The GMT-CfA, Carnegie, Catolica, Chicago Large Earth Finder (G-CLEF): a general purpose optical echelle spectrograph for the GMT with precision radial velocity capability

Szentgyorgyi, Andrew; Frebel, Anna; Fürész, Gábor; Hertz, Edward; Norton, Timothy; Bean, Jacob L.; Bergner, Henry; Crane, Jeffrey D.; Evans, Janet D.; Evans, I. N.; Gauron, Thomas; Jordán, Andrés; Park, S.; Uomoto, Alan; Barnes, Stuart; Davis, W.; Eisenhower, Michael J.; Guzmán, Dani; McCracken, K. G.; Ordway, Mark; Plummer, David A.; Podgorski, William; Weaver, D.

doi:10.1117/12.924957

Cited by 40 publications

(23 citation statements)

References 11 publications

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“…Among the new instruments being planned with TESS targets in mind are ESPRESSO, 24 NRES, 25 IRD, 26 CARMENES, 27 HPF, 28 HRS, 29 SPIRou, 30 MAROON-X, 31 CODEX, 32 and G-CLEF. 33 The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will likely be the most favorable targets for detailed investigations in the decades or even centuries that follow.…”

Section: Discussionmentioning

confidence: 99%

Transiting Exoplanet Survey Satellite

Ricker

Winn

Vanderspek

et al. 2014

J. Astron. Telesc. Instrum. Syst

3,173

1,691

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Abstract. The Transiting Exoplanet Survey Satellite (TESS) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its 2-year mission, TESS will employ four wide-field optical charge-coupled device cameras to monitor at least 200,000 main-sequence dwarf stars with I C ≈ 4 − 13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from 1 month to 1 year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10 to 100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every 4 months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations. © The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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Section: Discussionmentioning

confidence: 99%

Transiting Exoplanet Survey Satellite

Ricker

Winn

Vanderspek

et al. 2014

J. Astron. Telesc. Instrum. Syst

3,173

1,691

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“…However, if this is the case, GJ 9827 c would be the one of the most heavily irradiated super-Earths below the radius gap that still retains a substantial volatile envelope. Given the faintness of the star (V=10.3) and the expected RV amplitude (1 m s −1 for a rocky composition), it seems likely that only the next generation of high-precision velocimeters on large telescopes, such as ESPRESSO (Pepe et al 2010) or G-CLEF (Szentgyorgyi et al 2012), will allow a mass determination that has sufficient precision (better than ∼ 20%) to uncover its internal composition.…”

Section: K2-141bmentioning

confidence: 99%

Masses and radii for the three super-Earths orbiting GJ 9827, and implications for the composition of small exoplanets

Rice

Malavolta

Mayo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Super-Earths belong to a class of planet not found in the Solar System, but which appear common in the Galaxy. Given that some super-Earths are rocky, while others retain substantial atmospheres, their study can provide clues as to the formation of both rocky planets and gaseous planets, and -in particular -they can help to constrain the role of photo-evaporation in sculpting the exoplanet population. GJ 9827 is a system already known to host 3 super-Earths with orbital periods of 1.2, 3.6 and 6.2 days. Here we use new HARPS-N radial velocity measurements, together with previously published radial velocities, to better constrain the properties of the GJ 9827 planets. Our analysis can't place a strong constraint on the mass of GJ 9827 c, but does indicate that GJ 9827 b is rocky with a composition that is probably similar to that of the Earth, while GJ 9827 d almost certainly retains a volatile envelope. Therefore, GJ 9827 hosts planets on either side of the radius gap that appears to divide super-Earths into pre-dominantly rocky ones that have radii below ∼ 1.5R ⊕ , and ones that still retain a substantial atmosphere and/or volatile components, and have radii above ∼ 2R ⊕ . That the less heavily irradiated of the 3 planets still retains an atmosphere, may indicate that photoevaporation has played a key role in the evolution of the planets in this system.

