Search

Your search keyword '"Wishnow, Ed"' showing total 26 results
Start Over Author "Wishnow, Ed"

Refine your results

more »

more »
26 results on '"Wishnow, Ed"'

1. The Planet Formation Imager

Author

Monnier, John D., Kraus, Stefan, Ireland, Michael J., Baron, Fabien, Bayo, Amelia, Berger, Jean-Philippe, Creech-Eakman, Michelle, Dong, Ruobing, Duchene, Gaspard, Espaillat, Catherine, Haniff, Chris, Honig, Sebastian, Isella, Andrea, Juhasz, Attila, Labadie, Lucas, Lacour, Sylvestre, Leifer, Stephanie, Merand, Antoine, Michael, Ernest, Minardi, Stefano, Mordasini, Christoph, Mozurkewich, David, Olofsson, Johan, Paladini, Claudia, Petrov, Romain, Pott, Jorg-Uwe, Ridgway, Stephen, Rinehart, Stephen, Stassun, Keivan, Surdej, Jean, Brummelaar, Theo ten, Turner, Neal, Tuthill, Peter, Vahala, Kerry, van Belle, Gerard, Vasisht, Gautam, Wishnow, Ed, Young, John, and Zhu, Zhaohuan

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Planet Formation Imager (PFI, www.planetformationimager.org) is a next-generation infrared interferometer array with the primary goal of imaging the active phases of planet formation in nearby star forming regions. PFI will be sensitive to warm dust emission using mid-infrared capabilities made possible by precise fringe tracking in the near-infrared. An L/M band combiner will be especially sensitive to thermal emission from young exoplanets (and their disks) with a high spectral resolution mode to probe the kinematics of CO and H2O gas. In this paper, we give an overview of the main science goals of PFI, define a baseline PFI architecture that can achieve those goals, point at remaining technical challenges, and suggest activities today that will help make the Planet Formation Imager facility a reality., Comment: Published in Experimental Astronomy as part of topical collection "Future of Optical-infrared Interferometry in Europe"

Published
2018
Full Text
View/download PDF

2. Architecture design study and technology roadmap for the Planet Formation Imager (PFI)

Author

Monnier, John D., Ireland, Michael J., Kraus, Stefan, Baron, Fabien, Creech-Eakman, Michelle, Dong, Ruobing, Isella, Andrea, Merand, Antoine, Michael, Ernest, Minardi, Stefano, Mozurkewich, David, Petrov, Romain, Rinehard, Stephen, Brummelaar, Theo ten, Vasisht, Gautum, Wishnow, Ed, Young, John, and Zhu, Zhaohuan

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

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), Comment: 12 pages, 4 Figures, Proceedings of SPIE 2016

Published
2016
Full Text
View/download PDF

3. Quantifying Stellar Mass Loss with High Angular Resolution Imaging

Author

Ridgway, Stephen, Aufdenberg, Jason, Creech-Eakman, Michelle, Elias, Nicholas, Howell, Steve, Hutter, Don, Karovska, Margarita, Ragland, Sam, Wishnow, Ed, and Zhao, Ming

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Mass is constantly being recycled in the universe. One of the most powerful recycling paths is via stellar mass-loss. All stars exhibit mass loss with rates ranging from ~10(-14) to 10(-4) M(sun) yr-1, depending on spectral type, luminosity class, rotation rate, companion proximity, and evolutionary stage. The first generation of stars consisted mostly of hydrogen and helium. These shed material - via massive winds, planetary nebulae and supernova explosions - seeding the interstellar medium with heavier elements. Subsequent generations of stars incorporated this material, changing how stars burn and providing material for planet formation. An understanding of mass loss is critical for modeling individual stars as well as answering larger astrophysical questions. Understanding mass loss is essential for following the evolution of single stars, binaries, star clusters, and galaxies. Mass loss is one of our weakest areas in the modeling of fundamental stellar processes. In large part this is owing to lack of confrontation with detailed observations of stellar photospheres and the mass-loss process. High resolution optical imagery with telescope arrays is beginning to provide these data and, combined with spectroscopy and broad infrared and sub-mm coverage, supporting more sophisticated models on fast computers and promising a new era in mass-loss studies., Comment: Science white paper prepared for Astro2010

Published
2009

4. TEDI: the TripleSpec Exoplanet Discovery Instrument

Author

Edelstein, Jerry, Muterspaugh, Matthew Ward, Erskine, David J., Feuerstein, W. Michael, Marckwordt, Mario, Wishnow, Ed, Lloyd, James P., Herter, Terry, Muirhead, Phillip, Gull, George E., Henderson, Charles, and Parshley, Stephen C.

