OU3 is one of the six Operating Units of the Progetto Premiale T-REX. It is focused on the development of adaptive optics instrumentation for the European Extremely Large Telescope. The main activities of OU3 are the MAORY adaptive optics module, the MICADO infrared camera, the characterisation and forecast of atmospheric parameters for the E-ELT site and general developments for future adaptive optics systems. <P /

Abicca, R.

AGAPITO, GUIDO

Antichi, J.

ARCIDIACONO, CARMELO

BARUFFOLO, Andrea

BELLAZZINI, Michele

BERGOMI, Maria

Bregoli, G.

Butler, R. C.

CASCONE, Enrico

Cavazzani, S.

CILIEGI, Paolo

CORTECCHIA, Fausto

Cosentino, G.

DE CAPRIO, VINCENZO

DE ROSA, ADRIANO GIUSEPPE

DI RICO, Gianluca

DIMA, MARCO

DIOLAITI, EMILIANO

ESPOSITO, Simone

Falomo, R.

FANTINEL, Daniela

FARINATO, JACOPO

Fini, L.

FOPPIANI, ITALO

Giordano, C.

GIRO, Enrico

Greggio, L.

GULLIEUSZIK, MARCO

Lascaux, F.

LOMBINI, MATTEO

MAGRIN, DEMETRIO

Malaguti, G.

Marafatto, L.

MASCIADRI, ELENA

MORGANTE, GIANLUCA

Ortolani, S.

Paiano, S.

Patru, F.

Patti, Mauro

PORCEDDU, Ignazio Enrico Pietro

PORTALURI, ELISA

RAGAZZONI, Roberto

RICCARDI, Armando

RICCIARDI, SARA

RIVA, Marco

SALASNICH, Bernardo

SCHREIBER, LAURA

Spanò, P.

TURCHI, ALESSIO

USLENGHI, MICHELA

VIOTTO, VALENTINA

ZAGGIA, Simone

Zerbi, F. M.

Zitelli, V.

