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276 results on '"Beichman, Charles"'

1. Methane emission from a cool brown dwarf

Author

Faherty, Jacqueline K., Burningham, Ben, Gagné, Jonathan, Suárez, Genaro, Vos, Johanna M., Alejandro Merchan, Sherelyn, Morley, Caroline V., Rowland, Melanie, Lacy, Brianna, Kiman, Rocio, Caselden, Dan, Kirkpatrick, J. Davy, Meisner, Aaron, Schneider, Adam C., Kuchner, Marc Jason, Bardalez Gagliuffi, Daniella Carolina, Beichman, Charles, Eisenhardt, Peter, Gelino, Christopher R., Gharib-Nezhad, Ehsan, Gonzales, Eileen, Marocco, Federico, Rothermich, Austin James, and Whiteford, Niall

Published
2024
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3. Evidence for the volatile-rich composition of a 1.5-Earth-radius planet

Author

Piaulet, Caroline, Benneke, Björn, Almenara, Jose M., Dragomir, Diana, Knutson, Heather A., Thorngren, Daniel, Peterson, Merrin S., Crossfield, Ian J. M., M.-R. Kempton, Eliza, Kubyshkina, Daria, Howard, Andrew W., Angus, Ruth, Isaacson, Howard, Weiss, Lauren M., Beichman, Charles A., Fortney, Jonathan J., Fossati, Luca, Lammer, Helmut, McCullough, P. R., Morley, Caroline V., and Wong, Ian

Published
2023
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4. Searching for Planets Orbiting α Cen A with the James Webb Space Telescope

Author

Beichman, Charles, Ygouf, Marie, Sayson, Jorge Llop, Mawet, Dimitri, Yung, Yuk, Choquet, Elodie, Kervella, Pierre, Boccaletti, Anthony, Belikov, Ruslan, Lissauer, Jack J., Quarles, Billy, Lagage, Pierre-Olivier, Dicken, Daniel, Hu, Renyu, Mennesson, Bertrand, Ressler, Mike, Serabyn, Eugene, Krist, John, Bendek, Eduardo, Leisenring, Jarron, and Pueyo, Laurent

Published
2020

5. An ultrahot Neptune in the Neptune desert

Author

Jenkins, James S., Díaz, Matías R., Kurtovic, Nicolás T., Espinoza, Néstor, Vines, Jose I., Rojas, Pablo A. Peña, Brahm, Rafael, Torres, Pascal, Cortés-Zuleta, Pía, Soto, Maritza G., Lopez, Eric D., King, George W., Wheatley, Peter J., Winn, Joshua N., Ciardi, David R., Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Jenkins, Jon M., Beichman, Charles A., Bieryla, Allyson, Burke, Christopher J., Christiansen, Jessie L., Henze, Christopher E., Klaus, Todd C., McCauliff, Sean, Mori, Mayuko, Narita, Norio, Nishiumi, Taku, Tamura, Motohide, de Leon, Jerome Pitogo, Quinn, Samuel N., Villaseñor, Jesus Noel, Vezie, Michael, Lissauer, Jack J., Collins, Karen A., Collins, Kevin I., Isopi, Giovanni, Mallia, Franco, Ercolino, Andrea, Petrovich, Cristobal, Jordán, Andrés, Acton, Jack S., Armstrong, David J., Bayliss, Daniel, Bouchy, François, Belardi, Claudia, Bryant, Edward M., Burleigh, Matthew R., Cabrera, Juan, Casewell, Sarah L., Chaushev, Alexander, Cooke, Benjamin F., Eigmüller, Philipp, Erikson, Anders, Foxell, Emma, Gänsicke, Boris T., Gill, Samuel, Gillen, Edward, Günther, Maximilian N., Goad, Michael R., Hooton, Matthew J., Jackman, James A. G., Louden, Tom, McCormac, James, Moyano, Maximiliano, Nielsen, Louise D., Pollacco, Don, Queloz, Didier, Rauer, Heike, Raynard, Liam, Smith, Alexis M. S., Tilbrook, Rosanna H., Titz-Weider, Ruth, Turner, Oliver, Udry, Stéphane, Walker, Simon. R., Watson, Christopher A., West, Richard G., Palle, Enric, Ziegler, Carl, Law, Nicholas, and Mann, Andrew W.

Published
2020
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6. OGLE-2015-BLG-0845L: a low-mass M dwarf from the microlensing parallax and xallarap effects.

Author

(胡哲程), Zhecheng Hu, (祝伟), Wei Zhu, Gould, Andrew, Udalski, Andrzej, Sumi, Takahiro, (陈平), Ping Chen, Calchi Novati, Sebastiano, Yee, Jennifer C, Beichman, Charles A, Bryden, Geoffery, Carey, Sean, Fausnaugh, Michael, Gaudi, B Scott, Henderson, Calen B, Shvartzvald, Yossi, Wibking, Benjamin, Mróz, Przemek, Skowron, Jan, Poleski, Radosław, and Szymański, Michał K

Subjects
GRAVITATIONAL lenses, PARALLAX, MASS measurement, MICROLENSES, DATA analysis
Abstract

We present the analysis of the microlensing event OGLE-2015-BLG-0845, which was affected by both the microlensing parallax and xallarap effects. The former was detected via the simultaneous observations from the ground and Spitzer , and the latter was caused by the orbital motion of the source star in a relatively close binary. The combination of these two effects led to a mass measurement of the lens object, revealing a low-mass (⁠|$0.14 \pm 0.05 \, \mathrm{ M}_{\odot }$|⁠) M dwarf at the bulge distance (⁠|$7.6 \pm 1.0$| kpc). The source binary consists of a late F-type subgiant and a K-type dwarf of |$\sim 1.2$| and |$\sim 0.9 \mathrm{ M}_{\odot }$|⁠ , respectively, and the orbital period is |$70 \pm 10$| d. OGLE-2015-BLG-0845 is the first single-lens event in which the lens mass is measured via the binarity of the source. Given the abundance of binary systems as potential microlensing sources, the xallarap effect may not be a rare phenomenon. Our work thus highlights the application of the xallarap effect in the mass determination of microlenses, and the same method can be used to identify isolated dark lenses. [ABSTRACT FROM AUTHOR]

Published
2024
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11. Data Processing for High-Contrast Imaging with the James Webb Space Telescope

Author

Jewell, Jeffrey B, Greena, Joseph J, Uyama, Taichi, Perrin, Marshall, Pueyoe, Laurent A, Girard, Julien, Meyerd, Michael, De Furio, Matthew, Leisenring, Jarron, Greenbaum, Alexandra, Beichman, Charles, Rocha, Graca, and Ygouf, Marie

Abstract

The James Webb Space Telescope (JWST) will probe circumstellar environments at an unprecedented sensitivity.However, the performance of high-contrast imaging instruments is limited by the residual light from the star at close separations (<2-3”), where the incidence of exoplanets increases rapidly. There is currently no solution to get rid of the residual light down to the photon noise level at those separations, which may prevent some crucial discoveries. JWST’s debut is planned for October 2021 for a baseline mission lifetime of only five years. Thus,it is crucial to find a solution to this problem before its launch. We are further developing and implementing an innovative approach of post-processing built on a Bayesian framework that provides a more robust determination of faint astrophysical structures around a bright source. This approach uses a model of high-contrast imaging instrument that takes advantage of prior information, such as data from wavefront sensing (WFS) operations on JWST, to estimate simultaneously instrumental aberrations and the circumstellar environment. With this approach, our goal is to further improve the contrast gain over the contrast that can be achieved with JWST instruments, starting with NIRCam imaging and coronagraphic imaging. This work will pave the way for the future space-based high-contrast imaging instruments such as the Nancy Grace Roman Space Telescope Coronagraph Instrument (Roman CGI). This technique will be crucial to make the best use of the telemetry data that will be collected during the CGI operations.

Published
2020

20. Transiting Exoplanet Studies and Community Targets for JWST ʼs Early Release Science Program

Author

Stevenson, Kevin B., Lewis, Nikole K., Bean, Jacob L., Beichman, Charles, Fraine, Jonathan, Kilpatrick, Brian M., Krick, J. E., Lothringer, Joshua D., Mandell, Avi M., Valenti, Jeff A., Agol, Eric, Angerhausen, Daniel, Barstow, Joanna K., Birkmann, Stephan M., Burrows, Adam, Charbonneau, David, Cowan, Nicolas B., Crouzet, Nicolas, Cubillos, Patricio E., Curry, S. M., Dalba, Paul A., de Wit, Julien, Deming, Drake, Désert, Jean-Michel, Doyon, René, Dragomir, Diana, Ehrenreich, David, Fortney, Jonathan J., Muñoz, Antonio García, Gibson, Neale P., Gizis, John E., Greene, Thomas P., Harrington, Joseph, Heng, Kevin, Kataria, Tiffany, Kempton, Eliza M.-R., Knutson, Heather, Kreidberg, Laura, Lafrenière, David, Lagage, Pierre-Olivier, Line, Michael R., Lopez-Morales, Mercedes, Madhusudhan, Nikku, Morley, Caroline V., Rocchetto, Marco, Schlawin, Everett, Shkolnik, Evgenya L., Shporer, Avi, Sing, David K., Todorov, Kamen O., Tucker, Gregory S., and Wakeford, Hannah R.

