2017 ltd17 pajot athena x-ifu · the$athena x*ray$integral$field$unit françois$pajot...
TRANSCRIPT
The Athena X-‐ray Integral Field Unit François Pajot
Ins9tut de Recherche en Astrophysique et Planétologie
on behalf of Didier Barret, Thien Lam Trong, Jan-‐Willem den Herder, Luigi Piro, Massimo Cappi and the X-‐IFU team
17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017 François Pajot
Athena in a nutshell
-‐ Advanced Telescope for High Energy Astrophysics, for the study of the hot and energe9c universe
-‐ Second Large (L) mission of the ESA Cosmic Vision 2015-‐2035
-‐ Launch year: end of 2028 -‐ with the newly developed Ariane 6 (64)
-‐ A 7 ton spacecra] to be placed in a L2 (L1) orbit -‐ Unprecedented collec9ng area in X-‐rays: -‐ 2 m2
goal at 1 keV and 0.17 m2 at 7 keV
-‐ 5’’ angular resolu9on -‐ Two focal plane instruments with a movable mirror assembly
-‐ The Wide Field Imager (WFI) op9mized for surveys
-‐ The X-‐ray Integral Field Unit (X-‐IFU) op9mized for spa9ally resolved spectroscopy
2
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
The X-‐ray Integral Field Unit
3
Parameters Requirements
Energy range 0.2 — 12 keV
Energy resolu9on 1: E < 7 keV 2.5 eV
Energy resolu9on: E > 7 keV E/ΔE = 2800
Field of View 5ʹ′ (equivalent diameter)
Effec9ve area @ 0.3 keV > 1500 cm2
Effec9ve area @ 1.0 keV > 15000 cm2
Effec9ve area @ 7.0 keV > 1600 cm2
Gain calibra9on error (peak, 7 keV) 0.4 eVCount rate capability nominally bright point sources 2 1 mCrab (> 80% high-‐resolu9on events)
Count rate capability brightest point sources 1 Crab (> 30% throughput)
Time resolu9on 10 µs
Non X-‐ray background (2 — 10 keV) < 5 10-‐3 counts/s/cm2/keV (80% of the 9me)1 goal 1.5 eV, 2 goal 10 mCrab (> 80% high-‐resoluOon events) events
-‐ Consor9um led by CNES/IRAP-‐F, with SRON-‐NL, INAF-‐IT and other European partners, NASA and JAXA.
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
Spectroscopic capabili9es
-‐ 8.8 keV absorp9on line in NGC1313 X-‐1 seen by XMM-‐Newton and NuSTAR
-‐ Rela9vis9c oumlow Fe XXV (6.67 keV, 0.25 c) or Fe XXVI Kα (6.97 keV, 0.2 c)
-‐ Degeneracy in photoionisa9on modeling (FeXXV, log ξ ∼ 3.3, 0.25 c) or (Fe XXVI, log ξ ∼ 4.5, 0.2 c)
-‐ Turbulent velocity unconstrained
4
Walton et al. (ApJ, 2016)
X-IFUEPIC PNSXSNuSTAR
x 15
x 10x 100
Effec
tive
are
a (c
m2)
101
102
103
104
Energy (keV)1 10
Athena X-IFUHitomi SXSGratings
Figu
re o
f m
erit
(m k
eV-1
/2)
0
5
10
15
20
25
Energy (keV)1 10
Effec9ve area comparison between X-‐IFU and other facili9es Figure of merit for spectroscopy measurements
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
X-‐IFU simula9ons: spectroscopy on clusters
-‐ Reconstructed bulk mo9on velocity field of the hot intra-‐cluster gas for a 50 ks X-‐IFU observa9on of the central parts of a Perseus like cluster considered at a redshi] of 0.1
5
Athena X-IFUXMM-Newton EPIC PNHitomi SXS
O
Fe LMg
Fe LFe L SiS
ArCa
Fe-K
Coun
ts/s
/keV
10−4
10−3
10−2
10−1
1
Energy (keV)0.2 0.5 1 2 5
Barret+ SPIE 2016
-‐ Simulated X-‐IFU spectrum of a z = 1 galaxy group with kT = 3 keV and LX = 1 x 10
44 erg/s for 50 ks. Emission lines from elements which are key to understand chemical evolu9on can be clearly seen.
