Search

The James Webb Space Telescope's Near Infrared Imager and Slitless Spectrograph (JWST-NIRISS) flies a 7-hole non-redundant mask (NRM), the first such interferometer in space, operating at 3-5 \micron~wavelengths, and a bright limit of $\simeq 4$ magnitudes in W2. We describe the NIRISS Aperture Masking Interferometry (AMI) mode to help potential observers understand its underlying principles, present some sample science cases, explain its operational observing strategies, indicate how AMI proposals can be developed with data simulations, and how AMI data can be analyzed. We also present key results from commissioning AMI. Since the allied Kernel Phase Imaging (KPI) technique benefits from AMI operational strategies, we also cover NIRISS KPI methods and analysis techniques, including a new user-friendly KPI pipeline. The NIRISS KPI bright limit is $\simeq 8$ W2 magnitudes. AMI (and KPI) achieve an inner working angle of $\sim 70$ mas that is well inside the $\sim 400$ mas NIRCam inner working angle for its circular occulter coronagraphs at comparable wavelengths., 30 pages, 10 figures

Nulling interferometry is one of the most promising technologies for imaging exoplanets within stellar habitable zones. The use of photonics for carrying out nulling interferometry enables the contrast and separation required for exoplanet detection. So far, two key issues limiting current-generation photonic nullers have been identified: phase variations and chromaticity within the beam combiner. The use of tricouplers addresses both limitations, delivering a broadband, achromatic null together with phase measurements for fringe tracking. Here, we present a derivation of the transfer matrix of the tricoupler, including its chromatic behaviour, and our 3D design of a fully symmetric tricoupler, built upon a previous design proposed for the GLINT instrument. It enables a broadband null with symmetric, baseline-phase-dependent splitting into a pair of bright channels when inputs are in anti-phase. Within some design trade space, either the science signal or the fringe tracking ability can be prioritised. We also present a tapered-waveguide $180^\circ$-phase shifter with a phase variation of $0.6^\circ$ in the $1.4-1.7~\mu$m band, producing a near-achromatic differential phase between beams{ for optimal operation of the tricoupler nulling stage}. Both devices can be integrated to deliver a deep, broadband null together with a real-time fringe phase metrology signal., Comment: 20 pages, 17 figures, submitted to Journal of Astronomical Telescopes, Instruments, and Systems

We chart the expected Galactic distribution of neutron stars and black holes. These compact remnants of dead stars -- the Galactic underworld -- are found to exhibit a fundamentally different distribution and structure to the visible Galaxy. Compared to the visible Galaxy, concentration into a thin flattened disk structure is much less evident with the scale height more than tripling to 1260 +- 30 pc. This difference arises from two primary causes. Firstly, the distribution is in part inherited from the integration over the evolving structure of the Galaxy itself (and hence the changing distribution of the parent stars). Secondly, an even larger effect arises from the natal kick received by the remnant at the event of its supernova birth. Due to this kick we find 30% of remnants have sufficient kinetic energy to entirely escape the Galactic potential (40% of neutron stars and 2% of black holes) leading to a Galactic mass loss integrated to the present day of ~ 0.4% of the stellar mass of the Galaxy. The black hole -- neutron star fraction increases near the Galactic centre: a consequence of smaller kick velocities in the former (the assumption made is that kick velocity is inversely proportional to mass). Our simulated remnant distribution yields probable distances of 19 pc and 21 pc to the nearest neutron star and black hole respectively, while our nearest probable magnetar lies at 4.2 kpc. Although the underworld only contains of order ~ 1% of the Galaxy's mass, observational signatures and physical traces of its population, such as microlensing, will become increasingly present in data ranging from gravitational wave detectors to high precision surveys from space missions such as Gaia., Comment: 9 pages, 11 figures

Speckle Noise is the dominant source of error in high contrast imaging with adaptive optics system. We discuss the potential for wavefront sensing telemetry to calibrate speckle noise with sufficient precision and accuracy so that it can be removed in post-processing of science images acquired by high contrast imaging instruments. In such a self-calibrating system, exoplanet detection would be limited by photon noise and be significantly more robust and efficient than in current systems. We show initial laboratory and on-sky tests, demonstrating over short timescale that residual speckle noise is indeed calibrated to an accuracy exceeding readout and photon noise in the high contrast region. We discuss immplications for the design of space and ground high-contrast imaging systems., 12 pages, 7 figures, To appear in SPIE Proceedings of Astronomical Telescopes + Instrumentation, 2022. arXiv admin note: text overlap with arXiv:2109.13958

