a. collura – visiting committee presentation december 2007 x-ray instrumentation for astronomy...

A. Collura – Visiting Committee Presentation December 2007A. Collura – Visiting Committee Presentation December 2007

X-RAY INSTRUMENTATION FOR ASTRONOMY

Alfonso Collura

Istituto Nazionale di AstrofisicaOsservatorio Astronomico di Palermo


Other People Involved (Since)

Marco Barbera - Associate Professor DSFA (1992)

Roberto Candia - Technician (electronics – mechanical) (1996)

Salvatore Varisco - Technician (software – electronics) (1996)

Gaspare Di Cicca - Technician (mechanical) (2001)

Emanuele Perinati - Post Doc (1998)

Ugo Lo Cicero – PhD Student (Electronic Engineer) (2007)


I Will Talk About

History of the X-Ray Astronomy Calibration and Testing (XACT) Facility

Activities in the framework of space missions

Instrumentation development and other activities not for a specific mission


XACT Facility

Established under the impulse of G.S. Vaiana to partake to the development of CHANDRA instrumentation started operating in 1993

Designed with CHANDRA in mind, but privileging versatility to allow several other applications


XACT conceivment 1989

1991

1993

Upgrade I – Clean room; MCP detector; Transmission grating;UV beam line; 1997

1999ADR Cryostat

2003Upgrade II – See dedicated slide

XACT Development

Year

Beam line and basic equipment

1995

2001Vacuum control

Personnel (Sc/Tec)

Funding Source

1 / 2

1 / 22 / 2

2 / 3

2 / 3

2 / 2

2 / 3

400 SICILIAN GOV.

200 SICILIAN GOV.

100 OAPA

30 ASI

100 OAPA

90 ASI

110 ASI

100 OAPA

70 PRIN-MIUR

100 ASI100 OAPA

100 ASI100 OAPA120 ASI100 OAPA

50 CRA120 ASI100 OAPA

70 PRIN-MIUR

SEE DEDICATED SLIDE

20 CNR

200720072 / 3

Rental of buildingRental of building

First lightFirst light

2180 2180 before upgrade IIbefore upgrade II


First X-Ray Beamline


Clean Room

UV BeamlineGSPC detectorMCP detector

X-Ray Transmission grating Monochromator

8 m 8 m

X-ray Source Test Section

XACT - Upgrade I


UPGRADE II (2003-2007)

XACT DEVELOPMENTXACT DEVELOPMENT FundingFunding SourceSource

Longer (35 m) Beam LineLonger (35 m) Beam Line

2 m diameter Test Chamber2 m diameter Test Chamber

X-ray optics X-ray optics micropositioningmicropositioning

Double Cristal Double Cristal MonochromatorMonochromator

LTD Read-out ElectronicsLTD Read-out Electronics

Maglev oil-free pumpingMaglev oil-free pumping

New Machine ShopNew Machine Shop

Moving to Via IngrassiaMoving to Via Ingrassia

PON PON (co-funding (co-funding from EU, Ital. Gov. from EU, Ital. Gov. and OAPA)and OAPA)

680680

7070 ASIASI

6060 SICILIAN GOVSICILIAN GOV..

150150 OAPAOAPA

150150 MEF (PRISMA)MEF (PRISMA)

12101210

8585 PRIN-MIURPRIN-MIUR

PRIN-INAFPRIN-INAF1515

Not included: works on the buildingNot included: works on the building


The new beamline


Space Missions

CHANDRA XMM-NEWTON HINODE CHANG’E-1 LOXIA CORONAS PHOTON- SphinX SIMBOL-X EDGE


X-ray QE of MCP’s at Daresbury Synchrotron• CsI vs. KBr, X-ray QE modeling, Life tests

End to End test at Marshall Space Flight Center• HRC-I +HRMA, HRC-S + HRMA + Gratings

In Flight Calibration• Out of band sensitivity

• Design, Vibrational and Acoustic tests, Calibration plan

Development of the UV/Ion shields

X-ray transmission of the UV/Ion shields

UV transmission measurements of the UV/Ion shields• Out of band rejection

•X-ray Transmission modeling, XANES and EXAFS

Chandra HRC


UV transmission measurements of the UV/Ion shields

at XACT and DSFA-UNIPA

New filter design: Polyimide instead of Lexan, and single layer of aluminum (impact also on Chandra ACIS, Newton-XMM EPIC, JET-X CCD).

Aluminum oxidation and interferences


UV transmission measurements of Medium and Thin Filters • Out of band rejection

X-ray transmission measurements of Medium and Thin filters• X-ray Shadowgraphs• X-ray Transmission modeling, XANES and EXAFS

Medium and Thin Filter design and calibration plan

Newton-XMM EPIC

Monitoring ageing effects on Medium and Thin filters


Monitoring ageing effects of the Medium and Thin filters

July 1997 July 2002

Slight increase in transmission in a narrow band. No significant impact on the science with EPIC


Calibration of the Focal Plane 9 Filters

• X_ray shadowgraphs• X-ray transm. measurements and modeling

Calibration of the Telescope

• Participation in the end to end test at Marshall

XRT on board HINODE( PI: dr. Leon Golub, SAO, Cambridge, MA)


