Design of NEID, an extreme precision Doppler spectrograph for WIYN

Schwab, Christian; Rakich, Andrew; Gong, Qian; Mahadevan, Suvrath; Halverson, Samuel; Roy, Arpita; Terrien, Ryan C.; Robertson, Paul; Hearty, Fred; Levi, Eric; Monson, Andrew; Wright, Jason T.; McElwain, Michael W.; Bender, Chad F.; Blake, Cullen H.; Stürmer, Julian; Gurevich, Yulia V.; Chakraborty, Abhijit; Ramsey, Lawrence W.

doi:10.1117/12.2234411

Cited by 112 publications

(70 citation statements)

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“…Being an M-dwarf, K2-28 will be most efficiently observed with precise ultra-stabilized near-infrared radial velocity spectrographs, including e.g., CARMENES (Quirrenbach et al 2012), the stabilized Habitable-zone Planet Finder (HPF; Mahadevan et al (2012); Stefansson et al (2016)), the Infrared Doppler Instrument (IRD) for Subaru (Kotani et al 2014), or Spirou (Artigau et al 2014. Meanwhile K2-100b would be most efficiently be observed in the optical by e.g., CARMENES (Quirrenbach et al 2012), ESPRESSO (Pepe et al 2014), EXPRES (Jurgenson et al 2016), G-CLEF (Szentgyorgyi et al 2012), HARPS (Mayor et al 2003), or NEID (Schwab et al 2016), and/or other instruments in the growing worldwide network of precision radial velocity spectrographs (Wright & Robertson 2017).…”

Section: Possibility For Future Rv Observationsmentioning

confidence: 99%

Diffuser-assisted Photometric Follow-up Observations of the Neptune-sized Planets K2-28b and K2-100b

Stefánsson

Mahadevan

et al. 2018

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We present precision transit observations of the Neptune-sized planets K2-28b and K2-100b, using the Engineered Diffuser on the ARCTIC imager on the ARC 3.5m Telescope at Apache Point Observatory. K2-28b is a R p = 2.56R ⊕ mini-Neptune transiting a bright (J=11.7) metal-rich M4 dwarf, offering compelling prospects for future atmospheric characterization. K2-100b is a R p = 3.45R ⊕ Neptune in the Praesepe Cluster and is one of few planets known in a cluster transiting a host star bright enough (V = 10.5) for precision radial velocity observations. Using the precision photometric capabilities of the diffuser/ARCTIC system, allows us to achieve a precision of 105 +87 −37 ppm, and 38 +21 −11 ppm in 30 minute bins for K2-28b, and K2-100b, respectively. Our jointfits to the K2 and ground-based light-curves give an order of magnitude improvement in the orbital ephemeris for both planets, yielding a timing precision of 2 min in the JWST era. Although we show that the currently available broad-band measurements of K2-28b's radius are currently too imprecise to place useful constraints on K2-28b's atmosphere, we demonstrate that JWST/NIRISS will be able to discern between a cloudy/clear atmosphere in a modest number of transit observations. Our light-curve of K2-100b marks the first transit follow-up observation of this challenging-to-observe transit, where we obtain a transit depth of 819 ± 50 ppm in the SDSS i band. We conclude that diffuser-assisted photometry can play an important role in the TESS era to perform timely and precise follow-up of the expected bounty of TESS planet candidates.

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Section: Possibility For Future Rv Observationsmentioning

confidence: 99%

Diffuser-assisted Photometric Follow-up Observations of the Neptune-sized Planets K2-28b and K2-100b

Stefánsson

Mahadevan

et al. 2018

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“…In developing the comprehensive error budget for NEID 3 , close attention was paid to the impact of the light injection parameters not only on efficiency, but also on the minimum radial velocity error that the facility can achieve. Despite significant efforts to provide state of the art scrambling 4 and to make the spectrograph optical design as insensitive to input illumination as possible 5 , the science goals of the instrument demand that the stability and quality of the fiber injection meet extremely tight requirements. The three key features of the design are very good image quality (to allow optimal coupling into our 0.92" fiber), the best possible centroiding and guiding performance 6 (to achieve the best efficiency as well as the smallest guiding-induced radial velocity variation between exposures), and very good correction of atmospheric dispersion (to avoid wavelength-dependent radial velocity offsets between exposures).…”

Section: _____________________________________________________________mentioning

confidence: 99%

The NEID precision radial velocity spectrometer: optical design of the port adapter and ADC

Schwab

Liang

Gong

et al. 2018

Ground-Based and Airborne Instrumentation for Astronomy VII

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NEID is a new extreme precision Doppler spectrometer for the WIYN telescope. It is fiber fed and employs a classical white pupil Echelle configuration. NEID has a fiber aperture of only 0.92" on sky in high-resolution mode, and its tight radial velocity error budget resulted in very stringent stability requirements for the input illumination of the spectrograph optics. Consequently, the demands on the fiber injection are challenging. In this paper, we describe the layout and optical design of the injection module, including a broadband, high image quality relay and a high-performance atmospheric dispersion corrector (ADC) across the bandwidth of 380-930 nm.

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“…Here we carefully consider the impact of solar light contamination on RV measurements and explore the mitigation possible with a simultaneous sky fiber. Several upcoming instruments, e.g., NEID (Schwab et al 2016) and the Keck Planet Finder (Gibson et al 2018), include a dedicated sky fiber for the correction of telluric absorption and emission lines, and the removal of scattered sunlight. However, the sky fiber is highly spectrally dispersed in these instruments, making faint levels of solar contamination difficult to measure even when there is a consequential impact on RV precision.…”

Section: Introductionmentioning

confidence: 99%

Solar Contamination in Extreme-precision Radial-velocity Measurements: Deleterious Effects and Prospects for Mitigation

Roy

Halverson

Mahadevan

et al. 2020

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Solar contamination, due to moonlight and atmospheric scattering of sunlight, can cause systematic errors in stellar radial velocity (RV) measurements that significantly detract from the ∼10 cm s −1 sensitivity required for the detection and characterization of terrestrial exoplanets in or near Habitable Zones of Sun-like stars. The addition of low-level spectral contamination at variable effective velocity offsets introduces systematic noise when measuring velocities using classical mask-based or template-based cross-correlation techniques. Here we present simulations estimating the range of RV measurement error induced by uncorrected scattered sunlight contamination. We explore potential correction techniques, using both simultaneous spectrometer sky fibers and broadband imaging via coherent fiber imaging bundles, that could reliably reduce this source of error to below the photon-noise limit of typical stellar observations. We discuss the limitations of these simulations, the underlying assumptions, and mitigation mechanisms. We also present and discuss the components designed and built into the NEID precision RV instrument for the WIYN 3.5m telescope, to serve as an ongoing resource for the community to explore and evaluate correction techniques. We emphasize that while "bright time" has been traditionally adequate for RV science, the goal of 10 cm s −1 precision, on the most interesting exoplanetary systems may necessitate access to darker skies for these next-generation instruments.

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Design of NEID, an extreme precision Doppler spectrograph for WIYN

Cited by 112 publications

References 1 publication

Diffuser-assisted Photometric Follow-up Observations of the Neptune-sized Planets K2-28b and K2-100b

Diffuser-assisted Photometric Follow-up Observations of the Neptune-sized Planets K2-28b and K2-100b

The NEID precision radial velocity spectrometer: optical design of the port adapter and ADC

Solar Contamination in Extreme-precision Radial-velocity Measurements: Deleterious Effects and Prospects for Mitigation

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