Direct images of protoplanets embedded in disks around infant stars provide the key to understanding the formation of gas giant planets like Jupiter. Using the Subaru Telescope and Hubble Space Telescope, we find evidence for a jovian protoplanet around AB Aurigae orbiting at a wide projected separation (93 au), likely responsible for multiple planet-induced features in the disk. Its emission is reproducible as reprocessed radiation from an embedded protoplanet. We also identify two structures located at 430-580 au that are candidate sites of planet formation. These data reveal planet formation in the embedded phase and a protoplanet discovery at wide, > 50 au separations characteristic of most imaged exoplanets. With at least one clump-like protoplanet and multiple spiral arms, the AB Aur system may also provide the evidence for a long-considered alternative to the canonical model for Jupiter's formation: disk (gravitational) instability., Author's personal version: 19 pages, 5 Figures, 1 Table; 32 Supplementary pages, 18 Supplementary Figures, 1 Supplementary Table; Accepted for Publication in Nature Astronomy. Published version: https://www.nature.com/articles/s41550-022-01634-x

Sparse aperture masking interferometry (SAM) is a high resolution observing technique that allows for imaging at and beyond a telescope's diffraction limit. The technique is ideal for searching for stellar companions at small separations from their host star; however, previous analysis of SAM observations of young stars surrounded by dusty disks have had difficulties disentangling planet and extended disk emission. We analyse VLT/SPHERE-IRDIS SAM observations of the transition disk LkCa\,15, model the extended disk emission, probe for planets at small separations, and improve contrast limits for planets. We fit geometrical models directly to the interferometric observables and recover previously observed extended disk emission. We use dynamic nested sampling to estimate uncertainties on our model parameters and to calculate evidences to perform model comparison. We compare our extended disk emission models against point source models to robustly conclude that the system is dominated by extended emission within 50 au. We report detections of two previously observed asymmetric rings at $\sim$17 au and $\sim$45 au. The peak brightness location of each model ring is consistent with the previous observations. We also, for the first time with imaging, robustly recover an elliptical Gaussian inner disk, previously inferred via SED fitting. This inner disk has a FWHM of ~5 au and a similar inclination and orientation as the outer rings. Finally, we recover no clear evidence for candidate planets. By modelling the extended disk emission, we are able to place a lower limit on the near infrared companion contrast of at least 1000., Comment: Accepted for publication in ApJ

We describe the design and initial results from a visible-light Lyot coronagraph for SCExAO/VAMPIRES. The coronagraph is comprised of four hard-edged, partially transmissive focal plane masks with inner working angles of 36 mas, 55 mas, 92 mas, and 129 mas, respectively. The Lyot stop is a reflective, undersized design with a geometric throughput of 65.7%. Our preliminary on-sky contrast is 1e-2 at 0.1" to 1e-4 at 0.75" for all mask sizes. The coronagraph was deployed in early 2022 and is available for open use., Comment: Proceedings of SPIE 2022 Astronomical Instrumentation and Telescopes conference (#12184-163)

AST3-NIR is a new infrared camera for deployment with the AST3-3 wide-field survey telescope to Dome A on the Antarctic plateau. This project is designed to take advantage of the low Antarctic infrared sky thermal background (particularly within the Kdark near infrared atmospheric window at 2.4 μm) and the long Antarctic nights to provide high sensitivity temporal data from astronomical sources. The data collected from the Kunlun Infrared Sky Survey (KISS) will be used to conduct a range of astronomical science cases including the study of supernovae, exo-planets, variable stars, and the cosmic infrared background.

