1. Eduardo L. Martín¹, Ramarao Tata², Enrique Solano¹, Eder Martioli 3, Simon Hodgkin 4 Daniel Steeghs 5 1.- Centro de Astrobiología (INTA-CSIC), Madrid, Spain 2.- Instituto de Astrofísica de Canarias, Tenerife, Spain 3.- Canada-France-Hawaii Telescope 4.- Institute of Astronomy, Cambridge, UK 5.- University of Warwick, UK Ultracool KIS

2. Ultracool dwarfs (UCDs): Definition Ultracool dwarfs: Dwarfs with spectral type later than M7 (Teff<2600K). Dust grain condensation in atmospheres (Fe, Al 2 O 3, MgSiO 3 ).

3. UCDs: photometric variability Martin, Zapatero Osorio & Lehto 2001, ApJ, 557, 822

4. UCDs: photometric variability Bailer-Jones & Mundt 2001, A&A, 367, 218 ★ ✪ --------------------------------------------------------- Expected Kepler Precision @ Kp=18 in 30 min

5. Amazing flare in LP412-31 (dM8, Schmidt et al. 2007, AJ, 133, 2258)

7. First UCD in the Kepler field

8. UCDs in the Kepler Input Catalog UCD identification is very effective using reduced proper motions (Phan Bao et al. 2008, MNRAS, 383, 831). H_r=r+5.0*log10(PM)+5.0 > 20 KIC contains 13 million sources i-J>3.9; r-i>2.0; J-K>0.9 + proper motion in KIC = 15 UDC candidates Proper motions from UKIRT + 2MASS + Poss I, II + DSS = 15 UDC candidates +

9. UCDs in KIC: Spectroscopic follow-up  5 UCD candidates observed with KPNO 4m Mayall / RcSPEC (August 2011) : 1 L0, 2 M7, 1 M6, 1 M5  11 UCD candidates observed with NOT and TNG in Oct 2011, 13 validated 13/16 confirmed UCDs

10. UCDs in Kepler FoV: VO approach Cross correlation of archives of large-area surveys is very time-consuming task if performed by hand but, on the contrary, it is an approach that perfectly fits in the framework of the Virtual Observatory VO ultimate goal: Efficient access and analysis of the information available in the astronomical archives and services. Std s Tools Science

11. VO mining of KIS survey  KIS: Kepler-INT survey (Greiss et al. 2012 MNRAS) * 50 sq. deg. 6 million sources; U, g, r, i, Halpha  2MASS Point Source Catalogue. * Whole Sky (41253 sq. deg.). 471 million sources

12. UCD search: VO tools The tools: Aladin & TOPCAT

13. UCDs: VO criteria + VOSA validation All point sources in KIS with 2MASS counterparts within 10”, but no counterpart within 1” Color criteria (r-i)>2.0, (J-H) > 0.6 mag 5 new candidates UCD candidates validated with VOSA

14. UDCs are faint sources for Kepler!

15. UCDs in Kepler: Conclusions & Prospects 30 UDC candidates found in KIC: spectroscopic follow-up in 2011 confirmed 13/16 candidates  5 additional UDC candidates from KIS correlation with 2MASS using VO tools  GO Cycle 4 program accepted to observe 30 UDCs (GO40030)  Spectroscopic follow-up at KPNO and GTC scheduled in July 2012.  PSF photometric software for deblending faint sources. Photometric precision goal 5 mmag at Kp=19 for low cadence.  Expected results of Kepler observations of UDCs: Characterization of weather patterns; flare duty cycles; rotational periods & constrains on eclipsing binaries and close- in planets.