MagAO-X first light

Males, Jared R.; Close, Laird M.; Guyon, Olivier; Hedglen, Alexander D.; Gorkom, Kyle Van; Long, Joseph D.; Kautz, Maggie; Lumbres, Jennifer; Schatz, Lauren; Rodack, Alexander; Miller, Kelsey; Doelman, David; Snik, Frans; Bos, Steven P.; Knight, J. H.; Morzinski, Katie M.; Gasho, Victor; Keller, Christoph U.; Haffert, Sebastiaan Y.; Pearce, Logan

doi:10.1117/12.2561682

Cited by 26 publications

(19 citation statements)

References 16 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The first generation of extreme adaptive optics (AO) instruments, such as the Gemini Planet Imager (GPI; Macintosh et al 2014) and the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE; Beuzit et al 2019) at VLT, have achieved factors of 100 improvement, in contrast, at subarcsecond separations over conventional systems; but typically were only sensitive to Jovian exoplanets at projected separations beyond ∼10 au (e.g., Nielsen et al 2019;Vigan et al 2020). To more frequently identify companions at Jupiter-to-Saturn separations, upgraded versions of GPI/SPHERE and second-generation systems like the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system and MagAO-X (Jovanovic et al 2015b;Males et al 2020) must yield deeper contrasts at ρ < 0 4.…”

Section: Introductionmentioning

confidence: 99%

SCExAO/MEC and CHARIS Discovery of a Low-mass, 6 au Separation Companion to HIP 109427 Using Stochastic Speckle Discrimination and High-contrast Spectroscopy*

Steiger

Currie

Brandt

et al. 2021

Self Cite

View full text Add to dashboard Cite

We report the direct imaging discovery of a low-mass companion to the nearby accelerating A star, HIP 109427, with the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument coupled with the Microwave Kinetic Inductance Detector Exoplanet Camera (MEC) and CHARIS integral field spectrograph. CHARIS data reduced with reference star point spread function (PSF) subtraction yield 1.1-2.4 μm spectra. MEC reveals the companion in Y and J band at a comparable signal-to-noise ratio using stochastic speckle discrimination, with no PSF subtraction techniques. Combined with complementary follow-up L p photometry from Keck/NIRC2, the SCExAO data favors a spectral type, effective temperature, and luminosity of M4-M5.5, 3000-3200 K, and

show abstract

Section: Introductionmentioning

confidence: 99%

SCExAO/MEC and CHARIS Discovery of a Low-mass, 6 au Separation Companion to HIP 109427 Using Stochastic Speckle Discrimination and High-contrast Spectroscopy*

Steiger

Currie

Brandt

et al. 2021

Self Cite

View full text Add to dashboard Cite

show abstract

“…Current instruments include the Subaru Coronagraphic Extreme Adaptive Optics instrument (SCExAO), 6 the Spectro-Polarimetric High-contrast Exoplanet Research instrument (SPHERE), 7 the Gemini Planet Imager (GPI), 8 the Keck Planet Imager and Characterizer (KPIC), 9 and most recently the Magellan Extreme Adaptive Optics System (MagAO-X). 10 All of these instruments have common features: a high actuator count deformable mirror running at extreme speeds (at least 1kHz), a high-performance wavefront sensor (WFS), and a high-contrast coronagraph. These instruments are pathfinders for ExAO systems on the GSMTs.…”

Section: Introductionmentioning

confidence: 99%

The Three-Sided PyramidWavefront Sensor. I. Simulations and Analysis for Astronomical Adaptive Optics

