Astrophysics and exoplanets with a 4-m class telescope Ignasi - - PowerPoint PPT Presentation

Astrophysics and exoplanets with a 4-m class telescope

2nd

nd BINA Worksho

hop, Royal l Observator atory Brussels, els, Belgium um, , Oct 9, 2018

Ignasi Ribas

Institut d’Estudis Espacials de Catalunya (IEEC) Institut de Ciències de l’Espai (ICE, CSIC)

• 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
• CAHA 3.5m
• CTIO 4m

A new era of astronomical instrumentation

• Kitt Peak 4m
• La Silla 3.6m
• VISTA 4m

• Wide-field massive-multiplex spectrographs
• Low/intermediate dispersion spectrographs
• R>40000 echelle spectrographs
• Wide-field imagers
• Time domain photometry

• 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
• f stars in the Galaxy and nearby galaxies (complement to

Gaia, SP: V<15.5) ➩ R~5000 for RVs, R~30000 for abundances

Multiplex spectrographs

• 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)

• 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

Low/intermediate dispersion 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

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

PHZ (0.4 M) = 25 d PHZ (0.3 M) = 18 d PHZ (0.2 M) = 12 d M < 10 M⊕

Exoplanets from radial velocities

0 m/s

Wavelength (Angstroms)

+ 3 m/s

Wavelength (Angstroms)

+ 3 m/s

Wavelength (Angstroms)

Δλ = 0.00002 Å ➜ 15 nm on detector ➜ 1/1000 pixel ➜ 30 Si atoms ➜ ΔT = 0.001 K ➜ ΔP = 0.01 mbar Pressure & temperature control

High-precision spectrographs

ΔRV = 1 m/s

Calar Alto High-Resolution Search for M Dwarfs with Exo-Earths With Near-Infrared and Optical Echelle Spectrographs

The CARMENES instrument

• Single-purpose, high-stability instrument
• Wide wavelength coverage for discrimination against

intrinsic variability

Near-Infrared channel

• Precision ~1 m/s
• 520-970 nm, R = 93,500,

2.5-pix sampling

• In vacuum, stabilized at

ambient temperature

• 4kx4k CCD E2V
• U-Ne & U-Ar & Th-Ar

lamps (+F-P etalon)

Visible channel

• Precision ~1 m/s
• 970-1710 nm, R = 80,400,

2.8-pix sampling

• In vacuum, stabilized at 140 K
• Mosaic 2 2kx2k Hawaii2RG

2.5 µm

• U-Ne lamp (+F-P etalon)

VIS NIR

The CARMENES instrument

The CARMENES instrument

NIR 28 orders 0.97-1.71 μm VIS 55 orders 0.52-0.97 μm

<d> = 13 pc

The CARMENES survey

Typical target: M3-M4 & J=7-9 (50% of all)

• 342 targets
• From Jan 2016 to Oct

2018: > 12000 spectra 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

…

750 nights 60-70 obs. / star

1 m s-1 3 m s-1 activity jitter pure photon noise

2017, A&A From real survey, ½ along the way: 15 planets as sure detections

Planetary properties: Rossiter- McLaughlin effect

HD 189733 b Di Gloria et al. (2015, A&A) Mayor et al. (2014, Nature)

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)

MASCARA-2 b Casasayas-Barris et al. (2018, A&A)

Planetary atmospheres: the new revolution

HD 189733 b Wyttenbach et al. (2015, 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

NIR is NOT a scaled version of VIS Complex interplay with convective blueshift

Simulations with StarSim 2.0

(Herrero et al. 2016, A&A)

Starspots affect radial velocities and photometry

Herrero et al (2016, A&A); Rosich et al. (in prep)

Simultaneous RVs & space-based photometry StarSim 2.0

The exoplanet mission timeline

TESS follow-up

• Primary mission:

07/2018 – 07/2020

• Mission extension?

Barclay et al. (2018, ApJS)

~4300 planets

Barclay et al. (2018, ApJS)

TESS follow-up

López-Morales et al. (2016, AJ)

• ESA M-class mission
• Launch in 2026 (M3)
• 4 years @ L2
• 2 long pointings 2 years
• Large fraction of the

sky

• Detection and properties of habitable

exoplanets

• Thousands of rocky, icy and giant

exoplanets

• 1 million light curves

Earth twins

PLATO follow-up

PLATO follow-up

• 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 mm for RVs and NIR for atmospheres

• There seems to be room for more instruments

Conclusions: some thoughts