Agenda - PRIMA AOS CDR – Science Day, October 1st 2004

1. Agenda - PRIMA AOS CDR – Science Day, October 1st 2004 08:30 - 08:45 Setting the objectives of the day (RL) Session 1: Continuation PAOS activities 08:45 - 09:15 Target and reference star selection criteria (JS) Session 2: Rationale, definition, and tasks of the Science Team 09:15 - 09:45 Introduction: Rationale for a Science Team (DQ) 09:45 - 10:00 Recall of ESO Science Proposal and GTO time allocation (RL) 10:00 - 10:30 Tasks and duties of the Science Team & Internal MoU (RL + all) Session 3: Reports on current Science Team activities 10:45 - 11:00 Overview on current science team activities (RL) 11:00 - 11:20 Preparatory science (RL+SR+DS) 11:20 - 11:40 Current status of target and reference star selection (SR+SH+JS+DS) 11:40 - 12:00 Spectroscopic information from CORALIE and HARPS (DS) 12:00 - 13:00 Lunch 13:00 - 14:00 Closed session on contractual matters (PIs, Management board, ESO) 14:00 - 14:30 Preparatory observing programs and data access (JS) Session 4: Future Science Team activities 14:30 - 15:15 GTO program definition and preparations (RL + all) Session 5: Other business 15:15 - 16:00 Support to ESO, Observations, Post-docs at Paranal (DQ, RL + all) Science data handling, … 16:00 Summary of PAOS CDR (FP+EJB)

2. PRIMA AOS CDR – Science Day, October 1st 2004 Objectives of the Day • Continuation PAOS activities: Target and reference star selection criteria • Finish (sign) agreements with ESO • Sign the internal MoU on science activities, data rights, and publication policy (closed session) • PRIMA Astrometric Planet Search Science Team • Rationale for a Science team • Agree on composition of and duties of the Science Team • Report on current science team activities (in preparation of the astrometric planet search program)

4. Recall of the ESO Sience ProposalAstrometric Survey for Extra-Solar Planets with PRIMA • Proposal: contribute to the development of the PRIMA hard- and software to enable an early start of high-precision astrometric observations at the 10μarcsec level. Receive guaranteed observing time with the VLTI (2 ATs) to conduct a large astrometric survey for extra-solar planets. • Scientific Goals: ■ Resolve the sini uncertainty from planet masses. Fundamental for the planetary mass function, in particular the upper mass cut-off. ■ Confirmation of hints for long-period planets in RV surveys. ■ Inventory of planets around stars of different masses and ages, in particular stars that are not accessible to the RV method (M>1.2Msun and young stars). ■ Detection of multiple systems with masses decreasing from the inside out. (Different detection biases: RV: Astrometry: ■ Measure whether multiple systems are coplanar or not. • Scientific Program: Core Program 1:Accurate measurement of the mass of extrasolar planets detected by RV surveys Core Program 2:Planet search through the main sequence and time Observing Time:P1: 50 stars, 70-100 nights; P2: 100 stars, 100-150 nights

5. Astrometric Survey for Extra-Solar Planets with PRIMAGTO time allocation • Guaranteed observing time granted to the Consortium: 217 observing nights in total on the two ATs in the PRIMA astrometric mode during a period of 8 years after commissioning of the PRIMA DDLs (Conditional upon successful commissioning in Chile. 125 nights from DDL + 92 nights from AOS agreement) • Astrometry Commissioning and Provisional Acceptance in Chile: Feb. – June 2007 • GTO program:~ July 2007 – June 2010 • Time allocation is subject to a detailed and comprehensive observing programme, submitted by the Consortium and reviewed by the OPC on a yearly basis. • Results will become public one year after the end of the 3-year GTO program, but targets will not be blocked for more than the first year. • VISA guaranteed time allocations “should not allow one group to monopolize one of the important scientific goals of the VLTI” • For the follow-up of planetary systems detected by the radial velocity technique through the guaranteed time of HARPS, the Consortium shall observe only identified objects with their radial velocity curves already in the public domain.

