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

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1.5 From dreams to reality: Human resources Contrary to the funding situation, LAOG has been fortunate in getting a significant number of permanent positions for researchers, while the ITA population has remained stable (22). Over the 2002-2005 period, LAOG had 3 fresh CNRS positions, 2 astronomers, and 1 UJF assistant professor (unfortunately just compensating for the loss of M. Forestini). Overall, LAOG remains a young laboratory, not only because of a comparatively recent creation, but also because of the number of young researchers and engineers. This is testified by the demographics (see figure 1.9): the average age of permanent researchers is 44, while, even more remarkably, the average age of engineers and technicians is 40. In passing, we note that as a consequence most of the actors of the present prospective exercise will be able to conduct the proposed projects, even very long-term ones, themselves if they want to. This is a truly fortunate situation among similar-sized laboratories in France. Figure 1.9: LAOG age histogram Another asset of LAOG is its Technical Group, headed by P. Kern. Operationally distinct from GRIL, but sharing with it all of its engineers (14), backed by 6 assistant-engineers and technicians, this Group has the major responsibility to build instruments and make them work and used by the community. Its role is illustrated in the new LAOG histogram (see Figure 1.3). More details on its structure and internal organization are given in Appendix in chapter 18, and its impressive record in building instruments for ESO and CFHT, is described in the GRIL part. 1.6 The 2007-2010 prospective and beyond 1.6.1 Main scientific objectives Any scientific prospective spanning a rather long period (2007-2010 is just a step towards a longer term future) is a somewhat risky exercise because on many unknown external factors. Most importantly for LAOG, future projects of major agencies like ESO or ESA and their funding include highly political factors like the developments and future science priorities in France and in Europe, but we can at least describe LAOG’s objectives given the current general context. The present structure of LAOG in four teams has, among others, the advantage of allowing to streamline the main scientific issues and questions. Given the expected progress and projects, these can be synthesized as follows. • From local to global star formation. A major topic will remain the formation of solar-type stars, 34
in relation with planet formation. Currently unsolved problems involve the exact nature of gravitational collapse: what is the leading factor, magnetic fields or turbulence ? The physico-chemistry of protostellar envelopes and young protoplanetary disks, with a whole array of spectral diagnostics down to the innermost regions (< 1 AU), will give us precious indications about the velocity field and extent of the accretionejection phenomenon, the density and temperature conditions, the existence and abundance of possible prebiotic molecules, etc. The advent of Herschel (to be launched in early 2008) will allow LAOG to attack these questions with sophisticated chemistry and radiative transfer models to identify and interpret thousands of spectral lines. ALMA will later expand the result at high spectral resolution; however the spectral line diagnostic will be unable to include the lines that are undetectable from the ground. Currently, ALMA is not expected to be operational before 2012, so within the current prospective a major effort will be devoted by the Astromol team to the interpretation of Herschel data, while increasing the involvement in existing facilities like the IRAM telescopes (single-dish 30m and PdBI interferometer), JCMT and CSO in Hawaii, APEX in Chile (a precursor to ALMA antennae). A complementary view, mainly for comparison with the early solar system, will be offered by the laboratory study of irradiation effects by high-energy photons and particles emitted by the central protostar. At later stages, other issues related to global star formation emerge, also on the FOST side: e.g., why is it that star formation occurs in cluster mode and in isolated mode; more generally in so many different modes (including starbursts in galaxies for instance); what is the origin of brown dwarfs, and in particular of the “free-floating” low-mass objects far from star-forming regions ? To what extent is the IMF universal ? The FOST teams attacks some of these problems with modern tools like N-body simulations and extended surveys at CFHT like CFH12K and WIRCAM KP surveys of young open clusters, or extended nearby star-forming regions like Taurus. • Disk evolution and planet formation. One of the most exciting challenges of modern astronomy, with many deep implications like the universality of life, is to know whether the solar system is typical or exceptional among all planetary systems. Two different approaches can be considered. (i) On the one hand, to understand whether and how planets (especially terrestrial planets) form as the ultimate phase of evolution of circumstellar disks around young, solar-type stars. This requires an indepth study of the evolution of disks, from their young stages dominated by accretion and correlated jets, to later stages where dynamical interactions (instabilities, companions, etc.) deeply affect the growth of dust grains into planetesimals and planets, over timescales of ∼ 10-100 Myr. While LAOG currently is not directly involved in the study of planet formation per se, it is certainly in an enviable place to obtain constraints on prevailing physical conditions, and on the history of disk structure evolution (gaps, rings, spirals, etc.) from observations and models. (ii) The other approach is to consider already formed exoplanetary systems. With a sufficiently large sample (hundreds ?) of planetary systems down to the lowest possible planetary masses (Earthlike, ideally), one can start to apprehend the rules and the exceptions, in comparison with our solar system. The current arsenal of exoplanetary search consists of a majority of radial-velocity (stellar reflex motion) detection (30 of them have a LAOG member as co-discoverer), and of a handful of transits in front of the host star. Apart from the only confirmed (so far) recent detection of a planetary mass object around a brown dwarf (a situation hardly comparable to the solar system), no direct imaging of exoplanets is currently available. The development of instruments able to bridge this gap will open an entirely new era –if only because systems with orientations at large angles to the line of sight will become detectable, significantly enriching the parameter space for exoplanetary systems and putting new constraints on their origin. With the Astromol and FOST teams, LAOG has the expertise to have these two ends meet and study how well (or how badly) these two approaches may converge, in particular with the new instrumental projects (see below) it is leading. In short, at the horizon 2010 LAOG hopes to make radical advances in our current understanding of star and planet formation, with the ultimate goal to pin down the connection (or lack thereof) between exoplanetary systems and our solar system. • The close environment of accreting objects, from black holes to young stars. As its core activity, over the term of the present prospective (2010) the SHERPA team will focus on the physical processes that take place in the close environment of Black Holes. This includes the analysis of the gross phenomenon combining MHD and gravitation, to high energy radiation and astroparticle physics, via the turbulent transport theory and the kinetic theory of relativistic plasmas and particle acceleration. These theoretical developments will be applied to various physical environments: the Blazar phenomenon (stratified models, variability); micro-quasars (“two-flow” paradigm, modelization of the changes of state); signatures of the Kerr metric in the phenomenology of AGNs and micro-quasars; instabilities and turbulent transport in jets 35
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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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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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Table 15.1: List of the permanent S
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15.4 Transport phenomena in accreti
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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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- 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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20.10 Formation des utilisateurs La
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