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Formation and Multiplicity of Brown Dwarfs and Giant Exoplanets

Explore the formation, evolution, and multiplicity of brown dwarfs and giant exoplanets. Conduct deep imaging and direct imaging with near-infrared adaptive optics systems. Search for very low-mass objects surrounding nearby young stars.

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Formation and Multiplicity of Brown Dwarfs and Giant Exoplanets

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  1. Binarysystems: from 0.2 arcsecto 2 deg José Antonio Caballero Centro de Astrobiología (CSIC-INTA), Madrid Double stars observers 2010

  2. Formation, evolution and multiplicity of browndwarfs and giantexoplanets Planets in closeorbits: searchfortransits ( photometricvariability)Planets in wideorbits: deepwideimaging No planetswithCAIN-II/1.5m TCS… Anexample, a stable, “single” browndwarf: Kelu 1 Caballero 2006, PhD

  3. SubstellarobjectsDe fuscispusillisastris et giganteisexoplanetis Caballero 2006, PhD

  4. Searchforverylow-massobjectssurroundingnearbyyoungstarsDirectimagingwithnear-infraredadaptiveopticssystems at 4 m-classtelescopes: • Naomi+Ingrid / 4.2 m WHT • Alfa+Omega-Cass / 3.5 m Calar Alto • AdOpt-at-TNG / 3.6 m Telescopio Nazionale Galileo • And coronographywith: • NICMOS / HubbleSpaceTelescope Caballero 2006, PhD

  5. Searchforverylow-massobjectssurroundingnearbyyoungstarsComplement: wide-fieldsearchwith CAIN-II / TCS and otherinstrumentsAbletodetectallbrowndwarfsat s > 50 AU and allplanetswithM > 0.008 Msol at s > 100 AU... Example: G 196-3A and B, a youngstar in the Local Associationwithan L-typecompanionof… 0.020-0.030 Msol Caballero 2006, PhD

  6. Caballero 2006, PhD HD 189087 AB: from 7 x 7 arcmin2to 3 x 3 arcsec2

  7. Searchforverylow-massobjectssurroundingnearbyyoungstars51 systemswithfeatures of youth (lithium, chromosphericactivity, X-rayemission, membership in movinggroups):- 44 withages 600 Ma- 32 withages  100 Ma* 3-4 new stellarcompanions* Upperlimitsonthefrequency of companions* BUT...AB Dor CHD 160934 ACHN Peg B Caballero 2006, PhD

  8. Searchforverylow-massobjectssurroundingnearbyyoungstars51 systemswithfeatures of youth (lithium, chromosphericactivity, X-rayemission, membership in movinggroups):- 44 withages 600 Ma- 32 withages  100 Ma* 3-4 new stellarcompanions* Upperlimitsonthefrequency of companions* BUT...AB Dor CHD 160934 ACHN Peg B Caballero 2006, PhD

  9. “De Mayrit al cielo”: • Orioniscluster • ( ~ 3 Ma, d ~ 385 pc) • Themost complete initialmassfunction (from 18 to 0.003 Msol) • Brown dwarfs (with discs, X-rayemission, Haemission…) and “isolated” planetary-massobjects Caballero+

  10. “De Mayrit al cielo”: • Orioniscluster • ( ~ 3 Ma, d ~ 385 pc) • Verywidebinaries + Statisticalapproach • 3 resolved systemswithprobabilities of alignementby chance of 1% (2 are triple) • Separations: 7.6-14.1 arcsec (2700-5100 AU) • And… Caballero 2009, CoolStars15

  11. “De Mayrit al cielo”: • Orioniscluster • ( ~ 3 Ma, d ~ 385 pc) • “B”: S Ori 68: L5.0, ~5 MJup, Ha • “A”: [SE2004] 70: M6.0, ~45 MJup, low-gravity, X-rayflare, Ha, radial velocity, Li I • = 4.6 arcsec s =1700 AU • Thewidest “planetary” system? Caballero et al. 2006, A&A

  12. “De Mayrit al cielo”: • Orioniscluster • ( ~ 3 Ma, d ~ 385 pc) • Importantbecause: • itilluminatestheHorseheadNebula • X-rayemitterpopulation • discs at 3 Ma • a helium-rich, magnetically-active B2Vp star • Herbig-Haroobjects • accretionrates and frequency… Caballero+

  13. s Ori (Uranometria: Bayer 1603) 48 Ori (Flamsteed’s catalogue: Flamsteed 1712)BD-02 1326 (BonnerDurchmusterung des sudlichenHimmels: Schonfeld 1886)HD 37468 (Henry Draper catalogue: Cannon & Pickering 1925) Caballero 2006, PhD

  14.  Ori E (Tabula Nova StellarumDuplicium: Mayer 1779) Ori C, D (Struve et al. 1876)s Ori B (Burnham 1892) Caballero 2007, AN

  15. 10 000 AU A near-IR counterpart of a mid-IR source: sOri IRS1, anevaporatingproplyd? Alsodetected in X-rays (Caballero et al. 2010, A&A) Caballero 2005, AN

  16. s Ori IRS1 s Ori B s Ori A On-goinghigh-resolution (lucky) imaging (withFastCam/1.5 m TCS) A*: O9.5V, 18 Msol B: B0.5V, 12 Msol C: A2.0V, 2.7 Msol D: B2.0V, 6.8 Msol E: B2.0Vp, 7.4 Msol Caballero in prep.

