Universe observation from the Moon UltraViolet, Optics and InfraRed Frascati 07/05/2007 1 WP 1300...

Universe observation from the MoonUltraViolet, Optics and InfraRed

Frascati 07/05/2007

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WP 1300Optics UV/IR studies

Speaker: Carmelo Arcidiacono INAF – PD

Coordinator: Roberto Ragazzoni INAF - PD


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UltraViolet Optics and InfraRed Work Package

Formal and informal contributions coming from collaborators in throughout Italian Universities and Observatories

• Five themes– WP 1310 Solar Observations

• F. Berrilli, Roma Univ. Tor Vergata

– WP 1320 Solar System Minor Bodies Observations• M. Di Martino, A. Cellino INAF OA Torino

– WP 1330 Wide FoV Telescope – Mid Infrared Telescope– Interferometry for extremely high resolution


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WP1310 Sun ObservationScientific drivers description

is demanded to the talk:

High Priority and Heavier Payloads

16:00 TIGRE M. Feroci (INAF)

16:15 PIM C. Labanti (INAF)

16:30 High Resolution Solar Imaging from the Moon F. Berrilli (INAF, Tor Vergata Univ.)

16:45 Spectral Distortions of CMB C. Burigana (INAF)

17:00-17:30 General Discussion and Conclusions


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WP 1310 Sun Observations

• A 1 to 2 m Gregorian Diffraction limited UltraViolet telescope for Solar Observations.

• Aiming to explore magnetic tubes fluxes, their evolution and interaction with other Solar features.

• Spectrum-polarimetry essential• High Priority


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WP 1310 Sun ObservationsSite

Polar Zones

Crater Edge or rim

~Continous Sun Observation

High Visibilty from Earth for communications


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WP1310 Sun ObservationPayload Technical Specifications

• Gregorian Optical Design, Diameter 1.5m,25m focal length• Field of View: 100x100 arcsec • Bandwidth: 300-600 nm extended to 600-1600 nm• Angular Resolution: Diffraction-limited single dish ~0.1arcsec

resolution is needed in order to be competitive with other space missions at low orbit or in the Lagrangian Points.

• Spectral Resolution: FWHM of the spectro-polarimetric ~500pm Such as resolution could be obtained through the combination of a narrow band filter (~3-5Å) and a Fabry-Perot interferometer

• Temporal Resolution: – ~90sec are necessary to sample the photosphere and chromosphere

spectral line in his different polarization states and to characterize the related dynamics

– Heliosismology studies ~30-50s temporal sampling– Imaging 5 sec

• Weight estimation ~350kg


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WP1310 Sun ObservationCompetitors or Precursors?

• Large diameter size and high temporal resolution allow beating the forthcoming free flyers competitors (2007-2027):– SOLAR-B SOT (Solar Optical Telescope)– SDO HMI (Helioseismic and Magnetic Imager) – SOLAR ORBITER VIM (Visual Imager Magnetograph)

• A suite of solar instruments:– Imaging– Spectroscopy– Polarimetry


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WP 1320 Solar System Minor Bodies

• About 2 m Diffraction limited optical telescope

• Characterization of Inner Earth Asteroids (IEA), direct measurement of asteroid sizes, spin and shape properties, characterization of Kreuz family comets.

• Medium Priority


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Moon Advantages:

• Diffraction-limited images

• Observations of Regions at low solar elongations

• Long baseline Earth - Moon


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Why to make hi-res observations of asteroids?

• To measure their angular sizes

• To reconstruct their 3-D shapes

• To find binary systems

• To find surface heterogeneity (albedo spots)

• To investigate light scattering properties

including limb darkening

Speckle interferometry observations at TNG


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Resolving the apparent disks of asteroids leads to reconstruct the 3-D shape of the objects. Knowledge of the volume is then used to derive average density when the mass is known (from gravitational perturbations, or the presence of a satellite)

4 Vesta

(HST)


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1290 Antiope 45 Eugenia

Binary Asteroids

At present, about 24 near-Earth and 36 Main Belt asteroids are known or suspected to be binaries

Binaries are extremely important because they allow us to derive asteroid masses, and put constraints on the collisional evolution of the population.


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Asteroid families close to Earth orbit

• Atens– Average orbit < 1 AU – Perihelia < 1 AU, Afehelia > 1 AU

• Apollo– Average orbit > 1 AU – Perihelia < 1 AU, Afhelia > 1 AU

• Amors– Orbit 1.017 AU < distance < 1.17


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Solar elongations vs. Earth distanceAten objects:

< 1, Q > 0.983 AU

Large dots: Mv < 16

Medium dots: 16 < Mv < 18

Small dots: 18 < Mv < 20

Orbital evolution of 21 Atens (821 yrs). Plot of Solar elongation vs. Earth distance every 40 days.

(integrations made by Boattini and Carusi)

In addition to Atens, a new class of objects, with orbits completely inside Earth’s orbit, has been found to exist necessarily, through numerical integrations of NEO orbits. These objects have been called IEOs (objets Interior to Earth’s Orbit). Only a very few IEOs have been so far discovered, due to the difficulty of observing IEOs from ground, since they never are visible at large solar elongations. A Moon-based telescope would not be affected by such limitations.


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Numerical simulations indicate that currently active ground-based NEO surveys aimed at discovering Potentially Hazardous objects can be unable to discover in advance all the possible impactors larger than 1 km, even after 100 years of observations.

