Planets in Open Clusters

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1 Planets in Open Clusters Stars in OCs share the same distance, age and chemical composi0on, sta0s0cally determined M35 & NGC2158, Asiago OCs span a wide range in terms of age, metallicity, stellar density: we can probe the planet frequency as a func=on of these parameters Planet frequency as func=on of host stellar mass in the most reliable way Effects of the presence of a planetary system on the host star chemistry La ricerca dei piane0 extrasolari in Italia, WOW mee0ng, INAF- HQ Rome

2 Planets in Open Clusters There is a lack of old open clusters in the solar neighborhood. Main- sequence stars are therefore too faint Stars in young open clusters are very ac=ve, making RV detec=on difficult We have learnt how to deal with ac=vity only recently. Before that, OCs have been avoided by RV survey. Photometry has been the most favorite technique un=l recently

3 planets less common in clusters? Van Saders & Gaudi 2011: Insufficient sensi=vity to small planets, sample sizes barely large enough to find (less common) larger planets. Null detec3on Meibom et al b Rotation period (days) Photometric searches in M37, NGC188, NGC1245, NGC2158, NGC2362, NGC Without planets. Are Time from mid-transit 10 (hour V (mag) Photometry a Relative flux Searching for Planets in RESEARCH OCs: LETTER Figure 14 2 Transit light curves. a, b, The Kepler light curves for Kepler-66 (a) and Kepler-67 (b). The photometric measurements (grey points) were acquired in long cadence mode (30-min total exposures) and have been detrended28, normalized to the out-of-transit flux level, and phase-folded on the Kepler ,000 stars during the era of planet formation, including several at least Kepler-67 O stars (masses greater than 20 solar masses) and more than one hundred B stars (masses between 3 and 20 solar masses). The discovery of two mini-neptunes in NGC6811 thus provides evidence that the formation and long-term stability of small planets is robust against periods of the tra the same data ph mean, respective overplotted in re 5 stellar densities deaths and hig Received 6 Nove Published online 0 0 of planets inside and outside open clusters of stars. Number of planets Meibom et al. 2013: 2 mini- Neptunes, Kepler- 66b and Kepler- 67b detected in NGC6811 by Kepler mission over 377 cluster members. The same frequency Number of planets Lada, C. J. & L Astrophys. 41 B V (mag) a 2. The Extrasola Mayor, M. pa et a Figure 1 The colour magnitude and colour period diagrams for 1, Kepler-66b Kepler-67b Occurrence, Tm NGC6811. a, The colour magnitude diagram for stars within a 1-degreemembers Neptune-mas in t diameter field0.6 centred on NGC6811 with the locations of Kepler-66 and Kepler- variations abs/ Howard, A.pe et 67 marked by 0.4 black circles. Cluster members, marked with larger red dots, trace 4.of multiple Astrophys. J. S trac a well-defined relationship between stellar mass (colour, B 2 V) and luminosity 5.members Fressin, F. et 0.2 The (brightness, V) that can be fitted by stellar evolution models to determine the period. Astrophys. J.lo Sato, et al. markedb.by ora age and distance1of NGC6811 as well3 as the masses and radii 10 of its members. By 661, Radius (R billion ) this method NGC6811 is found to be years old and 7. Lovis, C. & Ma b substellar com 1.0 Astrophys. 47 Kepler-67b Kepler-66b or metallicity imply that the 0.8 planet frequency in NGC6811 is consistent with that of 8. Quinn, S. et a open cluster. distribution the field van Saders, J The members of NGC6811 fall entirely within the range of stellar Kepler-66b upper limits o 0.4 J. 7 frequenc spectral types0.2selected for the Kepler planet survey, and the slightly sub- theastrophys. 10. Pace, G., Pasq The comp solar metallicity of NGC6811 (ref. 17) is close to the average metallicity stars. Astron A. 1 from which 10the Kepler targets 100 1,000 66bFischer, and D.Kep of the Galactic0.1 disk population are drawn ( Period (days) that the size Therefore, correlations between planet frequency and stellar mass and/ La ricerca dei piane0 extrasolari in Italia, WOW mee0ng, INAF- HQ Rome 12. Meibom, S. T abstr. Figure 3 Distribution of planetary properties. a, b, Histograms of planetary those of the 13. Yi, S. et al. Tow s3ll in agreement with field frequency. 1.

4 Searching for Planets in OCs: Radial Veloci0es of Giant Stars J Giant Stars are brighter than Main Sequence counterparts Sato et al. 2007: A planetary companion to the Hyades Giant ε Tauri, P=594d Msini=7.6M J Lovis & Mayor 2007: Planets around evolved intermediate- mass stars. A P=714d Msini=10.6M J in NGC2423 and a P=678d Msini=19.8M J in NGC4349 L Li`le knowledge of giant star oscilla=ons prevent the discovery of small- mass planets

5 Searching for Planets in OCs: Radial Veloci0es of MS Stars Chocran et al. 2002, Searching for planets in the Hyades. I. The Keck Radial Velocity survey 94 F5V to M2V stars, magnitude range V= No planet found The survey was affected by the li`le knowledge of stellar ac=vity of young stars (RV jijer) Sparse sampling No simultaneous photometric observa=ons Only CaII H&K emission lines as ac=vity indicator. I 2 gas cell contaminates the spectra A small number of stars were then observed more intensively, spectroscopically and photometrically