Subjects
Astrophysics
Abstract

The TEDI (TripleSpec - Exoplanet Discovery Instrument) will be the first instrument fielded specifically for finding low-mass stellar companions. The instrument is a near infra-red interferometric spectrometer used as a radial velocimeter. TEDI joins Externally Dispersed Interferometery (EDI) with an efficient, medium-resolution, near IR (0.9 - 2.4 micron) echelle spectrometer, TripleSpec, at the Palomar 200" telescope. We describe the instrument and its radial velocimetry demonstration program to observe cool stars., Comment: 6 Pages, To Appear in SPIE Volume 6693, Techniques and Instrumentation for Detection of Exoplanets III

Published
2007
Full Text
View/download PDF

13. Architectures and Technologies for a Space Telescope for Solar System Science

Author

Sayanagi, Kunio, primary, Young, Cindy L., additional, Bowman, Lynn M., additional, Pitman, Joe, additional, Naasz, Bo J., additional, Meinke, Bonnie, additional, Becker, Tracy, additional, Bell, Jim, additional, Cartwright, Richard, additional, Chanover, Nancy, additional, Clarke, John T., additional, Colwell, Joshua, additional, Curry, Shannon, additional, Pater, Imke de, additional, Delory, Greg, additional, Feaga, Lori, additional, Fletcher, Leigh, additional, Greathouse, Thomas, additional, Hendrix, Amanda, additional, Holler, Bryan, additional, Holsclaw, Greg, additional, Jessup, Kandi, additional, Kelley, Michael, additional, Lillis, Robert, additional, Lopes, Rosaly M., additional, Luhmann, Janet, additional, MacDonnell, David G., additional, Marchis, Franck L., additional, McGrath, Melissa, additional, Milam, Stefanie N., additional, Peralta, Javier, additional, Poston, Michael J., additional, Retherford, Kurt, additional, Schneider, Nick, additional, Siegmund, Oswald, additional, Spencer, John, additional, Jr., Ronald Vervack,, additional, Vilas, Faith, additional, Wishnow, Ed, additional, and Wong, Mike, additional

