Jul 22 – 26, 2019
Europe/Rome timezone

Demonstration of fine-pitch high resolution X-ray transition-edge sensor microcalorimeters optimized for energies below 1 keV

Jul 25, 2019, 5:45 PM
1h 15m
Piazza Città di Lombardia (Milano)

Piazza Città di Lombardia


Piazza Città di Lombardia, 1, 20124 Milano MI
Poster Low Temperature Detector fabrication techniques and materials Poster session


Dr Kazuhiro Sakai (NASA-GSFC / UMBC)


We are developing arrays of fine-pitch X-ray transition-edge sensor (TES)
microcalorimeters for use in future space-based X-ray astrophysics missions
such as the proposed Lynx X-ray Microcalorimeter. In this contribution we
discuss arrays optimized to have the best possible energy resolution for a
limited energy range for the incoming X-rays, such as up to ~0.8 keV for the
Lynx Ultra-Hi-Res array. This array requires an energy resolution of 0.3 eV
full width half maximum (FWHM) for energies up to 0.8 keV. The test array we
have fabricated has 60 $\times$ 60 sensors on a pitch of 50 µm. The TES size is 20 µm,
and the pixels have 46 $\times$ 46 $\times$ 1 µm$^3$ gold absorbers. For this array, the
internal 64 pixels are wired using buried multilayer microstrip wires, wired
with a density consistent with being able to wire out the complete array. We
measured a spectral energy resolution of the same device using 3 eV EUV photons
delivered through an optical fiber. Due to difficulties associated with
directing a large number of photons into such a small pixel and produced by a
short pulse on the UV laser-diode, also due to difficulties in aligning the
optical fiber in our set-up we have only observed 3, 6, and 9 eV combs in
spectra. For the one-photon 3 eV line we have obtained an energy resolution of
0.26 eV FWHM, which is consistent with the estimated performance based on the
signal size and noise. Further measurements will determine how the energy
resolution degrades with energy. But it appears that this level of energy
resolution should be achievable up to 0.5 keV, and the performance gradually
degrades to a measured energy resolution of around 2.3 eV at 1.5 keV using
standard optimal filtering as the signals become non-linear. In this paper we
will describe the full design and characterization of this detector, and
discuss the performance limits of pixels designs like this.

Student (Ph.D., M.Sc. or B.Sc.) N
Less than 5 years of experience since completion of Ph.D Y

Primary author

Dr Kazuhiro Sakai (NASA-GSFC / UMBC)


Dr Joseph S. Adams (NASA-GSFC / UMBC) Dr Simon, R. Bandler (NASA-GSFC) Sophie Beaumont (NASA-GSFC / UMBC) Dr James, A. Chervenak Aaron Datesman (NASA-GSFC / Science Systems and Applications, Inc.) Dr Fred, M. Finkbeiner (NASA-GSFC / Sigma Space Corp.) Dr Ruslan Hummatov (NASA-GSFC / UMBC) Dr Richard, L Kelley (NASA-GSFC) Antoine Miniussi (NASA/GSFC - UMBC) Dr Frederick, S. Porter (NASA-GSFC) Dr Caroline Kilbourne (NASA-GSFC) Dr John, E. Sadleir (NASA-GSFC) Stephen Smith (NASA GSFC / UMBC) Dr Nicholas, A. Wakeham (NASA-GSFC / UMBC) Dr Edward, J. Wassell (NASA-GSFC / KBRwyle) Megan Eckart (Lawrence Livermore National Laboratory) Dr Kevin Ryu (MIT Lincoln Labs)

Presentation materials