From 1000 AU to 1000 pc from wide

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 El Escorial: just 30 km awaw from ESAC

What is VO? Aladin VODesktop VOSpec SPLAT Topcat VOPlot VOSA VOSED

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 mclass telescopes Space missions: 6 (from X-rays to midinfrared) Science groups and developement of new instrumentation: 6 Multi-wavelength: from 24 mm to 7. 5 ke. V 4. 2 m William Herschel Telescope (ORM): NAOMI+INGRID, LIRIS, ISIS, AF 2+WYFFOS, PFCAM * 3. 6 m Telescopio Nazionale Galileo (ORM): Ad. Opt/TNG, NICS, OIG * 3. 6 m ESO Telescope (LS): EFOSC-2 * 3. 6 m New Technology Telescope (LS): Sof. I * 3. 5 m Calar Alto Teleskop (CA): ALFA+W-Cass, W-2000 * 2. 6 m Nordic Optical Telescope (ORM): ALFOSC, Fast. CAM * 2. 5 m Isaac Newton Telescope (ORM): WFC, IDS * 2. 2 m Calar Alto Teleskop (CA): MAGIC * 1. 5 m Telescopio Carlos Sánchez (OT): CAIN-2, Fast. CAM * 1. 0 m European Space Agency Orbital Ground Station (OT): ESACCD * 1. 0 m Jacobus Kapteyn Telescope (ORM): JAG * 0. 8 m Telescopio IAC-80 (OT): old CCD, new CCD Keck Observatory: LRIS * Very Large Telescope: ISAAC, NACO * Gemini South: T-Re. CS * 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: Canari. CAM, EMIR, NAHUAL * 3. 5 m Calar Alto Teleskop: CARMENES * 2. 2 m Calar Alto Teleskop: PANIC * World Space Observatory-UV: ISSIS

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)

A long time ago, in a galaxy far, far away. . The Orionis cluster: probably the best current laboratory of star formation t ~ 3 Ma, d ~ 385 pc, AV ~ 0. 3 mag Massive, solar-like and low-mass stars, brown dwarfs and objects below the deuterium burning mass limit, IPMOs (from 18 to 0. 003 Msol): A couple of years ago, in the s Orionis cluster. . . • Opacity mass limit • Mass function • Discs, jets and angular momentum evolution • X-ray emission • Ultracool atmospheres. . .

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

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 (OVO 1) (Caballero 2007 b, A&A, 466, 917) Tycho+2 MASS (+IRAS, ROSAT, literature spectroscopy), 30 arcmin Aladin: proper motion, photometry, mid infrared, X-ray 26 stars with M = 18 -1. 2 Msol * Mass function * SEDs * Frequency of discs * X-ray variability * Overlapping of young populations. . .

Koenigstuhl 1 AB a serendipitous discovery in Caballero et al. (2007) A: LEHPM 494 [? ] B: DENIS J 0021. 0 -4244 [M 9. 5 V] 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 2 MASS 1999. 6 [3. 8 -8. 0] Spitzer 2004. 0

Koenigstuhl 1 AB (Caballero 2007 a, A&A, 462, L 61) The (second) widest ultracool binary: a challenge for very lowmass formation ejection scenarios! 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 Highlight of the week in A&A (February II 2007) Almost cover page!

Koenigstuhl 2 AB (Caballero 2007 d, Ap. J, 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: 2 M 0430 -08 (M 8. 0 V; Cruz et al. 2003) r = 450 ± 40 AU MA = 0. 26 ± 0. 04 Msol MB = 0. 086 ± 0. 004 Msol

Koenigstuhl 3 ABC (Caballero 2007 d, Ap. J, 667, 520) Frequency of wide multiples with late-type (>M 5) components: 5. 0 ± 1. 8 % The widest system containing an L dwarf component Primary: HD 221356 (F 8. 0 V; Hipparcos) Secondary: 2 M 2331 -04 AB (M 8. 0 V+L 3. 0 V; 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. )