Published
2021
Full Text
View/download PDF

14. Searches for Technosignatures: The State of the Profession

Author

Wright, Jason, Allen, Veronica, Alvarado-Gómez, Julián D., Angerhausen, Daniel, Apai, Daniel, Atri, Dimitra, Balbi, Amedeo, Barclay, Thomas, Barentsen, Geert, Beasley, Tony, Beatty, Thomas, Behmard, Aida, Berea, Anamaria, Boyajian, Tabetha, Bridge, Joanna S., Bryson, Steve, Bytof, Jeff, Cleaves, Henderson, Colon, Knicole, Cordes, James, Cowing, Keith, Curtis, Jason, Davenport, James, Davies, Paul, DeMarines, Julia, Denning, Kathryn, Dick, Steven, Dong, Chuanfei, Dutil, Yvan, Edmonds, Peter, Enriquez, Emilio, Eubanks, Marshall, Fernandez, Yan, Frank, Adam, De la Torre, Gabriel G., Gajjar, Vishal, Garrett, Michael, Gelino, Dawn, Geller, Harold, Giles, Daniel, Gillum, Eliot, Gomez, Jose L., Graham, R. J., Grimaldi, Claudio, Grinspoon, David, Haqq-Misra, Jacob, Hellbourg, Greg, Helman, Daniel, Horowitz, Paul, Howard, Andrew, Isaacson, Howard, Jackson, Albert, Jia, Tony Z., Kainu, Morgan, Kanodia, Shubham, Kawaler, Steven, Kendall, Shana, Khan, Afshin, Kipping, David, Kite, Edwin, Knuth, Kevin H., Kopparapu, Ravi, Korpela, Eric, Laine, Pauli, Lau, Graham, Lesyna, Larry, Loureiro, Rafael, MacDonald, Mariah, Margot, Jean-Luc, Mendez, Abel, Mishra, Amit, Morrison, Ian, Mullally, Susan, Mullan, Brendan, Nita, Gelu, O'Neil, Karen, Pass, Jim, Paulino-Lima, Ivan Glaucio, Piotelat, Elisabeth, Pope, Benjamin, Raymond, Sean N., Ricker, George, Riley, Crystal S., Robertson, Paul, Rocha, Graça, Rodriguez, Joseph, Rosenthal, Lee, Roy, Arpita, Rybarczyk, Daniel, de Souza, Rafael S., Sallmen, Shauna, Santander, Marcos, Scharf, Caleb, Schwieterman, Edward, Seiler, Douglas, Shabram, Megan, Sheikh, Sofia, Shostak, Seth, Shrestha, Pradipta, Siemion, Andrew, Sigurdsson, Steinn, Sneed, Evan, Socas-Navarro, Hector, Soderblom, David, Solmaz, Arif, Subramaniam, Sadasivan, Suresh, Akshay, Tan, Joshua, Tanner, Angelle, Tarter, Jill, Taylor, Stuart F., Terrien, Ryan, Turner, Jake D., Vakoch, Douglas, Villa, Ciro, Walkowicz, Lucianne, Wang, Sharon Xuesong, Weiss, Lauren, Werthimer, Dan, Williams, David, Winn, Joshua, Wishnow, Ed, Worden, Simon (Pete), Wright, Shelley, Zackrisson, Erik, Zanis, Michael, Zarka, Philippe, Center for Space and Habitability (CSH), University of Bern, Space Telescope Science Institute (STSci), NYUAD Center for Space Science, New York University [Abu Dhabi], NYU System (NYU)-NYU System (NYU), Dipartimento di Fisica, Università di Roma 'Tor Vergata', Università degli Studi di Roma Tor Vergata [Roma], NASA Ames Research Center Cooperative for Research in Earth Science in Technology (ARC-CREST), NASA Ames Research Center (ARC), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Department of Computer Science [Bath], University of Bath [Bath], Denver Museum of Nature and Science, Princeton University, Department of Physics and Astronomy [Rochester], University of Rochester [USA], Safran Aircraft Engines, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley], University of California-University of California, Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Space Sciences Laboratory [Berkeley] (SSL), Department of Biological Sciences (DBS), Central Campus, University of Essex, Laboratoire d'Informatique pour la Mécanique et les Sciences de l'Ingénieur (LIMSI), Université Paris Saclay (COmUE)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université - UFR d'Ingénierie (UFR 919), Sorbonne Université (SU)-Sorbonne Université (SU)-Université Paris-Saclay-Université Paris-Sud - Paris 11 (UP11), ECLIPSE 2019, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), Department of Astronomy [Berkeley], SETI Institute, Université de Montréal (UdeM), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; The small size of the SETI workforce is a major problem for NASA and the search for life elsewhere in the universe. The Astro2020 Decadal should address this issue by making nurturing the field an explicit priority for the next decade.

Published
2019

16. The planet formation imager

Author

Monnier, John D., primary, Kraus, Stefan, additional, Ireland, Michael J., additional, Baron, Fabien, additional, Bayo, Amelia, additional, Berger, Jean-Philippe, additional, Creech-Eakman, Michelle, additional, Dong, Ruobing, additional, Duchêne, Gaspard, additional, Espaillat, Catherine, additional, Haniff, Chris, additional, Hönig, Sebastian, additional, Isella, Andrea, additional, Juhasz, Attila, additional, Labadie, Lucas, additional, Lacour, Sylvestre, additional, Leifer, Stephanie, additional, Merand, Antoine, additional, Michael, Ernest, additional, Minardi, Stefano, additional, Mordasini, Christoph, additional, Mozurkewich, David, additional, Olofsson, Johan, additional, Paladini, Claudia, additional, Petrov, Romain, additional, Pott, Jörg-Uwe, additional, Ridgway, Stephen, additional, Rinehart, Stephen, additional, Stassun, Keivan, additional, Surdej, Jean, additional, Brummelaar, Theo ten, additional, Turner, Neal, additional, Tuthill, Peter, additional, Vahala, Kerry, additional, van Belle, Gerard, additional, Vasisht, Gautam, additional, Wishnow, Ed, additional, Young, John, additional, and Zhu, Zhaohuan, additional

