Astrophysics and exoplanets with a 4-m class telescope Ignasi Ribas Institut d’Estudis Espacials de Catalunya (IEEC) Institut de Ciències de l’Espai (ICE, CSIC) nd BINA Worksho 2 nd hop, Royal l Observator atory Brussels, els, Belgium um, , Oct 9, 2018
A new era of astronomical instrumentation • We are in the age of the 10-m class telescopes • And the new era of ELTs (E-ELT, TMT, GMT, etc) is about to commence (late 2020s) • In this landscape, 4-m class telescopes are moving from multi-purpose instruments to increasingly specialized instruments • It is quite common to see single-instrument telescopes addressing one science case: • LAMOST • Kitt Peak 4m • CAHA 3.5m • La Silla 3.6m • CTIO 4m • VISTA 4m
• Wide-field massive-multiplex spectrographs • Low/intermediate dispersion spectrographs • R>40000 echelle spectrographs • Wide-field imagers • Time domain photometry
Multiplex spectrographs • Science drivers • Evolution of the dark-energy density with cosmological epoch: BAOs (similar to BOSS or WiggleZ), lensing, clusters (complement to Euclid) ➩ R~5000 • Comprehensive census of the orbits, ages, and composition of stars in the Galaxy and nearby galaxies (complement to Gaia, SP: V<15.5) ➩ R~5000 for RVs, R~30000 for abundances • Instruments: • 2019: WEAVE at WHT: 1000x MOS, IFUs, red & blue arms, R~5000 & R~20000 • LAMOST (China 4m: 4000x, R~1000 & 5000), DESI (Kitt Peak 4m: 5000x, R~2000- 5000), 4MOST (VISTA 4m: 2400x, R~4000 & 20000); HERMES+2dF (AAO 4m)
Low/intermediate dispersion spectrographs • Science drivers: Point-like and extended objects (needs wide wavelength coverage) • Physics of compact objects: GRB afterglows, SNe, CVs, novae, WR, PNe, LBVs • Galaxy formation & evolution: mergers, starbursts, AGN • Nearby galaxies (IFU): populations, chemical composition • Instruments: • PMAS (CAHA 3.5m), DOLORES (TNG 3.6m), ISIS & LIRIS (WHT 4m) • SofI & EFOSC2 (NTT 3.5m) • Not so many future developments
High-resolution echelle spectrographs • Science drivers • Star formation • Stellar structure and evolution • Life cycle of matter • Diversity of exoplanets (detection & atmospheres) • Instruments: • HARPS (ESO 3.6m), HARPS-N & GIANO (TNG 3.6m), UCLES (3.9m), CARMENES (CAHA 3.5m; NIR) • Lots of new ones!… Let’s see them
High-resolution echelle spectrographs Wright & Robertson 2018
High-resolution echelle spectrographs • This “bonanza” of new instrumentation is driven by the search of exoplanets • More recently also by the follow-up of space missions (TESS, PLATO) • Different instruments have different approaches regarding wavelength coverage (red/NIR growing) • The study of transiting exoplanet atmospheres using high-res NIR spectrographs is gaining very strong momentum
P HZ (0.4 M � ) = 25 d P HZ (0.3 M � ) = 18 d M < 10 M ⊕ P HZ (0.2 M � ) = 12 d
Exoplanets from radial velocities
0 m/s Wavelength (Angstroms)
+ 3 m/s Wavelength (Angstroms)
+ 3 m/s Wavelength (Angstroms)
High-precision spectrographs Δ RV = 1 m/s Δλ = 0.00002 Å ➜ 15 nm on detector ➜ 1/1000 pixel ➜ 30 Si atoms ➜ Δ T = 0.001 K ➜ Δ P = 0.01 mbar Pressure & temperature control
C alar A lto High- R esolution Search for M Dwarfs with E xo-Earths With N ear-Infrared and Optical E chelle S pectrographs
The CARMENES instrument • Single-purpose, high-stability instrument • Wide wavelength coverage for discrimination against intrinsic variability Visible channel Near-Infrared channel • Precision ~1 m/s • Precision ~1 m/s • 520-970 nm, R = 93,500, • 970-1710 nm, R = 80,400, 2.5-pix sampling 2.8-pix sampling • In vacuum, stabilized at • In vacuum, stabilized at 140 K • Mosaic 2 2kx2k Hawaii2RG ambient temperature • 4kx4k CCD E2V 2.5 µm • U-Ne & U-Ar & Th-Ar • U-Ne lamp (+F-P etalon) lamps (+F-P etalon)
The CARMENES instrument VIS NIR
The CARMENES instrument
NIR 28 orders 0.97-1.71 μm VIS 55 orders 0.52-0.97 μm
The CARMENES survey <d> = 13 pc • 342 targets • From Jan 2016 to Oct Typical target: M3-M4 2018: > 12000 spectra & J=7-9 (50% of all) in VIS & NIR
… GX And: M1 Luyten’s star: M3.5 Teegarden’s star: M7 Maximum NIR precision at SNR150 @J Maximum VIS precision at SNR150 @J
Internal precision (1.2 m/s if no extra error)
… 2018, A&A
2017, A&A 750 nights activity jitter 3 m s -1 60-70 obs. / star pure photon 1 m s -1 noise From real survey, ½ along the way: 15 planets as sure detections
Planetary properties: Rossiter- McLaughlin effect Mayor et al. (2014, Nature) HD 189733 b Di Gloria et al. (2015, A&A)
Planetary atmospheres with high-res spectroscopy Birkby et al. (2013, Msngr)
Planetary atmospheres with high-res spectroscopy HD 209458 b Snellen et al. (2010, Nature)
Planetary atmospheres: the new revolution HD 189733 b Wyttenbach et al. (2015, A&A) MASCARA-2 b Casasayas-Barris et al. (2018, A&A)
Additional science • Binary systems • Stellar atmospheres • Stellar activity • Atomic diagnostics • Evolved stars • Planetary nebulae • … YZ CMi (M4.5 V)
2018, A&A 15%
Stellar atmospheric parameters Passegger et al (2018, A&A)
Wide- l range activity indicator Simulations with StarSim 2.0 (Herrero et al. 2016, A&A) NIR is NOT a scaled version of VIS Complex interplay with convective blueshift
Simultaneous RVs & space-based photometry StarSim 2.0 Starspots affect radial velocities and photometry Herrero et al (2016, A&A); Rosich et al. (in prep)
The exoplanet mission timeline
TESS follow-up • Primary mission: � 07/2018 – 07/2020 • Mission extension? Barclay et al. (2018, ApJS) ~4300 planets
TESS follow-up Barclay et al. (2018, ApJS) López-Morales et al. (2016, AJ)
PLATO follow-up • ESA M-class mission • Launch in 2026 (M3) • 4 years @ L2 • 2 long pointings 2 years • Large fraction of the sky Earth twins • Detection and properties of habitable exoplanets • Thousands of rocky, icy and giant exoplanets • 1 million light curves
PLATO follow-up
Conclusions: some thoughts • Golden era for precise high-resolution spectroscopy � Exoplanet surveys (targeted blind searches, e.g., nearby stars, volume limited) � Transit follow-up (TESS, PLATO) � Planetary atmospheres � Many additional science cases • For cool stars (majority of nearby planets), the sweet spot is 0.7 to 1.1 m m for RVs and NIR for atmospheres • There seems to be room for more instruments
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