Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

More documents

Recommendations

Info

Figure 11.2: NAOS-CONICA image of the double star GJ 263 for which the angular distance between the two components is only 0.030 arcsec. The raw image, as directly recorded by CONICA, is shown in the middle, with a computer-processed (using the ONERA MISTRAL myopic deconvolution algorithm) version to the right. The recorded Point-Spread-Function (PSF) is shown to the left. The CONICA pixel scale of 0.01325 arcsec/pixel was used with the FeII filter (1.257 µm). The exposure time was 10 seconds. This image was obtained during the NAOS/CONICA commissioning run in November 2003. Following presentations of the results of our phase A study to an ESO-appointed Review Board in December 2004 and to the ESO Scientific and Technical Committee in April 2005, our proposal has been recommended for phase B. We are currently preparing the contract for this phase B with ESO and also considering the possibility to include members of the competing team in order to broaden the capabilities of the Planet Finder instrument. First light of the Planet Finder is foreseen to occur by end of 2009 or beginning of 2010. 11.1.3 Instrumental Research and development activities DEFORMABLE MICRO-MIRRORS The LAOG R&D activities in adaptive optics are focused on the development of new deformable mirrors for the next generation of AO systems. The goal is two-fold: i/ obtain smaller and cheaper mirrors for astronomical applications such as AO systems for interferometry, Multi-Object Adaptive Optics (MOAO) systems, etc., or for non astronomical applications like ophthalmology, laser beam shaping, telecommunications; ii/ manufacture mirrors with several thousands actuators for astronomical applications in the fields of eXtreme AO, AO systems for the Extremely Large Telescopes (ELT), etc. These innovative works lead to three patents and two technology transfer during the 2001-2005 period (see 14.3). Magnetic deformable mirrors This technology is particularly well adapted to the production of low order, large stroke mirrors, therefore allowing to correct all wavefront errors without the need for the usual second tiptilt stage. These mirrors will for instance be used for interferometry, MOAO, ophthalmology, laser beam shaping, etc. We have already produced several 52-actuator devices (Figure 11.3), including their control electronics, and we are now offering these devices through two commercial partners (see below and in section 14.3). Further developments are considered in order to increase the number of actuators up to 400. The typical characteristics of these mirrors are given below: • the minimum actuator step is 2 mm with the current technology • the typical best-flat surface is ∼ 5 nm RMS (mirror surface) • typical strokes for the low order modes range from 10 to 15 µm (possibly up to 100 µm) • the linearity remains below 2% for large strokes (below 1% for +/- 5 µm stroke) 118
Figure 11.3: Left: the first 52-actuators magnetic deformable mirror prototype. Right: the MEMS-based electrostatic deformable mirror prototype • there is no measurable hysteresis • the mirrors can be used in systems with a typical rejection bandwidth of 100 to 200 Hz • standard coatings such as protected silver can be applied on the mirror membrane Electrostatic deformable mirrors The second technology is based on MEMS (Micro Electro Mechanical System) technology. It is first targeted at high performance applications needing a very large number of actuators, but we keep it compatible with potentially high volume applications such as ophthalmology. This compatibility allows us to use high-end manufacturing facility at CEA-LETI, that would otherwise be inaccessible. The current prototype, based on a novel (patented) actuator concept is being tested at LAOG. It already shows unique features, such as a large stroke (5 µm) with a truly continuous optical surface. This development is now being funded by EC as a specific OPTICON JRA1 workpakage, led by LAOG. Our goal is to provide a 2000-actuator deformable mirror by the end of 2007. Industrial development These innovative works led to three patents and two technology transfers during the 2001-2005 period (see the details in 14.3). The production and selling tasks of MMD have been transfered to two dedicated companies (FLORALIS for astronomical applications and Imagine Eyes for all other applications under specific licensing contracts, allowing LAOG to keep focused only on the very R&D, be it for components only until now or possibly extended to the full system later. OTHER TASKS Laboratory test bench As part of the prototyping efforts during the Planet Finder Phase A study, a simple adaptive optics test bench has been set-up at LAOG to validate various new control concepts. For instance the possibility to fully servo the position of the instrument pupil using only the data from the Schack-Hartman wavefront has been demonstrated (G. Montagnier, master thesis) using this test bench. These experimental validations were conducted in collaboration with our colleagues from ONERA (T. Fusco and M. Nicolle). Integral Field Spectroscopy with Adaptive Optics The research is progressing on the instrumental issues of the coupling of Integral Field Spectroscopy (IFS) with adaptive optics. This field of research was initiated at LAOG in 1994 with one of the first IFS instruments used with AO (GraF spectrograph successfully used with the ADONIS at the ESO 3.6m telescope 3 ) and pursued with the implementation of the GriF mode 3 Chalabaev, A.; Le Coarer, E.; Rabou, P.; Magnard, Y.; Petmezakis, P.; Le Mignant, D., 2002; The GraF instrument for Imaging Spectroscopy with the Adaptive Optics, Experimental Astronomy, 2002, 14, 147 119