6 Searching for Planets in OCs: Hot- Jupiters around OC stars Quinn et al. 2012: Two b s in the Beehive: the discovery of the first Hot Jupiters in an Open Cluster P=4.43d Msini=0.54M J P=2.14d Msini=1.84M J Radial Velocity (m s 1- ) Quinn et al. 2014: HD b: an eccentric Hot Jupiter in the Hyades Open Cluster P=6.09d Msini=0.54M J e=0.09 Observa=onal strategy focused on the detec=on of short- period, massive planets. O-C (m s 1 ) BS (m s 1 ) S index Orbital Phase

7 Searching for Planets in OCs: Hot- Jupiters around OC stars Brucalassi et al. 2014: Three planetary companions around M67 stars P=6.96d Msini=0.34M J, e=0.24 P=5.12d Msini=0.40M J, e=0.39 P=121d Msini=1.54M J e=0.35 (around a giant star) M67 is old (~4 Gyr), ac=vity has been neglected Observa=onal strategy focused on giant planets. HARPS in lower- resolu=on sefng.. Top: Lomb-Scargle periodogram for YBP1194. The dashe

8 RVs, OCs and stellar ac0vity Recent surveys have avoided to deal with ac=vity. However, knowledge in the field is rapidly advancing Corot- 7 (M=4.8 M ): RV jijer is not a random noise, but has a structure that can be removed Several works on the topic: Lanza et al. 2009, Boisse et al. 2011, Figuera et al. 2013, Dumusque et al D. Queloz et al.: The CoRoT-7 planetary system: t Fig. 1. AsyntheticviewoftheradialvelocityandspectroscopicinformationmeasuredfromHARPSdatafromNovember2008toFebruary2009. Agreement on the importance of rota0onal period of the star and simultaneous photometric observa0ons Queloz et al process, a This addit series of fi uncertaint locity data the harmo (ν = an orbital ters, one fi and e = 0 pre-whiten Simila 3.7-day or then looke spectrum peak with

9 Searching for Low- Mass Planets in OCs: The Open Cluster Survey in GAPS We are currently surveying two Open Clusters in GAPS: NGC752 (1.5 Gy) and M44 (600 My) GAPS Proposal, PI: A. Sozzef Strong a`en=on on members selec=on HARPS- N delivers long- term stability and short- term accuracy also Ac=vity (e.g. CaII H&K, Hα emission lines) and Asymmetry (Contrast, FWHM, Bisector Span, Vasy ) indicators

10 Searching for Low- Mass Planets in OCs: Photometry of OC- GAPS targets Simultaneous Photometry with Rota=onal period of the star Analysis by V. Nascimbeni Long term varia=on of photometric amplitude and modula=on (correlated to RVs) Knowing precisely the rota=onal period let us detect planets more easily

11 Searching for Low- Mass Planets in OCs: The importance of rota0onal periods Clear difference between a lonely active star and an active star with a planet!

12 Searching for Low- Mass Planets in OCs: Early results from OC- GAPS A complex system: A 2.14d planet (Quinn et al. 2012) 8 day rota=onal period A long- term trend with curvature ( 1200d?) AOT30 observa=on will put a strong limit on Period and Mass of the second body This discovery will put strong constraint on planet forma=on and evolu=on in crowded environment

13 Searching for Low- Mass Planets in OCs: Early results from OC- GAPS It s a new field and we had a lot to learn But now we are on the right track and several candidates are coming out

14 Searching for Low- Mass Planets in OCs: Chemical Star- Planet connec0on Melendez et al. 2009, Ramirez et al. 2014: stars with planets are depleted in elements used to form the planets Gonzalez Hernandez et al. 2013: chemical differences explainable in terms of Galaxy evolu=on Open Clusters: direct solu=on to this dilemma (and Lithium ques=on as well), work in progress Figure 5. Differences between [X Fe] of the Sun and the mean values in the

15 Planets in Star Clusters Ruprecht147 with HARPS 5 nights (50 hours) in P91, 8 nights (80 hours) in P93 Proposal for 8 nights in P95 submi]ed 25 ini=al targets Observa=onal strategy, ac=vity checks similar to M44 and NGC752 2 low- mass (K<10 m/s) candidate planets and a possible long- period Jupiter We are already exploi=ng the GAPS experience to gain visibility PI: D. Minni=

16 Searching for Planets in OCs: K2 observa0ons Many OCs included in K2 fields on specific request of community! Planets in OC are becoming hot- topic

17 Conclusions Photometry des not find a different frequency of planets in Open Clusters respect to the field Earlier RV surveys did not take ac=vity into account properly Later RV surveys focused on giant stars, or just to find Hot Jupiter We now have the hardware (HARPS- N@TNG, high- precision photometry) and the tools (Ac=vity indexes ) to discover low- mass planets in OCs Not only planet discoveries: star- planet chemical connec=on, dynamics of stellar encounters New interest from community in OCs: several K2 fields on clusters La ricerca dei piane0 extrasolari in Italia, WOW mee0ng, INAF- HQ Rome

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