Published
2016

21. Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets

Author

Blunt, Sarah, Carvalho, Adolfo, David, Trevor J., Beichman, Charles, Zink, Jon K., Gaidos, Eric, Behmard, Aida, Bouma, Luke G., Cody, Devin, Dai, Fei, Foreman-Mackey, Daniel, Grunblatt, Sam, Howard, Andrew W., Kosiarek, Molly, Knutson, Heather A., Rubenzahl, Ryan A., Beard, Corey, Chontos, Ashley, Giacalone, Steven, Hirano, Teruyuki, Johnson, Marshall C., Lubin, Jack, Murphy, Joseph M. Akana, Petigura, Erik A, Van Zandt, Judah, and Weiss, Lauren

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

Mass, radius, and age measurements of young (, Comment: 26 pages, 12 figures; published in AJ

Published
2023

22. Probing the Outskirts of M Dwarf Planetary Systems with a JWST Cycle 1 GTO Direct-Imaging Survey of Nearby, Young M Stars

Author

Bogat, Ell, Schlieder, Joshua, Beichman, Charles, Leisenring, Jarron, Meyer, Michael, Ygouf, Marie, Barclay, Tm\om, Bryden, Geoff, Calissendorff, Per, De Furio, Matthew, Groff, Tyler, Lawson, Kellen, McElwain, Michael, Llop-Sayson, Jorge, and Rieke, Marcia

Abstract

The population of giant planets on wide orbits around low-mass M dwarf stars is poorly understood. However, the discovery and characterization of these planets is key to understanding the architectures and evolution of M dwarf planetary systems and places their frequent and potentially habitable inner planets in context. While current ground-based imaging struggles to probe below a Jupiter mass at large separations, the unprecedented sensitivity of JWST NIRCam coronagraphic imaging provides direct access to planets significantly less massive than Jupiter beyond 10 AU around the closest, youngest M dwarfs. In this talk, I will introduce the key aspects of exoplanet direct imaging and present the survey design, observations, and preliminary results of JWST GTO Program 1184, a NIRCam coronagraphic imaging survey of very nearby and young low-mass stars.

Published
2023
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26. The Case for Probe-Class NASA Astrophysics Missions

Author

Elvis, Martin, Arenberg, Jon, Ballantyne, David, Bautz, Mark, Beichman, Charles, Booth, Jeffrey, Buckley, James, Burns, Jack O, Camp, Jordan, Conti, Alberto, Cooray, Asantha, Danchi, William, Delabrouille, Jacques, De Zotti, Gianfranco, Flauger, Raphael, Glenn, Jason, Grindlay, Jonathan, Hanany, Shaul, Hartmann, Dieter, Helou, George, Herranz, Diego, Hubmayr, Johannes, Johnson, Bradley R, Jones, William, Kasdin, N. Jeremy, Kouvoliotou, Chryssa, Kunze, Kerstin E, Lawrence, Charles, Lazio, Joseph, Lipscy, Sarah, Lillie, Charles F, Maccarone, Tom, Madsen, Kristin C, McEnergy, Julie E, Mcentaffer, Randall, Mushotzky, Richard, Olinto, Angela, Plavchan, Peter, Pogosian, Levon, Ptak, Andrew, Ray, Paul, Rocha, Graca M, Scowen, Paul, Seager, Sara, Tinto, Massimo, Tomsick, John, Tucker, Gregory, Ulmer, Mel, Wang, Yun, and Wollack, Edward J

Subjects
Astrophysics
Abstract

Astrophysics spans an enormous range of questions on scales from individual planets to the entire cosmos. To address the richness of 21st century astrophysics requires a corresponding richness of telescopes spanning all bands and all messengers. Much scientific benefit comes from having the multi-wavelength capability available at the same time. Most of these bands, or measurement sensitivities, require space-based missions. Historically, NASA has addressed this need for breadth with a small number of flagship-class missions and a larger number of Explorer missions. While the Explorer program continues to flourish, there is a large gap between Explorers and strategic missions.

Published
2019

27. OGLE-2018-BLG-0022: First Prediction of an Astrometric Microlensing Signal from a Photometric Microlensing Event

Author

Han, Cheongho, Bond, Ian A, Udalski, Andrzej, Gould, Andrew, Bozza, Valerio, Hirao, Yuki, Cas, Arnaud, Albrow, Michael D, Chung, Sun-Ju, Hwang, Kyu-Ha, Lee, Chung-Uk, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C, Jung, Youn Kil, Kim, Doeon, Kim, Woong-Tae, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W, Zang, Weicheng, Abe, Fumio, Barry, Richard, Bennett, David P, Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Itow, Yoshitaka, Kawasaki, Kohei, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Nagakane, Masayuki, Ranc, Clement, Rattenbury, Nicholas J, Suematsu, Haruno, Sullivan, Denis J, Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J, Yonehara, Atsunori, Mroz, Przemek, Szymanski, Michal K, Skowron, Jan, Poleski, Radek, Soszynski, Igor, Pietrukowicz, Pawel, Kozlowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A, Iwanek, Patryk, Wrona, Marcin, Beichman, Charles A, Bryden, Geoffery, Carey, Sean, Gaudi, B. Scott, and Henderson, Calen B

Subjects
Astrophysics
Abstract

In this work, we present the analysis of the binary microlensing event OGLE-2018-BLG-0022 that is detected toward the Galactic bulge field. The dense and continuous coverage with the high-quality photometry data from ground-based observations combined with the space-based Spitzer observations of this long timescale event enables us to uniquely determine the masses M1=0.40 ± 0.05Me and M2=0.13 ± 0.01Me of the individual lens components. Because the lens-source relative parallax and the vector lens-source relative proper motion are unambiguously determined, we can likewise unambiguously predict the astrometric offset between the light centroid of the magnified images (as observed by the Gaia satellite) and the true position of the source. This prediction can be tested when the individual-epoch Gaia astrometric measurements are released.

Published
2019
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28. Author Correction: An ultrahot Neptune in the Neptune desert

Author

Jenkins, James S., Díaz, Matías R., Kurtovic, Nicolás T., Espinoza, Néstor, Vines, Jose I., Rojas, Pablo A. Peña, Brahm, Rafael, Torres, Pascal, Cortés-Zuleta, Pía, Soto, Maritza G., Lopez, Eric D., King, George W., Wheatley, Peter J., Winn, Joshua N., Ciardi, David R., Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Jenkins, Jon M., Beichman, Charles A., Bieryla, Allyson, Burke, Christopher J., Christiansen, Jessie L., Henze, Christopher E., Klaus, Todd C., McCauliff, Sean, Mori, Mayuko, Narita, Norio, Nishiumi, Taku, Tamura, Motohide, de Leon, Jerome Pitogo, Quinn, Samuel N., Villaseñor, Jesus Noel, Vezie, Michael, Lissauer, Jack J., Collins, Karen A., Collins, Kevin I., Isopi, Giovanni, Mallia, Franco, Ercolino, Andrea, Petrovich, Cristobal, Jordán, Andrés, Acton, Jack S., Armstrong, David J., Bayliss, Daniel, Bouchy, François, Belardi, Claudia, Bryant, Edward M., Burleigh, Matthew R., Cabrera, Juan, Casewell, Sarah L., Chaushev, Alexander, Cooke, Benjamin F., Eigmüller, Philipp, Erikson, Anders, Foxell, Emma, Gänsicke, Boris T., Gill, Samuel, Gillen, Edward, Günther, Maximilian N., Goad, Michael R., Hooton, Matthew J., Jackman, James A. G., Louden, Tom, McCormac, James, Moyano, Maximiliano, Nielsen, Louise D., Pollacco, Don, Queloz, Didier, Rauer, Heike, Raynard, Liam, Smith, Alexis M. S., Tilbrook, Rosanna H., Titz-Weider, Ruth, Turner, Oliver, Udry, Stéphane, Walker, Simon. R., Watson, Christopher A., West, Richard G., Palle, Enric, Ziegler, Carl, Law, Nicholas, and Mann, Andrew W.

