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José A. Caballero Universidad Complutense de Madrd /ka-ba-jé-ro/

From 1000 AU to 1000 pc: from wide binaries in the solar neighbourhood, through the s Orionis cluster, to distant OB associations. José A. Caballero Universidad Complutense de Madrd /ka-ba-jé-ro/. Welcome! ¡Bienvenidos! Bienvenue! Willkommen! Benvenuti! Bem-vindo! Kalw   l  ate Aloha.

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José A. Caballero Universidad Complutense de Madrd /ka-ba-jé-ro/

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  1. From 1000 AU to 1000 pc:from wide binaries in the solar neighbourhood, through the s Orionis cluster, to distant OB associations José A. Caballero Universidad Complutense de Madrd /ka-ba-jé-ro/

  2. Welcome!¡Bienvenidos!Bienvenue!Willkommen!Benvenuti!Bem-vindo!KalwlateAlohaWelcome!¡Bienvenidos!Bienvenue!Willkommen!Benvenuti!Bem-vindo!KalwlateAloha El Escorial: just 30 km awaw from ESAC

  3. What is VO?AladinVODesktopVOSpecSPLATTopcatVOPlotVOSAVOSED

  4. 4.2m William Herschel Telescope (ORM): NAOMI+INGRID, INGRID, LIRIS, ISIS, AF2+WYFFOS, PFCAM * 3.6m Telescopio Nazionale Galileo (ORM): AdOpt/TNG, NICS, OIG * 3.6m ESO Telescope (LS): EFOSC-2 * 3.6m New Technology Telescope (LS): SofI * 3.5m Calar Alto Teleskop (CA): ALFA+W-Cass, W-2000 * 2.6m Nordic Optical Telescope (ORM): ALFOSC, FastCAM * 2.5m Isaac Newton Telescope (ORM): WFC, IDS * 2.2m Calar Alto Teleskop (CA): MAGIC * 1.5m Telescopio Carlos Sánchez (OT): CAIN-2, FastCAM * 1.0m European Space Agency Orbital Ground Station (OT): ESACCD * 1.0m Jacobus Kapteyn Telescope (ORM): JAG * 0.8m Telescopio IAC-80 (OT): old CCD, new CCD Keck Observatory: LRIS * Very Large Telescope: ISAAC, NACO * Gemini South: T-ReCS * Canada-France-Hawai’i Telescope: CFHT-IR Hubble Space Telescope: NICMOS * Spitzer Space Telescope: IRAC, MIPS * XMM-Newton Telescope: EPIC * Chandra Space Telescope: HRC-I, ACIS * International Ultraviolet Explorer: LWP, LWR * ROSAT: HRI Gran Telescopio Canarias: CanariCAM, EMIR, NAHUAL * 3.5m Calar Alto Teleskop: CARMENES * 2.2m Calar Alto Teleskop: PANIC * World Space Observatory-UV: ISSIS What is not VO?(I’m a “realistic” observer)In situ used: 23 instruments at 12 telescopes in 4 observatories (>250 nights)Analysis: 5 instruments at 10 to 4 m-class telescopesSpace missions: 6 (from X-rays to mid-infrared)Science groups and developement of new instrumentation: 6Multi-wavelength: from 24 mm to 7.5 keV

  5. Why VO?A comfortable open goldmine for observers: * No telescope time application* No telescope observations (no travel -cheap, ecological-, no bad weather, no family matters)* No data reduction* No calibration (astrometry, photometry)Is the VO useful? YES!(VO splinter session at the meeting of the Sociedad Española de Astronomía)

  6. The s Orionis cluster: probably the best current laboratory of star formation t ~ 3 Ma, d ~ 385 pc, AV ~ 0.3 mag A long time ago, in a galaxy far, far away.... • Massive, solar-like and low-mass stars, brown dwarfs and objects below the deuterium burning mass limit, IPMOs • (from 18 to 0.003 Msol): • Opacity mass limit • Mass function • Discs, jets and angular momentum evolution • X-ray emission • Ultracool atmospheres... A couple of years ago, in the s Orionis cluster...

  7. OVO: Orion Virtual Observatory. 0(Caballero 2006, PhD thesis, Universidad de La Laguna, Spain)The substellar mass function in s Orionis. II. Optical, near-infrared and IRAC/Spitzer photometry of young brown dwarfs and planetary-mass objects(Caballero et al. 2007, A&A, 470, 903)

  8. OVO: Orion Virtual Observatory. I“In spite of the importance of the cluster, its stellar population is paradoxically poorly known” (2006)The brightest stars of the s Orionis cluster (OVO1)(Caballero 2007b, A&A, 466, 917)Tycho+2MASS (+IRAS, ROSAT, literature spectroscopy), 30 arcminAladin: proper motion, photometry, mid infrared, X-ray26 stars with M = 18-1.2 Msol* Mass function * SEDs * Frequency of discs * X-ray variability * Overlapping of young populations...

