Vector-apodizing phase plate coronagraph: design, current performance, and future development [Invited]

Doelman, David; Snik, Frans; Por, Emiel H.; Bos, Steven P.; Otten, G. P. P. L.; Kenworthy, Matthew A.; Haffert, Sebastiaan Y.; Wilby, Michael J.; Bohn, A. J.; Sutlieff, Ben J.; Miller, Kelsey; Ouellet, Mireille; Boer, J. de; Keller, Christoph U.; Escuti, Michael J.; Shi, Shuojia; Warriner, Nathaniel Z.; Hornburg, Kathryn J.; Birkby, Jayne; Males, Jared R.; Morzinski, Katie M.; Close, Laird M.; Codona, Johanan L.; Long, Joseph D.; Schatz, Lauren; Lumbres, Jennifer; Rodack, Alexander; Gorkom, Kyle Van; Hedglen, Alexander D.; Guyon, Olivier; Lozi, Julien; Groff, Tyler D.; Chilcote, J.; Jovanović, Nemanja; Thibault, Simon; Jonge, C. de; Allain, Guillaume; Vallée, Catherine; Patel, Deven; Côté, Olivier; Marois, Christian; Hinz, Philip; Stone, Jordan; Skemer, Andrew J.; Briesemeister, Zackery; Boehle, Anna; Glauser, Adrian M.; Taylor, W. D.; Baudoz, Pierre; Huby, Elsa; Absil, Olivier; Carlomagno, Brunella; Delacroix, Christian

doi:10.1364/ao.422155

Cited by 21 publications

(19 citation statements)

References 93 publications

(137 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The double-grating 360°vector apodizing phase plate (dgvAPP360, Doelman et al 2020;Wagner et al 2020) suppresses the stellar diffraction halo by multiple orders of magnitude over the full 2-5 μm bandwidth. The dgvAPP360 is different from the more commonly used grating, vAPP (Snik et al 2012;Otten et al 2017;Doelman et al 2021), which creates two images of the star, each with D-shaped dark zones on opposite sides. The additional grating in the dgvAPP360 diffracts the light back on-axis, such that the two apodized images overlap, resulting in a single image of the star.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

L-band Integral Field Spectroscopy of the HR 8799 Planetary System

Doelman

Stone

Briesemeister

et al. 2022

Self Cite

View full text Add to dashboard Cite

Understanding the physical processes sculpting the appearance of young gas-giant planets is complicated by degeneracies confounding effective temperature, surface gravity, cloudiness, and chemistry. To enable more detailed studies, spectroscopic observations covering a wide range of wavelengths are required. Here we present the first L-band spectroscopic observations of HR 8799 d and e and the first low-resolution wide-bandwidth L-band spectroscopic measurements of HR 8799 c. These measurements were facilitated by an upgraded LMIRCam/ALES instrument at the Large Binocular Telescope, together with a new apodizing phase plate coronagraph. Our data are generally consistent with previous photometric observations covering similar wavelengths, yet there exists some tension with narrowband photometry for HR 8799 c. With the addition of our spectra, each of the three innermost observed planets in the HR 8799 system has had its spectral energy distribution measured with integral field spectroscopy covering ∼0.9–4.1 μm. We combine these spectra with measurements from the literature and fit synthetic model atmospheres. We demonstrate that the bolometric luminosity of the planets is not sensitive to the choice of model atmosphere used to interpolate between measurements and extrapolate beyond them. Combining luminosity with age and mass constraints, we show that the predictions of evolutionary models are narrowly peaked for effective temperature, surface gravity, and planetary radius. By holding these parameters at their predicted values, we show that more flexible cloud models can provide good fits to the data while being consistent with the expectations of evolutionary models.

show abstract

Section: Observations and Data Reductionmentioning

confidence: 99%

L-band Integral Field Spectroscopy of the HR 8799 Planetary System

Doelman

Stone

Briesemeister

et al. 2022

Self Cite

View full text Add to dashboard Cite

show abstract

“…Kreidberg et al 2014;Stevenson et al 2014;Wilson et al 2020;Arcangeli et al 2021;Panwar et al 2022a,b). We use a double-grating 360°vector Apodizing Phase Plate (dg-vAPP360) coronagraph (Doelman et al 2017(Doelman et al , 2020(Doelman et al , 2021Wagner et al 2020), which enables high-contrast companions to be detected without blocking the host star, hence leaving an unsaturated image of the host star available for use as a simultaneous reference. The more widely used grating vector Apodizing Phase Plate (gvAPP) coronagraph adjusts the phase of the incoming wavefront to modify the PSFs of all objects in the field of view, creating two images of the target star each with a 180°D-shaped 'dark hole', a region of deep flux suppression in which high-contrast companions can be observed, on opposing sides (Snik et al 2012;Otten et al 2014aOtten et al , 2017Bos et al 2020;Doelman et al 2021;Sutlieff et al 2021).…”