7. Science Team Consortium Memorandum of Understanding on science activities, data rights, and publication policy in the PRIMA-DDL astrometric planet search consortium • General: ►Consortium-internal agreement on science activities, data rights, and publication policy. The rules apply for the duration of the PRIMA-DDL/AOS project AND the execution and exploitation of the GTO astrometric planet search program. ►The consortium partners agree to seek an equal balance in efforts and contributions to the PRIMA-DDL/AOS Project as well as to the preparation and execution of the GTO Astrometric Planet Search Program. • Science activities:Clear distinction between PRIMA-DDL/AOS Project Scientific GTO Planet Search Program (set up by the consortium/PIs)

8. Memorandum of Understanding on science activities, data rights, and publication policy in the PRIMA-DDL astrometric planet search consortium • Data Rights: ►All data collected in the preparatory observing programare the common property of the Science Team. In addition, the partners agree to provide on best effort basis any useful information on target and reference stars available to them from theirown resources. ►All data obtained as part of the GTO program are the common property of the three PIs. • Publication policy:Authors: ►DDL/AOS Project: Consortium (part or all, always include PIs) ►GTO preparatory program: Science Team ►GTO Planet Search Program: First paper: All (Consortium and Science Team) Other papers: Science Team

9. PRIMA Astrometric Planet Search Science Team • Initial Core Science Team: CH NL D D. Queloz A. Quirrenbach Th. Henning D. Segransan S. Reiffert R. Launhardt (Coordinator) F. Pepe ???? J. Setiawan • Final Science Team: • Will be formed later by expanding Core Science Team • Maximum of 15 members • PIs appoint members • Composition shall reflect share of partners in the project • Scientists from outside the consortium institutions can be appointed

10. Tasks and Duties of the Science Team • Follow new scientific developments in the field to accordingly adjust the scientific goals and targets of the astrometric planet search program • Undertake all necessary scientific preparations for the GTO program (including building up a target data base and carry out preparatory observations) • Plan and carry out the GTO program.

12. Current Science Team activities - Overview • Study/model sources of astrometric uncertainties/noise, simulate astrometric observations • Pre-selection and characterization of target and reference stars for the astrometric planet search program → Report by SR/SH, JS, DS • Checking CORALIE and HARPS data bases (and consortia) for useful information on potential target stars → Report by Damien • Preparatory observations → Report by Johny • Setting up target data base → Report by Johny • Refine target groups and science goals → Start discussion

13. Current Science Team activities – Overview Pre-selection and characterization of target and reference for the astrometric planet search program • RV planet host stars → Geneva (Damien) • M, K dwarfs → Leiden (Sabine) • G, F, A dwarfs, PMS stars → HD (Johny, Ralf) • Target Data Base→ HD (Johny)

14. Current Science Team activities – OverviewStudy/model sources of astrometric uncertainties/noise, simulate astrometric observations • To refine target and reference star selection criteria, define preparatory observing needs and strategy, and prepare astrometric observing startegy • Collect results in living internal working document „Characterization of target and reference stars for extrasolar planet searches with PRIMA“ → Sources of astrometric uncertainties e.g. Perspective acceleration, Pulsations → Sabine Companions, Chromospheric Activity, Circumstellar Disks → Ralf → Parameters of target and reference stars that have to be known → Preparatory Observing Strategy • Publish particular results if study is completed

15. Stellar, substellar, and planetary companions • Most siutable and likely reference stars: K giants at 1-2 kpc • Binarity of K stars ≈ 40% • Average mass ratio: 0.7 • → Of order one third of all potential reference stars will have companions which produce a relevant astrometric singal • → Clever RV survey necessary!

16. Astrometric signal at VIS (SIM) and K-band (PRIMA) due to star spots on a G dwarf target star and K giant reference star. Rotational modulation due to starspots Chromospheric inhomogenities (e.g., spots) on the rotating stellar surface produce astrometric, radial velocity, and photometric signals. We have modeled the effects for simple edge-on (sini=1) geometry and a single spot, using realistic stellar parameters, spot temperatures, and limb darkening coefficients. The effects are much smaller at K-band (PRIMA@VLTI) than V-band (SIM). The simulations show that for ground-based differential astrometry at K-band and 10μarcs accuracy, spots are of concern only for the most nearby target and reference stars (typically distant K giants). Starspots appear to be of serious concern for SIM, especially for astrometric grid stars.

18. Future Science Team activities • Continue study/model sources of astrometric uncertainties/noise, simulate astrometric observations, and preparatory observing strategy • Investigate how many/which RV planet host stars we can/will observe with PRIMA → What kind of long-term RV trends do we follow? (3 yr GTO!) → Reasonable prognosis of number published RV planets until 2007 • Discuss primary science goals of core program 2 → Observe everything? → M dwarfs? (Lack of gas giants? Neptunes? Lower host star / disk mass cut-off?) → Solar type dwarfs (Systems with stable nishes in habitable zone? – Preparation for darwin) → More massive (>1.2Msun) MS stars? (not accessible to RV) → PMS stars (young systems, migration, many Jupiters? – not accessible to RV)

19. Future Science Team activities • More • More • More