Expectations and Limitations of Kepler Ground-Based Follow-Up Observations

1. Expectations and Limitations of Kepler Ground-Based Follow-Up Observations Joanna Molenda-Żakowicz Uniwersytet Wrocławski, Instytut Astronomiczny ul. Kopernika 11, 51-622 Wrocław POLAND

2. March 6, 2009 – launch of the Kepler spacecraft The aim of the Kepler mission: find out how many stars in the Milky Way can harbour potentially habitable Earth-size planets. The Kepler photometer being lowered onto spacecraft. Habitable zones at stars of different temperatures. • Field of View: continuously viewable; rich in stars similar to our Sun • One broad-band filter • Photometric precision: several ppm • Mission extended through 2016 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

3. 74 confirmed planets and 2321 candidates 160 planets in habitable zone Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

4. Behind each planet, there is a star! Kepler 10b – the first Kepler rocky planet Planet: Orbital period: 0.84 d Radius: 1.42±0.03 R⊕ Mass: 4.6±1.2 M⊕ Mean density: 8.8±2.5 g/cm3 Mean temperature: 1,800 K Star: Mass: 0.9 M±0.06 M⊙ Radius: 1.06±0.02 R⊙ Surface gravity: 4.3±0.01 dex Luminosity: 1.004 ± 0.059 L⊙ Batalha et al. 2011, ApJ 729, 27 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

5. Asteroseismic determination of mass e.g., Chaplin et al. 2011 ApJ, 732, 54 Evolutionary sequence of 1M⊙star: Silva Aguirre et al. 2011 ApJL 740, L2 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

6. Red Clump stars and ultra-cool dwarfs Mass of stars near the RC of NGC 6791 and NGC 6819: Corsaro et al. 2012 arXiv1205.4023 Greiss et al. 2012, AJ 144, 24 • Spectral type M7 and later: very low-mass stars as well as brown dwarfs. • 9 very low-mass dwarfs are actually being monitored by Kepler (Martin et al. 2011, AAS Meeting #220, #419.06) • Kepler Guest Observers Program: 'The Kepler View on Activity, Binarity, Habitability and Weather in Late-M and L Dwarfs' (P.I.: Eduardo Martin;) Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

7. Our precise methods of deriving atmospheric parameters are not particularly accurate... Kepler Input Catalog was designed to separate dwarfs from giants at Teff ~6,000 K

8. Differences between atmospheric parameters in the KIC and those derived from ground-based spectroscopy Bruntt et al. 2012, MNRAS 423, 122 Molenda-Żakowicz et al. 2010, AN 331, P26 Thygesen et al. 2012, A&A 543, 160 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

9. Differences between atmospheric parameters in the KIC and those derived from ground-based spectroscopy McNamara et al. 2012, AJ 143, 101 Yang X., Fu J.N., et al., in preparation Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

10. Differences between atmospheric parameters in the KIC and those derived from ground-based photometry Pinsonneault et al. 2012, ApJS 199, 30 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

11. Differences between atmospheric parameters derived from ground-based photometry and from spectroscopy 5 Molenda-Żakowicz, Sousa, et al., in preparation Pinsonneault et al. 2012, ApJS 199, 30; Tygesen et al. 2012, A&A 543, 160 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

12. Differences between atmospheric parameters derived by different methods from the same ground-based data Metcalfe et al. 2010, ApJ 723, 1583 Molenda-Żakowicz, Sousa, et al., in preparation Creevey et al. 2012 A&A 537A, 111 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

13. Why different methods of the data analysis produce significantly different results? • Spectroscopic: ROTFIT, ULySS, ARES, VWA, MOOG, SYNSPEC • Photometric: IRFM, various photometric calibrations for different sets of filters, SED Fröhlich et al. 2012, A&A 543, A146 Casagrande et al. 2010, A&A 512, A54 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

14. How important is the interstellar extinction? Camelot@IAC80 Observatory of Izaña, Tenerife, Spain; WFC@INT Observatorio del Roque de los Muchachos, La Palma, Spain – Katrien Uytterhoeven (P.I.), Joanna Molenda-Żakowicz, et al. WFC@INTBill Chaplin and Andrea Miglio (Birmingham, UK), Victor Silva Aguirre (Aarhus, DK) Chris Flynn (Tuorla, FIN) Sofia Feltzing (Lund, S) Antonino Milone (IAC, E) Simon Hodgkin at (IoA/Casu, UK), Martin Asplund and Luca Casagrande (ANU/Stromlo, AU) Molenda-Żakowicz et al. (2009) AcA 59, 213 Pointings done in June 2012 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

15. Calima in 2012 The telescope needs to be closed when the limit 0.025 is reached. (plot made by STELLA http://stella.aip.de/stella/status/status.php) Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

16. Why is it always the fainter stars that are so interesting?(Katrien Uytterhoeven) around 3,400 stars over 160,000 stars over 160,000 stars Pinsonneault et al. 2012, ApJS 199, 30 Yang X., Fu J.N., et al., in preparation Pinsonneault et al. 2012, ApJS 199, 30 Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

17. The future is BRITE BRITE-Constellation, short for “BRIght Target Explorer - Constellation,” is a group of six seven-kilogram nanosatellites from Poland, Austria, and Canada. Purpose: photometrically measure low-level oscillations and temperature variations in stars brighter than visual magnitude 4.0 (and fainter than 7.0) Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China

18. The future is BRITE 'While there are more than a dozen telescopes larger than 6.5 meters there is plenty of interesting astronomy which can be done with much smaller instruments.' Bohdan Paczyński 'Astronomy with small telescopes' Joanna Molenda-Żakowicz, IAU GA, 20-31 August 2012, Beijing, China