Published
2020
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29. Mid-infrared fine structure lines from the Galactic Warm Ionized Medium

Author

Kulkarni, S. R., Beichman, Charles, and Ressler, Michael E.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

Galaxy and occupies perhaps a quarter of the volume of the Galactic disk. Decoding the spectrum of the Galactic diffuse ionizing field is of fundamental interest. This can be done via direct measurements of ionization fractions of various elements. Based on current physical models for the WIM we predicted that mid-IR fine structure lines of Ne, Ar and S would be within the grasp of the Mid-Infrared Imager-Medium Resolution Spectrometer (MIRI-MRS), an Integral Field Unit (IFU) spectrograph, aboard the James Webb Space Telescope (JWST). Motivated thus we analyzed a pair of commissioning data sets and detected [NeII] 12.81 $\mu$m, [SIII] 18.71 $\mu$m and possibly [SIV] 10.51 $\mu$m. The inferred emission measure for these detections is about 10 ${\rm cm^{-6} pc}$, typical of the WIM. These detections are broadly consistent with expectations of physical models for the WIM. The current detections are limited by uncorrected fringing (and to a lesser extent by baseline variations). In due course, we expect, as with other IFUs, the calibration pipeline to deliver photon-noise-limited spectra. The detections reported here bode well for the study of the WIM. Along most lines-of-sight hour-long MIRI-MRS observations should detect line emission from the WIM. When combined with optical observations by modern IFUs with high spectral resolution on large ground-based telescopes, the ionization fraction and temperature of neon and sulfur can be robustly inferred. Separately, the ionization of helium in the WIM can be probed by NIRspec. Finally, joint JWST and optical IFU studies will open up a new cottage industry of studying the WIM on arcsecond scales., Comment: 17 pages, 15 Figures, 8 Tables

Published
2023

30. Keck/OSIRIS Paβ high-contrast imaging of the PDS 70 planetary system

Author

Uyama, Taichi, Xie, Chen, Aoyama, Yuhiko, Beichman, Charles, Hashimoto, Jun, Dong, Ruobing, Hasegawa, Yasuhiro, Ikoma, Masahiro, Mawet, Dimitri, Mcelwain, Michael, Ruffio, Jean-Baptiste, Wagner, Kevin, Wang, Jason, Zhou, Yifan, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

International audience; We present a high-contrast imaging search for Paβ line emission from protoplanets in the PDS 70 system with Keck/OSIRIS integral field spectroscopy. We applied the high-resolution spectral differential imaging technique to the OSIRIS J-band data but did not detect the Paβ line at the level predicted using the parameters of Hashimoto et al. (2020). This lack of Paβ emission suggests the VLT/MUSE-based study may have overestimated the line width of Hα. We compared our Paβ detection limits with the previous Hα flux and Hβ limits and estimated AV to be~0.9 and 2.0 for PDS 70 b and c respectively. In particular, PDS 70 b's AV is much smaller than implied by high-contrast near-infrared studies, which suggests the infrared-continuum photosphere and the hydrogen-emitting regions exist at different heights above the forming planet.

Published
2023

31. 2023 Astrophotonics Roadmap: pathways to realizing multi-functional integrated astrophotonic instruments

Author

Jovanovic, Nemanja, Gatkine, Pradip, Bourdarot, Guillaume, Bradford, Charles M., Broeke, Ronald, Bryant, Julia, Bundy, Kevin, Cheriton, Ross, Cvetojevic, Nick, Diab, Momen, Diddams, Scott A., Dinkelaker, Aline N., Anugu, Narsireddy, Duis, Jeroen, Eikenberry, Stephen, Ellis, Simon, Endo, Akira, Figer, Donald F., Fitzgerald, Michael, Gris-Sanchez, Itandehui, Gross, Simon, Grossard, Ludovic, Guyon, Olivier, Amezcua-Correa, Rodrigo, Haffert, Sebastiaan Y., Halverson, Samuel, Harris, Robert J., He, Jinping, Herr, Tobias, Hottinger, Philipp, Huby, Elsa, Ireland, Michael, Jenson-Clem, Rebecca, Jewell, Jeffrey, Basu Thakur, Ritoban, Jocou, Laurent, Kraus, Stefan, Labadie, Lucas, Lacour, Sylvestre, Laugier, Romain, Ławniczuk, Katarzyna, Lin, Jonathan, Leifer, Stephanie, Leon-Saval, Sergio, Martin, Guillermo, Beichman, Charles, Martinache, Frantz, Martinod, Marc-Antoine, Mazin, Ben, Minardi, Stefano, Monnier, John D, Moreira, Reinan, Mourard, Denis, Nayak, Abani Shankar Shankar, Norris, Barnaby, Obrzud, Ewelina, Bender, Chad, Perraut, Karine, Reynaud, François, Sallum, Steph, Schiminovich, David, Schwab, Christian, Serbayn, Eugene, Soliman, Sherif, Stoll, Andreas, Tang, Liang, Tuthill, Peter, Berger, Jean-Philippe, Vahala, Kerry, Vasisht, Gautam, Veilleux, Sylvain, Walter, Alexander B., Wollack, Edward J, Xin, Yinzi, Yang, Zongyin, Yerolatsitis, Stephanos, Zhang, Yang, Zou, Chang-Ling, Bigioli, Azzurra, and Bland-Hawthorn, Joss

Subjects
ddc:530
Abstract

Photonic technologies offer numerous functionalities that can be used to realize astrophotonic instruments. The most spectacular example to date is the ESO Gravity instrument at the Very Large Telescope in Chile that combines the light-gathering power of four 8-m telescopes through a complex photonic interferometer. Fully integrated astrophotonic devices offer critical advantages for instrument development, including extreme miniaturization when operating at the diffraction-limit, plus integration, superior thermal and mechanical stabilization owing to the small footprint, and high replicability offering significant cost savings. Numerous astrophotonic technologies have been developed to address shortcomings of conventional instruments to date, including the development of photonic lanterns to convert from multimode inputs to single mode outputs, complex aperiodic fiber Bragg gratings to filter OH emission from the atmosphere, beam combiners enabling long baseline interferometry with for example, ESO Gravity, and laser frequency combs for high precision spectral calibration of spectrometers. Despite these successes, the facility implementation of photonic solutions in astronomical instrumentation is currently limited because of 1) low throughputs from coupling to fibers, coupling fibers to chips, propagation and bend losses, device losses, etc., 2) difficulties with scaling to large channel count devices needed for large bandwidths and high resolutions, and 3) efficient integration of photonics with detectors. In this roadmap, we identify 23 key areas that need further development. We outline the challenges and advances needed across those areas covering design tools, simulation capabilities, fabrication processes, the need for entirely new components, integration and hybridization and the characterization of devices. To realize these advances the astrophotonics community will have to work cooperatively with industrial partners who have more advanced manufacturing capabilities. With the advances described herein, multi-functional integrated instruments will be realized leading to novel observing capabilities for both ground and space based platforms, enabling new scientific studies and discoveries.

Published
2023
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32. The James Webb Space Telescope Mission

