Transcript The new europian project ROPACS (Rocky Planets Around …

The ambitious europian project
ROPACS (Rocky Planets Around
Cool Stars)
Yakiv Pavlenko
Main Astronomical Observatory of the
National Academ of Sciences of Ukraine
[email protected]
www.mao.kiev.ua/staff/yp
Commision of the Europian
Communities
SP3 People
Support for training and career development of
researcher (Marie Curie)
Network for Initial Training
http://star.herts.ac.uk/RoPACS/
RoPACS
Grant Agreement Number 213646
PITN-GA-2008-213646
Members of ROPACS
Consorcium:
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University of Hertfordshire
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University of Cambridge
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Instituto de Astrofisica de Canarias
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Max Plank Gesellschaft fur Foerderung der
Wiesenshaften
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Instituto Naconal de Tecnica Aeroespacial
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Main Astronomical Observatory of NASU
Management docs:
Searching for transit
(IoA, MPE, UNED)
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Extract differential photometry from transit
survey data.
Calibrate colours/magnitudes and place
photometric constrains on host type.
Refine algorithm transit searches.
Identify transit candidates amongst cool star
population.
Develop complementary approach to analysis
with with a range of tools (e.g. WSA, Astrowise,
Gaudi).
Identifying false positives
(UH, MPE, IAC)
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Use best quality data to identify candidates that
are unresolved blends.
Measure spectral types of potential host stars
(VLT, HET, WT, ESO, etc).
Prioritise candidates for follow-up, by planet
size.
Measure intermediate spectroscopy to identify
eclipsing binary systems.
Set-up software (e.g. Astrowise) to analyse
data from a range of different instruments.
High resolution RV Spectroscopy
(UH,MPE,IAC,SIM)
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Measure high resolution cool star spectroscopy
of transit candidates using NIR and optical
instruments (e.g. CRIRES, PRVS-Pathfinder,
NIRSpec, VLT, HET, NAHUAL,PRVS).
Optimize cross-correlation techniques for
measuring RVs of cool stars, particularly in the
near-infrared.
Optimize techniques (e.g. bisector analysis) for
identifying false RV signatures.
Fit orbital solutions to confirmed systems, and
constrain companion masses.
Measuring planet radii and
densities (MPE, IAC)
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Plan and propose/implement space-based
follow-up efforts (i.e. HST, SST) to measure
detailed light curves of the transits.
Use ground-based facilities (e.g. VST, CST etc.)
to re-measure transit light curves.
Optimize transit fitting techniques for cool star
hosts (e.g. limb darkening, intrinsic variability).
Constrain radii of orbiting companions/planets.
Establish densities and constrain internal
structure and nature.
Detecting planetary light
(LAEFF, Astrium)
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Plan and propose/implement space-based
follow-up efforts to search for and measure
planetary light (in the near- and mid-infrared) as
they pass behind their host star.
Assess and test/use sensitive ground-based
facilities (e.g. GTC) to search for planetary light
in the infrared.
Optimize methods (in part via input from the
Astrium ESR) in terms of wavelength range and
observing techniques.
Understanding the planet host
stars (MAO, UH, SIM)
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Develop cool star atmospheric models.
Measure spectroscopy of cool star hosts over a
broad/useful spectral range.
Fit cool star properties with models, and
assess the implications for orbiting planets.
Search for wide binary companions to cool star
populations using astrometric techniques.
Constrain close companions using other (e.g.
AO) techniques.
Assess implications for planet formation.
Planet properties and ESA’s Cosmic
Vision (UH,Astrium,LAEFF)
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Review current state-of-the-art on extra-solar
planets (theory & observation).
Simulate observable properties of known and
potential planet types.
Set up models of Cosmic Vision missions.
Consider how enhanced techniques could be
used to study extra-solar planets.
Model the incorporation of appropriate
enhancements into these missions, and assess
mission capabilities.
Feedback to the network. assessments.
Gliese 581
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Gliese 581 (pronounced /ˈɡliːzə/) is a red
dwarf star with spectral type M3V, located
20.3 light years away from Earth. Its mass
is estimated to be approximately a third of
that of the Sun, and it is the 87th closest
known star system to the Sun.
Observations suggest that the star has at
least four planets: Gliese 581 b, c, d, e.
Gl 581
HO Librae
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The star system gained attention after Gliese
581 c, the first low mass extrasolar planet found
to be near its star's habitable zone, was
discovered in April 2007. It has since been
shown that under known terrestrial planet
climate models, Gliese 581 c is likely to have a
runaway greenhouse effect, and hence is
probably not habitable. However, Gliese 581 d
is within the outer edge of the habitable zone.
Gl 581
]Companion(in order from star) Mass Semimajor axis(AU)
Orbital period (days)
Eccentricity
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e ≥1.94 M⊕ 0.03 3.14942 ± 0.00045
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b ≥15.65 M⊕
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c ≥5.36 M⊕ 0.07 12.9292 ± 0.0047
0.17 ± 0.07
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d ≥7.09 M⊕ 0.22 66.80 ± 0.14
0.38 ± 0.
0
0.04 5.36874 ± 0.00019
0
Transmitted and reflected
spectrum of the Earth
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Conclusions I.
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Palle et al. (2009) observed really transmitted
and reflected light of the telluric atmosphere.
Earth is the first rocky planet discovered
spectroscopicvally.
If something is possible at once, it can be
repeated many times...
Conclusions II.
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We can provide a good fits to the observed
spectra of UCD in the selected spectral regions.
To provide any confident fits the existed input
data (molecular line lists, model atmospheres,
etc) have to be refined substancially.
Situation with modelling spectra of extra-solar
planets looks as very promising, if we use all
knowledge accumulated for planets of SolSys.
Any collaboration is very appreciated.
Some plans
Fundamental parameters of UCD determined by
EB's. Verification of the input data and theory.
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Lithium and deuterium test applications.
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Telluric and planetary spectra.