The ASTAROTH Project - enhanced low-energy sensitivity to Dark Matter annual modulation - Abstract and preliminary results

Q: What is the main goal of the ASTAROTH project?

To enhance the sensitivity of future direct dark matter detection experiments to the annual modulation signal using NaI(Tl) scintillating crystals, with a model-independent validation of DAMA’s claim.

Q: How does ASTAROTH aim to improve sensitivity to sub-keV events?

By lowering the detection energy threshold to observe sub-keV recoils, using NaI(Tl) scintillation light read out by arrays of Silicon PhotoMultipliers (SiPM) in a cryogenic environment.

Q: Why are SiPMs and cryogenic cooling important for the detector design?

SiPMs provide lower dark noise than photomultiplier tubes at temperatures below 150 K and enable higher light collection, while liquid argon offers scintillation and veto instrumentation against backgrounds.

Aug 26, 2026

Upload by Rowan

ASTAROTH is an R&D program designed to strengthen the physics reach of next-generation direct dark matter searches using NaI(Tl) scintillating crystals. The project targets a model-independent test of DAMA’s long-standing annual modulation claim with the same detector material. Sensitivity improvements rely on lowering the detection threshold to observe sub-keV nuclear recoils. The approach uses SiPM arrays read out at cryogenic temperatures, cooled with liquid argon for veto capability and reduced noise, and includes preliminary single-crystal measurements.

LanguageEnglish

CategoryResearch & Report

FormatPDF

Pages5

Reading Time13 min

AccessFree to download

ASTAROTH project overview

Introduction: Dark Matter annual modulation

Current technological status

Journal of Physics: Conference Series 2156 (2022) 012060 doi:10.1088/1742-6596/2156/1/012060 The ASTAROTH Project: enhanced low-energy sensitivity to Dark Matter annual modulation A. Zani 1 ;􀀃 , F. Alessandria2 ;3 , A. Andreani 1 ;3 , A. Castoldi4 ; 1 , S. Coelli 1 , D. Cortis5 , D. D'Angelo 1 ;3 , G. Di Carlo5 , L. Frontini 1 ;3 , N. Gallice 1 ;3 , M. Ghisetti4 ; 1 , C. Guazzoni4 ; 1 , V. Liberali 1 ;3 , M. Monti 1 , D. Orlandi5 , A. Pasini2 , D. Pedrini2 , M. Prioli2 , M. Sorbi2 ;3 , A. Stabile 1 ;3 , M. Statera2 1 INFN Sezione di Milano, via Celoria 16, 20133 Milano, IT 2 INFN LASA-Milano, via fratelli Cervi 201, 20054 Segrate (Milano), IT 3 Universit􀀒a degli Studi di Milano, Dip. di Fisica, via Celoria 16, 20133 Milano, IT 4 Politecnico di Milano, DEIB, piazza Leonardo da Vinci 32, 20133 Milano, IT 5 INFN LNGS-Laboratori Nazionali del Gran Sasso, 67100 Assergi (L'Aquila), ITE-mail: 􀀃 andrea .zani@mi .infn .it Abstract. ASTAROTH is a novel R&D project which aims at improving the physics reach of future direct dark matter detection experiments based on NaI(Tl) scintillating crystals. There is a strong need to test the long standing DAMA positive observation of an annual modulation that could be due to Dark Matter (DM), with the same target material and in a model independent way. ASTAROTH aim is the enhancement of the sensitivity to the annual modulation signal, compared with present technology, by lowering the detection energy threshold in order to observe sub-keV recoils for the 􀀌rst time. This can be achieved by reading the scintillation light from the NaI(Tl) crystals with arrays of Silicon PhotoMultipliers (SiPM), and placing the detectors in a cryogenic environment. SiPMs feature lower dark noise than Photomultiplier Tubes (PMTs) at T < 150 K and allow for higher light collection. The cooling medium is liquid Argon, as it isan excellent scintillator that can be instrumented to act as a veto against several backgrounds. Here we present the status of the ASTAROTH project, introducing the innovative design of the detector chamber that will be used for the demonstration of the technology. Then, we will show the preliminary results of our 􀀌rst ever measurements performed on a single NaI(Tl) crystal read out by one SiPM array in a cryogenic set-up cooled with liquid nitrogen. 1. Introduction: Dark Matter annual modulation The search and understanding of Dark Matter represents one of the most interesting challenges of contemporary astro-particle physics, still escaping physicists grasp. The lone claim of DM observation obtained so far by the DAMA experiment [1] has yet to be con􀀌rmed. Since over 20 years, at the underground Gran Sasso National Laboratory (LNGS, IT) DAMA has been observing an annual modulation of the interaction rate with their target array of NaI(Tl) crystals. Despite the claim that this modulation is due to DM interaction, a model-independent veri􀀌cation of the result has not been possible so far. Attempts to explain the DAMA observation in terms of Earth-bound background phenomena have always come short so far; as well, no other experiment around the world ever yielded a positive observation. Data comparison is di􀀎cult and model-dependent, since the detectors are either based on a di􀀋erent technique and/or target Content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Published under licence by IOP Publishing Ltd 1 Journal of Physics: Conference Series 2156 (2022) 012060 doi:10.1088/1742-6596/2156/1/012060 Figure 1: Modulation amplitude in the simple case of Weakly Interacting Massive Particles (WIMPs [9]) spin-independent elastic scattering o􀀋 NaI nuclei, for two combinations of WIMP parameters (m; 􀀛) favoured by DAMA Phase-I results (black dots-including Phase-II results worsens the 􀀌t, but it doe

FAQs

What is the main goal of the ASTAROTH project?

To enhance the sensitivity of future direct dark matter detection experiments to the annual modulation signal using NaI(Tl) scintillating crystals, with a model-independent validation of DAMA’s claim.

How does ASTAROTH aim to improve sensitivity to sub-keV events?

By lowering the detection energy threshold to observe sub-keV recoils, using NaI(Tl) scintillation light read out by arrays of Silicon PhotoMultipliers (SiPM) in a cryogenic environment.

Why are SiPMs and cryogenic cooling important for the detector design?

SiPMs provide lower dark noise than photomultiplier tubes at temperatures below 150 K and enable higher light collection, while liquid argon offers scintillation and veto instrumentation against backgrounds.

Aug 26, 2026

Upload by Rowan