  9. Koenigstuhl 1AB a serendipitous discovery in Caballero et al. (2007) 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

  10. Koenigstuhl 1 AB (Caballero 2007a, A&A, 462, L61) The (second) widest ultracool binary: a challenge for very low-mass formation ejection scenarios! Highlight of the week in A&A (February II 2007) Almost cover page! r = 77.76 ± 0.07 arcsec d = 23 ± 2 pc r = 1800 ± 170 AU MA = 0.103 ± 0.006 Msol MB = 0.079 ± 0.004 Msol

  11. Koenigstuhl 2 AB (Caballero 2007d, ApJ, 667, 520) A new very low-mass star in a wide binary: the third widest system with MA + MB < 0.4 Msol (in a draw) Primary: LP 655-23 (Luyten 1979) Secondary: 2M0430-08 (M8.0V; Cruz et al. 2003) r = 450 ± 40 AU MA = 0.26 ± 0.04 Msol MB = 0.086 ± 0.004 Msol

  12. Koenigstuhl 3 ABC (Caballero 2007d, ApJ, 667, 520) The widest system containing an L dwarf component Frequency of wide multiples with late-type (>M5) components: 5.0 ± 1.8 % Primary: HD 221356 (F8.0V; Hipparcos) Secondary: 2M2331-04AB (M8.0V+L3.0V; Gizis et al. 2000, 2003) r = 7.530 ± 0.007 arcmin r = 11900 ± 300 AU MA= 1.02 ± 0.07 Msol MBC= 0.088+0.072 Msol And Koenigstuhl 4 AB is coming! (Caballero, in prep.)

  13. OVO: Orion Virtual Observatory. IIStars and brown dwarfs in the s Orionis cluster: the Mayrit catalogue (OVO2)(Caballero 2008c, A&A, 478, 667)DENIS+2MASS (+literature information on spectral type, lithium, disc, proper motion, X-ray), 30 arcminCompilation of 241 very young stars and brown dwarfs, 115 fore- and background objects, 97 new cluster member candidates Mayra(“source of water”) + it  Mayrit  Matrit  MADRID

  14. OVO: Orion Virtual Observatory. IIThe Mayrit catalogue, a useful tool for investigating:* Spatial distribution (Caballero 2008b; Bouy et al. 2008)* Disc frequency as a function of stellar mass (Luhman et al. 2008)* X-ray emission (López-Santiago & Caballero 2008; Franciosini et al. in prep.)* Spectroscopic follow-up (González-Hernández et al. 2008; Cody et al. in prep.)* Wide binaries and mass function from 18 to 0.035 Msol(Caballero 2008d, CoolStars15, arXiv:0810:2029)

  15. OVO: Orion Virtual Observatory. IIILook for analogues to the s Orionis cluster (t, d, AV)Not far away: Alnilam and Mintaka in the Orion Belt (Ori OB1b)Tycho+2MASS, DENIS+2MASS (+literature information on spectral type, lithium, disc, proper motion, X-ray), 45 arcminDevelopment: 10 control fields at similar galactic latitude

  16. OVO: Orion Virtual Observatory. IIIYoung stars and brown dwarfs surrounding Alnilam (e Ori) and Mintaka (d Ori) (OVO3)(Caballero & Solano 2008, A&A, 485, 931)The Annizam/Mantaqah catalogue: * 136 very young stars* 289 photometric star candidates* 2 brown dwarf candidates* No confirmation of Collinder 70* A new star cluster surrounding Mintaka* Clusters? More massive, more extended, slightly older and less radially concentrated than s Orionis

  17. Albus 1 (Caballero & Solano 2007, ApJ, 665, L151) Serendipitous discovery of a very brightwhite dwarfcandidate... ...that is actually one of the brightest He-B subdwarfs (Vennes, Kawka & Smith 2007, ApJ, 668, L59; R. Oreiro et al., in prep.)

