The E-ELT program status

Tamai, Roberto; Cirasuolo, M.; González, Juan Carlos; Koehler, Bertrand; Tuti, Mauro

doi:10.1117/12.2232690

Cited by 25 publications

(14 citation statements)

References 7 publications

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“…An observatory like SPICA as presented in this paper, with a large, cold telescope complemented by an instrument suite that exploits the sensitivity attainable with the low thermal background, can in the mid/far-infrared achieve a gain of over two orders of magnitude in spectroscopic sensitivity as compared to Herschel, Spitzer and SOFIA (Becklin et al, 2016, see also Figure 4). In addition such a mission will provide access to wavelengths well beyond those accessible with the James Webb Space Telescope (JWST Gardner et al, 2006) and the new generation of extremely large telescopess (Tamai et al, 2016;McCarthy et al, 2016;Cohen, 2016). Sitting squarely between JWST and ALMA (Wootten & Thompson, 2009), SPICA will enable the discovery and detailed study of the coldest bodies in our Solar System, emerging planetary systems in the Galaxy, and the earliest star forming galaxies and growing super-massive black holes -a gigantic leap in capabilities for unveiling the 'hidden Universe'.…”

Section: The Power Of Infrared Diagnosticsmentioning

confidence: 99%

SPICA—A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

Roelfsema

Shibai

Armus

et al. 2018

Publ. Astron. Soc. Aust.

102

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Measurements in the infrared wavelength domain allow us to assess directly the physical state and energy balance of cool matter in space, thus enabling the detailed study of the various processes that govern the formation and early evolution of stars and planetary systems in the Milky Way and of galaxies over cosmic time. Previous infrared missions, from IRAS to Herschel, have revealed a great deal about the obscured Universe, but sensitivity has been limited because up to now it has not been possible to fly a telescope that is both large and cold. Such a facility is essential to address key astrophysical questions, especially concerning galaxy evolution and the development of planetary systems.SPICA is a mission concept aimed at taking the next step in mid-and far-infrared observational capability by combining a large and cold telescope with instruments employing state-of-the-art ultrasensitive detectors. The mission concept foresees a 2.5-meter diameter telescope cooled to below 8 K. Rather than using liquid cryogen, a combination of passive cooling and mechanical coolers will be used to cool both the telescope and the instruments. With cooling not dependent on a limited cryogen supply, the mission lifetime can extend significantly beyond the required three years. The combination of low telescope background and instruments with state-of-the-art detectors means that SPICA can provide a huge advance on the capabilities of previous missions.The SPICA instrument complement offers spectral resolving power ranging from R ∼50 through 11000 in the 17-230 µm domain as well as R ∼28.000 spectroscopy between 12 and 18 µm. Additionally SPICA will be capable of efficient 30-37 µm broad band mapping, and small field spectroscopic and polarimetric imaging in the 100-350 µm range. SPICA will enable far infrared spectroscopy with an unprecedented sensitivity of ∼ 5 × 10 −20 W/m 2 (5σ/1hr) -at least two orders of magnitude improvement over what has been attained to date. With this exceptional leap in performance, new domains in infrared astronomy will become accessible, allowing us, for example, to unravel definitively galaxy evolution and metal production over cosmic time, to study dust formation and evolution from very early epochs onwards, and to trace the formation history of planetary systems.

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Section: The Power Of Infrared Diagnosticsmentioning

confidence: 99%

SPICA—A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

Roelfsema

Shibai

Armus

et al. 2018

Publ. Astron. Soc. Aust.

102

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“…This solution, which naturally scales with the size, positions, rotation and number of segments comprising the mirror, is versatile per se. On the contrary to numerical solutions, the analytical expressions are independent from the physical size of the pupil and can be applied on small deformable mirrors [12,13] as well as on future large optical telescopes [10,11] without loss of precision in the decomposition.. While numerical methods require computational and memory cost which can be impressive, our analytical solution allows extremely quick results whatever the pupil complexity.…”

Section: Introductionmentioning

confidence: 99%

Analytical decomposition of Zernike and hexagonal modes over a hexagonal segmented optical aperture

Janin-Potiron¹,

Martínez²,

Carbillet³

2018

OSA Continuum

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Zernike polynomials are widely used to describe common optical aberrations of a wavefront as they are well suited to the circular geometry of various optical apertures. Non-conventional optical systems, such as future large optical telescopes with highly segmented primary mirrors or advanced wavefront control devices using segmented mirror membrane facesheets, exhibit an hexagonal geometry, making the hexagonal orthogonal polynomials a valued basis. Cost-benefit trade-off study for deriving practical upper limit in e.g., polishing, phasing, alignment, and stability of hexagons imposes analytical calculation to avoid time-consuming end-to-end simulations, and for the sake of exactness. Zernike decomposition over an hexagonal segmented optical aperture is important to include global modes over the pupil into the error budget. However, numerically calculated Zernike decomposition is not optimal due to the discontinuities at the segment boundaries that result in imperfect hexagon sampling. In this paper, we present a novel approach for a rigorous Zernike and hexagonal modes decomposition adapted to hexagonal segmented pupils by means of analytical calculations. By contrast to numerical approaches that are dependent on the sampling of the segment, the decomposition expressed analytically only relies on the number and positions of segments comprising the pupil. Our analytical method allows extremely quick results minimizing computational and memory costs. Further, the proposed formulae can be applied independently from the geometrical architecture of segmented optical apertures. Consequently, the method is universal and versatile per se. For instance, this work finds applications in optical metrology and active correction of phase aberrations. In modern astronomy with extremely large telescopes, it can contribute to sophisticated analytical specification of the contrast in the focal plane in presence of aberrations.

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“…MAORY [1] is one of the approved first-light instruments for the European Extremely Large Telescope (ELT) [2] [3] . It is an adaptive optics module, enabling high-angular resolution observations in the near infrared by real-time compensation of the wavefront distortions due to the atmospheric turbulence and other disturbances such as the wind action on the telescope.…”

Section: Introductionmentioning

confidence: 99%

On the road to the Preliminary Design Review of the MAORY adaptive optics module for ELT

Diolaiti¹

2017

Proceedings of the Adaptive Optics for Extremely Large Telescopes 5

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The E-ELT program status

Cited by 25 publications

References 7 publications

SPICA—A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

SPICA—A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

Analytical decomposition of Zernike and hexagonal modes over a hexagonal segmented optical aperture

On the road to the Preliminary Design Review of the MAORY adaptive optics module for ELT

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