The Gemini Planet Imager (GPI) Extreme Adaptive Optics Coronograph contains an interferometric mode: a 10-hole non-redundant mask (NRM) in its pupil wheel. GPI operates at $Y, J, H$, and $K$ bands, using an integral field unit spectrograph (IFS) to obtain spectral data at every image pixel. NRM on GPI is capable of imaging with a half resolution element inner working angle at moderate contrast, probing the region behind the coronagraphic spot. The fine features of the NRM PSF can provide a reliable check on the plate scale, while also acting as an attenuator for spectral standard calibrators that would otherwise saturate the full pupil. NRM commissioning data provides details about wavefront error in the optics as well as operations of adaptive optics control without pointing control from the calibration system. We compare lab and on-sky results to evaluate systematic instrument properties and examine the stability data in consecutive exposures. We discuss early on-sky performance, comparing images from integration and tests with the first on-sky images, and demonstrate resolving a known binary. We discuss the status of NRM and implications for future science with this mode., Comment: 14 pages, 14 figures. Proceedings of the SPIE, 9147-135

Commission 54 held its business meeting on 11 August 2009 at “Botequim” at Rua Visconde de Caravelas 184/186, Humaitá, Botafogo, Rio de Janeiro. Individual members in attendance reported on activities of relevance to C54.

The University of Sydney has a long history in optical stellar interferometry. The first project, in the 1960s, was the Narrabri Stellar Intensity Interferometer, which measured the angular diameters of 32 hot stars and established the temperature scale for spectral classes O - F. That instrument was followed by the Sydney University Stellar Interferometer (SUSI), which is now undergoing a third-generation upgrade, to use the multi-wavelength PAVO beam combiner. SUSI operates at visible rather than IR wavelengths and has baselines up to 160 m, so it is well suited to the study of hot stars. A number of studies have been carried out, and more are planned when commissioning of the PAVO system is complete. Conversion of the system to allow remote operation will allow larger scientific projects to be undertaken., 2 pages. To appear in RevMexAA(SC) 'The Interferometric View on Hot Stars' (Conference held at Vina del Mar, March 2-6, 2009)

ispartof: OPTICAL AND INFRARED INTERFEROMETRY AND IMAGING VIII vol:12183 ispartof: Conference on Optical and Infrared Interferometry and Imaging VIII Part of SPIE Astronomical Telescopes and Instrumentation Conference location:CANADA, Montreal date:17 Jul - 22 Jul 2022 status: published

