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 Orionis cluster, to distant OB associations

José A. CaballeroUniversidad Complutense de Madrd

/ka-ba-jé-ro/

Welcome!

¡Bienvenidos!

Bienvenue!

Willkommen!

Benvenuti!

Bem-vindo!

AlohaEl Escorial:

just 30 km awaw from ESAC

What is VO?

AladinVODesktopVOSpecSPLATTopcatVOPlotVOSAVOSED

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 telescopes

Space missions: 6 (from X-rays to mid-infrared)

Science groups and developement of new instrumentation: 6

Multi-wavelength: from 24 m to 7.5 keV

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+-

Cass, -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

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....

A couple of years ago, in the Orionis cluster...

The Orionis cluster: probably the best current

laboratory of star formation

~ 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):

•Opacity mass limit•Mass function

•Discs, jets and angular momentum evolution

•X-ray emission •Ultracool atmospheres...

OVO: Orion Virtual Observatory. 0(Caballero 2006, PhD thesis, Universidad de La Laguna, Spain)

The substellar mass function in 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)

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 Orionis cluster (OVO1)(Caballero 2007b, A&A, 466, 917)

Tycho+2MASS (+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 1AB a serendipitous discovery in Caballero et al. (2007)

A: LEHPM 494 [?]B: DENIS J0021.0-4244 [M9.5V] ~ 1.3 arcmin

B UK Schmidt 1977.6R 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

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!

= 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

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

Koenigstuhl 3 ABC (Caballero 2007d, ApJ, 667, 520)

The widest system containing an L dwarf component

Primary: HD 221356(F8.0V; Hipparcos)

Secondary: 2M2331-04AB (M8.0V+L3.0V; Gizis et al. 2000, 2003)

= 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.)

Frequency of wide multiples with

late-type (>M5) components: 5.0 ± 1.8 %

OVO: Orion Virtual Observatory. II

Stars and brown dwarfs in the 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 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 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)

OVO: Orion Virtual Observatory. III

Look for analogues to the Orionis cluster (, 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 arcmin

Development: 10 control fields at similar galactic latitude

OVO: Orion Virtual Observatory. III

Young stars and brown dwarfs surrounding Alnilam ( Ori) and Mintaka ( 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 Orionis

Albus 1 (Caballero & Solano 2007, ApJ, 665, L151)

Serendipitous discovery of a very bright white dwarf candidate...

...that is actually one of the brightest He-B subdwarfs

(Vennes, Kawka & Smith 2007, ApJ, 668, L59;

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, M47...•Ori OB1 super-agglomerate (e.g. Orion Nebula Cluster, 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+2MASS, DENIS+2MASS, bibliography...* Isochrones* Spatial distribution analysis

A new cluster: P Puppis (Escorial 25)

d = 470 ± 70 pc = 10+10

-5 Ma

And new sites for substellar searches: vdBH 23, Trumpler 10,

NGC 2232...

OVO: Orion Virtual Observatory. IV, V, VI...

Stars and brown dwarfs in the 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 I 6708Å (pseudo-)equivalent widths* H emission* Radial velocities* X-ray fluxes...

And 2XMM data and SEDs of stars surrounding Alnilam ( Ori,

Collinder 70), a new clustering analysis of Tycho-2 stars in Ori OB, the Mayrit3 catalogue, and

mucho more...

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 = 0.5-1.0 arcsec a-1

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 dozen new serendipitously-discovered physical

systems

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)

= 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

~ 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

* SU2: SDSS+USNO-B1+2MASS...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. all-sky Tycho+2MASS)

* Akari, UKIDSS, SDSS-III data on Aladin

* A new post-doc in 2010