High-resolution X-ray spectroscopy High-resolution X-ray spectroscopy with microcalorimeterswith microcalorimeters

L. PiroL. Piro

• Some key scientific drivers: – GRB engine and progenitors: X-ray lines and

absorption features– Outflowing plasmas in the Galaxy and the boundary

with the local cluster– X-Ray Cosmology: GRB and WHIM (Cosmology

section)

X-ray Iron features in GRBX-ray Iron features in GRB•GB970508 (Piro et al 1999)

•GB980828 (Yoshida et al 1999)

•GB990705 (Amati et al 2000)

•GB000214 (Antonelli et al 2000)

•GB991216 (Piro et al 2000)

Study of local and intergalactic medium in primeval galaxies with GRB with XEUS

• The Fe line in a GRB like GB970508 but at z=5

• Study of the metallicity of the ISM of a host galaxy of a GRB at z=5 through X-ray edges

TES (Transition Edge Sensor) microcalorimeters

TES

Al-Ag multi-layer

High purity Si glued on a Sn absorber

Electro – thermal links to the heat bath

Polycrystalline Sn energy

absorber

We are developing, in collaboration with Genova University, TES devices with the goal of conforming to XEUS specs

First single pixel prototype already working with DE=16 eV at 6 keV, we are now improved tecniques and are confident to achieve the target DE=4 eV in the next year

Multi-pixel prototype design under development

TES microcalorimeter program • TES microcalorimeters are the next generation X-ray spectroscopy devices, and have been selected

as focal plane instruments for ambitious astrophysical missions like XEUS (ESA) and Con-X (NASA). Groups developing these devices are NASA/Goddard, Wisconsin Uni. , NIST, SRON. 

• We have set up a collaboration with Genova University, that has built up a longstanding experience on micro-calorimeters for basic physics applications. After the realization and test of a first prototype of TES detector, we have realized a 2nd batch (currently under testing) and foresee to achieve in 1 year a 4-5 eV resolution @ 6 keV. We have already started the design of a prototype of a position sensitive detector, that we plan to realize in 2 years (pending funds availability)

• The final goal is to identify the techniques for the realization of a detector to the XEUS requirements.

• Manpower: IASF(Roma) 3 research staff, 1 phd student, 3 technicians: manpower for 2002: 25 men-months; Universita Genova: 2 research staff, 4 phd/fellows, 2 technicians: 42 man-months in 2002. Similar manpower in 2003.

• Most of the activities are currently carried out with INFN and EU funds devoted to basic physics applications. In order to develop detectors compliant to the astrophysical requirements we estimate a budget of about 1000 keuro in 3 years. Proposals to support this activity are and will be submitted to ASI, EU, CNR, MIUR.