Sufficient targets per pointing to realize adequate multiplexing
Relative to the sky density of interesting sources to deliver Telescope is available - i.e., one with large enough aperture toīe in a compelling diffraction-limited resolution regime, but with large enough FOV Obvious relevant requirements are that (1) an appropriate For the present discussion, we only briefly Speckle imaging using CFBs requires contemplation ofĪ number of practical considerations and potential design trade-offs Obviously, the proposition of multiplexed To our knowledge, use of CFBs in speckle imaging has notīeen previously explored. However, it is impractical and costly to attain this by paving telescope focal planes with fast readout detectors. TESS and Plato missions are poised to deliver of order 10 5 detections of exoplanet mass companions alone.Ĭlearly, the sheer number of interesting follow-up targets being produced by these surveys makes the task of wholesale high resolution imaging characterization much less practical with single-object instruments like the Differential Speckle Survey Instrument (DSSI), NN-EXPLORE Exoplanet Stellar Speckle Imager (NESSI), and Robo-AO. Have identified thousands of potential companions to nearby stars spanning the mass range from exo-Earths to equal-mass binaries, However, while the Kepler and K2 missions Multi-star systems the influence of long period companions onĮxoplanet host system architectures and dependencies of theseĪrchitectures on local environmental conditions. Providing a vast, and well-vetted database to address questions suchĪs: the frequency and stability of planet, stellar binary, and
Imaging of large numbers of systems in all evolutionary phases acrossĭiffraction-limited imaging can identify false positive exoplanetĭetections, as well as hierarchical star/planet systems, thereby Simultaneous speckle imaging over large field of views (FOVs) is desirable.įor example, understanding the wide variety of star and planet formation architectures being found by both transit and radial velocity surveys requires high resolution
On the other hand, there is a growing need for largescale, systematicĭiffraction-limited surveys of targets of sufficiently high sky density that developing techniques for Resolved with this fiber-fed speckle system and compared toīoth literature results and traditional speckle imaging taken with the same camera directly, with no intervening CFB. Results are presented of DL speckle imaging of well-known close (including subarcsecond) binary stars We have for the first time successfully demonstratedīoth optical and NIR detectors. Using this device on University of Virginia’s Fan Mountain Observatory 40-inch telescope We discuss various design considerations for coherent fiber speckle imaging with an eye toward a multiplexed system using numerous configurable CFBs, and we test its viability with a prototype instrument that uses a single CFB to transport speckle images from the telescope focal plane to a traditionally designed, fast readout speckle camera. However, for imaging we require the use of coherent fiber bundles (CFBs). To attain this by covering the entire focal plane with fast readout detectors.Īn alternative approach is to connect a relatively small number of detector pixels to multiple interesting targets spanning a large FOV through the use of optical fibers, a technique employed in spectroscopy for decades. The need for large DL surveys of targets with high sky density motivates a desire for simultaneous speckle imaging over large FOVs, however it is currently impractical The traditional observing method for speckle has been to observe a single, unresolved, source per telescope pointing over a relatively small field of view (FOV). Speckle imaging is a well known method to achieve diffraction-limited (DL) imaging from ground-based telescopes.
0 kommentar(er)
