metis, the thermal infrared instrument of the e-elt h ans ulrich käufl, european southern...

METIS, the Thermal Infrared Instrument of the E-ELT Hans Ulrich Käufl,

European Southern Observatory Future Ground Based Solar System Research: Synergies with Space Probes and Space Telescope

METIS, E-ELT-Thermal Infrared, Future Ground-based Solar System Research, Elba 2008 Ulli Käufl, Elba 2008 slide # 2

METIS the

Mid-IR E-ELT Imager and Spectrograph Who is Metis?

According to Greek mythology, METIS was the first spouse of Zeus and mother of Athena, the goddess of wisdom.

What is METIS?At the E-ELT METIS shall cover the frequencies < 100 000 GHz

(or in conventional units λ > ~3000nm : the L , M, N and Q-band) It shall be a multimode instrumentSelected by ESO for a Phase-A-study (May 2008 – Sept. 2009)Relating to the VLT-Instrumentation Suite:

METIS = NAOS-CONICA long-wave + CRIRES long-wave + VISIR short-wave


METIS

The Collaboration and Heritage

MICHELLE

E-ELT\ \ \

HERSCHEL

PACS

JWST-MIRI

CONICA

TIMMI2

TIMMI

VISIR

Saclay


METIS

The People standing behind it ( from Bernhard Brandl's 2008 SPIE presentation )

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METIS

The Basic Modes under Study

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Conceived as a multi-mode instrument with clear priorities:

Diffraction limited filter imaging, FOV 20” x 20”- bands: L, M, N, (Q) - standard broad and narrow-band filters- coronagraphy, classic and 4-quadrant phase masks

Low-resolution long slit grism spectroscopyHigh-resolution cross dispersed spectroscopy:

ν / Δν ~ 1-2 * 105 @ 62000 GHz aka 4.8μm or CO

2

fundamental bandAll modes will work with AO

- self referenced “classic” AO incl. IR – wave front sensing- more complex modes, e.g. LASER guide star assisted under study

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METIS in the λ / Δλ plane: E-ELT vs. VLT

Claim of METIS in frequency / wavelength / resolution space set by physics and not by detector technology:

Wien's Law: λmax

≈ 2898 μm / TBB

molecular vibrations: h * ν / c ≈ 3 ... 20 μmMETIS, E-ELT-Thermal Infrared, Future Ground-based Solar System Research, Elba 2008 Ulli Käufl, Elba 2008 slide # 6

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METIS in Imaging Mode

METIS, diffraction limited at a 42m telescope will have a diffraction limited high Strehl PSF:

Thermal-IR-special AO-unit:* IR wavefront sensor* atmospheric dispersion compensation * control of humidity induced seeing Some Imaging modes taylored for very high

contrast imaging:* coronagraphy* pupil masking* 4-quadrant phase mask


3 18 13.15 30 21.8

10 60 43.620 120 87.2

wavelength [μm]

1.22 λ / D [milli-arcsec]

PSF @ 1 AU [km]

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METIS in Imaging Mode (II)

METIS @ 10 μm will have the same PSF as today's K-Band adaptive optics imagers at 8 m -class telescopes (data, J,H,K false color from CRIRES-MACAO commissioning, Paufique and Marchetti, SPIE 2006)


How METIS @ 10 μm will image Io's hot spots (disk diameter 1.2”)

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METIS in Imaging Mode (III)

There will be various METIS imaging cases reviewed or discussed in great detail in this conference, so just 2 more examples close to this workshop topic not covered in the program:

Direct detection of extra-solar planets (Brandl et al., 2008)


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METIS in Imaging Mode (III)

Star Formation and Planetary Systems Formation, simulated METIS data:

From METIS Proposal Science Case

a Jupiter @ 20AU a flaring disk with inner gap“foot-print in dust disk” coronagraphy helps METIS, E-ELT-Thermal Infrared, Future Ground-based Solar System Research, Elba 2008 Ulli Käufl, Elba 2008 slide # 10

