MATISSE: perspective of imaging in the mid-infrared at the VLTI

López, B.; Wolf, S.; Lagarde, S.; Ábrahám, P.; Antonelli, P.; Augereau, J.-C.; Beckman, U.; Behrend, J.; Berruyer, N.; Bresson, Y.; Chesneau, O.; Clausse, J. M.; Connot, C.; Demyk, K.; Danchi, W. C.; Dugué, M.; Flament, S.; Glazenborg, A.; Graser, U.; Henning, Th.; Hofmann, K.-H.; Heininger, M.; Hugues, Y.; Jaffe, W.; Jankov, S.; Kraus, Stefan; Laun, W.; Leinert, Christoph; Linz, Hendrick; Mathias, P.; Meisenheimer, K.; Matter, A.; Menut, Jean-Luc; Millour, F.; Neumann, Udo; Nußbaum, E.; Niedzielski, A.; Mosonic, L.; Petrov, Romain G.; Ratzka, Thorsten; Robbe-Dubois, S.; Roussel, Alain; Schertl, D.; Schmider, F. X.; Stecklum, B.; Thiébaut, Éric; Vakili, F.; Wagner, K.; Waters, L. B. F. M.; Weigelt, G.

doi:10.1117/12.789412

Cited by 24 publications

(10 citation statements)

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“…Therefore, the powerspectrum (often called squared visibility) and the argument of the bispectrum (the so-called closure phase) were defined as the main observables of the geometrical information of the source's brightness distribution. However, the "new" available wavelength-dependent phase (the so-called "differential phase"), accessible through the spectro-interferometric capabilities of instruments like AMBER [30], GRAVITY [8], and MATISSE [17] provide much more information than the geometric information of the closure phase alone.…”

Section: Solving the Phase Problemmentioning

confidence: 99%

“…However, the standard use of several of these software packages was limited to recover monochromatic images. With the consolidation of the spectrointerferometric capabilities of the second generation instruments, GRAVITY [8] and MATISSE [17], at the Very Large Telescope Interferometer (VLTI), some of the aforementioned software have been updated, and new methods are being developed to obtain chromatic images in a systematic way. For example, at the VIII edition of the "Interferometric Imaging Beauty Contest" a benchmark of different algorithms was done with simulated chromatic data for the first time [34].…”

Section: Introductionmentioning

confidence: 99%

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Why chromatic imaging matters

et al. 2018

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During the last two decades, the first generation of beam combiners at the Very Large Telescope Interferometer has proved the importance of optical interferometry for high-angular resolution astrophysical studies in the near-and mid-infrared. With the advent of 4-beam combiners at the VLTI, the J. Sanchez-Bermudez works at European Southern Observatory, Alonso de Córdova 3107, 2 J. Sanchez et al.u − v coverage per pointing increases significantly, providing an opportunity to use reconstructed images as powerful scientific tools. Therefore, interferometric imaging is already a key feature of the new generation of VLTI instruments, as well as for other interferometric facilities like CHARA and JWST. It is thus imperative to account for the current image reconstruction capabilities and their expected evolutions in the coming years. Here, we present a general overview of the current situation of optical interferometric image reconstruction with a focus on new wavelength-dependent information, highlighting its main advantages and limitations. As an appendix we include several cookbooks describing the usage and installation of several state-of-the art image reconstruction packages. To illustrate the current capabilities of the software available to the community, we recovered chromatic images, from simulated MATISSE data, using the MCMC software SQUEEZE. With these images, we aim at showing the importance of selecting good regularization functions and their impact on the reconstruction.

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Section: Solving the Phase Problemmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Why chromatic imaging matters

et al. 2018

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“…Around 2013, the VLTI is expected to receive the first second-generation general user instruments making use of 4 telescopes simultaneously. These are Matisse working in the L, M, N bands (Lopez et al, 2008) and Gravity with dual beam operation and an astrometric capability (Eisenhauer et al, 2008).…”

Section: Vltimentioning

confidence: 99%

Imaging the heart of astrophysical objects with optical long-baseline interferometry

Berger

Malbet

Baron

et al. 2012

Astron Astrophys Rev

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The number of publications of aperture-synthesis images based on optical longbaseline interferometry measurements has recently increased due to easier access to visible and infrared interferometers. The interferometry technique has now reached a technical maturity level that opens new avenues for numerous astrophysical topics requiring milliarcsecond model-independent imaging. In writing this paper our motivation was twofold: 1) review and publicize emblematic excerpts of the impressive corpus accumulated in the field of optical interferometry image reconstruction; 2) discuss future prospects for this technique by selecting four representative astrophysical science cases in order to review the potential benefits of using optical long baseline interferometers.For this second goal we have simulated interferometric data from those selected astrophysical environments and used state-of-the-art codes to provide the reconstructed images that are reachable with current or soon-to-be facilities. The image reconstruction process was "blind" in the sense that reconstructors had no knowledge of the input brightness distributions. We discuss the impact of optical interferometry in those four astrophysical fields. We show that image reconstruction software successfully provides accurate morphological information on a variety of astrophysical topics and review the current strengths and weaknesses of such reconstructions. We investigate how to improve image reconstruction and the quality of the image possibly by upgrading the current facilities. We finally argue that optical interferometers and their corresponding instrumentation, existing or to come, with 6 to 10 telescopes, should be well suited to provide images of complex sceneries.

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“…In the following, the telescope simulation that is currently used is presented. Tools that are not yet developed include visibility calculations for current and future infrared interferometers, such as VLT-MATISSE (Lopez et al 2008).…”

Section: Simulating Observationsmentioning

confidence: 99%

A New Raytracer for Modeling Au-Scale Imaging of Lines From Protoplanetary Disks

Pontoppidan

Meijerink

Dullemond

et al. 2009

ApJ

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The material that formed the present-day solar system originated in feeding zones in the inner solar nebula located at distances within ∼ 20 AU from the Sun, known as the planet-forming zone. Meteoritic and cometary material contain abundant evidence for the presence of a rich and active chemistry in the planet-forming zone during the gas-rich phase of solar system formation. It is a natural conjecture that analogs can be found among the zoo of protoplanetary disks around nearby young stars. The study of the chemistry and dynamics of planet formation requires: (1) tracers of dense gas at 100-1000 K and (2) imaging capabilities of such tracers with 5-100 mas (0.5-20 AU) resolution, corresponding to the planet-forming zone at the distance of the closest star-forming regions. Recognizing that the rich infrared (2-200 μm) molecular spectrum recently discovered to be common in protoplanetary disks represents such a tracer, we present a new general ray-tracing code, RADLite, that is optimized for producing infrared line spectra and images from axisymmetric structures. RADLite can consistently deal with a wide range of velocity gradients, such as those typical for the inner regions of protoplanetary disks. The code is intended as a back-end for chemical and excitation codes, and can rapidly produce spectra of thousands of lines for grids of models for comparison with observations. Such radiative transfer tools will be crucial for constraining both the structure and chemistry of planet-forming regions, including data from current infrared imaging spectrometers and extending to the Atacama Large Millimeter Array and the next generation of Extremely Large Telescopes, the James Webb Space Telescope and beyond.

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MATISSE: perspective of imaging in the mid-infrared at the VLTI

Cited by 24 publications

References 1 publication

Why chromatic imaging matters

Why chromatic imaging matters

Imaging the heart of astrophysical objects with optical long-baseline interferometry

A New Raytracer for Modeling Au-Scale Imaging of Lines From Protoplanetary Disks

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