Section: Ground-based Differential Spectrophotometrymentioning

confidence: 99%

“…The mass of HD 1160 B also remains unclear, primarily due to the poorly constrained age of the system, with estimates ranging from that of a low mass brown dwarf (∼20 M Jup , Mesa et al 2020) to decisively in the stellar mass regime (0.12±0.01M ≈ 123M Jup , Curtis et al 2019) if the system is indeed a member of the Pisces-Eridanus stellar stream. HD 1160 C is a low-mass star (spectral type M3.5), and its separation of ∼530 au (∼5.1 ) places it beyond the field of view of most vAPPs currently in use (Maire et al 2016;Doelman et al 2021).…”

Section: The Hd 1160 Systemmentioning

confidence: 99%

“…The HD 1160 system was observed from an elevation of 29.4°at the start of the night to a maximum elevation of 61.7°, and then back down to an elevation of 27.5°. The dgvAPP360 creates an annular dark hole around the target PSF, with an inner radius close to the PSF core and an outer radius at the edge of the 2.2 field of view of the detector (2.7 -15 𝜆/D in ALES mode) (Doelman et al 2020(Doelman et al , 2021. For these observations, this meant that HD 1160 B was located in the dark hole of HD 1160 A across the entire wavelength range covered by the ALES L-band prism.…”

Section: Observationsmentioning

confidence: 99%

See 1 more Smart Citation

Measuring the variability of directly imaged exoplanets using vector Apodizing Phase Plates combined with ground-based differential spectrophotometry

Sutlieff¹,

Birkby²,

Stone³

et al. 2023

Preprint

View full text Add to dashboard Cite

Clouds and other features in exoplanet and brown dwarf atmospheres cause variations in brightness as they rotate in and out of view. Ground-based instruments reach the high contrasts and small inner working angles needed to monitor these faint companions, but their small fieldsof-view lack simultaneous photometric references to correct for non-astrophysical variations. We present a novel approach for making ground-based light curves of directly imaged companions using high-cadence differential spectrophotometric monitoring, where the simultaneous reference is provided by a double-grating 360°vector Apodizing Phase Plate (dgvAPP360) coronagraph. The dgvAPP360 enables high-contrast companion detections without blocking the host star, allowing it to be used as a simultaneous reference. To further reduce systematic noise, we emulate exoplanet transmission spectroscopy, where the light is spectrally-dispersed and then recombined into white-light flux. We do this by combining the dgvAPP360 with the infrared ALES integral field spectrograph on the Large Binocular Telescope Interferometer. To demonstrate, we observed the red companion HD 1160 B (separation ∼780 mas) for one night, and detect 8.8% semi-amplitude sinusoidal variability with a ∼3.24 h period in its detrended white-light curve. We achieve the greatest precision in ground-based high-contrast imaging light curves of sub-arcsecond companions to date, reaching 3.7% precision per 18-minute bin. Individual wavelength channels spanning 3.59-3.99 µm further show tentative evidence of increasing variability with wavelength. We find no evidence yet of a systematic noise floor, hence additional observations can further improve the precision. This is therefore a promising avenue for future work aiming to map storms or find transiting exomoons around giant exoplanets.

show abstract

“…At least two phase mask technologies exist that could be used to fabricate the above-described achromatic bPWFS piston mask: sub-wavelength gratings 17 and liquid crystals. 18…”

Section: Chromaticity and Fabricationmentioning

confidence: 99%

The Bright Pyramid Wavefront Sensor

Gerard¹,

Chambouleyron²,

Jensen-Clem³

et al. 2021

Preprint

View full text Add to dashboard Cite

Extreme adaptive optics (AO) is crucial for enabling the contrasts needed for ground-based high contrast imaging instruments to detect exoplanets. Pushing exoplanet imaging detection sensitivities towards lower mass, closer separations, and older planets will require upgrading AO wavefront sensors (WFSs) to be more efficient. In particular, future WFS designs will aim to improve a WFS's measurement error (i.e., the wavefront level at which photon noise, detector noise, and/or sky background limits a WFS measurement) and linearity (i.e., the wavefront level, in the absence of photon noise, aliasing, and servo lag, at which an AO loop can close and the corresponding closed-loop residual level). We present one such design here called the bright pyramid WFS (bPWFS), which improves both the linearity and measurement errors as compared to the non-modulated pyramid WFS (PWFS). The bPWFS is a unique design that, unlike other WFSs, doesn't sacrifice measurement error for linearity, potentially enabling this WFS to (a) close the AO loop on open loop turbulence utilising a tip/tilt modulation mirror (i.e., a modulated bPWFS; analogous to the procedure used for the regular modulated PWFS), and (b) reach deeper closed-loop residual wavefront levels (i.e., improving both linearity and measurement error) compared to the regular non-modulated PWFS. The latter approach could be particularly beneficial to enable improved AO performance using the bWFS as a second stage AO WFS. In this paper we will present an AO error budget analysis of the non-modulated bPWFS as well as supporting AO testbed results from the Marseille Astrophysics Laboratory.

show abstract

Vector-apodizing phase plate coronagraph: design, current performance, and future development [Invited]

Cited by 21 publications

References 93 publications

L-band Integral Field Spectroscopy of the HR 8799 Planetary System

L-band Integral Field Spectroscopy of the HR 8799 Planetary System

Measuring the variability of directly imaged exoplanets using vector Apodizing Phase Plates combined with ground-based differential spectrophotometry

The Bright Pyramid Wavefront Sensor

Contact Info

Product

Resources

About