Author

Gardner, Jonathan P., Mather, John C., Abbott, Randy, Abell, James S., Abernathy, Mark, Abney, Faith E., Abraham, John G., Abraham, Roberto, Abul-Huda, Yasin M., Acton, Scott, Adams, Cynthia K., Adams, Evan, Adler, David S., Adriaensen, Maarten, Aguilar, Jonathan Albert, Ahmed, Mansoor, Ahmed, Nasif S., Ahmed, Tanjira, Albat, Rüdeger, Albert, Loïc, Alberts, Stacey, Aldridge, David, Allen, Mary Marsha, Allen, Shaune S., Altenburg, Martin, Altunc, Serhat, Alvarez, Jose Lorenzo, Álvarez-Márquez, Javier, de Oliveira, Catarina Alves, Ambrose, Leslie L., Anandakrishnan, Satya M., Andersen, Gregory C., Anderson, Harry James, Anderson, Jay, Anderson, Kristen, Anderson, Sara M., Aprea, Julio, Archer, Benita J., Arenberg, Jonathan W., Argyriou, Ioannis, Arribas, Santiago, Artigau, Étienne, Arvai, Amanda Rose, Atcheson, Paul, Atkinson, Charles B., Averbukh, Jesse, Aymergen, Cagatay, Bacinski, John J., Baggett, Wayne E., Bagnasco, Giorgio, Baker, Lynn L., Balzano, Vicki Ann, Banks, Kimberly A., Baran, David A., Barker, Elizabeth A., Barrett, Larry K., Barringer, Bruce O., Barto, Allison, Bast, William, Baudoz, Pierre, Baum, Stefi, Beatty, Thomas G., Beaulieu, Mathilde, Bechtold, Kathryn, Beck, Tracy, Beddard, Megan M., Beichman, Charles, Bellagama, Larry, Bely, Pierre, Berger, Timothy W., Bergeron, Louis E., Darveau-Bernier, Antoine, Bertch, Maria D., Beskow, Charlotte, Betz, Laura E., Biagetti, Carl P., Birkmann, Stephan, Bjorklund, Kurt F., Blackwood, James D., Blazek, Ronald Paul, Blossfeld, Stephen, Bluth, Marcel, Boccaletti, Anthony, Boegner Jr., Martin E., Bohlin, Ralph C., Boia, John Joseph, Böker, Torsten, Bonaventura, N., Bond, Nicholas A., Bosley, Kari Ann, Boucarut, Rene A., Bouchet, Patrice, Bouwman, Jeroen, Bower, Gary, Bowers, Ariel S., Bowers, Charles W., Boyce, Leslye A., Boyer, Christine T., Boyer, Martha L., Boyer, Michael, Boyer, Robert, Bradley, Larry D., Brady, Gregory R., Brandl, Bernhard R., Brannen, Judith L., Breda, David, Bremmer, Harold G., Brennan, David, Bresnahan, Pamela A., Bright, Stacey N., Broiles, Brian J., Bromenschenkel, Asa, Brooks, Brian H., Brooks, Keira J., Brown, Bob, Brown, Bruce, Brown, Thomas M., Bruce, Barry W., Bryson, Jonathan G., Bujanda, Edwin D., Bullock, Blake M., Bunker, A. J., Bureo, Rafael, Burt, Irving J., Bush, James Aaron, Bushouse, Howard A., Bussman, Marie C., Cabaud, Olivier, Cale, Steven, Calhoon, Charles D., Calvani, Humberto, Canipe, Alicia M., Caputo, Francis M., Cara, Mihai, Carey, Larkin, Case, Michael Eli, Cesari, Thaddeus, Cetorelli, Lee D., Chance, Don R., Chandler, Lynn, Chaney, Dave, Chapman, George N., Charlot, S., Chayer, Pierre, Cheezum, Jeffrey I., Chen, Bin, Chen, Christine H., Cherinka, Brian, Chichester, Sarah C., Chilton, Zachary S., Chittiraibalan, Dharini, Clampin, Mark, Clark, Charles R., Clark, Kerry W., Clark, Stephanie M., Claybrooks, Edward E., Cleveland, Keith A., Cohen, Andrew L., Cohen, Lester M., Colón, Knicole D., Coleman, Benee L., Colina, Luis, Comber, Brian J., Comeau, Thomas M., Comer, Thomas, Reis, Alain Conde, Connolly, Dennis C., Conroy, Kyle E., Contos, Adam R., Contreras, James, Cook, Neil J., Cooper, James L., Cooper, Rachel Aviva, Correia, Michael F., Correnti, Matteo, Cossou, Christophe, Costanza, Brian F., Coulais, Alain, Cox, Colin R., Coyle, Ray T., Cracraft, Misty M., Noriega-Crespo, Alberto, Crew, Keith A., Curtis, Gary J., Cusveller, Bianca, Maciel, Cleyciane Da Costa, Dailey, Christopher T., Daugeron, Frédéric, Davidson, Greg S., Davies, James E., Davis, Katherine Anne, Davis, Michael S., Day, Ratna, de Chambure, Daniel, de Jong, Pauline, De Marchi, Guido, Dean, Bruce H., Decker, John E., Delisa, Amy S., Dell, Lawrence C., Dellagatta, Gail, Dembinska, Franciszka, Demosthenes, Sandor, Dencheva, Nadezhda M., Deneu, Philippe, DePriest, William W., Deschenes, Jeremy, Dethienne, Nathalie, Detre, Örs Hunor, Diaz, Rosa Izela, Dicken, Daniel, DiFelice, Audrey S., Dillman, Matthew, Disharoon, Maureen O., van Dishoeck, Ewine F., Dixon, William V., Doggett, Jesse B., Dominguez, Keisha L., Donaldson, Thomas S., Doria-Warner, Cristina M., Santos, Tony Dos, Doty, Heather, Douglas Jr., Robert E., Doyon, René, Dressler, Alan, Driggers, Jennifer, Driggers, Phillip A., Dunn, Jamie L., DuPrie, Kimberly C., Dupuis, Jean, Durning, John, Dutta, Sanghamitra B., Earl, Nicholas M., Eccleston, Paul, Ecobichon, Pascal, Egami, Eiichi, Ehrenwinkler, Ralf, Eisenhamer, Jonathan D., Eisenhower, Michael, Eisenstein, Daniel J., Hamel, Zaky El, Elie, Michelle L., Elliott, James, Elliott, Kyle Wesley, Engesser, Michael, Espinoza, Néstor, Etienne, Odessa, Etxaluze, Mireya, Evans, Leah, Fabreguettes, Luce, Falcolini, Massimo, Falini, Patrick R., Fatig, Curtis, Feeney, Matthew, Feinberg, Lee D., Fels, Raymond, Ferdous, Nazma, Ferguson, Henry C., Ferrarese, Laura, Ferreira, Marie-Héléne, Ferruit, Pierre, Ferry, Malcolm, Filippazzo, Joseph Charles, Firre, Daniel, Fix, Mees, Flagey, Nicolas, Flanagan, Kathryn A., Fleming, Scott W., Florian, Michael, Flynn, James R., Foiadelli, Luca, Fontaine, Mark R., Fontanella, Erin Marie, Forshay, Peter Randolph, Fortner, Elizabeth A., Fox, Ori D., Framarini, Alexandro P., Francisco, John I., Franck, Randy, Franx, Marijn, Franz, David E., Friedman, Scott D., Friend, Katheryn E., Frost, James R., Fu, Henry, Fullerton, Alexander W., Gaillard, Lionel, Galkin, Sergey, Gallagher, Ben, Galyer, Anthony D., Marín, Macarena García, Gardner, Lisa E., Garland, Dennis, Garrett, Bruce Albert, Gasman, Danny, Gáspár, András, Gastaud, René, Gaudreau, Daniel, Gauthier, Peter Timothy, Geers, Vincent, Geithner, Paul H., Gennaro, Mario, Gerber, John, Gereau, John C., Giampaoli, Robert, Giardino, Giovanna, Gibbons, Paul C., Gilbert, Karolina, Gilman, Larry, Girard, Julien H., Giuliano, Mark E., Gkountis, Konstantinos, Glasse, Alistair, Glassmire, Kirk Zachary, Glauser, Adrian Michael, Glazer, Stuart D., Goldberg, Joshua, Golimowski, David A., Gonzaga, Shireen P., Gordon, Karl D., Gordon, Shawn J., Goudfrooij, Paul, Gough, Michael J., Graham, Adrian J., Grau, Christopher M., Green, Joel David, Greene, Gretchen R., Greene, Thomas P., Greenfield, Perry E., Greenhouse, Matthew A., Greve, Thomas R., Greville, Edgar M., Grimaldi, Stefano, Groe, Frank E., Groebner, Andrew, Grumm, David M., Grundy, Timothy, Güdel, Manuel, Guillard, Pierre, Guldalian, John, Gunn, Christopher A., Gurule, Anthony, Gutman, Irvin Meyer, Guy, Paul D., Guyot, Benjamin, Hack, Warren J., Haderlein, Peter, Hagan, James B., Hagedorn, Andria, Hainline, Kevin, Haley, Craig, Hami, Maryam, Hamilton, Forrest Clifford, Hammann, Jeffrey, Hammel, Heidi B., Hanley, Christopher J., Hansen, Carl August, Hardy, Bruce, Harnisch, Bernd, Harr, Michael Hunter, Harris, Pamela, Hart, Jessica Ann, Hartig, George F., Hasan, Hashima, Hashim, Kathleen Marie, Hashimoto, Ryan, Haskins, Sujee J., Hawkins, Robert Edward, Hayden, Brian, Hayden, William L., Healy, Mike, Hecht, Karen, Heeg, Vince J., Hejal, Reem, Helm, Kristopher A., Hengemihle, Nicholas J., Henning, Thomas, Henry, Alaina, Henry, Ronald L., Henshaw, Katherine, Hernandez, Scarlin, Herrington, Donald C., Heske, Astrid, Hesman, Brigette Emily, Hickey, David L., Hilbert, Bryan N., Hines, Dean C., Hinz, Michael R., Hirsch, Michael, Hitcho, Robert S., Hodapp, Klaus, Hodge, Philip E., Hoffman, Melissa, Holfeltz, Sherie T., Holler, Bryan Jason, Hoppa, Jennifer Rose, Horner, Scott, Howard, Joseph M., Howard, Richard J., Huber, Jean M., Hunkeler, Joseph S., Hunter, Alexander, Hunter, David Gavin, Hurd, Spencer W., Hurst, Brendan J., Hutchings, John B., Hylan, Jason E., Ignat, Luminita Ilinca, Illingworth, Garth, Irish, Sandra M., Isaacs III, John C., Jackson Jr., Wallace C., Jaffe, Daniel T., Jahic, Jasmin, Jahromi, Amir, Jakobsen, Peter, James, Bryan, James, John C., James, LeAndrea Rae, Jamieson, William Brian, Jandra, Raymond D., Jayawardhana, Ray, Jedrzejewski, Robert, Jeffers, Basil S., Jensen, Peter, Joanne, Egges, Johns, Alan T., Johnson, Carl A., Johnson, Eric L., Johnson, Patricia, Johnson, Phillip Stephen, Johnson, Thomas K., Johnson, Timothy W., Johnstone, Doug, Jollet, Delphine, Jones, Danny P., Jones, Gregory S., Jones, Olivia C., Jones, Ronald A., Jones, Vicki, Jordan, Ian J., Jordan, Margaret E., Jue, Reginald, Jurkowski, Mark H., Justis, Grant, Justtanont, Kay, Kaleida, Catherine C., Kalirai, Jason S., Kalmanson, Phillip Cabrales, Kaltenegger, Lisa, Kammerer, Jens, Kan, Samuel K., Kanarek, Graham Childs, Kao, Shaw-Hong, Karakla, Diane M., Karl, Hermann, Kassin, Susan A., Kauffman, David D., Kavanagh, Patrick, Kelley, Leigh L., Kelly, Douglas M., Kendrew, Sarah, Kennedy, Herbert V., Kenny, Deborah A., Keski-Kuha, Ritva A., Keyes, Charles D., Khan, Ali, Kidwell, Richard C., Kimble, Randy A., King, James S., King, Richard C., Kinzel, Wayne M., Kirk, Jeffrey R., Kirkpatrick, Marc E., Klaassen, Pamela, Klingemann, Lana, Klintworth, Paul U., Knapp, Bryan Adam, Knight, Scott, Knollenberg, Perry J., Knutsen, Daniel Mark, Koehler, Robert, Koekemoer, Anton M., Kofler, Earl T., Kontson, Vicki L., Kovacs, Aiden Rose, Kozhurina-Platais, Vera, Krause, Oliver, Kriss, Gerard A., Krist, John, Kristoffersen, Monica R., Krogel, Claudia, Krueger, Anthony P., Kulp, Bernard A., Kumari, Nimisha, Kwan, Sandy W., Kyprianou, Mark, Labador, Aurora Gadiano, Labiano, Álvaro, Lafrenière, David, Lagage, Pierre-Olivier, Laidler, Victoria G., Laine, Benoit, Laird, Simon, Lajoie, Charles-Philippe, Lallo, Matthew