OA@INAF - Istituto Nazionale di Astrofisica

2015Publication Year2020-03-18T16:51:49ZAcceptance in OA@INAFT-REX Operating Unit 3TitleDIOLAITI, EMILIANO; Abicca, R.; AGAPITO, GUIDO; Antichi, J.; ARCIDIACONO, CARMELO; et al.Authorshttp://hdl.handle.net/20.500.12386/23371HandleMEMORIE DELLA SOCIETA ASTRONOMICA ITALIANAJournal86NumberMem. S.A.It. Vol. 86, 428c© SAIt 2015 Memorie dellaT-REX Operating Unit 3E. Diolaiti1, R. Abicca1, G. Agapito2, J. Antichi2, C. Arcidiacono1, A. Baruffolo3,M. Bellazzini1, M. Bergomi3, G. Bregoli1, R.C. Butler4, E. Cascone5, S. Cavazzani3,P. Ciliegi1, F. Cortecchia1, G. Cosentino6, V. De Caprio5, A. De Rosa4, G. Di Rico2,M. Dima3, S. Esposito2, R. Falomo3, D. Fantinel3, J. Farinato3, L. Fini2, I. Foppiani1,C. Giordano2, E. Giro3, L. Greggio3, M. Gullieuszik3, F. Lascaux2, M. Lombini1,D. Magrin3, G. Malaguti4, L. Marafatto3, E. Masciadri2, G. Morgante4, S. Ortolani7,S. Paiano3, F. Patru2, M. Patti1,6, I. Porceddu8, E. Portaluri3, R. Ragazzoni3,A. Riccardi2, S. Ricciardi4, M. Riva9, B. Salasnich3, L. Schreiber1, P. Spanò2,A. Turchi2, M. Uslenghi10, V. Viotto3, S. Zaggia3, F.M. Zerbi11, and V. Zitelli11 INAF-OABO, Via Ranzani 1, I-40127 Bologna, Italy2 INAF-Arcetri, L.go E. Fermi 5, I-50125 Firenze, Italy3 INAF-OAPD, Vicolo Osservatorio 5, I-35122 Padova, Italy4 INAF-IASFBO, Via Gobetti 101, I-40129 Bologna, Italy5 INAF-NA, Salita Moiariello 16, I-80131 Napoli, Italy6 Univ. di Bologna, Dip. di Fisica e Astronomia, V.le Berti Pichat 6/2 I-40127 Bologna,Italy7 Univ. di Padova, Dip. di Fisica e Astronomia, Via Marzolo 8, I-35131 Padova, Italy8 INAF-OA Cagliari, Via della Scienza 5, I-09047 Selargius (CA), Italy9 INAF-Brera, Via E. Bianchi 46, I-23807 Merate (LC), Italy10 INAF-IASF Milano, Via Bassini 15, I-20133 Milano, Italy11 INAF, Viale del Parco Mellini 84, I-00136 Roma, ItalyAbstract. OU3 is one of the six Operating Units of the Progetto Premiale T-REX. It isfocused on the development of adaptive optics instrumentation for the European ExtremelyLarge Telescope. The main activities of OU3 are the MAORY adaptive optics module, theMICADO infrared camera, the characterisation and forecast of atmospheric parameters forthe E-ELT site and general developments for future adaptive optics systems.Key words. Technology: adaptive optics – Telescopes: E-ELT1. IntroductionThe MAORY adaptive optics module and theMICADO infrared camera form part of thefirst light instrument suite for the EuropeanExtremely Large Telescope (E-ELT) (Tamai2014, 2015). These two instruments have beenapproved for construction (Ramsay et al.Diolaiti: T-REX OU3 4292014) and the phase B of the respectiveprojects is expected to start soon at the momentof this writing. INAF is the lead institute ofthe MAORY instrument project and is involvedin the MICADO instrument project. MAORYand MICADO were the core activity of theOperating Unit 3 (OU3) of T-REX in its firstyear. In the second year of T-REX the scopeof work of OU3 was extended to include twomore activities: forecast of atmospheric param-eters and development of new technologies forwide-field adaptive optics.This introductory paper contains anoverview of the activities which have beensupported by OU3. The interested reader willfind more details in the specific contributionspresented in this Conference.2. MAORYMAORY (Diolaiti et al. 2014) is a post-focaladaptive optics module for the E-ELT. It offerstwo adaptive optics modes to support theMICADO near-infrared camera (Davies etal. 2010): Multi-Conjugate Adaptive Optics(MCAO) and Single-Conjugate AdaptiveOptics (SCAO). In the MCAO mode, MAORYuses the adaptive mirror M4 and tip-tilt mirrorM5 in the telescope and up to two post-focaladaptive mirrors in the module itself to achievehigh performance with excellent uniformityof the point spread function across the fieldof view; wavefront sensing is performedby a suite of up to six Laser Guide Stars(LGS) and three Natural Guide Stars (NGS),ensuring high sky coverage. In the SCAOmode, MAORY uses only the telescope’s M4and M5 and a single NGS SCAO wavefrontsensor to achieve excellent performance on anarrow field of view around the NGS itself. Inboth modes wavefront sensing is performedin closed-loop fashion with optical feedbackfrom the sensors to the deformable mirrors.Support from T-REX has been essential fordefining a number of programmatic and techni-cal aspects of the MAORY instrument projectin preparation for phase B. These activities andachievements are summarised below.The MAORY