  17. Angular separation of r ~ 0.26 arcsec(withFastCam/2.5 m NOT) Caballero in prep.

  18. Angular separation of r ~ 0.26 arcsec(withFastCam/2.5 m NOT) And NaCo/8.4 m VLT resolvess Ori IRS1! Un-published

  19. sOrionis: Themostmassive “binary” withanastrometricorbit(Mason et al.) Caballero in prep.

  20. Orionis: Themostmassive “binary” withanastrometricorbit(Mason et al.) • New fit:a = 0.264  0.006 arcsece = 0.0528  0.013i = 154.9  1.0 degP = 155.4  0.5 a Caballero in prep.

  21. On-goinghigh-resolutionspectroscopy (P’~143 d; Aa: O9.5V, 18 Msol, Ab: B0V, 15 Msol) TAa= 34 kK, vsini = 110km/s TAb= 32 kK, vsini = 30km/s TB = 31 kK, vsini = 60km/s Up to 18+15+12 = 45 Msol! Simón-Díaz & Caballero in prep.

  22. Caballero 2008, A&A

  23. Themassfunctiondowntotheplanetarydomain in thesOrioniscluster Derivation of themassfunctionfrom 0.11 to 0.006 Msol, withindexa = 0.4-0.6 (DN/DMM-a; Salpeter: a = 2.35). Frequency of sOrionisbrowndwarfswith discs is 47 ± 9 % Caballero et al. 2007, A&A

  24. Themassfunctiondowntotheplanetarydomain in thesOrioniscluster Derivation of themassfunctionfrom 0.11 to 0.006 Msol, withindexa = 0.4-0.6 (DN/DMM-a; Salpeter: a = 2.35). Frequency of sOrionisbrowndwarfswith discs is 47 ± 9 % Caballero et al. 2007, A&A

  25. Caballero 2007a, A&A

  26. Koenigstuhl 1AB: a serendipitousdiscovery… A: LEHPM 494 [?] B: DENIS J0021.0-4244 [M9.5V] r ~ 1.3 arcmin B UK Schmidt 1977.6 R ESO 1984.9 IJK DENIS 1996.5 R UK Schmidt 1996.6 I UK Schmidt 1999.6 JHKs 2MASS 1999.6 [3.8:8.0]Spitzer 2004.0 Caballero 2007a, A&A

  27. Koenigstuhl 1AB:the (second) widestultracoolbinary: a challengeforverylow-massformationejectionscenarios! •  = 77.76 ± 0.07 arcsec • d = 23 ± 2 pc • s = 1800 ± 170 AU • MA = 0.103 ± 0.006 Msol • MB = 0.079 ± 0.004 Msol • Highlight of theweek in A&A.Almostcover page! Caballero 2007a, A&A

  28. Koenigstuhl 2 AB: A new verylow-massstar in a widebinary (thethirdwidestsystemwith MA + MB < 0.4 Msol) • Primary: LP 655-23 • (Luyten 1979) • Secondary: 2M0430-08 (M8.0V; Cruz et al. 2003) • s = 450 ± 40 AU • MA = 0.26 ± 0.04 Msol • MB = 0.086 ± 0.004 Msol Caballero 2007b, ApJ

  29. Koenigstuhl 3 ABC: thewidestsystemcontainingan L dwarfcomponent Primary: HD 221356 (F8.0V; Hipparcos) Secondary: 2M2331-04AB (M8.0V+L3.0V; Gizis et al. 2000, 2003) r = 7.530 ± 0.007 arcmin s = 11900 ± 300 AU MA= 1.02 ± 0.07 Msol MBC= 0.088+0.072 Msol Caballero 2007b, ApJ

  30. A Virtual ObservatorysearchforcompanionstoLuytenstars • 20physicalsystemswithbothstarcomponents in Hipparcos • 29physicalsystemswithonlyonestarcomponent in Hipparcos • 19physicalsystemswith no components in Hipparcos • Half a dozen new serendipitously-discoveredphysicalsystems Caballero, Miret et al. in prep

  31. G 125-15 AB + G 125-14 = WDS 19312+3607 (seepaper in folder) Caballero et al. 2010, A&A

  32. Caballero et al. 2010, A&A

  33. Reachingtheboundarybetweenstellarkinematicgroups and verywidebinaries. I • WDS starswiththewidest angular separations (r > 999 arcsec): N=30 • Visual orunidentifieddoubles: N=23 • Physicaldoublecandidates: N=7 (includingaCentauri A, B and C) Caballero 2009, A&A

  34. Reachingtheboundarybetweenstellarkinematicgroups and verywidebinaries. I • Sixstarswith s > 0.1 pc (previouslyassumedupperlimittothedistribution of widebinarysemimajoraxes) • Fourstarswith s > 0.2 pc • Comparison of gravitationalbindingenergies (U=-GMAMB/r) Caballero 2009, A&A

  35. Caballero 2009, A&A

  36. Reachingtheboundarybetweenstellarkinematicgroups and verywidebinaries. II Thewidestbinary! Caballero 2010, A&A

  37. Caballero 2007a, A&A

  38. Future: • Luytenstars (& Miret et al.) • nearbyyoungstars (& Alonso-Floriano, Montes) • ultracooldwarfs (& Montes) • and much, much more… Caballero & ???

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