José Antonio CaballeroCentro de Astrobiología (CSIC-INTA), Madrid

Brown dwarfs from Spain

I’m 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, Martín & Zapatero Osorio 1995)

In the Pleiadesτ ~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 marrón / café• Naine brune• Brauner Zwerg• Nana bruna• Anã marrom

Q2: Are brown dwarfs “brown”?A2: They are “infrared”… And faint!

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!)

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…

José Antonio CaballeroCentro de Astrobiología (CSIC-INTA), Madrid

Ultracool dwarfs from Spain

I’m not talking on CARMENES

yet

Telescope Instruments “today” Instruments “tomorrow”

10.4 m GTC OSIRIS, CanariCamOSIRIS, CanariCam, CIRCE, EMIR, FRIDA, ELMER, EMIR,

MEGARA, MIRADAS

6.5 m HEXA … HECATE, MONSUL, GEA

4.2 m WHT

ISIS, 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, Ω2kCARMENES, PMAS

2.6 m NOTALFOSC, NOTCam, FIES,

MOSCA, StanCam?

2.5 m INT WFC, IDS WFC, IDS

2.5 m J-T250

JPCam JPCam

2.2 m CAHABUSCA, CAFOS, CAFÉ, AstraLux, MAGIC

PANIC, CAFÉ

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 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?o Deptho Repetition (proper motions, monitoring)o Spatial resolution (@3.5mCA)o 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-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.

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)

Object 2H burning 1H burning

Mass(Msol [MJup])

(Zsol)

Star yes yes>0.075 [> 72]

Sub-stellar object

Brown dwarf

yes no0.075-0.013 [72-14]

Planet* no no<0.013 [< 14]

*:Planet or “planetary-mass object”