Report - School of Physics

More documents

Recommendations

Info

Figure 7: Links between detection methods in space (second column) and ground (fourth column), resulting statistical information (first column) and candidate detections (third column). Experiments which are not approved are shown as dashed boxes. The large dash-dotted boxes show the cumulative statistical knowledge, and the cumulative candidate lists respectively. Solid arrows show the candidates resulting from a particular observation. Dotted arrows indicate the follow-up observations needed. Note that the Kepler detections will all be in the northern hemisphere, and thus unobservable from ESO. STATISTICS SPACE DETECTIONS GROUND JWST and Spitzer Protoplanetary disks ALMA Statistics of low mass Astrometry SIM > 2010 Transits HST Tens to hundreds of low mass > 2008 Radial velocity follow−up (stacking for known periods) Transit follow−up: desirable but unfeasable? Statistics of Jupiter Systems (mass and orbit) Transits COROT/Kepler/ Eddington > 2006 Hundreds of high mass > 2008 Radial velocity detections Follow−up Statistics of nearby > 10 Earth mass Microlensing MPF > 2008 Astrometry (and photometry) Gaia > 2015 Darwin/TPF 300 GK to 25 pc 30 spectra Thousands of high mass > 2015 Characteristics (luminosity/dynamics) of all stars to 20 mag Specific target stars for Darwin/TPF Hundreds/thousands of Hot Jupiters Transit detections Follow−up Ground follow−up Spectroscopy/ Photometry GENIE Characterisation of nearby target stars Survey mission beyond 2015 ??? OWL Search for low mass + Spectroscopy 61
time will be required. Existing transit measurement facilities and amateur networks could contribute, although some new dedicated provision for follow-up is probably needed, in particular enlarging networks in longitude to significantly improve the efficiency of ground-based transit observations. Radial velocity follow-up will be needed for all high-mass candidates, of which Gaia will generate a very large number. Thousands of the more massive planets could be observed by ground-based radial velocity instruments, assisting the determination of multiple planets, relative orbital inclinations, etc. ESO could consider a coordinated large-scale follow-up of such radial velocity observations, and whether additional facilities will be needed. An assessment of telescope time/aperture needed for these projects has not been made — probably a combination of existing facilities and larger dedicated instruments would be needed. 4.2.2 Low-Mass Planets Low-mass (of order 1 M ⊕ ) planets will hopefully be detected by Kepler and Eddington, perhaps in moderately large numbers (some hundreds). They will typically be too low-amplitude for ground-based photometric follow-up, which in any case are unlikely to improve on the S/N of weak transit events detected by Kepler or Eddington – these missions will have years of lightcurves on a star, and if the signal is still weak after phasing and adding all data, it will be difficult to improve from the ground in a reasonable time. This is a potential problem, since such follow-up observations will be needed: (i) to confirm the reality of the lower S/N detections; (ii) to search for planetary periods for candidates for which only one transit is detected; (iii) to confirm candidate detections for which two or possibly more transits were detected (since periods and transit times are known, ground-based follow-up may be more feasible); (iv) to search for period changes due to planetary moons etc.; (v) to characterise the transit systems in terms of chemical abundances. Probably the only prospect is follow up with HST and/or JWST (see Section 2.2.1) for transits, and possibly SIM for astrometry, although many of the transit candidates will be too distant even for these instruments. Radial velocity measurements are again needed in principle to supplement the orbital information. Improvements in radial velocity precision for transits may be achieved by the stacking of repeated observations at the known planet period, as described in Section 1.3. If Eddington is approved (or for the study of Kepler candidates), the development of new telescope facilities should be considered, such as a high-precision spectrograph (like HARPS) based on an 8-m (or larger) telescope. Given the low expected surface density of accessible candidates, it is unlikely that a multi-object instrument would be effective and so a highly-optimised single object instrument offering a precision of ∼ 1 m s −1 would be preferred. The HARPS detection of a 14 M ⊕ planet demonstrates that it may be possible to characterise all the exo-planets detected by COROT (massive Earths with short periods) in this way. 62
Page 2 and 3:
Report by the ESA-ESO Working Group
Page 4 and 5:
The working group membership was es
Page 6:
3.2.2 The Darwin Ground-Based Precu
Page 9 and 10:
Figure 1: Detection methods for ext
Page 11 and 12:
those with masses between about 0.5
Page 13 and 14:
Figure 2: Detection domains for met
Page 15 and 16:
(c) Astrometric measurements do not
Page 17 and 18: Table 1: A summary of completed, op
Page 19 and 20: chemical composition of the primord
Page 21 and 22: Table 2: A summary of planned or op
Page 23 and 24: it passes behind the star. They arg
Page 25 and 26: shapes caused by extra-solar planet
Page 27 and 28: Table 3: A summary of completed, op
Page 29 and 30: ground requires simultaneous observ
Page 31 and 32: 0.35 arcsec of the centre, i.e. muc
Page 33 and 34: ferential phase observations with a
Page 35 and 36: 2.2 Space Observations: 2005-2015 I
Page 37 and 38: larger number of hot Jupiters would
Page 39 and 40: (Shao): this major SIM survey progr
Page 41 and 42: The planetary lensing events have a
Page 43 and 44: siting extra-solar planets are expe
Page 45 and 46: 2.3 Summary of Prospects 2005-2015
Page 47 and 48: 3 The Period 2015-2025 3.1 Ground O
Page 49 and 50: Table 6: Magnitudes and separations
Page 51 and 52: per star in order to sample the (po
Page 53 and 54: een produced, diffraction effects c
Page 55 and 56: 3.2 Space Observations: 2015-2025 T
Page 57 and 58: Table 8: Detection capabilities: Ea
Page 59 and 60: 3.2.3 Terrestrial Planet Finder (TP
Page 61 and 62: ∼ 5 × 10 5 m, or 1.5 × 10 −4
Page 63 and 64: of Earth-like planets in general, a
Page 66 and 67: 4 The Role of ESO and ESA Facilitie
Page 70 and 71: 4.2.3 Summary of Follow-Up Faciliti
Page 72 and 73: 4.4 Astrophysical Characterisation
Page 74 and 75: Without any further mission dedicat
Page 76 and 77: and their suitability for supportin
Page 78 and 79: overlap of public and research inte
Page 80 and 81: 2.4. Evaluate observation time for
Page 82 and 83: A Space Precursors: Interferometers
Page 84 and 85: B Beyond 2025: Life Finder and Plan
Page 86 and 87: C ESO 1997 Working Group on Extra-S
Page 88 and 89: Table 10: ESO Working Group 1997: R
Page 90 and 91: Charbonneau, D., Brown, T. M., Noye
Page 92 and 93: Pedretti, E., Labeyrie, A., Arnold,
show all

Report - School of Physics

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?