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Vulcano Workshop 2010

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New Trends in Astronomical New Trends in Astronomical X-ray Optics X-ray Optics

 Achieving wide FOV: WF (Lobster) Optics  Achieving very fine angular resolution: Active X-ray

Optics

 Optics for large X-ray Telescopes with good angular

resolution at affordable price: K-B Optics

 Use of new materials e.g. Silicon wafers

Vulcano Workshop 2010

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 Goal: sensitive all-sky X-ray monitoring  Improvement factor vs. RXTE: 100-1000  ! Important for many objects discussed

here!

Vulcano Workshop 2010

Lobster Eye Lobster Eye X-ray Optics X-ray Optics

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 Novel Wide Field X-ray Telescopes  FOV of 100 sq. deg. and more

easily possible (classical X-ray

• ptics only 1 deg or less)

 Analogy with lobster eyes Vulcano Workshop 2010

Lobster Eye Lobster Eye (LE) (LE)

The biomimetics – learning from the nature

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The biomimetics – learning from the nature The refractive eyes of a lobster

Vulcano Workshop 2010

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Vulcano Workshop 2010

The eye of a lobster, viewed with a microscope. Right: close up of a small area of the eye. The eye consists of millions of square "channels"; each channel measures approximately 20 µm (or two hundredths of a millimeter) across.

„ „Real Real“ “ Lobster Eye Lobster Eye (LE) (LE)

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number of photons detected inside the FWHM circle with the LE number of photons detected inside the FWHM circle without the LE

G =

Gain as a function of energy - for various designs (for E)

Vulcano Workshop 2010

The LE Optics can be designed for E = 0-10 keV. The gain can be ~ 1000 for low energies and ~100 for higher energies

Gain Gain

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The front wiew of the mini - lobster module, Schmidt arrangement, based on 100 micron thick plates spaced by 300 microns, 23 x 23 mm each The X-ray measurement at 8 keV in comparison with mathematical simulation

measured model

Vulcano Workshop 2010

Micro LE: 3 x 3 x 14 mm module glass Foils 30 µm thick separated by 70 µm Focal image 8 keV

Modular concept to achieve large FOV

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• daily limiting flux 10-12 erg/s/cm2
• one module 2 x 195 plates 78 x 11.5 x 0.1 mm, 0.3 mm spacing
• detector pixel size 150 µm
• total front area 1825 cm2
• energy range 0.1 - 10 keV
• FOV 180 x 6 degrees (30 modules 6 x 6 degrees)
• angular resolution 3 - 4 arcmin
• total mass < 200 kg

Vulcano Workshop 2010

LE Sky coverage per revolution LE Sky coverage per revolution

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Scientific goals

• 1. Alert System for X-ray transients

fast recognition of new X-ray sources and/or sudden changes in X-ray flux of known sources, prompt emission study, precise positioning, alert system for narrow-field instruments

Vulcano Workshop 2010

• GRB prompt and afterglow X-ray emission (20-60 triggers/year)
• X-ray flashes (> 8 triggers/year)
• orphan GRBs (detectable in X-rays but not in gamma)
• SNe prompt emission (thermal flash) 10-20 triggers/year
• X-ray binary & CVs flux changes
• Stellar events in the Sun's vinicity

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• 2. Long-term X-ray source monitoring

long-term monitoring of large number of X-ray sources with sampling of hours to days (depending on the source flux). Light curves for all the sources together with rough spectra (continuum monitoring, strong lines, iron detectable). In the list below we assume the limiting flux of 10-12 erg/s/cm2 (but we can go deeper):

Vulcano Workshop 2010

• X-ray binaries ~ 700 triggers
• Cataclysmic Variables ~ 200 triggers
• stars ~ 600 triggers
• AGN ~ 4 000 triggers
• galaxy clusters ~ 400 triggers
• SN remnants

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Lobster eye P25 was tested in quasi parallel beam full imaging mode using the 35 meters long X-ray beam line of INAF-OAPA in Palermo (Italy). X-ray images at the focal plane have been taken with a MCP detector with spatial resolution 100µm.

Vulcano Workshop 2010

Tested lobster eye was placed on device allowing remote controlled rotations figured by red color. MCP detector was placed on device allowing remote controlled translations in all directions.

• 2510

Estimated spatial resolution ~13arcmin. FWHM 12~13arcmin at all energies (theoretical 5 arcmin)

Tests in Palermo X-ray facility Tests in Palermo X-ray facility

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1500eV 1500eV 930eV 930eV 280eV 280eV 8000eV 8000eV 4500eV 4500eV 2900eV 2900eV

Vulcano Workshop 2010

X-ray images X-ray images

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 Goal: scientific payload for a picosatellite

10 x 10 x 30 cm

Vulcano Workshop 2010

Mini Lobster Telescope for Mini Lobster Telescope for picosatellite picosatellite

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LE Telescope on German Picosatellite LE Telescope on German Picosatellite

Tests with Lobster Eye X-ray Optics & Medipix at 8 keV

CTU Prague member of Medipix Collaboration

Feasibility study of small LE X-ray telescope for Picosatellite

Vulcano Workshop 2010

The Medipix detector represents suitable imaging detector for use in space LE telescopes

Based on UWE concept, Univ of Wurzburg, DE F=25 cm,L=30 cm Picosatellite 10 x 10 x 30 cm Technological experiment but still some science

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 Goal: ultra-precise angular resolution < 1

arcsec

 Computer controlled substrates for ultraprecise

X-ray optics (sub-arcsec)

 Goal: super-precise optics (sub arcsec angular

resolution) for NASA Project Generation X

Vulcano Workshop 2010

Active X-ray Optics Active X-ray Optics

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Arrangement of piezoelectric actuators on a Wolter I – principle of active X-ray optics.

