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

More documents

Recommendations

Info

• ANR Alterdetect, with IMEP : simultaneous demonstration of Lippmann spectroscopic capability using Radio then millimetric waves and Near Infrared guided optics. • ANR Nanodesir, with CEA-DRFMC : The Lippmann effect coupled supraconducting SSPD to generate a nanosystem achieving photon counting and spectroscopy is one driver to develop research on superconductivity. 136
Chapter 13 Recruitment plan GRIL needs are two-fold: researchers with instrumental skills able to fullfill key responsabilities in large projects or with research programs in specific technological fields that are at the heart of our R&D projects; engineers with a strong motivation in R&D activities and expertise in the fields that are of importance for our developments. Because of the strong commitment the LAOG has towards the VLT Planet Finder realisation and that of the VLTI 2µm imager, very likely to be scheduled soon, it is essential to increase our resources in some very specific fields of expertise in order to maintain and consolidate our R&D capabilities. For this reason, during the next quadrennal period, GRIL should either recruit or welcome external persons on the various profiles described below according to the two categories, pure instrumental profiles (GRIL recruitments) and mixed astrophysical-instrumental profiles (thematic team recruitement with participation to GRIL activities). GRIL profiles 1. Adaptive optics R&D and system Goal: Increase the LAOG capabilities in AO instrumentation. Because of our major involvement in the large PF project, most of our capabilities connected to AO expertise will be focused on the realisation of this instrument. In order to succeed in this whole pursuing our innovative R&D activities in AO, we need to increase our global capabilities in AO components R&D and/or system definition by recruiting an AO-oriented instrumentalist researcher accompaning the recruitment of an AO-dedicated project manager/system engineer (IR1). This should occur in the fall of 2006. Target: 2007 or 2008 2. Nulling interferometry at thermal IR wavelengths Goal: Preparation studies for Darwin. In parallel and support to R&D on thermal IR guiding optics, such as IODA and other possible studies in preparation for DARWIN, we have identified the need for a researcher strongly dedicated to the search for planets in MIR in general and personally involved in the preparation of DARWIN or precursor missions. He would have to pilot the preparatory studies that LAOG is performing and possibly going to enlarge in the frame of its pluriannual commitment to ESA and ALCATEL ALENIA partnership. Target: 2007 3. JMMC support for 4-6T exploitation Goal: Participation to the JMMC developments supporting the VLTI evolution toward more than 3 beams. LAOG has a special role in the JMMC since it harbors the coordination center and some key members of the working groups. Because of its probable involvement in a second generation instrument, it should also help in developing the dedicated tools for the VLTI exploitation. Target: 2008 It should be noted that these profiles might evolve according to the actual profile of the MdC who should be recruited in section 34 or any other recruitment possibly achieved in 2006. 137
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 118 and 119: Figure 11.2: NAOS-CONICA image of t
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 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?