D., Lam, May Yen, LaMassa, Stephanie Marie, Lambros, Scott D., Lampenfield, Richard Joseph, Lander, Matthew Ed, Langston, James Hutton, Larson, Kirsten, Larson, Melora, LaVerghetta, Robert Joseph, Law, David R., Lawrence, Jon F., Lee, David W., Lee, Janice, Lee, Yat-Ning Paul, Leisenring, Jarron, Leveille, Michael Dunlap, Levenson, Nancy A., Levi, Joshua S., Levine, Marie B., Lewis, Dan, Lewis, Jake, Lewis, Nikole, Libralato, Mattia, Lidon, Norbert, Liebrecht, Paula Louisa, Lightsey, Paul, Lilly, Simon, Lim, Frederick C., Lim, Pey Lian, Ling, Sai-Kwong, Link, Lisa J., Link, Miranda Nicole, Lipinski, Jamie L., Liu, XiaoLi, Lo, Amy S., Lobmeyer, Lynette, Logue, Ryan M., Long, Chris A., Long, Douglas R., Long, Ilana D., Long, Knox S., López-Caniego, Marcos, Lotz, Jennifer M., Love-Pruitt, Jennifer M., Lubskiy, Michael, Luers, Edward B., Luetgens, Robert A., Luevano, Annetta J., Lui, Sarah Marie G. Flores, Lund III, James M., Lundquist, Ray A., Lunine, Jonathan, Lützgendorf, Nora, Lynch, Richard J., MacDonald, Alex J., MacDonald, Kenneth, Macias, Matthew J., Macklis, Keith I., Maghami, Peiman, Maharaja, Rishabh Y., Maiolino, Roberto, Makrygiannis, Konstantinos G., Malla, Sunita Giri, Malumuth, Eliot M., Manjavacas, Elena, Marini, Andrea, Marrione, Amanda, Marston, Anthony, Martel, André R, Martin, Didier, Martin, Peter G., Martinez, Kristin L., Maschmann, Marc, Masci, Gregory L., Masetti, Margaret E., Maszkiewicz, Michael, Matthews, Gary, Matuskey, Jacob E., McBrayer, Glen A., McCarthy, Donald W., McCaughrean, Mark J., McClare, Leslie A., McClare, Michael D., McCloskey, John C., McClurg, Taylore D., McCoy, Martin, McElwain, Michael W., McGregor, Roy D., McGuffey, Douglas B., McKay, Andrew G., McKenzie, William K., McLean, Brian, McMaster, Matthew, McNeil, Warren, De Meester, Wim, Mehalick, Kimberly L., Meixner, Margaret, Meléndez, Marcio, Menzel, Michael P., Menzel, Michael T., Merz, Matthew, Mesterharm, David D., Meyer, Michael R., Meyett, Michele L., Meza, Luis E., Midwinter, Calvin, Milam, Stefanie N., Miller, Jay Todd, Miller, William C., Miskey, Cherie L., Misselt, Karl, Mitchell, Eileen P., Mohan, Martin, Montoya, Emily E., Moran, Michael J., Morishita, Takahiro, Moro-Martín, Amaya, Morrison, Debra L., Morrison, Jane, Morse, Ernie C., Moschos, Michael, Moseley, S. H., Mosier, Gary E., Mosner, Peter, Mountain, Matt, Muckenthaler, Jason S., Mueller, Donald G., Mueller, Migo, Muhiem, Daniella, Mühlmann, Prisca, Mullally, Susan Elizabeth, Mullen, Stephanie M., Munger, Alan J, Murphy, Jess, Murray, Katherine T., Muzerolle, James C., Mycroft, Matthew, Myers, Andrew, Myers, Carey R., Myers, Fred Richard R., Myers, Richard, Myrick, Kaila, Nagle IV, Adrian F., Nayak, Omnarayani, Naylor, Bret, Neff, Susan G., Nelan, Edmund P., Nella, John, Nguyen, Duy Tuong, Nguyen, Michael N., Nickson, Bryony, Nidhiry, John Joseph, Niedner, Malcolm B., Nieto-Santisteban, Maria, Nikolov, Nikolay K., Nishisaka, Mary Ann, Nota, Antonella, O'Mara, Robyn C., Oboryshko, Michael, O'Brien, Marcus B., Ochs, William R., Offenberg, Joel D., Ogle, Patrick Michael, Ohl, Raymond G., Olmsted, Joseph Hamden, Osborne, Shannon Barbara, O'Shaughnessy, Brian Patrick, Östlin, Göran, O'Sullivan, Brian, Otor, O. Justin, Ottens, Richard, Ouellette, Nathalie N. -Q., Outlaw, Daria J., Owens, Beverly A., Pacifici, Camilla, Page, James Christophe, Paranilam, James G., Park, Sang, Parrish, Keith A., Paschal, Laura, Patapis, Polychronis, Patel, Jignasha, Patrick, Keith, Pattishall Jr., Robert A., Paul, Douglas William, Paul, Shirley J., Pauly, Tyler Andrew, Pavlovsky, Cheryl M., Peña-Guerrero, Maria, Pedder, Andrew H., Peek, Matthew Weldon, Pelham, Patricia A., Penanen, Konstantin, Perriello, Beth A., Perrin, Marshall D., Perrine, Richard F., Perrygo, Chuck, Peslier, Muriel, Petach, Michael, Peterson, Karla A., Pfarr, Tom, Pierson, James M., Pietraszkiewicz, Martin, Pilchen, Guy, Pipher, Judy L., Pirzkal, Norbert, Pitman, Joseph T., Player, Danielle M., Plesha, Rachel, Plitzke, Anja, Pohner, John A., Poletis, Karyn Konstantin, Pollizzi, Joseph A., Polster, Ethan, Pontius, James T., Pontoppidan, Klaus, Porges, Susana C., Potter, Gregg D., Prescott, Stephen, Proffitt, Charles R., Pueyo, Laurent, Neira, Irma Aracely Quispe, Radich, Armando, Rager, Reiko T., Rameau, Julien, Ramey, Deborah D., Alarcon, Rafael Ramos, Rampini, Riccardo, Rapp, Robert, Rashford, Robert A., Rauscher, Bernard J., Ravindranath, Swara, Rawle, Timothy, Rawlings, Tynika N., Ray, Tom, Regan, Michael W., Rehm, Brian, Rehm, Kenneth D., Reid, Neill, Reis, Carl A., Renk, Florian, Reoch, Tom B., Ressler, Michael, Rest, Armin W., Reynolds, Paul J., Richon, Joel G., Richon, Karen V., Ridgaway, Michael, Riedel, Adric Richard, Rieke, George H., Rieke, Marcia, Rifelli, Richard E., Rigby, Jane R., Riggs, Catherine S., Ringel, Nancy J., Ritchie, Christine E., Rix, Hans-Walter, Robberto, Massimo, Robinson, Michael S., Robinson, Orion, Rock, Frank W., Rodriguez, David R., del Pino, Bruno Rodríguez, Roellig, Thomas, Rohrbach, Scott O., Roman, Anthony J., Romelfanger, Frederick J., Romo Jr., Felipe P., Rosales, Jose J., Rose, Perry, Roteliuk, Anthony F., Roth, Marc N., Rothwell, Braden Quinn, Rouzaud, Sylvain, Rowe, Jason, Rowlands, Neil, Roy, Arpita, Royer, Pierre, Rui, Chunlei, Rumler, Peter, Rumpl, William, Russ, Melissa L., Ryan, Michael B., Ryan, Richard M., Saad, Karl, Sabata, Modhumita, Sabatino, Rick, Sabbi, Elena, Sabelhaus, Phillip A., Sabia, Stephen, Sahu, Kailash C., Saif, Babak N., Salvignol, Jean-Christophe, Samara-Ratna, Piyal, Samuelson, Bridget S., Sanders, Felicia A., Sappington, Bradley, Sargent, B. A., Sauer, Arne, Savadkin, Bruce J., Sawicki, Marcin, Schappell, Tina M., Scheffer, Caroline, Scheithauer, Silvia, Scherer, Ron, Schiff, Conrad, Schlawin, Everett, Schmeitzky, Olivier, Schmitz, Tyler S., Schmude, Donald J., Schneider, Analyn, Schreiber, Jürgen, Schroeven-Deceuninck, Hilde, Schultz, John J., Schwab, Ryan, Schwartz, Curtis H., Scoccimarro, Dario, Scott, John F., Scott, Michelle B., Seaton, Bonita L., Seely, Bruce S., Seery, Bernard, Seidleck, Mark, Sembach, Kenneth, Shanahan, Clare Elizabeth, Shaughnessy, Bryan, Shaw, Richard A., Shay, Christopher Michael, Sheehan, Even, Sheth, Kartik, Shih, Hsin-Yi, Shivaei, Irene, Siegel, Noah, Sienkiewicz, Matthew G., Simmons, Debra D., Simon, Bernard P., Sirianni, Marco, Sivaramakrishnan, Anand, Slade, Jeffrey E., Sloan, G. C., Slocum, Christine E., Slowinski, Steven E., Smith, Corbett T., Smith, Eric P., Smith, Erin C., Smith, Koby, Smith, Robert, Smith, Stephanie J., Smolik, John L., Soderblom, David R., Sohn, Sangmo Tony, Sokol, Jeff, Sonneborn, George, Sontag, Christopher D., Sooy, Peter R., Soummer, Remi, Southwood, Dana M., Spain, Kay, Sparmo, Joseph, Speer, David T., Spencer, Richard, Sprofera, Joseph D., Stallcup, Scott S., Stanley, Marcia K., Stansberry, John A., Stark, Christopher C., Starr, Carl W., Stassi, Diane Y., Steck, Jane A., Steeley, Christine D., Stephens, Matthew A., Stephenson, Ralph J., Stewart, Alphonso C., Stiavelli, Massimo, Stockman Jr., Hervey, Strada, Paolo, Straughn, Amber N., Streetman, Scott, Strickland, David Kendal, Strobele, Jingping F., Stuhlinger, Martin, Stys, Jeffrey Edward, Such, Miguel, Sukhatme, Kalyani, Sullivan, Joseph F., Sullivan, Pamela C., Sumner, Sandra M., Sun, Fengwu, Sunnquist, Benjamin Dale, Swade, Daryl Allen, Swam, Michael S., Swenton, Diane F., Swoish, Robby A., Litten, Oi In Tam, Tamas, Laszlo, Tao, Andrew, Taylor, David K., Taylor, Joanna M., Plate, Maurice te, Van Tea, Mason, Teague, Kelly K., Telfer, Randal C., Temim, Tea, Texter, Scott C., Thatte, Deepashri G., Thompson, Christopher Lee, Thompson, Linda M., Thomson, Shaun R., Thronson, Harley, Tierney, C. M., Tikkanen, Tuomo, Tinnin, Lee, Tippet, William Thomas, Todd, Connor William, Tran, Hien D., Trauger, John, Trejo, Edwin Gregorio, Truong, Justin Hoang Vinh, Tsukamoto, Christine L., Tufail, Yasir, Tumlinson, Jason, Tustain, Samuel, Tyra, Harrison, Ubeda, Leonardo, Underwood, Kelli, Uzzo, Michael A., Vaclavik, Steven, Valenduc, Frida, Valenti, Jeff A., Van Campen, Julie, van de Wetering, Inge, Van Der Marel, Roeland P., van Haarlem, Remy, Vandenbussche, Bart, Vanterpool, Dona D., Vernoy, Michael R., Costas, Maria Begoña Vila, Volk, Kevin, Voorzaat, Piet, Voyton, Mark F., Vydra, Ekaterina, Waddy, Darryl J., Waelkens, Christoffel, Wahlgren, Glenn Michael, Walker Jr., Frederick E., Wander, Michel, Warfield, Christine K., Warner, Gerald, Wasiak, Francis C., Wasiak, Matthew F., Wehner, James, Weiler, Kevin R., Weilert, Mark, Weiss, Stanley B., Wells, Martyn, Welty, Alan D., Wheate, Lauren, Wheeler, Thomas P., White, Christy L., Whitehouse, Paul, Whiteleather, Jennifer Margaret, Whitman, William Russell, Williams, Christina C., Willmer, Christopher N. A., Willott, Chris J., Willoughby, Scott P., Wilson, Andrew, Wilson, Debra, Wilson, Donna V., Windhorst, Rogier, Wislowski, Emily Christine, Wolfe, David J., Wolfe, Michael A., Wolff, Schuyler, Wondel, Amancio, Woo, Cindy, Woods, Robert T., Worden, Elaine, Workman, William, Wright, Gillian S., Wu, Carl, Wu, Chi-Rai, Wun, Dakin D., Wymer, Kristen B., Yadetie, Thomas, Yan, Isabelle C., Yang, Keith C., Yates, Kayla L., Yeager, Christopher R., Yerger, Ethan John, Young, Erick T., Young, Gary, Yu, Gene, Yu, Susan, Zak, Dean S., Zeidler, Peter, Zepp, Robert, Zhou, Julia, Zincke, Christian A., Zonak, Stephanie, and Zondag, Elisabeth

