SPIRou @ CFHT: spectrograph optical design

Thibault, Simon; Rabou, Patrick; Donati, J.‐F.; Desaulniers, Pierre; Dallaire, Xavier; Artigau, Étienne; Pepe, F.; Micheau, Yoan; Vallée, Philippe; Barrick, Greg; Решетов, В. А.; Hernandez, O.; Saddlemyer, Leslie; Pazder, John; Parès, L.; Doyon, René; Delfosse, X.; Kouach, Driss; Loop, David

doi:10.1117/12.926697

Cited by 25 publications

(9 citation statements)

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“…The planetary parameters of the TRAPPIST-1 planets are also typical of the population of small planets around late K to early M-dwarfs which we assume extrapolates down towards ultracool dwarfs given the lack observational constraints on the planet occurrence rate around ultracool dwarfs; a population which will be probed by the next generation of high precision near-IR spectrographs (i.e. SPIRou; Thibault et al 2012;Artigau et al 2014). This extrapolation may be reasonable given the high number of small planets predicted to form around these cool stars via core-accretion (Payne & Lodato 2007).…”

Section: How Typical Is the Trappist-1 System?mentioning

confidence: 94%

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Prospects for detecting the Rossiter–McLaughlin effect of Earth-like planets: the test case of TRAPPIST-1b and c

Cloutier

Triaud

2016

Mon. Not. R. Astron. Soc.

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The Rossiter-McLaughlin effect is the principal method of determining the skyprojected spin-orbit angle (β) of transiting planets. Taking the example of the recently discovered TRAPPIST-1 system, we explore how ultracool dwarfs facilitate the measurement of the spin-orbit angle for Earth-sized planets by creating an effect that can be an order of magnitude more ample than the Doppler reflex motion caused by the planet if the star is undergoing rapid rotation. In TRAPPIST-1's case we expect the Rossiter-McLaughlin semi-amplitudes to be 40−50 m s −1 for the known transiting planets. Accounting for stellar jitter expected for ultracool dwarfs and instrumental noise, and assuming radial velocity precisions both demonstrated and anticipated for upcoming near-infrared spectrographs, we quantify the observational effort required to measure the planets' masses and spin-orbit angles. We conclude that if the planetary system is well-aligned then β can be measured to a precision of 10• if the spectrograph is stable at the level of 2 m s −1 . We also investigate the measure of ∆β, the mutual inclination, when multiple transiting planets are present in the system. Lastly, we note that the rapid rotation rate of many late M-dwarfs will amplify the RossiterMcLaughlin signal to the point where variations in the chromatic Rossiter-McLaughlin effect from atmospheric absorbers should be detectable.

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Section: How Typical Is the Trappist-1 System?mentioning

confidence: 94%

“…SPECU-LOOS ; Gillon et al 2013a) and radial velocity surveys in the near-IR (e.g. SPIRou; Thibault et al 2012;Artigau et al 2014, CARMENES ;Quirrenbach et al 2014, HPF Mahadevan et al 2012, and IRD spectrograph Tamura et al 2012. The detection significance curves presented in Figs.…”

Section: Application To Other Systemsmentioning

confidence: 99%

Prospects for detecting the Rossiter–McLaughlin effect of Earth-like planets: the test case of TRAPPIST-1b and c

Cloutier

Triaud

2016

Mon. Not. R. Astron. Soc.

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“…Barnes et al (2014) demonstrated precision down to ∼ 2.5 ms −1 is possible with current technology operating at red-optical wave-lengths, and Gao et al (2016) have demonstrated similar precision down to ∼ 2 ms −1 in the near infrared K band. There are also dedicated RV surveys, including the Habitable Zone Planet Finder (Mahadevan et al 2014) and Spec-troPolarimètre Infra-Rouge (SPIRou) (Thibault et al 2012) that will target the lowest mass stars at the bottom of the main sequence with 1 ms −1 instrumental RV precision. For M dwarfs, although the red-optical contains more Doppler information in the thousands of available absorption lines, enabling greater radial velocity precision to be achieved , the spectral energy distribution of low mass stars peaks at near infrared wavelengths.…”

Section: Introductionmentioning

confidence: 99%

Recovering planet radial velocity signals in the presence of starspot activity in fully convective stars

Barnes

Jeffers

Anglada-Escudé

et al. 2016

Mon. Not. R. Astron. Soc.

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Accounting for stellar activity is a crucial component of the search for ever-smaller planets orbiting stars of all spectral types. We use Doppler imaging methods to demonstrate that starspot induced radial velocity variability can be effectively reduced for moderately rotating, fully convective stars. Using starspot distributions extrapolated from sunspot observations, we adopt typical M dwarf starspot distributions with low contrast spots to synthesise line profile distortions. The distortions are recovered using maximum entropy regularised fitting and the corresponding stellar radial velocities are measured. The procedure is demonstrated for a late-M star harbouring an orbiting planet in the habitable zone. The technique is effective for stars with v sin i = 1 -10 km s −1 , reducing the stellar noise contribution by factors of nearly an order of magnitude. With a carefully chosen observing strategy, the technique can be used to determine the stellar rotation period and is robust to uncertainties such as unknown stellar inclination. While demonstrated for late-type M stars, the procedure is applicable to all spectral types.

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“…This design also ensures a high total throughput of 45% detector included. For a more complete description of the spectrograph optical design, the reader is referred to Thibault et al (2012).…”

Section: The Cryogenic High-resolution Spectrographmentioning

confidence: 99%

SPIRou: A nIR Spectropolarimeter/High-precision Velocimeter for the CFHT

Donati

Kouach

Lacombe

et al. 2017

Handbook of Exoplanets

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SPIRou is a near-infrared (nIR) spectropolarimeter / velocimeter for the Canada-France-Hawaii Telescope (CFHT), that will focus on two forefront science topics, (i) the quest for habitable Earth-like planets around nearby M stars, and (ii) the study of low-mass star/planet formation in the presence of magnetic fields. SPIRou will also efficiently tackle many key programmes beyond these two main goals, from weather patterns on brown dwarfs to Solar-System planet and exoplanet atmospheres. SPIRou will cover a wide spectral domain in a single exposure (0.98-2.44 µm) at a resolving power of 70 K, yielding unpolarized and polarized spectra of low-mass stars with a 15% average throughput at a radial velocity (RV) precision of 1 m s −1 . It consists of a Cassegrain unit mounted at the Cassegrain focus of CFHT and featuring an achromatic polarimeter, coupled to a cryogenic spectrograph cooled down at 80 K through a fluoride fiber link. SPIRou is currently integrated at IRAP/OMP and will be mounted at CFHT in 2017 Q4 for a first light scheduled in late 2017. Science operation is predicted to begin in 2018 S2, allowing many fruitful synergies with major ground and space instruments such as the JWST, TESS, ALMA and later-on PLATO and the ELT.

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SPIRou @ CFHT: spectrograph optical design

Cited by 25 publications

References 0 publications

Prospects for detecting the Rossiter–McLaughlin effect of Earth-like planets: the test case of TRAPPIST-1b and c

Prospects for detecting the Rossiter–McLaughlin effect of Earth-like planets: the test case of TRAPPIST-1b and c

Recovering planet radial velocity signals in the presence of starspot activity in fully convective stars

SPIRou: A nIR Spectropolarimeter/High-precision Velocimeter for the CFHT

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