Download Launhardt

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)
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)
Recall of the ESO Sience Proposal
Astrometric 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
Astrometric Survey for Extra-Solar Planets with PRIMA
GTO 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.
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
Consortium
Science Team
(set up by the consortium/PIs)
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 program are 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 their own resources.
►All data obtained as part of the GTO program are the common property of
the three PIs.
 Publication policy:
►DDL/AOS Project:
Authors:
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
PRIMA Astrometric Planet Search Science Team
 Initial Core Science Team:
CH
D. Queloz
D. Segransan
F. Pepe
NL
A. Quirrenbach
S. Reiffert
????
D
Th. Henning
R. Launhardt (Coordinator)
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
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.
Current Science Team activities - Overview
1.
Study/model sources of astrometric uncertainties/noise, simulate
astrometric observations
2.
Pre-selection and characterization of target and reference stars
for the astrometric planet search program
→ Report by SR/SH, JS, DS
3.
Checking CORALIE and HARPS data bases (and consortia) for
useful information on potential target stars → Report by Damien
4.
Preparatory observations
5.
Setting up target data base → Report by Johny
6.
Refine target groups and science goals → Start discussion
→ Report by Johny
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)
Current Science Team activities – Overview
Study/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

Publish particular results if study is completed
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
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!
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 Vband (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.
Astrometric signal at VIS (SIM)
and K-band (PRIMA) due to star
spots on a G dwarf target star
and K giant reference star.
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)
Future Science Team activities



More
More
More