Numerical simulations indicate that most impactors are visible in advance only by observing systematically the regions of the sky within 90o from the Sun, whereas surveys hardly observe beyond this limit.

Limits of current ground-based NEO surveys


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Observations of Sun-grazing comets

Due to the lack of atmosphere, a Moon-based telescope, equipped with a solar coronograph, would be very efficient in observing Sun-grazing comets.

Sun-razing comet observed by the SOHO solar observatory


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A Moon-based telescope would nicely complement future large sky surveys, since it would permit to determine the distance of newly-discovered objects by means of measurements of the diurnal parallax (having the Earth-Moon distance as the baseline). This would be very useful for NEO-discovery surveys.


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Parallax measurements would be also extremely useful to constrain the orbits of Trans-Neptunian objects.

By observing an object as seen in quadrature from two opposite locations along the Moon’s orbit around the Earth, it should be possible to measure the parallax, and to derive the distance of the object.

This could be done in principle also from the Earth’s ground, using the Earth’s orbit diameter as the baseline and observing the same object after six months. This has never be done so far due to practical problems (telescope scheduling, etc.). A Moon-based telescope could do the same using the Moon’s orbit as a baseline and observing the same object after (about) 15 days, only.

Such parallax measurements would improve very much the computation of TNOs, that are poorly known due to their very slow motion on the sky sphere.


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WP1320 Solar System Bodies ObservationPayload Technical Specifications

• Diameter: 2m, • Focal length: >3m• Field of View: 30x30 arcsec • Bandwidth: 500-800 nm extended to

300-1000 nm• Angular Resolution: Diffraction-limited

single dish ~0.05arcsec• Spectral Resolution: Wide Filters • Weight estimation ~500kg


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WP 1330 Wide Field Telescope

• 4m to 8m Diffraction limited telescope • Survey for detection:

– Micro-lensing, – search for planetary systems through photometric

eclipses, – study of optical transient due to Gamma Ray Bursts– Search for extragalactic clusters. – Search for extragalactic Supernovae.

• Large Spectral range 0.3-2.2 micron• Field of View required (2x2-5x5 degrees)• Site: Polar Zones

– In a crater to be shielded by Solar radiation


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WP1330 Wide FieldPayload Technical Specifications

• Diameter: 4m,

• Focal length: 6m

• Field of View: 2x2 deg / 5x5 deg

• Bandwidth: 0.3 -2.2 micron

• Angular Resolution: Diffraction-limited single dish ~0.02arcsec

• Spectral Resolution: Wide Filters

• Weight estimation >1000kg


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Mid Infrared facility

• Competitors/Precursors– A mid infrared telescope to be placed on the Moon represent the

natural update of the James Webb Space Telescope (JWST)

• A thermal InfraRed telescope for Galactic Astronomy and Cosmology

• Scientific Objectives– Stellar formation in low-z Universe, ultra-luminous IR galaxies

and far-z isotopical abundances, spectroscopy “JWST” very high redshift galaxy

• High Resolution Spectroscopy necessary• Survey towards ecliptical poles to minimize thermal

background emission (Zodiacal Light)• Site: Polar Zones

– In a crater to be shielded by Solar radiation


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Mid Infrared facility

•Unique advantage with respect to free space:

•gravity

•Very long integration time

•Liquid Mirror technology already proven on Earth (6meter) will allow to build huge facility on the Moon

•Zenithal telescope

•Anionic Liquid T<150K


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Mid Infrared facility Payload Technical Specifications

• Diameter: 20m• Focal length: 30-50m• Field of View: 15’x15’ • Bandwidth: Thermal Infrared• Angular Resolution: Diffraction-limited single

dish ~0.01arcsec• Technology: liquid mirror• Spectral Resolution: high • Weight estimation 1000kg only the mirror..


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Interferometry

• Interferometry uses the unique ability of the Moon surface to provide extremely long, stable and remotely re-deployable baselines

• A few to several 1 to 2m classes telescopes and more than one recombining focal stations

• Very high spatial resolution• Compact objects studies

(Galactic center BHs, BHs in nearby Galaxies) by differential astrometry

• Site: Big (up to several km) free surface


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Priorities List

Priority 1: Imaging-Spectro-Polarimetry Solar Observation

Priority 2: Minor Bodies Solar System Observation

Priority 3: Wide Field, Mid Infrared telescope and interferometry


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Can be a precursor mission planned?

• Spectro-Polarimetry Solar Observation– Already planned Free Flyers missions

• Minor Bodies Solar System Observations– 0.5-1m robotic telescope on the Moon surface can anticipate a

fraction of the “big brother” results

• Wide Field telescope:– Difficult on the Moon, LSST on Earth

• Mid Infrared telescope:– JWST

• Interferometry– Concept can be proven on a small array of 0.2-0.5m telescopes on

short fixed baseline (30-50 m to give top results on very bright targets)


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WP1300 conclusions

Sun and Solar System observations could open the UV/optical/IR window from the Moon with leading science and reasonable projects

The other proposed cases could represent the first step toward a large facility, larger than any other expected on Earth and to be lunched in space (E-ELT, with 42m diameter, and JWST, a 6.5m), will satisfy most of any possible scientific rationale which can be conceived

Universe observation from the Moon UltraViolet, Optics and InfraRed Frascati 07/05/2007 1 WP 1300...

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