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José Antonio Caballero Centro de Astrobiología (CSIC-INTA), Madrid

Brown dwarfs from Spain. I’m not talking on CARMENES. José Antonio Caballero Centro de Astrobiología (CSIC-INTA), Madrid. Theoretical prediction: Kumar 1963 Hayashi & Nakano 1963 Given name: Tarter 1976. Q1: Who discovered the first brown dwarf? And when?.

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José Antonio Caballero Centro de Astrobiología (CSIC-INTA), Madrid

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  1. Brown dwarfs from Spain I’m not talking on CARMENES José Antonio Caballero Centro de Astrobiología (CSIC-INTA), Madrid

  2. Theoretical prediction: Kumar 1963 Hayashi & Nakano 1963 Given name: Tarter 1976 Q1: Who discovered the first brown dwarf? And when?

  3. Teide 1 (Rebolo, Martín & Zapatero Osorio 1995) In the Pleiades τ ~125 Ma d = 118 pc SpT: M8V (with lithium!) M = 50 MJup

  4. De fuscis pusillis astris et giganteis exoplanetis: • Pumilio fusca • Brown dwarf • Enana marrón / café • Naine brune • Brauner Zwerg • Nana bruna • Anã marrom Kelu 1 AB with CAIN-II at 1.5m TCS (Teide) Q2: Are brown dwarfs “brown”? A2: They are “infrared”… And faint!

  5. Mass-effective temperature-colour sequence: • Aguerri: galaxy clusters • Sánchez-Blanco: nearby/distant galaxies • Simón-Díaz: massive stars in the Local Group • Bouy: stars in the Galaxy • Caballero: brown dwarfs? • Pallé: exoplanets • Ortiz: TNOs in Solar System O Be A Fine Girl Kiss My Lips Tonight (Yeah!)

  6. 1997: Delfosse et al. (DENIS) found the first objects with L spectral type Teff ≈ 2200-1300 K

  7. 1995: Nakajima et al. found the first object with T spectral type (GJ 229B) Teff ≈ 1300-700 K

  8. Q3: Do all brown dwarfs have spectral types L or T (or Y)? And do all stars have spectral types M and earlier? A3: No. There are (young) M-type brown dwarfs and (old) L-type stars! It depends on age... This way… 

  9. Ultracool dwarfs from Spain I’m not talking on CARMENES yet José Antonio Caballero Centro de Astrobiología (CSIC-INTA), Madrid

  10. Future of ultracool studies: • 10.4 m GTC: out of discussion • 6.5 m HEXA: HECATEGaia-machine with substellar potential (esp., young brown dwarfs in open clusters) • 4.2 m WHT: WEAVEGaia-machine with (limited) substellar potential (“super-WYFFOS”) + ? • 3.6 m TNG: HARPS-N for exoplanets, GIANO for M dwarfs? Italian… • 3.5 m CAHA: CARMENES for exoplanets (around M dwarfs) • 2.6 m NOT: ? Nordic… • 2.5 m INT: WFC Wide-field optical imager • 2.5 m J-T250: JPCamUltrawide-field optical imager • 2.2 m CAHA: PANIC Wide-field near-infraredimager

  11. Complementary to ETSRC report, but focused on ultracool dwarfs: • Wide-field optical imagers: • WFC, JPCam (South: VST Paranal, LSST Cerro Pachón; North: SuperSDSS) What else!? WFC age? • Wide-field near-infrared imager: • PANIC (South: VISTA; “North”: UKIDSS) Perfect for δ > +20 deg, but overlaps with VISTA below (ZYJHKs) • PANIC’s dilemma: complement VISTA, UKIDSS,2MASS? • Depth • Repetition (proper motions, monitoring) • Spatial resolution (@3.5mCA) • New sites (or VLS?) / new filters

  12. Missing instruments: • Hi-throughtput optical imagers with good pixel sampling: ACAM/WHT, MOSCA/NOT… • Lucky imagers: AstraLux/2.2mCA (only WideFastCam/TCS) • Hi-throughput, wide-λ-coverage, mid- and lo-res long-slit spectrographs: ISIS/WHT, CAFOS/2.2mCA (only at GTC…) New X-Shooter-like instrument at a 2-4m telescope? ELMER at another one? OSIRIS/GTC: Caballero, García-Álvarez, Cabrera and the GTC/VSOP Team, in prep.

  13. To Marc Balcells: • Service-mode observations; better “Phase-2” • Pipeline-reduced data • Everything in VO after proprietary time • To David Barrado: • If, e.g., PANIC repeats the VISTA Galaxy Cluster Survey in only one band with same depth  order of magnitude of 100 nights • To both: • Do not forget efficient, multipurpose instruments at 2-m telescopes (e.g., X-ISIS)

  14. *:Planet or “planetary-mass object”

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