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Progress in TES Detector Development for Solar and Astrophysical Research at LMSAL

Explore the development of X-ray microcalorimeters for solar physics with TES technology, applicable to astrophysical instruments. Enhance understanding of magnetic reconnection in the solar corona for advanced research. Collaborating with key institutions and researchers for future space missions.

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Progress in TES Detector Development for Solar and Astrophysical Research at LMSAL

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  1. Progress in TES Detector Development forSolar and Astrophysical Research at LMSALRobert Stern, Steve Deiker, Dennis Martínez-Galarce, Adam Rausch, Lawrence Shing (LMSAL*) +NIST, Stanford, Santa Clara U. & LM ATC*Lockheed MartinSolar and Astrophysics LaboratoryLM Advanced Technology Centerstern@lmsal.com

  2. Outline • Some science motivation: why are microcalorimeters useful in solar physics ? • Characteristics of a solar physics X-ray mission concept using TES’s • Laboratory work at LMSAL on TES’s, ADRs • Applicability to astrophysical X-ray instruments • Summary

  3. Exploring Magnetic Reconnectionin the Solar Corona • New instruments needed to investigate dynamics of faint (EM < 1046 cm-3), hot ( > 107 K) material produced by reconnection in microflares and early stages of solar flares • previous flare instruments were mostly based on Bragg Xtal spectrometers with limited (SMM BCS) or no (Yohkoh BCS) imaging capability and very low effective area (0.025-0.1 cm2) • RHESSI (RMC + cooled HP Ge detector) is seeing many such microflaring events, but has limited spectral resolution at low energies ( ~1 keV at 3-10 keV) • High spectral ( R > 1000), spatial, and time resolution of hot (>10MK) plasma (e.g Fe XXV) is required (same Fe K-shell lines as seen in astrophysical sources)

  4. (Liu et al. 2004) RHESSI Fe Line Results • SMEX Launched (finally) in February 2002 • HP Ge (cf. HEAO-3) photon counter with RMC (cf. Minoru Oda, HINOTORI) • designed for hard (> 10keV) X-ray and gamma ray imaging and spectroscopy, but has ~15 cm2 at Fe XXV (6.7 keV) with ~ 1 keV FWHM, ~5 "

  5. Hannah et al. (2004) SOHO Workshop

  6. Explorer Class Mission Concept • Science driven: reconnection physics throughout cycle • 3-8 keV bandpass, < 4 eV energy resolution (R~1700 at Fe XXV 6.7 keV complex) • Combination allows LOS velocity determination to 200 km s-1 and better with centroiding + velocities perpendicular to LOS – 3D velocity field • Grazing Incidence Telescope - Focal Length ~2 m • FOV ~ 2.5 – 3 arc-min with ~few arcsec resolution • Count rate > 103 c/s for event studied (accumulate 10Kct spectrum in 10 sec); time stamping of photon events to sec accuracy

  7. Simulated TES Solar Explorer Spectrum from FeXXV Complex (20 MK) using CHIANTI SMM BCS (~1.25 mA thermal width) “RHESSI”-like microflare / 4 eV FWHM

  8. Key Technology Developments Needed • Up till now, most technology for X-ray TES driven by, e.g., Constellation-X, NeXT and XEUS (10-50 m focal lengths) • Small solar payload with F.L ~ 2 m  needs effective pixels of 10-20 m or so • Smaller effective pixels also help larger missions such as RAM (Reconnection And Microscale Mission) • Solar payloads need large number of spatial resolution elements to cover active region with high angular resolution • will likely require “tiled” or modular focal plane • High countrate ( kcts/sec) in microflare/flare region to accumulate spectrum quickly • Low mass cryocooler + Adiabatic Demagnetization Refrigerator (ADR) with long life