consortium has been consol-idated and is now in its final configuration. Itconsists of three partner organisations: INAF(Italy), INSU-IPAG (France) and ESO. INAFis the lead institute, bearing responsibility forthe system development, for its delivery toESO and for several sub-systems, includingthe instrument platform and, among the adap-tive optics sub-systems, the optical relay withadaptive mirrors, the NGS and SCAO wave-front sensor, the real-time computer. IPAG isresponsible for the development and deliveryof the LGS wavefront sensor sub-system. ESOis responsible for the supply of componentsand tools, i.e. wavefront sensor cameras, com-mon specifications and toolkit for the real-timecomputer development, software simulator ofthe telescope control system.The technological choice for the adaptivemirrors in MAORY has been changed sincephase A. The current design is based on voice-coil motor actuator adaptive mirrors (Biasi etal. 2010). This technology has been chosen forits high technology readiness level and recog-nised performance. Considering that the sametechnology has been adopted by ESO for thetelescope M4, commonalities are possible andwill be exploited as much as possible. An in-dustrial study on the MAORY adaptive mir-rors, fully funded by T-REX, will be launchedin parallel to the MAORY project phase B.The optical design of MAORY has beenchanged (Lombini et al. 2014) in order to takeinto account the new choice of adaptive mirrorsand new telescope interfaces. The instrument islocated on the telescope straight-through focuson the Nasmyth platform. The optical relay in-side MAORY forms a 1-to-1 image of the tele-scope focal plane. The exit port for MICADOis gravity invariant. A second gravity invariantport is also provided for an instrument to bedefined yet. The optical relay design containstwo identical voice coil adaptive mirrors; thetrade-off between flat and curved shape is stillin progress. The current status of the opticaldesign has been presented in this Conferenceby Lombini et al. (2015).The NGS wavefront sensor is an essentialcomplement to the LGS wavefront sensor inthe MCAO mode. The NGS wavefront sensorrequires three natural stars, even very faint, tobe found over a technical field of view of 160430 Diolaiti: T-REX OU3arcsec. In order to implement the above men-tioned SCAO mode of MAORY, a fourth spe-cialised wavefront sensor has been added in thedesign volume allocated to the NGS wavefrontsensor, in the framework of a joint develop-ment between the MICADO and MAORY con-sortia. Recent work on the MAORY NGS andSCAO wavefront sensor has been shown in thisConference by Esposito et al. (2015).An end-to-end simulation code is under de-velopment (Arcidiacono et al. 2014; Schreiberet al. 2015): it is an essential tool for the adap-tive optics system modelling and design. Thecode has modular structure and relies on theuse of Graphic Processing Units to speed upthe time demanding parts of the simulations.Specific functions are available for detailedmodelling of the sodium layer where the LGSsare generated (Schreiber et al. 2014a). Thecode allows the user to choose between twosimulation modes: accurate mode, for detailedmodelling, and fast mode, which is useful forexploring the parameter space or for statisticalcalculations such as sky coverage evaluation.To provide experimental support to numericalsimulations, a reduced-scale laboratory proto-type of the MAORY wavefront sensing systemhas been developed (Patti et al. 2015), offeringthe possibility to emulate realistic LGS imagesunder different working conditions.A complex and big instrument as MAORYrequires special facilities for its integration.The selected assembly hall is an existing lab-oratory at IASF-Bologna, one of the INAF in-stitutes involved in the project. The hall hassuitable size and is under remodelling to beadapted to the needs of the MAORY project.The design of the civil works has been com-pleted and the necessary authorisations by pub-lic offices have been obtained. The contract forthe civil works is expected to be awarded inthe next few months and the works themselvesare expected to be completed well in advancebefore the start of the instrument integration.Tools and equipment have also been purchasedto support the instrument integration. A sec-ond laboratory is under remodelling at INAFOsservatorio Astrofisico di Arcetri for the inte-gration of the NGS and SCAO wavefront sen-sor sub-system.3. MICADOThe participation of INAF in the MICADO