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

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heart attack. Manuel went back to this topic after his well-known work on pre-main sequence (PMS) stellar evolution. This challenge was all the more formidable that, contrary to PMS stars which draw their energy only from gravitation, the late stages of stellar evolution involve a highly complex network of nuclear reactions. His main legacy is the Starevol code, which is publicly available on the web and is now widely used by the stellar evolution community worldwide. In addition to his time-consuming high-level responsibilities at UJF, Manuel was a whole scientific team in himself, although he was on his way to build a real one with a PhD student (see Siess and Leclair 2005); when he passed away, however, there was no one to continue this activity at LAOG. (Fortunately, the field is continuing, chiefly under Manuel’s former PhD student Lionel Siess, now a Professor in Marcel Arnould’s group in Brussels.) The proceedings of an international scientific colloquium held at LAOG in 2004 “Stars and Nuclei: a Tribute to Manuel Forestini” is in preparation (EDP Sciences, edited by T. Montmerle and C. Kahane). Ancient Astronomy One must also mention the work of C. Nozières on History of ancient Astronomy (Michel-Nozières 2002). She is studying in the original Assyrian language, old astronomical texts on the measurement of the variation of lunar visibility through the year. 1.1.3 A brief overview of the scientific teams of LAOG We here give a brief “identity card” of each team. The following parts of this report (III to VI) will be devoted to a much more detailed, individual account of their recent activities and prospective. • The first axis (Origins: low-mass star formation and early evolution, and the path to planet formation), is shared by all four teams. In alphabetical order: (i) the “Astromol” (= molecular astrophysics) team mainly studies the physico-chemistry of the earliest stages of star formation (molecular clouds, prestellar cores, protostars, and also young disks and molecular outflows; timescale ∼ 10 5 − 10 6 yrs), but also includes fundamental astrochemistry (reaction rates, transition probabilities, etc.). Permanent staff: 10. PhDs completed: 2; underway: 2. Team leader: C. Ceccarelli (Astronomer). (ii) the “FOST” (= star and planet formation, brown dwarfs) team focuses on later stages of star formation, mainly the physics of star-disk interactions, evolved disks and the conditions for planet formation (structural features like gaps and rings, dust grain evolution in disks, etc.; timescale ∼ 10 6 −10 7 yrs), and also on the formation mechanisms of binaries and the “Initial Mas Function” (IMF). A specific activity within the team is the study of brown dwarfs, both as astronomical objects by themselves, and as intermediate bodies between low-mass stars and exoplanets. The search and characterization of exoplanets are themselves an increasing part of the FOST activities. The team contributes a lot to observations made with LAOG-built instruments and to their interpretation. Permanent staff: 13 + 7 shared with GRIL. PhDs completed: 5 + 1 with GRIL; underway: 9 + 3 with GRIL + 1 with Sherpas. Team leader: F. Ménard (CNRS). (iii) the “GRIL” (= instrumental research group at LAOG) team concentrates on strategic issues in research & development (R&D) for future instruments and detectors. While the situation may evolve, so far GRIL’s responsibility has been to contribute to the development of optical and near-IR instruments for large ground-based telescopes (ESO, CFH) with the highest spatial resolution (for instance with the goal to resolve the inner parts of protoplanetary disks, i.e., within 1 AU at 450 pc, say), by way of adaptive optics and interferometry, and/or the highest dynamic range (adaptive optics to image exoplanets as closely as possible from their host star). Permanent staff: 9 (including 8 engineers) + 7 shared with FOST. 1 PhDs completed: 3 + 1 with FOST; underway: 8 + 3 with FOST. Team leader: C. Perrier (Astronomer). (iv) the “Sherpas” (= “sources of high energies and relativistic physics in accretion-ejection structures”, in full) team is essentially involved in MHD theory calculations, with particular emphasis on the accretion-ejection phenomenon in astrophysics. Here it mainly applies models to star-disk interactions and disk-driven jets, where magnetic fields, instead of gravitation, play a dominant role. 1 two engineers qualified to supervised PhDs (’HDR’ in french) 24
Permanent staff: 7. PhDs completed: 2; underway: 2 + 1 with FOST. Team leader: G. Pelletier (UJF Professor). • The second axis (High energies and astrophysical plasmas: the accretion-ejection phenomenon and its implications for astroparticle physics) is specific to Sherpas team. The team studies the accretion-ejection phenomenon, here in the context of compact X-ray binaries and AGNs (“two-fluid jets”), where gravitation (in addition to magnetic fields) plays a dominant role, and also fundamental research on accretion disk transport and jet stability, as well as cosmic-ray acceleration to ultra-high energies (UHE) by relativistic shock waves. The Sherpas team is actively involved in the HESS European collaboration, which operates an array of ˘ Cerenkov telescopes in Namibia with the capability to detect very high-energy γ-rays (≥ 10 12 eV). • The third axis (Instrumental research in the field of high angular resolution and high dynamic range for large telescopes), is specific to GRIL. Because of the current wavelength range, there are significant interactions with the FOST (young stars) and Sherpas (AGNs) teams, but nothing in principle prevents GRIL to get LAOG involved in mm and/or high-energy instrumentation at the initiative of Astromol or Sherpas (there are currently no such projects however.) Note that once an instrument reaches the actual building stage, it leaves GRIL and becomes a “project” of the technical group, headed by P. Kern. GRIL is also in charge of helping decide strategic orientations of LAOG for the long-term future, like contributing to ELTs (extremely large telescopes), interferometric developments in Antarctica at Dome C, or future space missions (e.g., Darwin, ESA, > 2015). (These questions will be expanded below.) 