MARE Microcalorimeter Arrays for a Rhenium Experiment. COLLABORATION: INFN sez. Genova and Università di Genova, Dipartimento di Fisica, ITALY NASA Goddard Space Flight Center, USA Universität Heidelberg, Kirchhoff-Institut für Physik, GERMANY - PowerPoint PPT Presentation
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LTD11 - Tokyo 01/08/2005 1 H10 - MARE H10 - MARE Alessandro Monfardini MARE MARE Microcalorimeter Arrays for a Rhenium Microcalorimeter Arrays for a Rhenium Experiment Experiment COLLABORATION: COLLABORATION: INFN sez. Genova and Università di Genova, Dipartimento di Fisica, ITALY NASA Goddard Space Flight Center, USA Universität Heidelberg, Kirchhoff-Institut für Physik, GERMANY Università dell’Insubria, Dipartimento di Fisica e Matematica, ITALY INFN sez. Milano and Università di Milano-Bicocca, Dipartimento di Fisica, ITALY ITC-IRST, Trento, ITALY University of Wisconsin, Physics Department, USA ... STILL OPEN
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LTD11 - Tokyo 01/08/2005 1
H10 - MAREH10 - MARE
Alessandro Monfardini
MARE MARE Microcalorimeter Arrays for a Rhenium ExperimentMicrocalorimeter Arrays for a Rhenium Experiment
COLLABORATION:COLLABORATION:
INFN sez. Genova and Università di Genova, Dipartimento di Fisica, ITALY
NASA Goddard Space Flight Center, USA
Universität Heidelberg, Kirchhoff-Institut für Physik, GERMANY
Università dell’Insubria, Dipartimento di Fisica e Matematica, ITALY
INFN sez. Milano and Università di Milano-Bicocca, Dipartimento di Fisica, ITALY
Neutrinoless double beta decay - 0Neutrinoless double beta decay - 0 (model-dependent): (model-dependent):..but direct insights on the neutrino nature (Majorana ?) and access to Majorana phases
Effective Majorana mass: mee < 0.35 eV (Heidelberg-Moscow 76Ge)
mee < 0.2÷1.1 eV (CUORICINO 130Te)
mee = 0.1÷0.9 eV (Klapdor: 76Ge reanalysis)
Cosmology (indirect):Cosmology (indirect):U. Seljak, Physics Review D 71 (2005) 103515 mi
< 0.42 eV (CMB+SDSS+SN)
Direct (Direct ( decay) sub-eV SAFE determination NEEDED !! decay) sub-eV SAFE determination NEEDED !! … … and such a 1and such a 1stst class Physics deserves more than just one experiment. class Physics deserves more than just one experiment.
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Calorimetric technique: statusCalorimetric technique: status
Lowest-Q (2.5keV) beta decay (most sensitive to small m): 187Re
GOALS: - eliminate as much systematics as possible (sub-eV!!)- scaling (in principle) possible up to the nth generation
Source Detector (neutrino is the only allowed to escape from the bulk)
Published results: < 15 eV (90% C.L.) Milano MIBETA AgreO4
< 26 eV (95% C.L.) Genova MANU metallic Re
STATUS: still one order of magnitude worse than spectrometers, but some pros in principle. To be competitive with KATRIN, we need a two orders of magnitude improvement in sensitivity.
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MARE: a two stages effortMARE: a two stages effortTwo orders of magnitudes is a (too) big task for a single step.
Phase I: - Present technology detectors(2006-2009) - Optimization of the single channel
- Scaling up to hundreds of devices (MIBETA2, MANU2)Goals:Goals: - m < 2eV before KATRIN
- phase II preliminary (systematics, technology..)