  18. A revisit to agglomerates of early-type Hipparcos stars (Caballero & Dinis 2008, 329, 801) New hunting grounds for young brown dwarfs = OB associations Hipparcos stars with BT-VT < -0.05 mag (van Leeuwen 2007) Densitity-Based Spatial Clustering of Applications with Noise Data and bibliographic compilation of stars in agglomerates (“clusters”) Caballero (astrophysicist) & Dinis (theoretical physicist): El Escorial, 1977

  19. A revisit to agglomerates of early-type Hipparcos stars • 35 agglomerates (Escorial 1-35): • Pleiades, NGC 2264, M47... • Ori OB1 super-agglomerate (e.g. Orion Nebula Cluster, s Orionis, Collinder 70, 25 Orionis...) • Upper Cma-Pup super-agglomerate (Collinder 121...) • Pup-Vel super-agglomerate (IC 2391, NGC 2451 A...) • d = 100-1000 pc

  20. A revisit to agglomerates of early-type Hipparcos stars * Tycho+2MASS, DENIS+2MASS, bibliography... * Isochrones * Spatial distribution analysis A new cluster: P Puppis (Escorial 25) d = 470 ± 70 pc t = 10+10-5 Ma And new sites for substellar searches: vdBH 23, Trumpler 10, NGC 2232...

  21. OVO: Orion Virtual Observatory. IV, V, VI...Stars and brown dwarfs in the s Orionis cluster: the Mayrit catalogue 2.0 (OVO4)(Caballero in prep.)* Updated bibliography* YZJHK UKIDSS photometry* [3.6, 4.5, 5.8, 8.0, 24.0] Spitzer photometry* Spectral types* Li Il6708Å (pseudo-)equivalent widths* Ha emission* Radial velocities* X-ray fluxes... And 2XMM data and SEDs of stars surrounding Alnilam (e Ori, Collinder 70), a new clustering analysis of Tycho-2 stars in Ori OB, the Mayrit3 catalogue, and mucho more...

  22. Preliminary results on a Virtual Observatory search for companions to Luyten stars (Caballero, Miret, Genebriera, Tobal, Cairol, Montes 2008, SEA08, arXiv:0810.2030) The Garraf survey: an Aladin-based search for common-, high-proper motion pairs 1947 stars in the New Luyten Two Tenths (NLTT)catalogue (Luyten 1979) with improved astrometry in Salim & Gould (2003) and m = 0.5-1.0 arcsec a-1

  23. Preliminary results on a Virtual Observatory search for companions to Luyten stars • Methodology: • Data loading and cross-matching: USNO-B1+2MASS (Aladin) • Proper-motion diagram and candidate selection (VOPlot) • Follow-up with catalogues and images: DSS1, DSS2, CMC14, DENIS, SDSS, 2MASS, UKIDSS... • 20 physical systems with both star components in Hipparcos • 29 physical systems with only one star component in Hipparcos • 19 physical systems with no components in Hipparcos • Half a dozennew serendipitously-discovered physical systems

  24. Garraf 1AB: a bright, young, very wide, low-mass binary in the solar neighbourhood (Caballero, Genebriera, Miret, Tobal, Cairol, Montes, Pedraz, to be submitted to A&A Letters) Multi-epoch relative astrometry: 1952 Jul POSSI Red 1988 Jun POSSII Blue 1992 Aug POSSII Red 1993 Jun POSSII Infrared 1998 Jun 2MASS 2001 Aug CMC14 2008 Mar Tacande 2008 Apr CAFOS/2.2m CAHA 2008 Oct Tacande BVRIJHKs photometry and low-resolution spectroscopy A: G 125-15, M4.5e, X-ray, variable B: G 125-14, M5.5: Known binary in Giclas et al. (1971) r = 46.0 ± 0.3 arcsec  = 347.34 ± 0.16 deg d = 17+6-5 pc r = 800+300-200 AU MA = 0.21+0.08-0.05 Msol MB = 0. 12+0.04-0.03 Msol t ~ 300 Ma?

  25. On-going work(Caballero in prep.; Caballero et al. in prep.)* Reaching the boundary between stellar kinematic groups and very wide binaries - I. The widest systems in the Washington Double Star Catalogue- II. ... and ...: a common proper motion pair in Castor separated by 1.0 pc- III. Very wide Hipparcos binaries* Proper motion companions to exoplanet host stars * New members in nearby young stellar moving groups* SU2: SDSS+USNO-B1+2MASS... Image not available... Yet!

  26. Open questionWhat will be a trained investigator be able to do with: SDSS + UKIDSS + LSST + Pan-STARRS + RAVE + GAIA + ...?

  27. Final remarksQueridos Reyes Magos de Oriente / Heilige Drei Könige-Weihnachtsmann / Santa Claus / Père Noël / Saint Nicholas / Babbo Natale / Father Christmas / Joulupukki / Sinterklaas...This year I conducted very well, and I want:* Not to get crazy with updating 32-bit Java plugins in my 64-bit Linux machine* Not to write “ps –fu caballero | grep aladin” and “kill –9 xxxx” again* A tool for huge cross-matching (e.g. all-sky Tycho+2MASS)* Akari, UKIDSS, SDSS-III data on Aladin* A new post-doc in 2010

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