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least $4m$. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the $6.5m$ James Webb Space Telescope. A generation of astronomers will celebrate their accomplishments for the life of the mission, potentially as long as 20 years, and beyond. This report and the scientific discoveries that follow are extended thank-you notes to the 20,000 team members. The telescope is working perfectly, with much better image quality than expected. In this and accompanying papers, we give a brief history, describe the observatory, outline its objectives and current observing program, and discuss the inventions and people who made it possible. We cite detailed reports on the design and the measured performance on orbit., Comment: Accepted by PASP for the special issue on The James Webb Space Telescope Overview, 29 pages, 4 figures

Published
2023
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33. Observations of Transiting Exoplanets with the James Webb Space Telescope ( JWST )

Author

Beichman, Charles, Benneke, Bjoern, Knutson, Heather, Smith, Roger, Lagage, Pierre-Olivier, Dressing, Courtney, Latham, David, Lunine, Jonathan, Birkmann, Stephan, Ferruit, Pierre, Giardino, Giovanna, Kempton, Eliza, Carey, Sean, Krick, Jessica, Deroo, Pieter D., Mandell, Avi, Ressler, Michael E., Shporer, Avi, Swain, Mark, Vasisht, Gautam, Ricker, George, Bouwman, Jeroen, Crossfield, Ian, Greene, Tom, Howell, Steve, Christiansen, Jessie, Ciardi, David, Clampin, Mark, Greenhouse, Matt, Sozzetti, Alessandro, Goudfrooij, Paul, Hines, Dean, Keyes, Tony, Lee, Janice, McCullough, Peter, Robberto, Massimo, Stansberry, John, Valenti, Jeff, Rieke, Marcia, Rieke, George, Fortney, Jonathan, Bean, Jacob, Kreidberg, Laura, Ehrenreich, David, Deming, Drake, Albert, Loïc, Doyon, René, and Sing, David

Published
2014
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36. W. M. Keck observatory instrumentation status and future direction.

Author

Kassis, Marc, Allen, Steven L., Alverez, Carlos, Baker, Ashley, Banyal, Ravinder K., Bertz, Robert, Beichman, Charles, Brown, Aaron, Brown, Matthew, Bundy, Kevin, Cabak, Gerald, Cetre, Sylvain, Chin, Jason, Chun, Mark R., Cooke, Jeff, Delorme, Jacques, Deich, William, Dekany, Richard G., Devenot, Mark, and Doppmann, Greg

Subjects
OBSERVATORIES, COOPERATIVE research, ASTRONOMICAL observatories, ADAPTIVE optics, STRATEGIC planning
Abstract

Since the start of science operations in 1993, the twin 10‐m W. M. Keck Observatory (WMKO) telescopes have continued to maximize their scientific impact and to produce transformative discoveries that keep the observing community on the frontiers of astronomical research. Upgraded capabilities and new instrumentation are provided through collaborative partnerships with Caltech, the University of California, and the University of Hawaii instrument development teams along with industry and other organizations. The observatory adapts and responds to the observers' evolving needs as defined in the observatory's strategic plan periodically refreshed in collaboration with the science community. This paper is an overview of the instrumentation projects that range from commissioning to early conceptual stages. An emphasis is placed on the detector, detector controllers, and capability needs that are driven by the desired future technology defined in the 2022 strategic plan. [ABSTRACT FROM AUTHOR]

Published
2023
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37. A Neptune-sized transiting planet closely orbiting a 5-10-million-year-old star

Author

David, Trevor J., Hillenbrand, Lynne A., Petigura, Erik A., Carpenter, John M., Crossfield, Ian J.M., Hinkley, Sasha, Ciardi, David R., Howard, Andrew W., Isaacson, Howard T., Cody, Ann Marie, Schlieder, Joshua E., Beichman, Charles A., and Barenfeld, Scott A.