Phase II: - R&D during the phase I data taking(2010-2015) - New approach (multiplexed TES or MMC)
- More than 104 fast (~s) devices with < 5eV resolution Goals:Goals: - 0.2eV sensitivity in 2015
- still upper limits (e.g. hierarchical pattern) ? Starting point for a 4th generation (NDET > 106)
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Science requirements: MC simulationsScience requirements: MC simulations
~ 1010 beta decays required E and fpup achievable
Phase I
~ 1014 beta decays required fpup ~ 10-5 is required E < 5eV is enough
Phase II
fpup ~ AR
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Systematic effectsSystematic effectsPeculiar and common effects under investigation:
- theoretical spectral shape of the 1st forbidden 187Re decay;- solid state BEFS effect*;- internal detector response function calibration*;- unidentified pile-up spectrum;- external radioactive background;- energy scale calibration;- surface electron escape*;- data reduction.
MARE phase I is partially devoted to the study of these effects.* See poster H102 for a preliminary analysis based on MIBETA AgReO4 array results.
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MARE PHASE IMARE PHASE I
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MARE phase I: MIBETA2 optionsMARE phase I: MIBETA2 options
ITC-IRST ITC-IRST TMAH micromachined array. Implanted silicon with the technology developed for the MIBETA single devices.STATUS:STATUS: ongoing production run, tests in October.
NASA NASA 66 silicon array (XRS2).STATUS:STATUS: encouraging firstresults with 450g AgReO4. Coupling and electronics to be optimized. Baseline choice.
NTD NTD Ge array (LBL + Bonn).STATUS:STATUS: preferred from themodel point-of-view. Excess noise observed; reproducibilityto be demonstrated.
NNDETDET = 288 = 288
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MARE phase I: MANU2MARE phase I: MANU2
???????
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MARE PHASE IIMARE PHASE II
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MARE phase II: critical issuesMARE phase II: critical issuesThe kick-off of the phase II will be subordinated to:
- safe reduction of all the known sources of systematic uncertainties;
- verification that no new sources come up to impair the sensitivity;
- understanding of the 187Re decay spectrum with the required precision;
- demonstration that the estimated sensitivity can be maintained though
the experiment is segmented in a large number of channels.
All these goals will be achieved making use of the 1010 beta decays acquired in the phase I. Preliminary feelings from MIBETA and MANU(~107) events are positive, but the full MARE phase I dataset is required to drawn a definitive conclusion.
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MARE phase II strategyMARE phase II strategy
Requirements: fast detectors (~s), energy resolution (<5eV), high granularity (>104), big absorbers (~10 mg).
Thermistors: TES or MMC (Heidelberg) depending on single devices performances. Also involved: Como, Genova, Milano, NASA, Wisconsin.
Absorbers: metallic rhenium vs. dielectric (AgReO4) depending onthe results of MARE phase I and MMC R&D.Mainly involved: Genova, Milano, Heidelberg.
Cryogenics: no critical issues (mTOT ~ kg). Method: modularity (104 detectors modules to be deployed).
(reminder)
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Conclusions: MARE and KATRINConclusions: MARE and KATRINClassic EM spectrometers are now less than one order of magnitude ahead. KATRIN, probably the ultimate classic experimentprobably the ultimate classic experiment, is reaching 0.2eV sensitivity by means of a BIG (10m23m) electrostatic spectrometer.
For the very first time, a concrete opportunityconcrete opportunity of checking the spectrometers results is open (before KATRIN !!) as a result of a relatively straightforward optimization and scaling of the present calorimeters arrays (MARE phase IMARE phase I).
In parallel, constructive but feasible R&D is required to prepare the MARE 2MARE 2ndnd phase phase. Assuming KATRIN will be successfully deployed and run, we predict two scenarios:- positive detection by KATRIN.positive detection by KATRIN. Only a 187Re calorimetric cross-check could then disprove or confirm the result for the History; - mm < 0.2eV by KATRIN < 0.2eV by KATRIN (..according to the Cosmology indications). Again, the cross-check is crucial. Given the lower bounds from oscillation experiments, the even next generation experiments will probably, finally measure m directly.
