Published June 2016
| Version v1
Conference paper
Architecture design study and technology road map for the Planet Formation Imager (PFI)
Creators
- Monnier, John
- Ireland, Michael
- Kraus, Stefan
- Baron, Fabien
- Creech-Eakman, Michelle
- Dong, Ruobing
- Isella, Andrea
- Merand, Antoine
- Michael, Ernest
- Minardi, Stefano
- Mozurkewich, David
- Petrov, Romain
- Rinehart, Stephen
- ten Brummelaar, Theo
- Vasisht, Gautam
- Wishnow, Ed
- Young, John
- Zhu, Zhaohuan
- Monnier, John D.
- Ireland, Michael J.
- Rinehard, Stephen
- Brummelaar, Theo Ten
- Vasisht, Gautum
Contributors
Others:
- University of Michigan [Ann Arbor] ; University of Michigan System
- Australian National University - Department of engineering (ANU) ; Australian National University (ANU)
- School of Physics and Astronomy [Exeter] ; University of Exeter
- Georgia State University ; University System of Georgia (USG)
- New Mexico Institute of Mining and Technology [New Mexico Tech] (NMT)
- University of California [Berkeley] (UC Berkeley) ; University of California (UC)
- Rice University [Houston]
- European Southern Observatory (ESO)
- Universidad de Chile = University of Chile [Santiago] (UCHILE)
- Astrophysical Institute and University Observatory [Jena] (AIU) ; Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany]
- Joseph Louis LAGRANGE (LAGRANGE) ; Université Nice Sophia Antipolis (1965 - 2019) (UNS) ; COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur ; COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Description
The Planet Formation Imager (PFI) Project has formed a Technical Working Group (TWG) to explore possible facility architectures to meet the primary PFI science goal of imaging planet formation in situ in nearby star- forming regions. The goals of being sensitive to dust emission on solar system scales and resolving the Hill-sphere around forming giant planets can best be accomplished through sub-milliarcsecond imaging in the thermal infrared. Exploiting the 8-13 micron atmospheric window, a ground-based long-baseline interferometer with approximately 20 apertures including 10km baselines will have the necessary resolution to image structure down 0.1 milliarcseconds (0.014 AU) for T Tauri disks in Taurus. Even with large telescopes, this array will not have the sensitivity to directly track fringes in the mid-infrared for our prime targets and a fringe tracking system will be necessary in the near-infrared. While a heterodyne architecture using modern mid-IR laser comb technology remains a competitive option (especially for the intriguing 24 and 40{\mu}m atmospheric windows), the prioritization of 3-5{\mu}m observations of CO/H2O vibrotational levels by the PFI-Science Working Group (SWG) pushes the TWG to require vacuum pipe beam transport with potentially cooled optics. We present here a preliminary study of simulated L- and N-band PFI observations of a realistic 4-planet disk simulation, finding 21x2.5m PFI can easily detect the accreting protoplanets in both L and N-band but can see non-accreting planets only in L band. (abridged -- see PDF for full abstract)
Abstract
12 pages, 4 Figures, Proceedings of SPIE 2016Abstract
International audienceAdditional details
Identifiers
- URL
- https://hal.archives-ouvertes.fr/hal-03539985
- URN
- urn:oai:HAL:hal-03539985v1
Origin repository
- Origin repository
- UNICA