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1. MIRC-X polarinterferometry at CHARA

   https://doi.org/10.1117/12.2562407  

   Setterholm, Benjamin R. ; Monnier, John D. ; Le Bouquin, Jean-Baptiste ; Anugu, Narsireddy ; Labdon, Aaron ; Ennis, Jacob ; Johnson, Keith J. ; Kraus, Stefan ; ten Brummelaar, Theo A. ( December 2020 , Proceedings of the SPIE)

   Mérand, Antoine ; Sallum, Stephanie ; Tuthill, Peter G. (Ed.)

   We present a new polarimetric mode for the MIRC-X 6-telescope beam combiner at CHARA. Utilizing the extensive u - v coverage afforded by CHARA this mode will be able to resolve and constrain scattered light in environs at milliarcsecond separations of target stars, a largely unexplored parameter space to-date in astronomy. Notably, this upgrade will allow for the investigation of the scattering properties of the inner dust wall at the sublimation radius of Herbig Ae/Be star disks, dust shells surrounding evolved stars, and gas-rich disks around Be stars. Our design adds a series of rotating half-wave plates, achromatic across J- and H-bands, and a polarizing beamsplitter into the MIRC-X beam path. In this work, we also preview on-sky observations, discussing ongoing work calibrating instrumental polarization effects in the CHARA beam path as well as upgrades to the MIRC-X data reduction pipeline.
2. Ultrafast laser inscription of asymmetric integrated waveguide 3  dB couplers for astronomical K-band interferometry at the CHARA array

   https://doi.org/10.1364/JOSAB.423727  

   Benoît, Aurélien ; Pike, Fraser A. ; Sharma, Tarun K. ; MacLachlan, David G. ; Dinkelaker, Aline N. ; Nayak, Abani S. ; Madhav, Kalaga ; Roth, Martin M. ; Labadie, Lucas ; Pedretti, Ettore ; et al ( August 2021 , Journal of the Optical Society of America B)

   We present the fabrication and characterization of 3 dB asymmetric directional couplers for the astronomical K-band at wavelengths between 2.0 and 2.4 µm. The couplers were fabricated in commercial Infrasil silica glass using an ultrafast laser operating at 1030 nm. After optimizing the fabrication parameters, the insertion losses of straight single-mode waveguides were measured to be$\sim <\#comment/>1.2\pm <\#comment/>0.5\mathrm{d}\mathrm{B}$across the full K-band. We investigate the development of asymmetric 3 dB directional couplers by varying the coupler interaction lengths and by varying the width of one of the waveguide cores to detune the propagation constants of the coupled modes. In this manner, we demonstrate that ultrafast laser inscription is capable of fabricating asymmetric 3 dB directional couplers for future applications in K-band stellar interferometry. Finally, we demonstrate that our couplers exhibit an interferometric fringe contrast of$><\#comment/>90\mathrm{\%<\#comment/>}$. This technology paves the path for the development of a two-telescope K-band integrated optic beam combiner for interferometry to replace the existing beam combiner (MONA) in Jouvence of the Fiber Linked Unit for Recombination (JouFLU) at the Center for High Angular Resolution Astronomy (CHARA) telescope array.
3. Viscous heating in the disk of the outbursting star FU Orionis

   https://doi.org/10.1051/0004-6361/202039370  

   Labdon, Aaron ; Kraus, Stefan ; Davies, Claire L. ; Kreplin, Alexander ; Monnier, John D. ; Le Bouquin, Jean-Baptiste ; Anugu, Narsireddy ; ten Brummelaar, Theo ; Setterholm, Benjamin ; Gardner, Tyler ; et al ( February 2021 , Astronomy & Astrophysics)

   null (Ed.)

   Context. FU Orionis is the archetypal FUor star, a subclass of young stellar objects (YSOs) that undergo rapid brightening events, often gaining between four and six magnitudes on timescales of days. This brightening is often associated with a massive increase in accretion, which is one of the most ubiquitous processes in astrophysics for bodies ranging from planets and stars to super-massive black holes. We present multi-band interferometric observations of the FU Ori circumstellar environment, including the first J -band interferometric observations of a YSO. Aims. We investigate the morphology and temperature gradient of the innermost regions of the accretion disk around FU Orionis. We aim to characterise the heating mechanisms of the disk and comment on potential outburst-triggering processes. Methods. Recent upgrades to the MIRC-X instrument at the CHARA array have allowed for the first dual-band J and H observations of YSOs. Using baselines up to 331 m, we present high-angular-resolution data of a YSO covering the near-infrared bands J , H , and K . The unprecedented spectral range of the data allowed us to apply temperature gradient models to the innermost regions of FU Ori. Results. We spatially resolved the innermost astronomical unit of the disk and determinemore »the exponent of the temperature gradient of the inner disk to T ∝ r −0.74 ± 0.02 . This agrees with theoretical works that predict T ∝ r −0.75 for actively accreting, steady-state disks, which is a value only obtainable through viscous heating within the disk. We found a disk that extends down to the stellar surface at 0.015 ± 0.007 au, where the temperature is found to be 5800 ± 700 K. We found a disk inclined at 32 ± 4° with a minor-axis position angle of 34 ± 11°. Conclusions. We demonstrate that J -band interferometric observations of YSOs are feasible with the MIRC-X instrument at CHARA. The temperature gradient power-law derived for the inner disk is consistent with theoretical predictions for steady-state, optically thick, viciously heated accretion disks.« less
4. EXPRES. III. Revealing the Stellar Activity Radial Velocity Signature of ϵ Eridani with Photometry and Interferometry