Published
2018
Full Text
View/download PDF

17. The planet formation imager

Author

Monnier, John J.D., Kraus, Stefan, Ireland, Michael M.J., Baron, Fabien, Bayo, Amelia, Berger, Jean-Philippe, Creech-Eakman, Michelle, Dong, Ruobing, Duchêne, Gaspard, Espaillat, Catherine, Haniff, Chris, Hönig, Sebastian S.F., Isella, Andrea, Juhasz, Attila, Labadie, Lucas, Lacour, Sylvestre, Leifer, Stephanie, Mérand, Antoine, Michael, Ernest, Minardi, Stefano, Mordasini, Christoph, Mozurkewich, David, Olofsson, Johan, Paladini, Claudia, Petrov, Romain, Pott, Jörg Uwe, Ridgway, Stephen, Rinehart, Stephen, Stassun, Keivan, Surdej, Jean, Brummelaar, Theo A Ten, Turner, Neal, Tuthill, Peter P.G., Vahala, Kerry, Van Belle, Gerard G.T., Vasisht, Gautam, Wishnow, Ed, Young, John, Zhu, Zhaohuan, Monnier, John J.D., Kraus, Stefan, Ireland, Michael M.J., Baron, Fabien, Bayo, Amelia, Berger, Jean-Philippe, Creech-Eakman, Michelle, Dong, Ruobing, Duchêne, Gaspard, Espaillat, Catherine, Haniff, Chris, Hönig, Sebastian S.F., Isella, Andrea, Juhasz, Attila, Labadie, Lucas, Lacour, Sylvestre, Leifer, Stephanie, Mérand, Antoine, Michael, Ernest, Minardi, Stefano, Mordasini, Christoph, Mozurkewich, David, Olofsson, Johan, Paladini, Claudia, Petrov, Romain, Pott, Jörg Uwe, Ridgway, Stephen, Rinehart, Stephen, Stassun, Keivan, Surdej, Jean, Brummelaar, Theo A Ten, Turner, Neal, Tuthill, Peter P.G., Vahala, Kerry, Van Belle, Gerard G.T., Vasisht, Gautam, Wishnow, Ed, Young, John, and Zhu, Zhaohuan

Abstract

The Planet Formation Imager (PFI, www.planetformationimager.org) is a next-generation infrared interferometer array with the primary goal of imaging the active phases of planet formation in nearby star forming regions. PFI will be sensitive to warm dust emission using mid-infrared capabilities made possible by precise fringe tracking in the near-infrared. An L/M band combiner will be especially sensitive to thermal emission from young exoplanets (and their disks) with a high spectral resolution mode to probe the kinematics of CO and H2O gas. In this paper, we give an overview of the main science goals of PFI, define a baseline PFI architecture that can achieve those goals, point at remaining technical challenges, and suggest activities today that will help make the Planet Formation Imager facility a reality., SCOPUS: ar.j, DecretOANoAutActif, info:eu-repo/semantics/published

Published
2018

19. Architecture design study and technology road map for the Planet Formation Imager (PFI)

Author

Monnier, John D., additional, Ireland, Michael J., additional, Kraus, Stefan, additional, Baron, Fabien, additional, Creech-Eakman, Michelle, additional, Dong, Ruobing, additional, Isella, Andrea, additional, Merand, Antoine, additional, Michael, Ernest, additional, Minardi, Stefano, additional, Mozurkewich, David, additional, Petrov, Romain, additional, Rinehart, Stephen, additional, ten Brummelaar, Theo, additional, Vasisht, Gautam, additional, Wishnow, Ed, additional, Young, John, additional, and Zhu, Zhaohuan, additional

Published
2016
Full Text
View/download PDF

20. The many faces of Betelgeuse

Author

Ravi, Vikram, Wishnow, Ed, Lockwood, Sean, Townes, Charles, and Johns-Krull, Christopher

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The dynamics of the surface and inner atmosphere of the red supergiant star Betelgeuse are the subject of numerous high angular resolution and spectroscopic studies. Here, we present three-telescope interferometric data obtained at 11.15 μm wavelength with the Berkeley Infrared Spatial Interferometer (ISI), that probe the stellar surface continuum. We find striking variability in the size, effective temperature, and degree of asymmetry of the star over the years 2006–2009. These results may indicate an evolving shell of optically thick material close to the stellar photosphere.

Published
2012

21. Quantifying Stellar Mass Loss with High Angular Resolution Imaging

Author

NATIONAL OPTICAL ASTRONOMY OBSERVATORIES TUCSON AZ, Ridgeway, Stephen, Aufdenberg, Jason, Creech-Eakman, Michelle, Elias, Nicholas, Howell, Steve, Hutter, Don, Karovska, Margarita, Ragland, San, Wishnow, Ed, Zhao, Ming, NATIONAL OPTICAL ASTRONOMY OBSERVATORIES TUCSON AZ, Ridgeway, Stephen, Aufdenberg, Jason, Creech-Eakman, Michelle, Elias, Nicholas, Howell, Steve, Hutter, Don, Karovska, Margarita, Ragland, San, Wishnow, Ed, and Zhao, Ming