Subjects
Observations, Extrasolar planets -- Observations, Neptune (Planet) -- Observations, Transits (Astronomy) -- Observations, Transits -- Observations
Abstract

The star [PGZ2001] J161014.7-191909, hereafter K2-33, is an M-type star several million years (Myr) old that was observed by NASA's Kepler Space Telescope during campaign 2 of the K2 mission. [...], Theories of the formation and early evolution of planetary systems postulate that planets are born in circumstellar disks, and undergo radial migration during and after dissipation of the dust and gas disk from which they formed (1,2). The precise ages of meteorites indicate that planetesimals--the building blocks of planets--are produced within the first million years of a star's life (3). Fully formed planets are frequently detected on short orbital periods around mature stars. Some theories suggest that the in situ formation of planets close to their host stars is unlikely and that the existence of such planets is therefore evidence of large-scale migration (4,5). Other theories posit that planet assembly at small orbital separations may be common (6-8). Here we report a newly born, transiting planet orbiting its star with a period of 5.4 days. The planet is 50 per cent larger than Neptune, and its mass is less than 3.6 times that of Jupiter (at 99.7 per cent confidence), with a true mass likely to be similar to that of Neptune. The star is 5-10 million years old and has a tenuous dust disk extending outward from about twice the Earth-Sun separation, in addition to the fully formed planet located at less than one-twentieth of the Earth-Sun separation.

Published
2016

38. VaTEST I: Validation of Sub-Saturn Exoplanet TOI-181b in Narrow Orbit from its Host Star

Author

Mistry, Priyashkumar, Pathak, Kamlesh, Lekkas, Georgios, Prasad, Aniket, Bhattarai, Surendra, Maity, Mousam, Beichman, Charles A., Ciardi, David R., Evans, Phil, Bieryla, Allyson, Eastman, Jason D., Latham, David W., Esquerdo, Gilbert A., and Lucero, Jennifer P.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present here a validation of sub-Saturn exoplanet TOI-181b orbiting a K spectral type star TOI-181 (Mass: 0.822 $\pm$ 0.04 M$_{\odot}$, Radius: 0.745 $\pm$ 0.02 R$_{\odot}$, Temperature: 4994 $\pm$ 50 K) as a part of Validation of Transiting Exoplanets using Statistical Tools (VaTEST) project. TOI-181b is a planet with radius 6.95 $\pm$ 0.08 R$_{\oplus}$, mass 46.16 $\pm$ 2.71 M$_{\oplus}$, orbiting in a slightly eccentric orbit with eccentricity 0.15 $\pm$ 0.06 and semi-major axis of 0.054 $\pm$ 0.004 AU, with an orbital period of 4.5320 $\pm$ 0.000002 days. The transit photometry data was collected using Transiting Exoplanet Survey Satellite (TESS) and spectroscopic data for radial velocity analysis was collected using The European Southern Observatory's (ESO) High Accuracy Radial Velocity Planet Searcher (HARPS) telescope. Based on the radial velocity best-fit model we measured RV semi-amplitude to be 20.56 $\pm$ 2.37 m s$^{-1}$. Additionally, we used \texttt{VESPA} and \texttt{TRICERATOPS} to compute the False Positive Probability (FPP), and the findings were FPP values of $1.68\times10^{-14}$ and $3.81\times10^{-04}$, respectively, which are significantly lower than the 1% threshold. The finding of TOI-181b is significant in the perspective of future work on the formation and migration history of analogous planetary systems since warm sub-Saturns are uncommon in the known sample of exoplanets., 13 pages, 10 figures, submitted to MNRAS, Structural changes are made, New results

Published
2022

39. A disintegrating minor planet transiting a white dwarf

Author

Vanderburg, Andrew, Johnson, John Asher, Rappaport, Saul, Bieryla, Allyson, Irwin, Jonathan, Lewis, John Arban, Kipping, David, Brown, Warren R., Dufour, Patrick, Ciardi, David R., Angus, Ruth, Schaefer, Laura, Latham, David W., Charbonneau, David, Beichman, Charles, Eastman, Jason, McCrady, Nate, Wittenmyer, Robert A., and Wright, Jason T.

Subjects
Observations, Minor planets -- Observations, White dwarfs -- Observations
Abstract

Most stars become white dwarfs after they have exhausted their nuclear fuel (the Sun will be one such). Between one-quarter and one-half of white dwarfs have elements heavier than helium [...]

Published
2015

40. Observing Exoplanets with the James Webb Space Telescope

Author

Beichman, Charles A and Greene, Thomas P

Subjects
Astronomy
Abstract

The census of exoplanets has revealed an enormous variety of planets or- biting stars of all ages and spectral types: planets in orbits of less than a day to frigid worlds in orbits over 100 AU; planets with masses 10 times that of Jupiter to planets with masses less than that of Earth; searingly hot planets to temperate planets in the Habitable Zone. The challenge of the coming decade is to move from demography to physical characterization. The James Webb Space Telescope (JWST) is poised to open a revolutionary new phase in our understanding of exoplanets with transit spectroscopy of relatively short period planets and coronagraphic imaging of ones with wide separations from their host stars. This article discusses the wide variety of exoplanet opportunities enabled by JWSTs sensitivity and stability, its high angular resolution, and its suite of powerful instruments. These capabilities will advance our understanding of planet formation, brown dwarfs, and the atmospheres of young to mature planets.

Published
2017
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43. Taking the Measure of the Universe: Precision Astrometry with SIM PlanetQuest

Author

Unwin, Stephen C., Shao, Michael, Tanner, Angelle M., Allen, Ronald J., Beichman, Charles A., Boboltz, David, Catanzarite, Joseph H., Chaboyer, Brian C., Ciardi, David R., Edberg, Stephen J., Fey, Alan L., Fischer, Debra A., Gelino, Christopher R., Gould, Andrew P., Grillmair, Carl, Henry, Todd J., Johnston, Kathryn V., Johnston, Kenneth J., Jones, Dayton L., Kulkarni, Shrinivas R., Law, Nicholas M., Majewski, Steven R., Makarov, Valeri V., Marcy, Geoffrey W., Meier, David L., Olling, Rob P., Pan, Xiaopei, Patterson, Richard J., Pitesky, Jo Eliza, Quirrenbach, Andreas, Shaklan, Stuart B., Shaya, Edward J., Strigari, Louis E., Tomsick, John A., Wehrle, Ann E., and Worthey, Guy

Published
2008
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45. Star-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties Determination.

Author

Tang, Shih-Yun, Stahl, Asa G., Prato, L., Schaefer, G. H., Johns-Krull, Christopher M., Skiff, Brian A., Beichman, Charles A., and Uyama, Taichi

Subjects
MAGNETIC flux density, ORBITS (Astronomy), LUNAR occultations, SPECKLE interferometry, OCCULTATIONS (Astronomy), STELLAR evolution
Abstract

The stellar companion to the weak-line T Tauri star DI Tau A was first discovered by the lunar occultation technique in 1989 and was subsequently confirmed by a speckle imaging observation in 1991. It has not been detected since, despite being targeted by five different studies that used a variety of methods and spanned more than 20 yr. Here, we report the serendipitous rediscovery of DI Tau B during our Young Exoplanets Spectroscopic Survey (YESS). Using radial velocity data from YESS spanning 17 yr, new adaptive optics observations from Keck II, and a variety of other data from the literature, we derive a preliminary orbital solution for the system that effectively explains the detection and (almost all of the) non-detection history of DI Tau B. We estimate the dynamical masses of both components, finding that the large mass difference (q ∼ 0.17) and long orbital period (≳35 yr) make the DI Tau system a noteworthy and valuable addition to studies of stellar evolution and pre-main-sequence models. With a long orbital period and a small flux ratio (f2/f1) between DI Tau A and B, additional measurements are needed for a better comparison between these observational results and pre-main-sequence models. Finally, we report an average surface magnetic field strength ( B ¯ ) for DI Tau A, of ∼0.55 kG, which is unusually low in the context of young active stars. [ABSTRACT FROM AUTHOR]

Published
2023
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46. JWST Observations of the Enigmatic Y-Dwarf WISE 1828+2650. I. Limits to a Binary Companion.

