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Multiplicity in the young s Orionis cluster: from massive stars to planets

Multiplicity in the young s Orionis cluster: from massive stars to planets. José Antonio Caballero Max-Planck-Institut für Astronomie. Koenigstuhl 1 AB (Caballero 2007a, A&A, 462, L61). B UK Schmidt 1977.6 R ESO 1984.9 IJK DENIS 1996.5 R UK Schmidt 1996.6 I UK Schmidt 1999.6

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Multiplicity in the young s Orionis cluster: from massive stars to planets

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  1. Multiplicity in the young s Orionis cluster: from massive stars to planets José Antonio Caballero Max-Planck-Institut für Astronomie

  2. Koenigstuhl 1 AB (Caballero 2007a, A&A, 462, L61) 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 r = 77.76(7) arcsec, r = 1800(170) AU, MA = 0.103(6) Msol,MB = 0.079(4) Msol

  3. Koenigstuhl 2 AB (Caballero 2007d, ApJ, to appear) Primary: LP 655-23 (Luyten 1979) Secondary: 2M0430-08 (M8.0V; Cruz et al. 2003) r = 19.7(2) arcsec, r = 450(40) AU, MA = 0.26(4) Msol,MB = 0.086(4) Msol

  4. Koenigstuhl 3 ABC (Caballero 2007d, ApJ, to appear) Primary: HD 221356 (F8.0V; Perryman et al. 1997) Secondary: 2M2331-04AB (M8.0V+L3.0V; Gizis et al. 2000, 2003) r = 7.530(7) arcmin ! r = 451.8(4) arcsec, r = 11900(300) AU, MA = 1.02(7) Msol,MBC = 0.088+0.072 Msol

  5. Artigau et al. (2007) Kö1AB Kö2AB Kö3ABC h CrB AB Proxima Centauri + a Cen AB The Bubbles diagram [M2< 0.2 Msol, Age > 10 Ma](Caballero 2007e, A&A, submitted)

  6. s Orionis: age = 3 Ma, d = 360 pc, AV < 0.3 mag Central Trapezium-like star system Ae/Be stars, T Tauri stars, ~100 brown dwarfs... The star-forming region with the largest number of candidate IPMOs: 27 (12 with spectroscopy) IPMO: isolated planetary-mass object (Caballero et al. 2007, A&A, in astro-ph) Multiplicity: not investigated... yet!

  7. s Orionis: the s Ori system 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 (2007b, A&A, 466, 917) rAB-E = 42 arcsec (15000 AU) Mayrit 21023 Mayrit 30241 Mayrit 36273 Mayrit 50279... Caballero (2007c, AN, in astro-ph) Where does the multiple system end and where does the cluster start?

  8. 10 000 AU s Ori IRS1 s Ori B s Ori A s Orionis: the s Ori system, zoom in • Ori IRS1: a “dust cloud” at 3.3 arcsec (1200 AU) to an OB-type pair (van Loon & Oliveira 2003)  a proplyd J- and H-band observations with NAOMI/WHT Caballero (AN, 2005, 326, 1007) X-ray observations with HRC-I/Chandra Caballero (AN, 2007c, in astro-ph) I-band Lucky-imaging observations with FastCam/TCS Caballero et al. (in prep.) s Ori AB: r = 0.250 arcsec, P = 158 a (Heintz 1997)

  9. s Orionis: more known resolved multiples A “classic” binary (Bonner Durchmusterung): HD 294272 AB (r = 8.472(10) arcsec, r = 3000 AU, MA = 3.8 Msol,MB = 3.0 Msol) AO binaries (Caballero 2005, AN, 326, 1007): HD 37525 AB (B5Vp, r = 0.47 arcsec) [W96] 4771-899 AB (K7V, r = 0.40 arcsec) Close low-mass binaries: Mayrit 707162 (r ~ 1.0 arcsec) (Caballero 2006, PhD thesis) Mayrit 92149 (r ~ 1.9 arcsec) (Caballero 2007c, AN, in astro-ph) And some “doubles” from Sherry, Walter & Wolk (2004)

  10. s Orionis: and more binaries... Spectroscopic binaries: OriNTT 429 AB (Lee et al. 1994) RX J0539.6-0242 AB (Alcalá et al. 1996; T Tauri) Two pre-main sequence stars (Wolk 1996) S Ori 36 (Kenyon et al. 2005; a brown dwarf!) Very close binaries, partially resolved (r < 1.0 arcsec): 2E 0537.2-0227 AB V605 Ori AB V604 Ori AB SWW 118 AB (Caballero 2007f, A&A, submitted) Kenyon also showed more SB1 brown-dwarf candidates

  11. Orionis: SE70 + S Ori 68 (Caballero et al. 2006, A&A, 460, 635) S Ori 68: I=23.8 mag, L5.0, M ~5 MJup SE 70: I=17.1 mag, M ~45 MJup, no variable (Scholz & Eislöffel 2004), low gravity (Burningham et al. 2005), X-ray flare (Franciosini et al. 2006), Li I, chromospheric Ha, radial velocity (Caballero et al. 2006) r = 4.6 arcsec (1700±300 AU) The widest planetary system?

  12. s Orionis A B (C D) HD 294271 HD 37525 HD 37686 HD 37333 4771-899

  13. Orionis: very wide binaries? (Caballero 2007f, A&A, submitted) 12 resolved systems with probabilities of alignement by chance 1-5% Statistical approach Separations: 7.6-19 arcsec (2700-7000 AU) Five triples Two star-brown dwarf systems More details: /Xosé Kabajéro/

  14. Multiplicity in s Orionis: summary Previously known: the massive central system, some tight and spectroscopic binaries From now on: binary candidates at very wide separations (r > 1500 AU) Caveats: are they really bound? Very low proper motion   LBT, JWST (imaging), Keck, Gran Telescopio Canarias (radial velocity) ¡Gracias!

  15. Ca07f #1 AB Ca07f #2 AB Ca07f #3 AB Ca07f #4 AB SE70 + S Ori 68 The Bubbles diagram [M2< 0.2 Msol, final] (Caballero 2007e, A&A, submitted)

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