Page 3:
LABORATOIRE D’ASTROPHYSIQUE DE GR
Page 6 and 7:
III Team ASTROMOL 41 2 Presentation
Page 8 and 9:
8.1.3 Graduate Students . . . . . .
Page 10 and 11:
VI Team SHERPA 145 15 Results 147 1
Page 13:
Part I Foreword: Presentation of th
Page 17:
Part II Executive Summary A 18th ce
Page 20 and 21:
of CNRS for technicians and enginee
Page 22 and 23:
Figure 1.3: New LAOG organigram (20
Page 24 and 25:
heart attack. Manuel went back to t
Page 26 and 27:
Figure 1.6: PhD student repartition
Page 28 and 29:
• LAOG researchers (and publishin
Page 30 and 31:
and published 95 papers in four yea
Page 32 and 33:
• National astronomy programs. 4
Page 34 and 35:
1.5 From dreams to reality: Human r
Page 36 and 37:
and accretion disks with heavy nume
Page 38 and 39:
emphasis on the chemistry of planet
Page 41:
Part III TEAM ASTROMOL Sub-arcsecon
Page 44 and 45:
• we develop quantum and classica
Page 46 and 47:
Table shows not only the volume of
Page 48 and 49:
• Herschel-HIFI: Astromol is invo
Page 50 and 51:
particular, we calculated a 9D H2O-
Page 52 and 53:
• The hot corinos. More spectacul
Page 54 and 55:
the massive deeply embedded protost
Page 56 and 57:
tens of visual magnitudes, hence pr
Page 58 and 59:
quantum VCC-IOS approximation may f
Page 60 and 61:
Rate constant (cm 3 s -1 ) 1e-09 1e
Page 62 and 63:
• One of us (PV) is strongly invo
Page 64 and 65:
sublimation of water ice trapped ei
Page 66 and 67:
If the chemistry in the first phase
Page 68 and 69: 4.2.2 Molecular Physics The theoret
Page 70 and 71: Source Herschel Time Astromol Class
Page 72 and 73: several important studies that anti
Page 74 and 75: Chapter 5 Selected Publications •
Page 77: Part IV TEAM FOST The first image o
Page 80 and 81: 393254 (5MJup at 55 AU) & AB Pic (1
Page 82 and 83: 2.2 µ m 0.5" 11.7 µ m Figure 6.1:
Page 84 and 85: Figure 6.3: Contribution of heating
Page 86 and 87: such mid-term (several weeks) magne
Page 88 and 89: systems: HD 141569, HD 32297, HD 18
Page 90 and 91: C2D Spitzer/IRAC and MIPS data of s
Page 92 and 93: et al. 2002; 2003). We have found t
Page 94 and 95: Figure 6.8: Distribution of separat
Page 96 and 97: with only three known to date. Most
Page 98 and 99: 300 objects, a size sufficient for
Page 100 and 101: therefore no surprise that vast eff
Page 102 and 103: data to verify the predictions we a
Page 104 and 105: Chapter 8 Appendices 8.1 Members of
Page 106 and 107: 106
Page 108 and 109: 108
Page 110 and 111: equipments for these tasks, from de
Page 112 and 113: 10.1.3 Current trend of large equip
Page 114 and 115: • Improving High Angular Resoluti
Page 116 and 117: Chapter 11 Results 11.1 Towards hig
Page 120 and 121: on PUEO at CFHT. The IFS experts (A
Page 122 and 123: Figure 11.5: Image of the binary st
Page 124 and 125: Figure 11.7: PICNIC low noise infra
Page 126 and 127: have taken responsibilities: A. Che
Page 128 and 129: Figure 11.10: thermal modeling of W
Page 130 and 131: Figure 12.1: All the GRIL projects
Page 132 and 133: 12.2 Optical interferometry As for
Page 134 and 135: the VLTI. CHARA is equipped with an
Page 136 and 137: • ANR Alterdetect, with IMEP : si
Page 138 and 139: Mixed GRIL-other team profiles 1. A
Page 140 and 141: Name Grade Comm. Project Berger Jea
Page 142 and 143: • First fringes in the H band wit
Page 144 and 145: 144
Page 146 and 147: 146
Page 148 and 149: Table 15.1: List of the permanent S
Page 150 and 151: 15.4 Transport phenomena in accreti
Page 152 and 153: Figure 15.2: Spectral energy distri
Page 154 and 155: states, combining a still powerful
Page 156 and 157: Excitation of turbulence by Cosmic
Page 158 and 159: Table 15.2: Former PhD students of
Page 160 and 161: Chapter 16 Perspectives The distinc
Page 162 and 163: Ray background. The second project
Page 164 and 165: 164
Page 166 and 167: - Ceccarelli Cecilia (AT) - Delfoss
Page 168 and 169:
Among the various areas of expertis
Page 170 and 171:
-responsable du groupe ”logiciel
Page 172 and 173:
Chef de l’ Equipe ASTROMOL du LAO
Page 174 and 175:
jury de concours: 1 concours IR CNR
Page 176 and 177:
Chapter 20 Appendix 4: The Jean Mar
Page 178 and 179:
20.7 Production informatique ¡¢£
Page 180 and 181:
20.10 Formation des utilisateurs La
Page 182 and 183:
20.13 Darwin ¡¢£¤¥¦§¨©�
show all

Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

Create successful ePaper yourself

Delete template?

Save as template?