Author

De Furio, Matthew, Lew, Ben, Beichman, Charles, Roellig, Thomas, Bryden, Geoffrey, Ciardi, David, Meyer, Michael, Rieke, Marcia, Greenbaum, Alexandra, Leisenring, Jarron, Llop-Sayson, Jorge, Ygouf, Marie, Albert, Loic, Boyer, Martha, Eisenstein, Daniel, Hodapp, Klaus, Horner, Scott, Johnstone, Doug, Kelly, Doug, and Misselt, Karl

Subjects
ADAPTIVE optics, BROWN dwarf stars, PHOTOMETRY, GAS giants, BINARY stars, SPECTROMETRY, SPACE telescopes
Abstract

The Y-dwarf WISE 1828+2650 is one of the coldest known brown dwarfs with an effective temperature of ∼300 K. Located at a distance of just 10 pc, previous model-based estimates suggest WISE1828+2650 has a mass of ∼5–10 M J, making it a valuable laboratory for understanding the formation, evolution, and physical characteristics of gas giant planets. However, previous photometry and spectroscopy have presented a puzzle, with the near impossibility of simultaneously fitting both the short- (0.9–2.0 μ m) and long-wavelength (3–5 μ m) data. A potential solution to this problem has been the suggestion that WISE 1828+2650 is a binary system whose composite spectrum might provide a better match to the data. Alternatively, new models being developed to fit JWST/NIRSpec, and MIRI spectroscopy might provide new insights. This article describes JWST/NIRCam observations of WISE 1828+2650 in six filters to address the binarity question and to provide new photometry to be used in model fitting. We also report adaptive optics imaging with the Keck I0 m telescope. We find no evidence for multiplicity for a companion beyond 0.5 au with either JWST or Keck. Companion articles will present low- and high-resolution spectra of WISE 1828 obtained with both NIRSpec and MIRI. [ABSTRACT FROM AUTHOR]

Published
2023
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47. VaTEST I: validation of sub-Saturn exoplanet TOI-181b in narrow orbit from its host star.

Author

Mistry, Priyashkumar, Pathak, Kamlesh, Lekkas, Georgios, Prasad, Aniket, Bhattarai, Surendra, Maity, Mousam, Beichman, Charles A, Ciardi, David R, Evans, Phil, Bieryla, Allyson, Eastman, Jason D, Esquerdo, Gilbert A, and Lucero, Jennifer P

Subjects
ORBITS (Astronomy), PLANETARY systems, EXTRASOLAR planets, OBSERVATORIES, VELOCITY, PHOTOMETRY, SATURN (Planet)
Abstract

We present here a validation of sub-Saturn exoplanet TOI-181b orbiting a K spectral type star TOI-181 (mass: 0.822 ± 0.04 M⊙, radius: 0.745 ± 0.02 R⊙, temperature: 4994 ± 50 K) as a part of Validation of Transiting Exoplanets using Statistical Tools (VaTEST) project. TOI-181b is a planet with radius 6.95 ± 0.08 R⊕, mass 46.16 ± 2.71 M⊕, orbiting in a slightly eccentric orbit with eccentricity 0.15 ± 0.06 and semimajor axis of 0.054 ± 0.004 au, with an orbital period of 4.5320 ± 0.000002 d. The transit photometry data were collected using Transiting Exoplanet Survey Satellite (TESS) and spectroscopic data for radial velocity analysis were collected using The European Southern Observatory's (ESO) High Accuracy Radial Velocity Planet Searcher (HARPS) telescope. Based on the radial velocity best-fit model we measured RV semi-amplitude to be 20.56 ± 2.37 m s−1. Additionally, we used VESPA and TRICERATOPS to compute the False Positive Probability (FPP), and the findings were FPP values of 1.68 × 10−14 and 3.81 × 10−04, respectively, which are significantly lower than the 1 per cent threshold. The finding of TOI-181b is significant in the perspective of future work on the formation and migration history of analogous planetary systems since warm sub-Saturns are uncommon in the known sample of exoplanets. [ABSTRACT FROM AUTHOR]

Published
2023
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48. JWST/NIRCam Discovery of the First Y+Y Brown Dwarf Binary: WISE J033605.05–014350.4.

Author

Calissendorff, Per, De Furio, Matthew, Meyer, Michael, Albert, Loïc, Aganze, Christian, Ali-Dib, Mohamad, Bardalez Gagliuffi, Daniella C., Baron, Frederique, Beichman, Charles A., Burgasser, Adam J., Cushing, Michael C., Faherty, Jacqueline Kelly, Fontanive, Clémence, Gelino, Christopher R., Gizis, John E., Greenbaum, Alexandra Z., Kirkpatrick, J. Davy, Leggett, Sandy K., Martinache, Frantz, and Mary, David

Published
2023
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49. Stellar and Planetary Parameters for K2's Late-Type Dwarf Systems from C1 to C5

Author

Martinez, Arturo O, Crossfield, Ian J. M, Schlieder, Joshua E, Dressing, Courtney, Obermeier, Christian, Livingston, John, Ciceri, Simona, Peacock, Sarah, Beichman, Charles A, Lépine, Sébastien, Aller, Kimberly M, Chance, Quadry A, Petigura, Erik A, Howard, Andrew W, and Michael W. Werner

Subjects
Astrophysics
Abstract

The NASA K2 (Kepler-2) mission uses photometry to find planets transiting stars of various types. M dwarfs are of high interest since they host more short-period planets than any other type of main-sequence star and transiting planets around M dwarfs have deeper transits compared to other main-sequence stars. In this paper, we present stellar parameters from K and M dwarfs hosting transiting planet candidates discovered by our team. Using the SOFI (Son OF Isaac - ESA's earlier, similar instrument) spectrograph on the European Southern Observatory's New Technology Telescope, we obtained R approximately equal to 1000 J-, H-, and K-band (0.95-2.52 micron) spectra of 34 late-type K2 planet and candidate planet host systems and 12 bright K4-M5 dwarfs with interferometrically measured radii and effective temperatures. Out of our 34 late-type K2 targets, we identify 27 of these stars as M dwarfs. We measure equivalent widths of spectral features, derive calibration relations using stars with interferometric measurements, and estimate stellar radii, effective temperatures, masses, and luminosities for the K2 planet hosts. Our calibrations provide radii and temperatures with median uncertainties of 0.059 solar radii (16.09 percent) and 160 degrees Kelvin (4.33 percent), respectively. We then reassess the radii and equilibrium temperatures of known and candidate planets based on our spectroscopically derived stellar parameters. Since a planet's radius and equilibrium temperature depend on the parameters of its host star, our study provides more precise planetary parameters for planets and candidates orbiting late-type stars observed with K2. We find a median planet radius and an equilibrium temperature of approximately 3 solar radii and 500 degrees Kelvin, respectively, with several systems (K2-18b and K2-72e) receiving near-Earth-like levels of incident irradiation.

Published
2017
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50. Transiting Exoplanet Studies and Community Targets for JWST's Early Release Science Program

Author

Stevenson, Kevin B, Lewis, Nikole K, Bean, Jacob L, Beichman, Charles, Fraine, Jonathan, Kilpatrick, Brian M, Krick, J. E, Lothringer, Joshua D, Mandell, Avi M, Valenti, Jeff A, Agol, Eric, Angerhausen, Daniel, Barstow, Joanna K, Birkmann, Stephan M, Burrows, Adam, Charbonneau, David, Cowan, Nicolas B, Crouzet, Nicolas, Cubillos, Patricio E, Curry, S. M, Dalba, Paul A, de Wit, Julien, Greene, Thomas P, Line, Michael R, and Wakeford, Hannah R

Subjects
Lunar And Planetary Science And Exploration
Abstract

The James Webb Space Telescope (JWST) will likely revolutionize transiting exoplanet atmospheric science, due to a combination of its capability for continuous, long duration observations and its larger collecting area, spectral coverage, and spectral resolution compared to existing space-based facilities. However, it is unclear precisely how well JWST will perform and which of its myriad instruments and observing modes will be best suited for transiting exoplanet studies. In this article, we describe a prefatory JWST Early Release Science (ERS) Cycle1 program that focuses on testing specific observing modes to quickly give the community the data and experience it needs to plan more efficient and successful transiting exoplanet characterization programs in later cycles. We propose a multi-pronged approach wherein one aspect of the program focuses on observing transits of a single target with all of the recommended observing modes to identify and understand potential systematics, compare transmission spectra at overlapping and neighboring wavelength regions, confirm throughputs, and determine overall performances. In our search for transiting exoplanets that are well suited to achieving these goals, we identify 12 objects (dubbed community targets) that meet our defined criteria. Currently, the most favorable target is WASP-62b because of its large predicted signal size, relatively bright host star, and location in JWSTs continuous viewing zone. Since most of the community targets do not have well-characterized atmospheres, we recommend initiating preparatory observing programs to determine the presence of obscuring cloudshazes within their atmospheres. Measurable spectroscopic features are needed to establish the optimal resolution and wavelength regions for exoplanet characterization. Other initiatives from our proposed ERS program include testing the instrument brightness limits and performing phase-curve observations. The latter are a unique challenge compared to transit observations because of their significantly longer durations. Using only a single mode, we propose to observe a full-orbit phase curve of one of the previously characterized, short-orbital-period planets to evaluate the facility-level aspects of long, uninterrupted time-series observations.

Published
2016
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