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
X-‐IFU design
6
thermal filtersfilter wheelMXS
microcalorimeter array
focal plane assembly
cryo anti coincidence
dewar
readout electronics
door
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
X-‐IFU key design driving items (1)
-‐ Detectors -‐ Alloca9on 2.1 eV -‐> X-‐IFU energy resolu9on budget
-‐ Detector speed /event record -‐> X-‐IFU count rate capability
-‐ 3840 microcalorimeter array with Mo/Au TES from NASA-‐Goddard (SRON backup) under AC bias
-‐ Intrinsic energy resolu9on
-‐ Opera9on of TES under AC bias
-‐ Extreme sensi9vity to EMI/EMC, magne9c field, microphonics
(Goodwin Pappas+ O-‐23, GoWardi+ O-‐24, Wakeham+ O-‐27, Sakai+ PA-‐40, Khosropanah+ PA-‐41, Nagayoshi+ PA-‐47, Miniussi+ PA-‐50, Ridder+ PC-‐22)
7
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
X-‐IFU key design driving items (2)
-‐ Readout chain -‐ Alloca9on 1.2 eV -‐> X-‐IFU energy resolu9on budget
-‐ Frequency domain mul9plexing 1-‐5 MHz range with 40 pixels for each 96 chains
-‐ Cryogenic two stage SQUID amplifica9on and low noise amplifier at ambiant temperature
-‐ Base Band Feedback implementa9on to linearize SQUID opera9on
-‐ Event processor based on op9mal filtering and pulse templates
-‐ Digital to Analog Converter
-‐ Crosstalk
-‐ Gain/thermal stability and monitoring with Modulated X-‐ray Source -‐> X-‐IFU energy scale
(Prêle+ O-‐59, Akamatsu+ O-‐60, Bruijn+ O-‐75, den Hartog +PB-‐3, van der Kuur+ PB-‐13,DeNigris+ PC-‐14, Cucched+ PE-‐49)
8
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
X-‐IFU key design driving items (3)
-‐ Cryogenic chain and aperture cylinder -‐ Alloca9on 0.6 eV -‐> X-‐IFU energy resolu9on budget
-‐ Rejec9on of IR-‐visible-‐UV photons and EMI
-‐ 50 mK base temperature with 0.9µK rms thermal stability
-‐ Thermal filters including mesh insuring EMI immunity
-‐ Impact of Cosmic Ray on thermal stability of the detector
-‐ Preserving the X-‐ray Quantum Efficiency
(Yamasaki+ PD-‐17, SciorOno+ O-‐82, Barbera+ PE-‐62)
-‐ Cryogenic an9-‐coincidence detector -‐ Rejec9ng non X-‐ray events (cosmic rays, …) to 5 10-‐3 counts/s/cm2/keV -‐> low brightness capability
-‐ Ac9ve 4 TES pixels Cryo AC below the X-‐ray detector array
-‐ Secondary electrons/back scaxering on array
(Biasod+ PE-‐47, D’Andrea+ PE-‐52, D’Andrea+ PE-‐53)
9
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
High count rate and defocussing
-‐Mirror defocus capability up to 35 mm is now in the baseline
-‐ Spreading of the PSF over an increasingly larger number of pixels
-‐ Allows enhanced throughput on point sources(at the cost of a loss of imaging capabili9es of these point sources)
10
Courtesy of D. Willingale
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
Count rate capability
11
(See Peille+ PE-45)
High resolution / 25 mmHigh resolution / 35 mm10 eV resolution / 25 mm10 eV resolution / 35 mm
High res goal (10 mCrab)
Old 30 eV throughput requirement (1 Crab)
Broa
dban
d th
roug
hput
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.0
Source flux [mCrab]1 10 100 1000
-‐ Exceeds goal requirement at 10 mCrab (high resolu9on) and 1 Crab (10 eV resolu9on)
-‐ Even higher count rate in the 5-‐8 keV band with use of a beryllium filter
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
Cryochain and dewar
12
Outer vessel(300K)
Outer Cold Shield(OCS -100K)
Inner Cold Shield(ICS -30K)
Aperture cylinder(allocated volume)
Pulse tubes and JTs flange
4K shield
2K structure
-‐ Present baseline, a simplified cryochain is being studied
François Pajot17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017
X-‐IFU design status
-‐ Current status: a ~800 kg instrument
-‐ Op9miza9on in progress (mass, power consump9on, margins)
-‐ Progressing well towards TRL 5 in key technologies -‐ Phase A un9l end of 2018 (might evolve)
-‐ Phase B1 up to mission adop9on in June 2020
13
Science Instrument Module
15 m
17th International Workshop on Low Temperature Detectors Kurume, Fukuoka, Japan, July 16th-‐21st 2017 François Pajot
Conclusion
-‐ Thanks to challenging and innova9ve technologies in microcalorimeters operated at low temperature, X-‐IFU will provide breakthrough capabili9es in high resolu9on X-‐ray spectroscopy for the study of the hot and energe9c Universe.
14François Pajot
Conclusion