josé a. caballero universidad complutense de madrd /ka-ba-jé-ro
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
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