Eduardo L. Martín¹, Ramarao Tata², Enrique

Solano¹, Eder Martioli3, Simon Hodgkin4

Daniel Steeghs5

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

Ultracool dwarfs (UCDs): Definition

Ultracool dwarfs: Dwarfs with spectral type

later than M7 (Teff<2600K). Dust grain

condensation in atmospheres (Fe, Al2O3, MgSiO3).

UCDs: photometric variability •

Martin, Zapatero Osorio & Lehto 2001, ApJ, 557, 822

UCDs: photometric variability •

Bailer-Jones & Mundt 2001, A&A, 367, 218

★✪

---------------------------------------------------------Expected Kepler Precision @ Kp=18 in 30 min

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

First UCD in the Kepler field

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 +

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

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

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

UCD search: VO tools• The tools: Aladin & TOPCAT

UCDs: VO criteria + VOSA validationAll 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

UDCs are faint sources for Kepler!

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.