OVO: Orion Virtual Observatory. II Stars and brown dwarfs in the s Orionis cluster: the Mayrit catalogue (OVO 2) (Caballero 2008 c, A&A, 478, 667) DENIS+2 MASS (+literature information on spectral type, lithium, disc, proper motion, X-ray), 30 arcmin Compilation 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

OVO: Orion Virtual Observatory. II The Mayrit catalogue, a useful tool for investigating: * Spatial distribution (Caballero 2008 b; 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 2008 d, Cool. Stars 15, ar. Xiv: 0810: 2029)

OVO: Orion Virtual Observatory. III Look for analogues to the s Orionis cluster (t, d, AV) Not far away: Alnilam and Mintaka in the Orion Belt (Ori OB 1 b) Tycho+2 MASS, DENIS+2 MASS (+literature information on spectral type, lithium, disc, proper motion, Xray), 45 arcmin Development: 10 control fields at similar galactic latitude

OVO: Orion Virtual Observatory. III Young stars and brown dwarfs surrounding Alnilam (e Ori) and Mintaka (d Ori) (OVO 3) (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

Albus 1 (Caballero & Solano 2007, Ap. J, 665, L 151) Serendipitous discovery of a very bright white dwarf candidate. . . that is actually one of the brightest He-B subdwarfs (Vennes, Kawka & Smith 2007, Ap. J, 668, L 59; R. Oreiro et al. , in prep. )

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

A revisit to agglomerates of early-type Hipparcos stars 35 agglomerates (Escorial 1 -35): • Pleiades, NGC 2264, M 47. . . • Ori OB 1 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

A revisit to agglomerates of early-type Hipparcos stars * Tycho+2 MASS, DENIS+2 MASS, 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: vd. BH 23, Trumpler 10, NGC 2232. . .

OVO: Orion Virtual Observatory. IV, V, VI. . . Stars and brown dwarfs in the s Orionis cluster: the Mayrit catalogue 2. 0 (OVO 4) (Caballero in prep. ) * Updated bibliography * YZJHK UKIDSS photometry * [3. 6, 4. 5, 5. 8, 8. 0, 24. 0] Spitzer photometry * Spectral types * Li I l 6708Å (pseudo-)equivalent widths * Ha emission * Radial velocities * X-ray fluxes. . . And 2 XMM data and SEDs of stars surrounding Alnilam (e Ori, Collinder 70), a new clustering analysis of Tycho -2 stars in Ori OB, the Mayrit 3 catalogue, and mucho more. . .

Preliminary results on a Virtual Observatory search for companions to Luyten stars (Caballero, Miret, Genebriera, Tobal, Cairol, Montes 2008, SEA 08, ar. Xiv: 0810. 2030) The Garraf survey: an Aladinbased search for common-, highproper motion pairs 1947 stars in the New Luyten Two Tenths (NLTT) catalogue (Luyten 1979) with improved astrometry in Salim & Gould (2003) and m = 0. 51. 0 arcsec a-1

Preliminary results on a Virtual Observatory search for companions to Luyten stars Methodology: • Data loading and cross-matching: USNO-B 1+2 MASS (Aladin) • Proper-motion diagram and candidate selection (VOPlot) • Follow-up with catalogues and images: DSS 1, DSS 2, CMC 14, DENIS, SDSS, 2 MASS, 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 dozen new serendipitouslydiscovered physical systems

Garraf 1 AB: 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 A: G 125 -15, M 4. 5 e, X-ray, variable 1988 Jun POSSII Blue B: G 125 -14, M 5. 5: 1992 Aug POSSII Red Known binary in Giclas et al. (1971) 1993 Jun POSSII Infrared 1998 Jun 2 MASS 2001 Aug CMC 14 2008 Mar Tacande 2008 Apr CAFOS/2. 2 m CAHA 2008 Oct Tacande BVRIJHKs photometry and lowresolution spectroscopy 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?

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 * SU 2: SDSS+USNO-B 1+2 MASS. . . Image not available. . . Yet!

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

Final remarks Queridos 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. allsky Tycho+2 MASS) * Akari, UKIDSS, SDSS-III data on Aladin * A new post-doc in 2010