CHISL: the combined high-resolution and imaging spectrograph for the LUVOIR surveyor

Fleming, Brian; Hoadley, Keri

doi:10.1117/12.2231080

Cited by 3 publications

(3 citation statements)

References 27 publications

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“…The Colorado High-resolution Echelle Stellar Spectrograph (CHESS) 48,49 is a rocket-borne farultraviolet spectrograph that serves as a pathfinder instrument and technology testbed for highresolution spectrographs for future NASA astrophysics missions (e.g., LUVOIR 50 ). The CHESS A future flight of CHESS will incorporate an echelle grating fabricated using advanced electron-beam etching techniques developed at Pennsylvania State University, and the payload will be further reconfigured to replace the MCP detector with a delta-doped, SNAP CCD-a 3508×3512 pixel, 10.5-m square pixel format, high-resistivity, p-channel CCD designed by Lawrence Berkeley National Laboratory (LBNL) (Fig.…”

Section: Chess: High Purity P-channel Ccdmentioning

confidence: 99%

“…(c) A "flat field" image taken with the device in response to protons and (d) a typical electron response of device 47. 4.1.4 CHESS: High Purity P-channel CCDThe Colorado High-resolution Echelle Stellar Spectrograph (CHESS)48,49 is a rocket-borne farultraviolet spectrograph that serves as a pathfinder instrument and technology testbed for highresolution spectrographs for future NASA astrophysics missions (e.g., LUVOIR50 ). The CHESS rocket experiment is designed to quantify the composition and physical state of the interstellar medium (ISM), specifically the interface regions between translucent clouds and the ambient diffuse ISM; quantifying the temperature, composition, and kinematics of nearby interstellar clouds.…”

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confidence: 99%

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High-efficiency UV/optical/NIR detectors for large aperture telescopes and UV explorer missions: development of and field observations with delta-doped arrays

Nikzad

Jewell

Hoenk

et al. 2017

J. Astron. Telesc. Instrum. Syst

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A number of exciting concepts are under development for Flagship, Probe class, Explorer class, and Suborbital class NASA missions in the ultraviolet/optical spectral ranges. These missions will depend on high performance silicon detector arrays being delivered affordably and in high numbers. In a focused effort we have advanced delta-doping technology to high throughput and high yield wafer-scale processing, encompassing a multitude of state-of-the-art silicon-based detector formats and designs. As part of this technology advancement and in preparation for upcoming missions, we have embarked on a number of field observations, instrument integrations, and independent evaluations of delta-doped arrays. In this paper, we present recent data and innovations from the Advanced Detectors and Systems program at JPL, including two-dimensional doping technology; our end-to-end postfabrication processing of high performance UV/Optical/NIR arrays; and advanced coatings for detectors and optical elements. Additionally, we present examples of past, in-progress, and planned observations and deployments of deltadoped arrays.

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Section: Chess: High Purity P-channel Ccdmentioning

confidence: 99%

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confidence: 99%

High-efficiency UV/optical/NIR detectors for large aperture telescopes and UV explorer missions: development of and field observations with delta-doped arrays

Nikzad

Jewell

Hoenk

et al. 2017

J. Astron. Telesc. Instrum. Syst

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“…The possibility of detecting and studying H 2 within the Milky Way, for any astrophysical purpose, is strongly endangered after HST and its instruments reach the end of their lifetime. A possible follow-up mission is that of the Large/UV/Optical/Infrared (LUVOIR) surveyor covering the H 2 absorption wavelength range, which is however still in a preparation phase (France et al 2016).…”

Section: Future Opportunities and Instrumentationmentioning

confidence: 99%

Search for Varying Constants of Nature from Astronomical Observation of Molecules

Ubachs¹

2017

Space Sciences Series of ISSI

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The status of searches for possible variation in the constants of nature from astronomical observation of molecules is reviewed, focusing on the dimensionless constant representing the proton-electron mass ratio µ = m p /m e . The optical detection of H 2 and CO molecules with large ground-based telescopes (as the ESO-VLT and the Keck telescopes), as well as the detection of H 2 with the Cosmic Origins Spectrograph aboard the Hubble Space Telescope is discussed in the context of varying constants, and in connection to different theoretical scenarios. Radio astronomy provides an alternative search strategy bearing the advantage that molecules as NH 3 (ammonia) and CH 3 OH (methanol) can be used, which are much more sensitive to a varying µ than diatomic molecules. Current constraints are |∆µ/µ| < 5 × 10 −6 for redshift z = 2.0 − 4.2, corresponding to look-back times of 10-12.5 Gyrs, and |∆µ/µ| < 1.5 × 10 −7 for z = 0.88, corresponding to half the age of the Universe (both at 3σ statistical significance). Existing bottlenecks and prospects for future improvement with novel instrumentation are discussed.

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The effect of ISM absorption on stellar activity measurements and its relevance for exoplanet studies

Fossati

Marcelja

Staab

et al. 2017

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Past ultraviolet and optical observations of stars hosting close-in Jupiter-mass planets have shown that some of these stars present an anomalously low chromospheric activity, significantly below the basal level. For the hot Jupiter planet host WASP-13, observations have shown that the apparent lack of activity is possibly caused by absorption from the intervening interstellar medium (ISM). Inspired by this result, we study the effect of ISM absorption on activity measurements (S and log R ′ HK indices) for main-sequence late-type stars. To this end, we employ synthetic stellar photospheric spectra combined with varying amounts of chromospheric emission and ISM absorption. We present the effect of ISM absorption on activity measurements by varying several instrumental (spectral resolution), stellar (projected rotational velocity, effective temperature, and chromospheric emission flux), and ISM parameters (relative velocity between stellar and ISM Ca ii lines, broadening b-parameter, and Ca ii column density). We find that for relative velocities between the stellar and ISM lines smaller than 30-40 km s −1 and for ISM Ca ii column densities log N CaII 12, the ISM absorption has a significant influence on activity measurements. Direct measurements and three dimensional maps of the Galactic ISM absorption indicate that an ISM Ca ii column density of log N CaII = 12 is typically reached by a distance of about 100 pc along most sight lines. In particular, for a Sun-like star lying at a distance greater than 100 pc, we expect a depression (bias) in the log R ′ HK value larger than 0.05-0.1 dex, about the same size as the typical measurement and calibration uncertainties on this parameter. This work shows that the bias introduced by ISM absorption must always be considered when measuring activity for stars lying beyond 100 pc. We also consider the effect of multiple ISM absorption components. We discuss the relevance of this result for exoplanet studies and revise the latest results on stellar activity versus planet surface gravity correlation. We finally describe methods with which it would be possible to account for ISM absorption in activity measurements and provide a code to roughly estimate the magnitude of the bias. Correcting for the ISM absorption bias may allow one to identify the origin of the anomaly in the activity measured for some planet-hosting stars.

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CHISL: the combined high-resolution and imaging spectrograph for the LUVOIR surveyor

Cited by 3 publications

References 27 publications

High-efficiency UV/optical/NIR detectors for large aperture telescopes and UV explorer missions: development of and field observations with delta-doped arrays

High-efficiency UV/optical/NIR detectors for large aperture telescopes and UV explorer missions: development of and field observations with delta-doped arrays

Search for Varying Constants of Nature from Astronomical Observation of Molecules

The effect of ISM absorption on stellar activity measurements and its relevance for exoplanet studies

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