setup: 15

16 Prototype booster Upgrade: 20 disc setup: 16

17 Prototype booster Upgrade: 20 disc setup: 17

18 OUTLOOK: Sensitivty for QCD dark matter axions with A=1m², B =10T, T sys = 8K, β 2 = tan δ 10-4 (???) 18

19 OUTLOOK: Sensitivty for hidden photons with A=1m², T sys = 8K, β 2 = tan δ 10-4 (???) 19

20 OUTLOOK: Sign MoU officially establish collaboration Magnet innovation partnership with (2018) Bilfinger Bacock Noell CEA IRFU Desin study for booster realization (2018) Build prototype 3-4 T magnet & 20 discs 30cm diameter booster (2021?) First QCD axions results 2021 Build full scale experiment (>2022) Considering DESY as site

21 Horn antenna Mirror First prototype booster setup: Wave guides Removable copper mirror Dielectric discs Mirror Precision motors Prototype setup partly funded as seed project by: Slides for discs Cryo-tank Germanium Array 21

22 Axion DM: Scenario PQ Inflation (Pre Inflationary PQ breaking) Scenario II: PQ symmetry breaking first: θ i has a single random value which determines the dark matter density No topological defects QCD dark matter axions can have any mass 1meV! Our universe Cosmic axion string

23 Axion DM: Scenario Inflation PQ (Post Inflationary PQ breaking) Scenario Inflation first: PQ broken after inflation θ i has random values in every casual region, with the dark matter density determined by the average Topological defects such as strings and domain walls exist in the early universe decay leads to axion production influence axion density Random θ i Cosmic axion string Predicted axion mass ~ 100 μev 23

24 First measurements: Low noise preamp: InP HEMT preamplifier from LowNoiseFactory Frequency range: 6-20 GHz detector noise: T~7K (measured, quick and dirty) T ds ~ 6K (data sheet) Gain (db) Datasheet Detector Noise Temperature (K) (short cooling time) (short cooling time) Datasheet NRAO Cryo3-Amplifier 10 13G 14G 15G 16G 17G 18G 19G 20G 21G 22G Frequency (Hz) 0 13G 14G 15G 16G 17G 18G 19G 20G 21G 22G Frequency (Hz) Research Seminar at MPP, 2 June