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METIS in Imaging Mode (IV)

Exo-Planetary Systems, simulated METIS performance at 30 000 GHz(aka 10μm):

From Brandl et al. METIS at SPIE 2008


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METIS in Spectroscopy Mode

Again, there will be a variety of specialized contributions, so I picked from what is left over my favorite choice:

TIMMI2 low resolution (ν/Δν~200) spectro-astrometry: spatial structures down to 30 mas: extrapolated to METIS one could resolve structures down to at least 3 mas (less than 1AU at Chameleon)


star formation: W33A

CO gas and ice features slit centered on Maser region (data courtesy Siebenmorgen & Menten) black: W33Agray: telluric absorption

- CRIRES as an AO imagerK-band (logarithmic intensity scale) allows for slit registration with~100 mas precision


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METIS, the Site Matters ... more than Instrument Technicalities

Performance Simulations have been done for various spectral bands as a function of site

comparisons is between Paranal: low altitude, hot and humid site

and Cerro Macon: ~ 4800m, a lot colder and dryer ... ( probably one of the most extreme “realistic” sites )

While K-band low-res spectroscopy profits most from this site selection, it is not part of METIS but we have natural allies there

Example shown here is the CO-fundamental band

Detailed simulations can be done using the ESOE-ELT exposure time calculator METIS, E-ELT-Thermal Infrared, Future Ground-based Solar System Research, Elba 2008 Ulli Käufl, Elba 2008 slide # 14

M-band: comparison Paranal vs. 5050m

Ulli Käufl, Towards the European ELT Dec 1st 2006slide 15

MM5 ►Radiances

CO

Schematics of METISimaging part


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Additional Modes under Trade-Off Studies

medium resolution IFU spectroscopy

larger FOV for both imager and IFU spectrograph

extended wavelength coverage to include red Q-band (site!)

linear polarimetry for both imaging and spectroscopy

spectral differential imaging mode

parallel observing modes

Expected Performance of METIS

Calculations based on atmospheric model for Cerro Macon(high,dry and cold) assuming over-all back-ground-noise limited performance.

Keep in mind, IR-atmospheric windows are “Venitian Blinds”;a detailed view in an ETC based on realistic spectroscopy always pays off


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Road Map for METIS


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Phase-A-study till end of 2009 in the general context described by d'Odorico

detector selection: * baseline design assumes for

N,Q: the availability of 1k x 1k AsSi detectors with ~25μm pixel pitch

L,M,N: InSb or HgCdTe, many options* in the context of VISIR upgrade, ESO does the prototyping for λ > 5μm * fall-back solutions exist

read-out electronics, data-flow etc. are in the extrapolation range of today's systems and the VISIR/CRIRES upgrades

Background subtraction techniques need some prototyping which is – unfortunately – only partially covered by VISIR

METIS conclusionsfrequency coverage: < 100 000 GHz

or in conventional units λ > ~3000nm :very well suited to the Solar system

spectral resolution: ν / Δ ν ≈105 and ν / Δ ν ≈102 very well suited to study gas and dust

spatial resolution: classical imaging matches in-situ space craft cameras☞ spectroastrometry opens up the ☞ μ-arcsec domain

Calibration (see Delbo, Fernandez & Müller): thermal IR-fluxes can be absolutly calibrated in a meaningful way: Itokawa – observations, the “coming-of-age” of thermal IR-photometry!

METIS, thus has the portential to be a very powerful instrument for future Solar system research; the higher, the dryer and the colder the site, the better

and more ideas on the science case more than welcome!METIS, E-ELT-Thermal Infrared, Future Ground-based Solar System Research, Elba 2008 Ulli Käufl, Elba 2008 slide # 20

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More Conclusions METIS

extra solar planets

Extra-terrestrial life

Earths in habitable zones ... an outsiders view ...


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metis, the thermal infrared instrument of the e-elt h ans ulrich käufl, european southern...

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