Abstract

Mass is constantly being recycled in the universe. One of the most powerful recycling paths is via stellar mass-loss. All stars exhibit mass loss with rates ranging from approximately 10(-14) to 10(-4) solar mass yr(-1), depending on spectral type, luminosity class, rotation rate, companion proximity, and evolutionary stage. The first generation of stars consisted mostly of hydrogen and helium. These shed material - via massive winds, planetary nebulae and supernova explosions - seeding the interstellar medium with heavier elements. Subsequent generations of stars incorporated this material, changing how stars burn and providing material for planet formation. An understanding of mass loss is critical for modeling individual stars as well as answering larger astrophysical questions. Understanding mass loss is essential for following the evolution of single stars, binaries, star clusters, and galaxies. Mass loss is one of our weakest areas in the modeling of fundamental stellar processes. In large part this is owing to lack of confrontation with detailed observations of stellar photospheres and the mass-loss process. High resolution optical imagery with telescope arrays is beginning to provide these data and, combined with spectroscopy and broad infrared and sub-mm coverage, supporting more sophisticated models on fast computers and promising a new era in mass-loss studies., Science white paper prepared for Astro2010. Prepared in collaboration with Embry-Riddle Aeronautical Univ., New Mexico Tech, Univ. of Heidelberg, US Naval Observatory, Harvard-Smithsonian CfA, Keck Observatory, Univ. of California Berkeley, and Univ. of Michigan. The original document contains color images. All DTIC reproductions will be in black and white.

Published
2009

22. Precision Radial Velocities in the Near Infrared with TEDI

Author

Lloyd, James P., primary, Czeszumska, Agnieszka, additional, Edelstein, Jerry, additional, Erskine, David, additional, Feuerstein, Michael, additional, Halverson, Sam, additional, Marckwordt, Mario, additional, Mercer, Tony, additional, Muirhead, Philip, additional, Schwehr, Jackie, additional, Muterspaugh, Matthew, additional, Wishnow, Ed, additional, and Wright, Jason, additional

Published
2008
Full Text
View/download PDF

23. TEDI: the TripleSpec Exoplanet Discovery Instrument

Author

Edelstein, Jerry, primary, Muterspaugh, Matthew Ward, additional, Erskine, David J., additional, Feuerstein, W. Michael, additional, Marckwordt, Mario, additional, Wishnow, Ed, additional, Lloyd, James P., additional, Herter, Terry, additional, Muirhead, Phillip, additional, Gull, George E., additional, Henderson, Charles, additional, and Parshley, Stephen C., additional

Published
2007
Full Text
View/download PDF

24. Architecture design study and technology road map for the Planet Formation Imager (PFI)

Author

Malbet, Fabien, Creech-Eakman, Michelle J., Tuthill, Peter G., Monnier, John D., Ireland, Michael J., 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, and Zhu, Zhaohuan

Published
2016
Full Text
View/download PDF

25. The planet formation imager

Author

Monnier, John D., Kraus, Stefan, Ireland, Michael J., Baron, Fabien, Bayo, Amelia, Berger, Jean-Philippe, Creech-Eakman, Michelle, Dong, Ruobing, Duchêne, Gaspard, Espaillat, Catherine, Haniff, Chris, Hönig, Sebastian, Isella, Andrea, Juhasz, Attila, Labadie, Lucas, Lacour, Sylvestre, Leifer, Stephanie, Merand, Antoine, Michael, Ernest, Minardi, Stefano, Mordasini, Christoph, Mozurkewich, David, Olofsson, Johan, Paladini, Claudia, Petrov, Romain, Pott, Jörg-Uwe, Ridgway, Stephen, Rinehart, Stephen, Stassun, Keivan, Surdej, Jean, Brummelaar, Theo Ten, Turner, Neal, Tuthill, Peter, Vahala, Kerry, Van Belle, Gerard, Vasisht, Gautam, Wishnow, Ed, Young, John, and Zhu, Zhaohuan

Subjects
13. Climate action, 530 Physics, 520 Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 500 Science, 620 Engineering, 7. Clean energy, Astrophysics::Galaxy Astrophysics
Abstract

The Planet Formation Imager (PFI, www.planetformationimager.org) is a next-generation infrared interferometer array with the primary goal of imaging the active phases of planet formation in nearby star forming regions. PFI will be sensitive to warm dust emission using mid-infrared capabilities made possible by precise fringe tracking in the near-infrared. An L/M band combiner will be especially sensitive to thermal emission from young exoplanets (and their disks) with a high spectral resolution mode to probe the kinematics of CO and H2O gas. In this paper, we give an overview of the main science goals of PFI, define a baseline PFI architecture that can achieve those goals, point at remaining technical challenges, and suggest activities today that will help make the Planet Formation Imager facility a reality.

Catalog

Books, media, physical & digital resources
See catalog results