The dust- and gas-rich disks surrounding numerous pre-main-sequence stars are of key interest for unveiling how planetary system are formed; they are the initial conditions for planetary formation. Protoplanetary disks have a rich structure, with different physics playing a role in different regions of the disk. The dynamic ranges involved span two to five orders of magnitudes on spatial scales, orbital times, temperatures, and much more in dust- or gas-densities. The extreme dynamic ranges involved in the structure and composition of these objects mean that very different observational techniques have to be combined together to probe their various regions.This PhD makes use of new K, L and M-band imaging and Sparse-Aperture-Masking (SAM) Interferometric measurements, 3-4 micron spectroscopy, together with published 8.6 and 18.7 micron images and spectral energy distribution (SED) fluxes from UV to mm-wavelength to instruct a new comprehension of the famous IRS-48 object, and uncover the delicate balance of physical processes at stake.This PhD reports the first ever direct imaging of the full extents of a polycyclic aromatic hydrocarbon (PAH) and very small grains (VSG) ring in a young circumstellar disk, presents a revised model for the IRS-48 object to explain the rich and complex dust- and gas-environment observed from near-infrared to centimeter wavelengths, and sets limits on how much silicates grains - hence replenishment - is to be expected in the PAH and VSG ring.Radiative transfer modelling of the disk-structure and grains compositions converges to a classical-grains outer-disk from 55 AU combined with an unsettled VSG & PAH-ring, where the inner- and outer-rim are resolved: 11 and 26 AU. A brighter hence larger central-star with modified extinction parameters accounts for the near-infrared flux observed in the SED: the inner-most disk at ~1 AU is not needed. The revised stellar parameters place this system on a 4 Myr evolutionary track, much younger than the previous estimations, in better agreement with the surrounding region and disk-dispersal observations. Using closure-phases, two over-luminosities are found in the PAH-ring, at color-temperatures consistent with the radiative transfer simulations; one follows a sub-Keplerian circular orbit. This PhD also shows that only very few settled thermal silicates can be co-located with the PAH-ring, with a depletion factor of ~5-6 compared to classical circumstellar dust-to-PAH abundances. A ~3 Jupiter-masses companion on a 40 AU orbit is compatible with the new disk structure and the previous mm-grains asymmetry.The IRS-48 disk is found to be void of dust-grains in the first 55 AU, except for a 3.7e-10 Solar-masses of a mixture of ionized and neutral PAH, and VSG. This places IRS-48 at the final stage of transition disks, when photo-evaporation dominates the disk evolution and eventually causes dispersal. Given the highly radiating environment, this PhD also highlights the probable replenishment of the inner PAH & VSG-ring through the channeling of such particles from the outer reservoir, due to the on-going accretion on the companion.; La poussière et le gaz qui entourent beaucoup d'étoiles jeunes sont d'un intérêt critique pour comprendre la formation planétaire ; ils représentent les conditions initiale de la formation planétaire. Les disques proto-planétaire ont une structure riche, avec différents processus physiques à l'oeuvre dans différentes régions du disque. Les grandeurs en jeu s'étalent sur 2 à 5 ordres de grandeur en échelles spatiales, période orbitale, températures, et bien plus en ce qui concerne la densité de gaz et poussière. Les variations extrêmes de ces paramètres clés impliqués dans la structure et la compositions de ces objets implique nécessairement l'utilisation combinée de différentes techniques d'observation.Cette recherche se base sur l'utilisation de nouvelles données d'imagerie et de masquage de pupille (SAM) en bandes K, L et M, de spectres entre 3 et 4 microns, en plus d'images à 8.6 et 18.7 microns et de données de densité spectrale de flux (SED) issus de la littérature. Ces données des UV aux longueurs d'ondes millimétriques ont permis de construire une nouvelle compréhension de l'objet IRS-48, et de mettre en avant l'équilibre subtil des processus physiques en jeu. Ce travail a permis d'imager pour la première fois l'intégralité spatiale d'un disque composé d'hydrocarbures polycyclique aromatique (PAH) et de très petits grains (VSG) autour d'un objet stellaire jeune. Il propose un modèle révisé pour cet objet de façon à expliquer l'environnement riche et complexe de gaz et poussières observé en proche infrarouge et en ondes millimétriques, et pose des limites sur la quantité attendue de grains silicatés - synonymes de renouvelle du disque - qui peut se trouver dans ce disque de PAH/VSG.Une modélisation en transfert radiatif de la structure du disque et de la composition des grains converge vers un disque externe à 55 AU composé de grains classiques, en plus d'un disque non-sédimenté de PAH et VSG dont les bords internes et externes sont résolus: 11 et 26 AU. Une étoiles plus brillante - donc plus large - associée à une adaptation des courbes de rougissement permet d'expliquer les flux observés dans le proche-infrarouge: le disque très interne à l'étoile, à 1 AU environ, n'est plus nécessaire. Les nouveaux paramètres stellaire permettent d'estimer un âge de 4 millions d'années pour cet objet, beaucoup plus jeune que les estimations précédentes, et en meilleur accord avec l'environnement direct de l'étoile et les statistiques de dispersion de tels disques. L'utilisation de clôtures de phase a permis de détecter deux sur-brillance au sein du disque de PAH, dont la température de couleur correspond à la température de ce disque trouvé grâce au transfert radiatif. Une sur-brillance suit une orbite circulaire sous-Keplerienne. Ce travail a permis de montrer qu'une quantité limitée de grains classiques silicatés pouvait être localisé dans le disque de PAH, avec un facteur de déplétion de 5-6 par rapport aux abondances classiques de poussière-à-PAH. Un compagnon d'environ 3 masses de Jupiter sur une orbite à 40 AU est compatible avec la nouvelle structure du disque et l'observation précédente d'une asymétrie de grain millimétriques.Le disque d'IRS-48 est dépourvu de poussière dans ses premiers 55 AU, à l'exception de 3.7e-10 masses solaire d'une mixture de PAH neutres et ionisés, et de VSG. Ceci place IRS-48 au stade final des disques de transition, alors que la photo-evaporation commence à dominer l'évolution du disque jusqu'à provoqué sa dispersion. Etant donné le fort environnement radiatif, the doctorat permet aussi de mettre en avant un probable renflouement du disque interne de PAH et VSG par le disque externe grâce à des effets gravitationnels induits par le compagnon.