  9. Current Program of TES Research at LMSAL • Operate NIST-supplied devices (single pixel on NIST array) • Fe55 X-ray spectrum from 1st gen setup; 2nd gen in progress • Recent SR&T awards (Solar & Heliospheric) from NASA • Position Sensitive X-ray Strip Detectors (with NIST, SU) • Al:Mn Magnetically Insensitive TES (with Santa Clara, SU) • Solar TES Rocket (lower energies ~ 1 keV) – with SU, LLNL • New initiative: rocket ADR adapted for TES/SQUID readout (with LMATC Thermal Group, U. Wisconsin) • Pending: collaboration with MIT (Tali Figueroa), GSFC, U. Wisc on X-ray imaging TES rocket payload • Current goals: solar X-ray TES Explorer; Reconnection and Microscale Mission (long term)

  10. Key Collaborators in TES Instrumentation • NIST (TES’s, SQUIDs, Strip Detectors) • Kent Irwin, Gene Hilton, Joel Ullom, Randy Doriese • Stanford (TES principles, Al:Mn, Lab ADR experience) • Blas Cabrera, Paul Brink, Steve Leman, T.J. Bay • Santa Clara University (Al:Mn devices) • Betty Young • University of Wisconsin (Rocket ADR) • Dan McCammon • Lockheed Martin Advanced Technology Center Thermal Sciences Department (cryogenic technology, rocket ADR project) • Ted Nast, Dean Read

  11. Mn K-α and K-β. Measured resolution is 15.5 eV FWHM Fe55 Spectrum With 1st Generation Base Stage (late 2005) Single pixel achieved 2.4 eV FWHM (at NIST) • Need improved LMSAL base stage/noise reduction to separate Kα1, Kα2 LMSAL Lab Base Stage

  12. 2nd Generation Base Stage (under construction) Nb shield 1st stage SQUID slots (4) • Improvements: • Full Nb shield, • Axis of field-canceling coil perpendicular to axis of SQuID coils • Accomodates thermometry near TES, • Easier bonder access • Decreased size / weight. TES Slot

  13. NIST/LMSAL Strip Detector Concept Prototype Array • 32 parallel 10m wide strips each 320m long with ~ 10m position resolution (32  x 32  at 2m FL) MUXed at each end

  14. Strip Detector Test Wafer (LMSAL/NIST Grant(s) from NASA) with Pd layer (6/06)

  15. Manganese-doped Aluminum TES (NASA Grant with SU and SCU) Alternative to bi-layers: • Simplicity of fabrication. • Low noise • comparable to bi-layers • Design flexibility (not limited in thickness). • Apparent insensitivity to magnetic fields.

  16. Lockheed Martin Rocket ADR re-design (collab with U. Wisc.) Modify Design and Construct 3-D Solid Model Original U. of Wisc.design McCammon et al 2002 Low magnetic field required for TES operation

  17. Full 8.5 A => 4 T in core Operating ~ 150 mA => 700 G in core Passive Shields: Van. Perm. or Cryoperm Detector plate ≤ 3 G at detector plane Magnetic Field Modeling B-field at detector ≤ 0.05 G • Status: • 2nd iteration of design; FEM dynamics analysis to be re-run • Order and test magnet/shield in CY 2006 • Modify with additional shielding/bucking coil if required

  18. Astrophysics Applicability • Strip detectors • Short focal length telescopes • Multiplex capability results in fewer wires/resolution element • Al:Mn • detector thickness constraint removed • potential to significantly reduce magnetic shield requirements • Prototype (Rocket) ADR • new design will provide flight test of TES/SQUID operation

  19. Summary • LMSAL (with considerable help from NIST/SU/ Wisc./SCU) is pursuing a vigorous program of TES-related research focused on solar physics (with potential applicability to astrophysics) • Laboratory work (begun ~ 2 ½ yrs ago) is close to achieving noise goals for single-pixel devices • Position-sensitive strip detectors have been fabricated and are about to begin testing at NIST and LMSAL. • Al:Mn detector work with SCU/SU has begun • ADR Prototype design for TES solar rocket is nearly complete; magnet/shielding tests to begin this year

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