Planet Formation Instrument for the Thirty Meter Telescope

Macintosh, Bruce; Troy, Mitchell; Graham, James R.; Doyon, René

doi:10.2172/919210

Cited by 13 publications

(15 citation statements)

References 23 publications

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“…Specifically, Microwave Kinetic Inductance Detectors, or MKIDs, and Superconducting Tunnelling Junctions, STJs, have high quantum efficiency and are being multiplexed into larger arrays (Peacock et al 1996;Day et al 2003;Mazin et al 2012). Another possible approach would be to use an integral field unit spectrograph, such as that used on the Gemini Planet Imager (Macintosh et al 2006). The wave bands that are used could in principle be selected after the observations are made: the smaller body tends to dominate at wavelengths where the larger body is dimmest, so the wavebands can be selected based on the observed molecular band features that are found after the initial spectrum is measured.…”

Section: Discussionmentioning

confidence: 99%

The Center of Light: Spectroastrometric Detection of Exomoons

Agol

Jansen

Lacy

et al. 2015

ApJ

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Direct imaging of extrasolar planets with future space-based coronagraphic telescopes may provide a means of detecting companion moons at wavelengths where the moon outshines the planet. We propose a detection strategy based on the positional variation of the center of light with wavelength, "spectroastrometry." This new application of this technique could be used to detect an exomoon, to determine the exomoon's orbit and the mass of the host exoplanet, and to disentangle the spectra of the planet and moon. We consider two model systems, for which we discuss the requirements for detection of exomoons around nearby stars. We simulate the characterization of an Earth-Moon analog system with spectroastrometry, showing that the orbit, the planet mass, and the spectra of both bodies can be recovered. To enable the detection and characterization of exomoons we recommend that coronagraphic telescopes should extend in wavelength coverage to 3 μm, and should be designed with spectroastrometric requirements in mind.

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Section: Discussionmentioning

confidence: 99%

The Center of Light: Spectroastrometric Detection of Exomoons

Agol

Jansen

Lacy

et al. 2015

ApJ

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“…This probes both bright planets in small orbits (10-15 AU in star forming regions) and bright "self-luminous" wide separation planets [10]. Plans also exist for the Planet Finding Imager (PFI), which exploits the large primary aperture and high-contrast adaptive optics [11]. E-ELT also has a Phase A instrument (EPICS) targeting exoplanets through direct imaging, spectroscopy and polarimetry [12,13].…”

Section: Pos(bash11)011mentioning

confidence: 99%

Spectroscopy and the Age of Giant Telescopes

Tuttle¹

2012

Proceedings of Frank N. Bash Symposium 2011: New Horizons in Astronomy — PoS(Bash11)

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Is your 4 meter telescope just not cutting it anymore? Embarrassed to mention the telescope time you had just the other week when talking about your newest data project? Don't worry, the age of the giant telescope is upon us. I will review the status of the three current ELT projects, as well as spectroscopic technologies focusing on multi-object spectroscopy. HETDEX (the Hobby Eberly Dark Energy Experiment) uses a new approach to large instruments, replicating a spectrograph channel 150 times to produce 33,600 individual spectra across a 22 arcminute field. The technology being built can be easily modified and ported to other telescopes to take quick advantage of the integral field approach. I will touch on the many experiments that await first light as these instruments come to fruition. Let's discuss why we are pouring massive resources into these telescopes and see what they can do for us.

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“…However, a number of different project are either now running (e.g. Project 1640 at the 5 m Palomar Telescope -see Crepp et al 2011) or are going to begin like the Gemini Planet Imager (GPI) at the Gemini South Telescope (Macintosh et al 2006) or SPHERE at the ESO Very Large Telescope (Beuzit et al 2006). This last instrument, in particular, includes three scientific channels that are a differential imager and dual band polarimeter called IRDIS operating in the near infrared between the Y and the Ks band (Dohlen et al 2008), a polarimeter called ZIMPOL that will look for old planets at visible wavelengths (Thalmann et al 2008) and an Integral Field Spectrograph 2 Dino Mesa et al…”

Section: Introductionmentioning

confidence: 99%

Performance tests on the SPHERE-IFS

et al. 2013

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Abstract. Until now, just a few extrasolar planets ( 30 out of 860) have been found through the direct imaging method. This number should greatly improve when the next generation of High Contrast Instruments like Gemini Planet Imager (GPI) at Gemini South Telescope or SPHERE at VLT will became operative at the end of this year. In particular, the Integral Field Spectrograph (IFS), one of the SPHERE subsystems, should allow a first characterization of the spectral type of the found extrasolar planets. Here we present the results of the last performance tests that we have done on the IFS instrument at the Institut de Planetologie et d'Astrophysique de Grenoble (IPAG) in condition as similar as possible to the ones that we will find at the telescope. We have found that we should be able to reach contrast down to 5x10 −7 and make astrometry at sub-mas level with the instrument in the actual conditions. A number of critical issues have been identified. The resolution of these problems could allow to further improve the performance of the instrument.

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Planet Formation Instrument for the Thirty Meter Telescope

Cited by 13 publications

References 23 publications

The Center of Light: Spectroastrometric Detection of Exomoons

The Center of Light: Spectroastrometric Detection of Exomoons

Spectroscopy and the Age of Giant Telescopes

Performance tests on the SPHERE-IFS

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