Calibration of the rst detector ight models for the HERMES constellation and the SpIRIT mission Riccardo Campanaa Giulia Baroniab Giovanni Della Casac Giuseppe Dilillod

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Calibration of the ﬁrst detector ﬂight models for the

HERMES constellation and the SpIRIT mission

Riccardo Campanaa, Giulia Baronia,b, Giovanni Della Casac, Giuseppe Dilillod,

Ezequiel J. Marchesinia, Francesco Ceraudod, Alejandro Guzm´ane, Paul Heddermane, and

Yuri Evangelistad

aINAF/OAS, Bologna, Italy

bUniversity of Bologna, Department of Physics and Astronomy, Bologna, Italy

cUniversity of Udine, Department of Mathematical, Physical and Computer Sciences, Udine,

Italy

dINAF/IAPS, Rome, Italy

eEberhard Karls Universit¨at, Institute for Astronomy and Astrophysics, T¨ubingen, Germany

ABSTRACT

HERMES (High Energy Rapid Modular Ensemble of Satellites) is a space-borne mission based on a constellation

of six 3U CubeSats ﬂying in a low-Earth orbit, hosting new miniaturized instruments based on a hybrid Silicon

Drift Detector/GAGG:Ce scintillator photodetector system sensitive to X-rays and γ-rays. Moreover, the HER-

MES constellation will operate in conjunction with the Australian-Italian Space Industry Responsive Intelligent

Thermal (SpIRIT) 6U CubeSat, that will carry in a Sun-synchronous orbit (SSO) an actively cooled HERMES

detector system payload. In this paper we provide an overview of the ground calibrations of the ﬁrst HERMES

and SpIRIT ﬂight detectors, outlining the calibration plan, detector performance and characterization.

Keywords: CubeSat, HERMES, Gamma-ray detectors, Scintillators, Silicon Drift Detectors

1. INTRODUCTION

The HERMES-Technologic and Scientiﬁc pathﬁnder∗(HERMES-TP/SP)1–3project involves a constellation of

six 3U nanosatellites hosting simple but innovative X-ray detectors for the monitoring of cosmic high energy

transients, such as Gamma Ray Bursts and the electromagnetic counterparts of Gravitational Wave events. The

main objective of HERMES-TP/SP is to prove that accurate position of high energy cosmic transients can be

obtained using miniaturized hardware, with cost at least one order of magnitude smaller than that of conventional

scientiﬁc space observatories and development time as short as a few years.

The HERMES-TP project is funded by the Italian Ministry for education, university and research and the

Italian Space Agency. The HERMES-SP project is funded by the European Union’s Horizon 2020 Research

and Innovation Programme under Grant Agreement No. 821896. The constellation should be tested in orbit in

∼2023–24.

HERMES-TP/SP is intrinsically a modular experiment that can be naturally expanded to provide a global,

sensitive all sky monitor for high energy transients. As such, one HERMES detector will ﬂy onboard the SpIRIT

(Space Industry Responsive Intelligent Thermal ) mission,4designed by the University of Melbourne.

The foreseen detector for this experiment employs the solid-state Silicon Drift Detectors (SDD) developed

by INFN and FBK in the framework of the ReDSoX Collaboration†. These devices, characterized by a very

low intrinsic electronic noise, are sensitive to both X-ray and optical photons. Hence they can be exploited

in the so-called “siswich” architecture, acting both as direct X-ray detectors (the operative “X-mode”) and as

On behalf of the HERMES collaboration.

Further author information: send correspondence to R.C., E-mail: riccardo.campana@inaf.it

∗https://www.hermes-sp.eu

†http://redsox.iasfbo.inaf.it

arXiv:2210.13860v1 [astro-ph.IM] 25 Oct 2022

photodetectors for the scintillation light produced by the absorptions of a γ-ray in a scintillator cyrstal (“S-

mode”). This allows for the realisation of a single, compact experiment with a sensitivity band from a few keV

up to a few MeVs for X and γ-rays, and with a high temporal resolution (<µs).

Figure 1shows a sketch of the payload (which ﬁts in a standard 1U CubeSat platform). Each of the sixty

12.10 ×6.94 ×15.00 mm3scintillation crystals (made of cerium-doped gadolinium-aluminium-gallium garnet,

GAGG:Ce) is coupled to two SDD channels. Ten SDD channels are integrated in a single monolithic 2×5

matrix. The crystals are contained in a stainless steel box, shielded with a tungsten layer.

During the period from October 2021 to April 2022 the ﬁrst ﬂight model for the HERMES constellation

(PFM, or Proto Flight Model) and the ﬂight model for the SpIRIT detector (FM1, or Flight Model 1 ) have been

integrated and calibrated. In this paper we provide an overview of the ground calibrations of the ﬁrst HERMES

and SpIRIT ﬂight detectors, outlining the calibration plan, detector performance and characterization.

Figure 1. Exploded view of the HERMES detector.

2. DETECTOR WORKING PRINCIPLE

The total number of channels in a HERMES payload is 120. Each SDD anode is connected to a front-end

chipset, composed of two diﬀerent ASICs. The ﬁrst one, LYRA-FE, is placed on the FEE board (Figure 1) as

close as possible to the SDD anodes, and contains the preampliﬁer and the ﬁrst stage of the shaping ampliﬁer

in a ∼0.5 mm2die, one for each channel. The signal is then routed to the side wing of the FEE board, to a

multi-channel LYRA-BE ASIC, which handles the rest of the spectroscopic acquisition chain (second stage of the

shaping ampliﬁer, threshold discriminator, peak and hold circuit, analog output multiplexer). Each LYRA-BE

handles 30 FE channels, and the whole detector is split in four totally independent quadrants. The conﬁguration

and communication with the ASICs, and the analog-to-digital conversion of their signal, is handled by the BEE

board (Figure 1), based on a Altera Cyclone V FPGA architecture.

When the signal on a given channel crosses a programmable threshold, a trigger is raised by the LYRA-BE,

which then holds the signal in an above-threshold channel to its peak value. The BEE FPGA then commands

the analog multiplexer, scanning ﬁrst a multiplexed trigger output and identifying the triggering channel(s)

address(es), and ﬁnally the analog output multiplexer is addressed and the signal converted to digital. The BEE

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CalibrationoftherstdetectorightmodelsfortheHERMESconstellationandtheSpIRITmissionRiccardoCampanaa,GiuliaBaronia,b,GiovanniDellaCasac,GiuseppeDilillod,EzequielJ.Marchesinia,FrancescoCeraudod,AlejandroGuzmane,PaulHeddermane,andYuriEvangelistadaINAF/OAS,Bologna,ItalybUniversityofBologna,DepartmentofP...

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Calibration of the rst detector ight models for the HERMES constellation and the SpIRIT mission Riccardo Campanaa Giulia Baroniab Giovanni Della Casac Giuseppe Dilillod

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