Vulcano Workshop 2010

Technical challenge: the total number of piezoelectric elements must be of

• rder of 100 000 – 1 000 000, due to large area of the mirror array

Alternatives: (1) Piezoelectric actuators (2) Electrostatic shaping

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Vulcano Workshop 2010

• Future space X-ray telescope such as IXO (International X-ray

Observatory) require novel technologies:

• Light-weight (large apertures, multiply nested)
• Precise (angular resolutions better than 5 arcsec)
• Low-cost, mass-production (need for huge geometrical area)
• Old technologies cannot be used as they are either too heavy (thick glass

ceramics, e.g. Chandra) or not enough accurate, or both (electroformed Ni, e.g. XMM Newton).

• Key requirements:

Effective area ~3 m2 @ 1.25 keV Angular Resolution <= 5 arcsec

• Single segmented optic with

design optimized to minimize mass and maximize collecting area

Future of X-ray Astronomy: IXO Future of X-ray Astronomy: IXO

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 Goal: decrease expenses in future X-ray

• ptics

 High angular resolution ~5 arcses at

affordable price

Vulcano Workshop 2010

Kirkpatrick-Baez Optics Kirkpatrick-Baez Optics

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• Double reflection X-ray Optics consists of

two mirror sets – one is aligned vertically and the second is aligned horizontally.

• The quality of the focal spot image depend
• n quality of substrates (shape,

microroughness).

Vulcano Workshop 2010

Kirkpatrick-Baez Optics Kirkpatrick-Baez Optics

• Both mirrors are curved parabolically – the first mirror focuses in vertical

plane and the second mirror focuses in horizontal plane. Single focal point is formed in the crossection of the two focal planes. Nested systems possible.

• Technology is not necessarily based on precise and expensive mandrels

hence

• Cost-effective manufacture

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Wolter system KB system If W and KB have the same aperture, focal length of KB system is twice as large as Wolter system.

Vulcano Workshop 2010

Focal length

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Vulcano Workshop 2010

Focal peak intensity - normalized

(Focal length 20m KB and 10m W)

KB system Wolter system

Focal FWHM [mm] – not normalized

Wolter system KB system

D [m] A [m2] F [m] Aeff [m2]* Arel [%]** Aeff [m2]*** Arel [%]**

W10 dia 1.8 2.6 10 0.70 26.63 0.66 25.11 W20 dia 3.6 10.9 20 2.83 25.89 2.76 25.26 KB20 1.8 x 1.8 3.3 20 0.93 27.80 0.62 18.49 KB40 3.6 x 3.6 13.9 40 3.11 22.33 2.46 17.66

* for detector 100 x 100 mm ** proportion of effective area to aperture *** for peak (area 4 x 4 mm)

K-B vs. Wolter: comparable ef area at f =2f, comparable angular resolution

Comparison K-B vs. Wolter

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• Model based on ray-tracing (11 profiles)‏
• Two sets of mirrors from Si chips 100x100x0.525 mm
• Total optics length 600 mm, aperture 40x40 mm
• Major problems of Wolter optics avoided (need of expensive

mandrels, need to bent to radii ~ 50 cm) = less expensive alternative

Vulcano Workshop 2010

TEST K-B modules

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Delivered April 2010 PI R. McEntaffer

• R. Hudec co-I,

participation of CTU Optics by Rigaku Prague KB X-ray space telescope

A high resolution X-ray spectrometer utilizing Kirkpatrick-Baez optics and

• ff-plane gratings

Vulcano Workshop 2010

NASA K-B Rocket Proposal

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Organization of workshops and conferences Organization of workshops and conferences

International Workshop on Astronomical X-ray Optics AXRO Prague Dec 2008, 2009, 2010 US-Czech Seminar on Astronomical X-ray Optics Prague May 2007 SPIE EUV & X-Ray Optics Conference Prague April 2009, April 2011

Vulcano Workshop 2010

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• The LE ASM will very significantly contribute to various

regions of recent astrophysics

• The necessary technical background is already available,

making proposals for space project based on Lobster Eye

• ptics possible
• Applications also in other areas, e.g. atmospheric science
• Space Lobster projects recently considered by ESA and by

the Chinese Space Agency

Vulcano Workshop 2010

Conclusion Conclusion

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The End

Vulcano Workshop 2010

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 Goal: focussing of neutrons

– The refraction index is less than unity for most

materials for x-rays and neutrons.

– Imaging optics based on the grazing incidence

• ptical geometries developed for the x-ray

beams can be designed for the neutron beams.

Vulcano Workshop 2010

Applications of X-ray Optics as Applications of X-ray Optics as Neutron Optics Neutron Optics

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Vulcano Workshop 2010

The feasibility of grazing- incidence neutron imaging optics have been successfully demonstrated. Possible applications of the neutron optics need to be explored

Mildner et al., 2010

Neutron Optics