in-strument project is mainly related to the defini-tion of the instrument science cases. The mainscience cases investigated by the INAF teamare related to the study of the stellar popula-tion of nearby and high redshift galaxies withELTs. The study has been carried out by sim-ulation of E-ELT observations, taking into ac-count the expected performance of the E-ELT- MAORY - MICADO system, and by analy-sis of the simulated images by standard photo-metric analysis methods to assess the feasibil-ity of the science cases. The interested readermay find detailed descriptions of the sciencecases which have been analysed and of the re-sults in Greggio et al. (2012), Gullieuszik etal. (2014), Schreiber et al. (2014b) and in thecontribution by Gullieuszik et al. (2015) in thisVolume.4. Atmospheric parametersEvaluation and forecast of atmospheric condi-tions are essential elements for planning scien-tific observations. Two different concepts havebeen studied in OU3. The first concept is basedon the use of a meso-scale atmospheric modelfor the forecast of optical turbulence and atmo-spheric parameters. The final goal of this studyis the implementation of an automatic forecastsystem to be installed at the E-ELT site. Resultscan be found in Lascaux et al. (2014) andMasciadri et al. (2015). The second conceptrelies on the use of multi-wavelength satelliteobservations of the Earth for the forecast of thecould cover and of the photometric quality ofthe sky. Results are presented in Cavazzani etal. (2014). A further extension of this methodis under study for the forecast of the turbulencestrength accordingly to a step-wise scale suchas strong-regular-quiet.5. Technology developments foradaptive opticsThe development of new technologies foradaptive optics within OU3 has been mainlyfocused on Global Multi-Conjugate AdaptiveDiolaiti: T-REX OU3 431Optics (GMCAO). In the GMCAO approach,wavefront sensing is performed by naturalstars. In order to achieve high sky coverage,the stars have to be searched on a wide fieldof view at the telescope focal plane, whichcorresponds to the entrance focal plane of apost-focal module such as MAORY: relayingthe same focal plane at the exit port of thepost-focal module would be extremely diffi-cult for optical design reasons. The shape ofthe post-focal adaptive mirrors, which are notseen by the wavefront sensor, is monitored byfast metrology. Description of the GMCAO ap-proach and preliminary results of the simula-tions can be found in Viotto et al. (2014) andRagazzoni (2015).6. ConclusionsSupport by T-REX to the E-ELT activities atINAF has been essential. In the frameworkof OU3, T-REX has funded general expenses,13 grants for young researchers and 1 PhDgrant and, in the specific case of the MAORYproject, T-REX has allowed INAF to set up thefacilities for the instrument integration and tosupport the instrument design.Acknowledgements. This work has been supportedby the Italian Ministry for Education University andResearch (MIUR) under grants Progetto PremialeE-ELT 2011 and Progetto Premiale E-ELT 2012.Thanks are due to Philippe Feautrier (IPAG) andhis team for their contribution to the MAORYproject. E.D. would like to thank Mark Casali andJason Spyromilio for useful discussions during theConference.ReferencesArcidiacono, C., et al. 2014, Proc. SPIE, 9148,91486FBiasi, R., et al. 2010, Proc. SPIE, 7736,77362BCavazzani, S., Ortolani, S., & Zitelli, V. 2014,MNRAS, 452, 2185Davies, R., I., et al. 2010, Proc. SPIE, 7735,77352ADiolaiti, E., et al. 2014, Proc. SPIE, 9148,91480YEsposito, S., et al. 2015, MmSAI, 86, 446Greggio, L., et al. 2012, PASP, 124, 653Gullieuszik, M. et al. 2014, A&A, 568, A89Gullieuszik, M., et al. 2015, MmSAI, 86, 458Lascaux, F., Masciadri, E., & Fini, L. 2014,Proc. SPIE, 9148, 914865Lombini, M., & Diolaiti, E., & De Rosa, A.2014, Proc. SPIE, 9148, 91486KLombini, M., & Diolaiti, E. 2015, MmSAI, 86,432Masciadri, E., et al. 2015, MmSAI, 86, 454Patti, M. et al. 2015, MmSAI, 86, 441Ragazzoni, R. 2015, MmSAI, 86, 450Ramsay, S., K., et al. 2014, Proc. SPIE, 9147,91471ZSchreiber, L., et al. 2014a, Proc. SPIE, 9148,91486QSchreiber, L., et al. 2014b, MNRAS, 437, 2966Schreiber, L. et al. 2015, MmSAI, 86, 436Tamai, R., & Spyromilio, J. 2014, Proc. SPIE,9145, 91451ETamai, R. 2015, this ConferenceViotto, V., et al. 2014, Proc. SPIE, 9148,91486H

T-REX Operating Unit 3

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T-REX Operating Unit 3

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