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

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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?. - PowerPoint PPT Presentation

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

  • Jos Antonio CaballeroCentro de Astrobiologa (CSIC-INTA), MadridBrown dwarfs from SpainIm not talking on CARMENES

  • Q1: Who discovered the first brown dwarf? And when?Theoretical prediction: Kumar 1963Hayashi & Nakano 1963

    Given name:Tarter 1976

  • Teide 1 (Rebolo, Martn & Zapatero Osorio 1995)

    In the Pleiades ~125 Mad = 118 pcSpT: M8V (with lithium!)M = 50 MJup

  • Kelu 1 AB with CAIN-II at 1.5m TCS (Teide)De fuscis pusillis astris et giganteis exoplanetis: Pumilio fusca Brown dwarf Enana marrn / caf Naine brune Brauner Zwerg Nana bruna An marromQ2: Are brown dwarfs brown?A2: They are infrared And faint!

  • Mass-effective temperature-colour sequence:

    Aguerri: galaxy clusters Snchez-Blanco: nearby/distant galaxies Simn-Daz: massive stars in the Local Group Bouy: stars in the Galaxy Caballero: brown dwarfs? Pall: exoplanets Ortiz: TNOs in Solar SystemO Be A Fine Girl Kiss My Lips Tonight (Yeah!)

  • 1997: Delfosse et al. (DENIS) found the first objects with L spectral type

    Teff 2200-1300 K

  • 1995: Nakajima et al. found the first object with T spectral type (GJ 229B)

    Teff 1300-700 K

  • 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

  • Jos Antonio CaballeroCentro de Astrobiologa (CSIC-INTA), MadridUltracool dwarfs from SpainIm not talking on CARMENES yet

  • TelescopeInstruments todayInstruments tomorrow10.4 m GTCOSIRIS, CanariCamOSIRIS, CanariCam, CIRCE, EMIR, FRIDA, ELMER, EMIR, MEGARA, MIRADAS6.5 m HEXAHECATE, MONSUL, GEA4.2 m WHTISIS, LIRIS, AutoFib2/WYFFOS, ACAM, PFIP, NAOMI/Ingrid-Oasis-Osca, (VIs)WEAVE, +?3.6 TNGDOLORES, NICS, SARG, HARPS-NHARPS-N, GIANO, +?3.5 m CAHALAICA, MOSCA, PMAS, TWIN, 2kCARMENES, PMAS2.6 m NOTALFOSC, NOTCam, FIES, MOSCA, StanCam?2.5 m INTWFC, IDSWFC, IDS2.5 m J-T250JPCamJPCam2.2 m CAHABUSCA, CAFOS, CAF, AstraLux, MAGICPANIC, CAF

  • Future of ultracool studies:

    10.4 m GTC: out of discussion 6.5 m HEXA: HECATE Gaia-machine with substellar potential (esp., young brown dwarfs in open clusters) 4.2 m WHT: WEAVE Gaia-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: JPCam Ultrawide-field optical imager 2.2 m CAHA: PANIC Wide-field near-infrared imager

  • Complementary to ETSRC report, but focused on ultracool dwarfs:

    Wide-field optical imagers: WFC, JPCam (South: VST Paranal, LSST Cerro Pachn; North: SuperSDSS) What else!? WFC age?

    Wide-field near-infrared imager: PANIC (South: VISTA; North: UKIDSS) Perfect for > +20 deg, but overlaps with VISTA below (ZYJHKs)

    PANICs dilemma: complement VISTA, UKIDSS, 2MASS? Depth Repetition (proper motions, monitoring) Spatial resolution (@3.5mCA) New sites (or VLS?) / new filters

  • 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--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, Garca-lvarez, Cabrera and the GTC/VSOP Team, in prep.

  • 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)

  • *:Planet or planetary-mass object

    Object2H burning1H burningMass(Msol [MJup])

    (Zsol)Staryesyes>0.075 [> 72]Sub-stellar objectBrown dwarfyesno0.075-0.013 [72-14]Planet*nono