1.1.4 Studentship at LAOG Students have always been a large component of LAOG personnel. On average, there are about 20 PhD being prepared in our lab (6 new students hired every year). The majority of these students get a research grant from the French Ministry of research, while other are paid by specific grants based on instrumental projects. Since the year 2001 (TBC), the LAOG also welcomes an increasing number of young researchers on post-doctoral positions. These positions are awarded by the ministry of research, or the CNRS on the basis of a scientific project. They are also provided by the European networks we are more and more involved into. LAOG has defined a number of procedures to associate its PhD students to the lab every day life: • two students are elected members of the LAOG advisory board • every year, we organize a “thesis workshop” during a full day where the PhD students can present their work before the rest of the lab. Table 1.1: Number of PhD students from 2003 to 2005 in LAOG Year 2003 2004 2005 22 16 18 1.1.5 Selected highlights and comparison with objectives of the previous report Given the large differences between the old and the new structures of LAOG, it is difficult to compare the prospective of the old teams, as presented in the previous prospective report, and the resulting “activity” part of the present report, without going into unnecessary details. The most important changes were due to movements of researchers leaving or joining LAOG, namely an increase in mm astronomy activities, and the arrival of a new expertise: X-rays, taken mainly as tracers of magnetic fields in young stars. Most of the other results have been obtained acording to plans, sometimes even faster (like the first image of an exoplanetary mass object.) Consequently, we prefer to summarize the main results obtained by the teams over the 2002-2005 period, as follows. 25
Page 3: LABORATOIRE D’ASTROPHYSIQUE DE GR
Page 6 and 7: III Team ASTROMOL 41 2 Presentation
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Chapter 5 Selected Publications •
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Part IV TEAM FOST The first image o
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393254 (5MJup at 55 AU) & AB Pic (1
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2.2 µ m 0.5" 11.7 µ m Figure 6.1:
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Figure 6.3: Contribution of heating
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such mid-term (several weeks) magne
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systems: HD 141569, HD 32297, HD 18
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C2D Spitzer/IRAC and MIPS data of s
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et al. 2002; 2003). We have found t
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Figure 6.8: Distribution of separat
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with only three known to date. Most
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300 objects, a size sufficient for
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therefore no surprise that vast eff
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data to verify the predictions we a
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Chapter 8 Appendices 8.1 Members of
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equipments for these tasks, from de
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10.1.3 Current trend of large equip
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• Improving High Angular Resoluti
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Chapter 11 Results 11.1 Towards hig
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Figure 11.2: NAOS-CONICA image of t
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on PUEO at CFHT. The IFS experts (A
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Figure 11.5: Image of the binary st
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Figure 11.7: PICNIC low noise infra
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have taken responsibilities: A. Che
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Figure 11.10: thermal modeling of W
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Figure 12.1: All the GRIL projects
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12.2 Optical interferometry As for
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the VLTI. CHARA is equipped with an
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• ANR Alterdetect, with IMEP : si
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Mixed GRIL-other team profiles 1. A
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Name Grade Comm. Project Berger Jea
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• First fringes in the H band wit
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144
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Table 15.1: List of the permanent S
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15.4 Transport phenomena in accreti
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Figure 15.2: Spectral energy distri
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states, combining a still powerful
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Excitation of turbulence by Cosmic
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Table 15.2: Former PhD students of
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Chapter 16 Perspectives The distinc
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Ray background. The second project
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164
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- Ceccarelli Cecilia (AT) - Delfoss
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Among the various areas of expertis
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-responsable du groupe ”logiciel
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Chef de l’ Equipe ASTROMOL du LAO
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jury de concours: 1 concours IR CNR
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Chapter 20 Appendix 4: The Jean Mar
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20.7 Production informatique ¡¢£
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20.10 Formation des utilisateurs La
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20.13 Darwin ¡¢£¤¥¦§¨©�
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