X-Ray Shadowgraphs

6 – 25 μm Al Filter Shadograph at 1.49 keV


X-Ray Transmission measurements and modeling

6 – 25 μm Al Filter


CHANG’E-1 LOXIAChinese experiment to study the composition of the lunar surface


SphinX

October 15, 2007 ~13:13 Fe anodeAmp A

October 11, 2007 ~12:31 Fe anodeAmp B

Comparison of SphinX measurements wit and without apertures on detector D2 and D3

With apertures

Withoutapertures

D2 and D3 ovelap

D1

Log plot Log plot

dots - D4


SIMBOL X Thermal Shields

average radial temp. variation in the mirror shells

0

5

10

15

20

25

0 10 20 30 40 50 60 70 80 90 100

shell number

Avera

ge T

em

pera

ture

°C

average radial temp. variation in the mirror shells

18,5

18,6

18,7

18,8

18,9

19

19,1

19,2

19,3

0 10 20 30 40 50 60 70 80 90 100

shell number

Avera

ge T

em

pera

ture

°C

No shieldsNo shieldsT ~ 7 °CT ~ 7 °C

With shieldsWith shieldsT < 1 °CT < 1 °C

X-Ray TransmissionX-Ray Transmission

Polyimide+AlPolyimide+Al

AlAl

20 °C20 °C

15 °C15 °C

18.6 °C18.6 °C

19.2 °C19.2 °C


EDGEDesign of the Narrow Field Imager Telescope

in collaboration with INAF-IASFPA

Contribution to the Design and Optimization of the Narrow Field Contribution to the Design and Optimization of the Narrow Field Imager Telescope equipped with an X-Ray Microcalorimeter Array Imager Telescope equipped with an X-Ray Microcalorimeter Array Focal Plane DetectorFocal Plane Detector

Design of the Baffles for the Wide Field Telescope equipped with an Design of the Baffles for the Wide Field Telescope equipped with an X-Ray CCD Focal Plane DetectorX-Ray CCD Focal Plane Detector


R&D Activities (not for a specific mission)

NTD Germanium Microcalorimeters

Plastic Foil light weight X-ray Optics

Bio samples irradiation (next presentation)


X-Ray Microcalorimeters with NTD Ge Sensors

•In collaboration since 1997with SAO (PI: Eric Silver) we are investigating X-ray microcalorimeters with NTD Germanium sensors for laboratory and astrophysical applications.

•More recently we have started a collaboration with UNIPA-DIEET to develope a fully Planar approach for the construction of 2-D arrays with a large number of pixels.


State of the Art

• Energy Resolution: - 3.1 eV FWHM at 6 keV - 50 eV FWHM at 60 keV

• Time Resolution: - Counting Rate up to ~ 50 Hz per pixel without significant energy resolution degradation.

• Construction Technique: - Micromachining. 2x2 arrays currently in use. The proposed approach for 2-D arrays with large number of pixels is based on the superposition of linear arrays.


• Single Stage ADR Cryostat built in house. Minimum Temperature 42 Single Stage ADR Cryostat built in house. Minimum Temperature 42 mK. Hold Time at 60 mK longer than 2 days.mK. Hold Time at 60 mK longer than 2 days.

• Four channel fully wired read-out electronics to operate small arrays Four channel fully wired read-out electronics to operate small arrays of Semiconductor Thermistor Microcalorimetersof Semiconductor Thermistor Microcalorimeters..

Study of Absorber MaterialsStudy of Absorber Materials


(a) Lapped doped NTD-Ge wafer

(b) Attachment of a monolithic absorber foil

(c)Resist coating - Laser Microlithography

(d) Deep Wet Etching of Ge (~ 100 μm)

(e) Evaporation of electrical contacts on Ge

(g) Electrical connection to the support membrane

(h) Separation of absorbers

(f) Evaporation of electrical circuit on support thin membrane

Proposed Fully Planar Approach for the Construction of Arrays of Microcalorimeters with Ge Sensors


Orientation (100) 4 hours etching

Orientation (100) 3 hours etching

Pyramidal Geometry Toroidal Geometry

Deep Wet Etching of Ge


Plastic foils grazing incidence X-ray Optics (Collaboration with SAO and DSRI)

• Plastic is very light, elastic, cheap

• Plastic foils from common industrial applications have high surface smoothness by a combination of stretching and rolling

•Plastic foils replicate the figure of the mandrel but not the smoothness. Expensive superpolished mandrels not required

• Plastic has strong affinity to coating (single and multilayer)


Surface roughness

AFM measurements show micro roughness of uncoated foils of 4 ÷ 7 Å (Chandra-HRMA has 3 ÷4 Å)


Mounting the foils

• Vacuum hold-down mandrels to form cylindrical or conical shells• Foils hold inside grooves of the supporting wheels

• Epoxy cured while foils are still inside the mandrel


X-ray imaging tests of Cylindrical optics at XACT

FWHM ~ 10”

HPD ~ 2’

Imaging detectorX-ray Source

8 m 8 m


Irradiation of Organic Samples

The XACT FACILITY is being used for the irradiation of organic samples in a program of Astrobiology that will be the subject of next talk

a. collura – visiting committee presentation december 2007 x-ray instrumentation for astronomy...

Documents

committee presentation

xray microcalorimeters

construction of arrays

d arrays

2x2 arrays

cheap plastic foils

superposition of linear

dsri plastic