TES microcalorimeters for future X ray missions. Athena and Beyond: TES detectors for future X-ray missions. Luigi Piro IAPS/INAF

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Clifford Gerard Stokes
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1 Athena and Beyond: TES detectors for future X-ray missions IAPS/INAF 1

2 Setting the stage Science drivers for a Integral Field Spectrometer in X-rays Driving Requirements and mapping into detector Scenarios for L2 stage Technological roadmap 2

3 Topical Science Drivers for X-ray IFS Formation and evolution of large scale structures First objects in the Universe Formation and evolution of metals in the Universe 3

4 S / N A T exp E B Requirements Main driver: energy resolution Faint/Diffuse sources: (WHIM, Proto-clusters, cluster outskirts): area, background, FOV Bright sources/ diffuse( Cluster cores, SNR,.): area, FOV, angular resolution Bright sources/ point like (Compact Gal and Extr., GRBs, stellar coronae): area, c/r capability, TOO mode (at mission level) 4

TES cryogenic microcalorimeters ev resolution, kpixel imaging and high count rate: the first X-ray Integral Field Spectrometer International TES consortium: IAPS with SRON,

5 TES cryogenic microcalorimeters ev resolution, kpixel imaging and high count rate: the first X-ray Integral Field Spectrometer International TES consortium: IAPS with SRON, GSFC/NASA, ISAS/JAXA founding members Consortium in Italy: IAPS + INFN-Genova, INAF: Oss & IASF Palermo, IASF/Bologna, IASF/Mi, IFN/CNR-Rome & Thales Alenia Milano Ir-Au Tc=76 mk 5

GSFC/NASA, ISAS/JAXA founding members Consortium in Italy: IAPS + INFN-Genova, INAF: Oss

6 Instrument implementation Read-out: demonstrated performance on 2 x 8 array with E < 3 ev, potential for significantly better resolution; Detector with 32 x 32 array size build Cooling system various options: JAXA, European based on Herschel/Planck heritage + ADR ASTRO-H MICRO-X rocket: First TES-based instrument flight in 2014: 128 pixel array, 13 FOV, PuppisA 6

Cooling system various options: JAXA, European based on Herschel/Planck heritage + ADR

7 DE FWHM = 2.35z kt 2 C Theoretical limit: 0.3 ev Energy resolution Bandler et al

8 Arrays and Number of Pixels Bottleneck is readout Multiplx is required (Frequency or Time domain) FDM: ~ 5 channels/mhz SQUID linearity requires feedback => bandwidth limitation due to cable delay Demodulation(baseband feedback: SRON, JAXA): 1-4 kpixel 8

linearity requires feedback => bandwidth limitation due to

9 Double loop cryo feedback Devised and under development by Italian consortium Short loop in cryo environment First prototype: badwidth (8MHz) consistent with kpix array Potential bandwith: 200 MHz Megapixel array FLL_slow electronics 9

prototype: badwidth (8MHz) consistent with kpix array

10 Hydra Pixels Absorber attachment stems Thermal links TES Bias leads ~ 1 mm Kelley et al 10

10 5 10 4 10 3 0.01 10 5 10 4 10 3 0.01 TES microcalorimeters for future X ray missions Background reduction Extensive simulations/design and TES AC detector by Italian consortium CLJ1449 0856 z=2.

11 TES microcalorimeters for future X ray missions Background reduction Extensive simulations/design and TES AC detector by Italian consortium CLJ z= ks CLJ z= ks bkg nom F(5 )=10-13 c.g.s Fe Ka x6 x20 normalized counts s 1 kev 1 normalized counts s 1 kev 1 σ(t) =3.3% σ(z) =15% Energy (kev) Energy (kev) Cluster at the formation epoch (z=2) F=10-15 erg/cm 2 /s, A=0.2 arcmin 2, kt=2.0 kev, Abundance 0.3, area=1m2,f/l=12m Astronomia X, INAF, Roma Nov.7, March , March ,

CLJ1449 0856 z=2.07 250ks CLJ1449 0856 z=2.07 250ks bkg nom F(5 )=10-13 c.g.s Fe Ka x6 x20 normalized counts s 1 kev 1 normalized counts s 1 kev 1 σ(t) =3.

12 Based on a large area (4x 0.25 cm2)tes-based detector pixels TES Antico Main requirements: fast (rise time <30 usec) and low energy threshold 20 kev Fast response vs large (high C)pixel: a- thermal phonon: large collecting area Last (5 th gen) prototype already close to req.s (for 1cm2 array) AC-S1 Area [mm 2 ] AC-S2 Area Collecting [mm 2 ] area (%) AC-S3,4 Area [mm 2 ] Collecting area (%) Collecting area (%) 100 ~ 20 12

threshold 20 kev Fast response vs large (high C)pixel: a- thermal phonon: large collecting area Last (5 th

13 Quantum efficiency already >90% Mirror area: cost limited Optical blocking filters Effective area 13

14 Count rates and high and bright sources Upto 10 Kct/s with customized chip (~ Crab for ~ m 2 mirror) At System level, for a TOO reaction time of ~1 hour, High resolution spectroscopy of transients Already proved for an Athena-like envelope by TAS-Turin system study 14

TOO reaction time of ~1 hour, High resolution spectroscopy of

15 High res. X-ray spectroscopy of high z GRB GRB afterglow at z=

16 A Technological roadmap L mission launch date at X, TRL>5 at X-10 L2: 6-7 years of tech development A demonstrator model for end-to-end test with cryochain in the ESA tech programme Best realistic performances (but need trade-off and ): DE<1 ev (small pixels), 2-3 ev ~ 4 kpix array (e.g. 10 x10 for 10 HEW or 5 x5 for 5 ) Lower background (<4x) High count rate (Crab) High throughput mirrors 16

realistic performances (but need trade-off and ): DE<1 ev (small pixels), 2-3 ev ~ 4 kpix array (e.

17 A Technological roadmap II Longer time scale (~2020) >100 kpixel array (FDM) Best candidate: TES (already DE<2eV) Non-bolometric detector (KID,MMC) in principle more easily tunable with large b/w FDM Effectively a CCD with 1 ev resolution E.g. for 2 a FOV of ~20 x20 Or.. An X-ray IFS with R=3000 Better than O-IR instrumentation 17

more easily tunable with large b/w FDM Effectively a CCD with 1 ev resolution E.g. for 2 a FOV of ~20 x20 Or.

18 18

19 TES microcalorimeters for future X ray missions Background Factor Factor cts s 1 cm 2 kev 1 arcmin Background components A = 1m2 f = 11.5 m Energy (kev) 10 Simone Lotti 19 15, 2013 March 19

1 Factor 10 10 3 Factor 6 10 4 10 5 cts s 1 cm 2 kev 1

20 Simulations, antico and instrument GEANT simul in L2 environment (solar+cr) Without antico bkg x25 larger than requirements. design With present design + antico compatible with req.s Residual background is dominated by secondary e- produced close to detector Substantial reduction (x6) by kapton liner and thin filter 20

design With present design + antico compatible with req.

Yukikatsu Terada (Saitama Univ, Japan), on behalf of the Astro-H Software Calibration board

Yukikatsu Terada (Saitama Univ, Japan), on behalf of the Astro-H Software Calibration board SKIP (Rob Introduction) The sixth series of the Japanese X-ray satellite. Collaboration with JAXA, NASA, and