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“…The smallest of those ELTs is the Giant Magellan Telescope (GMT; www.gmto.org) with an effective diameter of 24.5 meters. One of the first light instruments on the GMT will be G-CLEF (Szentgyorgyi et al 2012), which will be a high-resolution spectrograph with resolution modes between R = 25,000-120,000 and spectral coverage between 350-950 nm, suitable to study the O 2 A-band.…”

Section: Telescope+instrument Setupmentioning

confidence: 99%

“…4 are not yet fully defined, we adopt two dif-ferent pixel grid scales; one with a velocity resolution of 0.75 km s −1 pixel −1 and the other 1.2 km s −1 pixel −1 . The 0.75 km s −1 pixel −1 grid scale corresponds to the planned scale of G-CLEF for resolutions R > 25, 000 (Szentgyorgyi et al 2012), while the 1.2 km s −1 pixel −1 grid scale corresponds to UVES (Dekker et al 2000), which is currently mounted at the 8.2 Very Large Telescopes (VLT) of the European Southern Observatory (ESO).…”

Section: Generation Of Model Spectramentioning

confidence: 99%

FEASIBILITY STUDIES FOR THE DETECTION OF O₂IN AN EARTH-LIKE EXOPLANET

Rodler¹,

López‐Morales²

2014

ApJ

177

150

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We present the results of simulations on the detectability of O 2 in the atmosphere of Earth twins around nearby low mass stars using high resolution transmission spectroscopy. We explore such detectability with each of the three upcoming Extremely Large Telescopes (ELTs), i.e. GMT, TMT and E-ELT, and high resolution spectrographs, assuming such instruments will be available in all ELTs. With these simulations we extend previous studies by taking into account atmospheric refraction in the transmission spectrum of the exo-Earth and observational white and red noise contributions. Our studies reveal that the number of transits necessary to detect the O 2 in the atmosphere of an Earth twin around M-dwarfs is by far higher than the number of transits estimated by Snellen et al. (2013). In addition, our simulations show that, when accounting for typical noise levels associated to observations in the optical and near-infrared, the O 2 A-band at 760 nm is more favorable to detect the exoplanetary signal than the O 2 band at 1268 nm for all the spectral types, except M9V. We conclude that, unless unpredicted instrumental limitations arise, the implementation of pre-slit optics such as image slicers appear to be key to significantly improve the yield of this particular science case. However, even in the most optimistic cases, we conclude that the detection of O 2 in the atmosphere of an Earth twin will be only feasible with the ELTs if the planet is orbiting a bright close-by (d ≤ 8 pc) M-dwarf with a spectral type later than M3.

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The GMT-CfA, Carnegie, Catolica, Chicago Large Earth Finder (G-CLEF): a general purpose optical echelle spectrograph for the GMT with precision radial velocity capability

Abstract: Large Earth Finder (G-CLEF): a general purpose optical echelle spectrograph for the GMT with precision radial velocity capability," Proc. SPIE 8446, Ground-based and Airborne Instrumentation for Astronomy IV, 84461H (

Cited by 40 publications

References 11 publications

Transiting Exoplanet Survey Satellite

Transiting Exoplanet Survey Satellite

Masses and radii for the three super-Earths orbiting GJ 9827, and implications for the composition of small exoplanets

FEASIBILITY STUDIES FOR THE DETECTION OF O₂IN AN EARTH-LIKE EXOPLANET

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The GMT-CfA, Carnegie, Catolica, Chicago Large Earth Finder (G-CLEF): a general purpose optical echelle spectrograph for the GMT with precision radial velocity capability

Abstract: Large Earth Finder (G-CLEF): a general purpose optical echelle spectrograph for the GMT with precision radial velocity capability," Proc. SPIE 8446, Ground-based and Airborne Instrumentation for Astronomy IV, 84461H (

Cited by 40 publications

References 11 publications

Transiting Exoplanet Survey Satellite

Transiting Exoplanet Survey Satellite

Masses and radii for the three super-Earths orbiting GJ 9827, and implications for the composition of small exoplanets

FEASIBILITY STUDIES FOR THE DETECTION OF O2IN AN EARTH-LIKE EXOPLANET

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FEASIBILITY STUDIES FOR THE DETECTION OF O₂IN AN EARTH-LIKE EXOPLANET