Schatz,

Males,

Correia

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

The Giant Segmented Mirror Telescopes (GSMTs) including the Giant Magellan Telescope (GMT), the Thirty Meter Telescope (TMT), and the European Extremely Large Telescope (E-ELT), all have extreme adaptive optics (ExAO) instruments planned that will use pyramid wavefront sensors (PWFS). The ExAO instruments all have common features: a high-actuator-count deformable mirror running at extreme speeds (greater than 1 kHz); a highperformance wavefront sensor (WFS); and a high-contrast coronagraph. A current limitation in ExAO wavefront sensor performance is the detector because ExAO needs high spatial sampling of the wavefront which requires a large detector. For ExAO instruments for the next generation of telescopes, alternative architectures of WFS are under consideration because there is a trade-off between detector size, speed, and noise that reduces the performance of GSMT-ExAO wavefront control. One option under consideration for a GSMT-ExAO wavefront sensor is a threesided PWFS (3PWFS). The 3PWFS creates three copies of the telescope pupil for wavefront sensing, compared to the conventional four-sided PWFS (4PWFS) which uses four pupils. The 3PWFS uses fewer detector pixels than the 4PWFS and should therefore be less sensitive to read noise. Here we develop a mathematical formalism based on the diffraction theory description of the Foucault knife edge test that predicts the intensity pattern after the PWFS. Our formalism allows us to calculate the intensity in the pupil images formed by the PWFS in the presence of phase errors corresponding to arbitrary Fourier modes. We use these results to motivate how we process signals from a 3PWFS. We compare the Raw Intensity method which uses the signal in the pupils as is and derive the Slopes Maps calculation for the 3PWFS which combines the three pupil images of the 3PWFS to obtain the X and Y slopes of the wavefront. We then use the Object Oriented MATLAB Adaptive Optics toolbox (OOMAO) to simulate an end-to-end model of an adaptive optics system using a PWFS with modulation and compare the performance of the 3PWFS to the 4PWFS. In the case of a low read noise detector, the Strehl ratios of the 3PWFS and 4PWFS are within 0.01. When we included higher read noise in the simulation, we found a Strehl ratio gain of 0.036 for the 3PWFS using Raw Intensity over the 4PWFS using Slopes Maps at a stellar magnitude of 10. At the same magnitude the 4PWFS RI also outperformed the 4PWFS SM, but the gain was only 0.012 Strehl. This is significant because 4PWFS using Slopes Maps is how the PWFS is conventionally used for AO wavefront sensing. We have found that the 3PWFS is a viable wavefront sensor that can fully reconstruct a wavefront and produce a stable closed-loop with correction comparable to that of a 4PWFS, with modestly better performance for high read-noise detectors.

show abstract

“…For on-sky operations, a likely strategy would be to use PD, cMWS and AP-WFS to minimize the non-common path aberrations before observing and use LDFC to remove any drifts. MagAO-X had first light in 2019, where it demonstrated a Strehl ratio of 46%, and a 5 post-processed gvAPP contrast of 10 −4 at 3 / at 900 nm (z') [79]. These results are promising for discovering exoplanets during formation through direct detection of from accretion of hydrogen onto these protoplanets.…”

Section: Magellan/magao-xmentioning

confidence: 88%

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

et al. 2021

View full text Add to dashboard Cite

Over the last decade, the vector-apodizing phase plate (vAPP) coronagraph has been developed from concept to on-sky application in many high-contrast imaging systems on 8-m class telescopes. The vAPP is an geometric-phase patterned coronagraph that is inherently broadband, and its manufacturing is enabled only by direct-write technology for liquid-crystal patterns. The vAPP generates two coronagraphic PSFs that cancel starlight on opposite sides of the point spread function (PSF) and have opposite circular polarization states. The efficiency, that is the amount of light in these PSFs, depends on the retardance offset from half-wave of the liquid-crystal retarder. Using different liquid-crystal recipes to tune the retardance, different vAPPs operate with high efficiencies (> 96%) in the visible and thermal infrared (0.55 µm to 5 µm). Since 2015, seven vAPPs have been installed in a total of six different instruments, including Magellan/MagAO, Magellan/MagAO-X, Subaru/SCExAO, and LBT/LMIRcam. Using two integral field spectrographs installed on the latter two instruments, these vAPPs can provide lowresolution spectra (R∼30) between 1 m and 5 m. We review the design process, development, commissioning, on-sky performance, and first scientific results of all commissioned vAPPs. We report on the lessons learned and conclude with perspectives for future developments and applications.

show abstract

MagAO-X first light

Cited by 26 publications

References 16 publications

SCExAO/MEC and CHARIS Discovery of a Low-mass, 6 au Separation Companion to HIP 109427 Using Stochastic Speckle Discrimination and High-contrast Spectroscopy*

SCExAO/MEC and CHARIS Discovery of a Low-mass, 6 au Separation Companion to HIP 109427 Using Stochastic Speckle Discrimination and High-contrast Spectroscopy*

The Three-Sided PyramidWavefront Sensor. I. Simulations and Analysis for Astronomical Adaptive Optics

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

Contact Info

Product

Resources

About