   https://doi.org/10.3847/1538-3881/ac3235  

   Roettenbacher, Rachael M. ; Cabot, Samuel H. ; Fischer, Debra A. ; Monnier, John D. ; Henry, Gregory W. ; Harmon, Robert O. ; Korhonen, Heidi ; Brewer, John M. ; Llama, Joe ; Petersburg, Ryan R. ; et al ( December 2021 , The Astronomical Journal)

   Abstract The distortions of absorption line profiles caused by photospheric brightness variations on the surfaces of cool, main-sequence stars can mimic or overwhelm radial velocity (RV) shifts due to the presence of exoplanets. The latest generation of precision RV spectrographs aims to detect velocity amplitudes ≲ 10 cm s −1 , but requires mitigation of stellar signals. Statistical techniques are being developed to differentiate between Keplerian and activity-related velocity perturbations. Two important challenges, however, are the interpretability of the stellar activity component as RV models become more sophisticated, and ensuring the lowest-amplitude Keplerian signatures are not inadvertently accounted for in flexible models of stellar activity. For the K2V exoplanet host ϵ Eridani, we separately used ground-based photometry to constrain Gaussian processes for modeling RVs and TESS photometry with a light-curve inversion algorithm to reconstruct the stellar surface. From the reconstructions of TESS photometry, we produced an activity model that reduced the rms scatter in RVs obtained with EXPRES from 4.72 to 1.98 m s −1 . We present a pilot study using the CHARA Array and MIRC-X beam combiner to directly image the starspots seen in the TESS photometry. With the limited phase coverage, our spot detections are marginal withmore »current data but a future dedicated observing campaign should allow for imaging, as well as allow the stellar inclination and orientation with respect to the debris disk to be definitively determined. This work shows that stellar surface maps obtained with high-cadence, time-series photometric and interferometric data can provide the constraints needed to accurately reduce RV scatter.« less
5. Dusty disk winds at the sublimation rim of the highly inclined, low mass young stellar object SU Aurigae

   https://doi.org/10.1051/0004-6361/201935331  

   Labdon, Aaron ; Kraus, Stefan ; Davies, Claire L. ; Kreplin, Alexander ; Kluska, Jacques ; Harries, Tim J. ; Monnier, John D. ; ten Brummelaar, Theo ; Baron, Fabien ; Millan-Gabet, Rafael ; et al ( July 2019 , Astronomy & Astrophysics)

   Context. T Tauri stars are low-mass young stars whose disks provide the setting for planet formation. Despite this, their structure is poorly understood. We present new infrared interferometric observations of the SU Aurigae circumstellar environment that offer resolution that is three times higher and a better baseline position angle coverage than previous observations. Aims. We aim to investigate the characteristics of the circumstellar material around SU Aur, constrain the disk geometry, composition and inner dust rim structure. Methods. The CHARA array offers unique opportunities for long baseline observations, with baselines up to 331 m. Using the CLIMB three-telescope combiner in the K -band allows us to measure visibilities as well as closure phase. We undertook image reconstruction for model-independent analysis, and fitted geometric models such as Gaussian and ring distributions. Additionally, the fitting of radiative transfer models constrain the physical parameters of the disk. For the first time, a dusty disk wind is introduced to the radiative transfer code TORUS to model protoplanetary disks. Our implementation is motivated by theoretical models of dusty disk winds, where magnetic field lines drive dust above the disk plane close to the sublimation zone. Results. Image reconstruction reveals an inclined disk with slight asymmetrymore »along its minor-axis, likely due to inclination effects obscuring the inner disk rim through absorption of incident star light on the near-side and thermal re-emission and scattering of the far-side. Geometric modelling of a skewed ring finds the inner rim at 0.17 ± 0.02 au with an inclination of 50.9 ± 1.0° and minor axis position angle 60.8 ± 1.2°. Radiative transfer modelling shows a flared disk with an inner radius at 0.18 au which implies a grain size of 0.4 μ m assuming astronomical silicates and a scale height of 15.0 at 100 au. Among the tested radiative transfer models, only the dusty disk wind successfully accounts for the K -band excess by introducing dust above the mid-plane.« less