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Your search keyword '"Misselt, K. A."' showing total 15 results
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15 results on '"Misselt, K. A."'

1. JWST observations of the Horsehead photon-dominated region I. First results from multi-band near- and mid-infrared imaging

Author

Abergel, A., Misselt, K., Gordon, K. D., Noriega-Crespo, A., Guillard, P., Van De Putte, D., Witt, A. N., Ysard, N., Baes, M., Beuther, H., Bouchet, P., Brandl, B. R., Elyajouri, M., Kannavou, O., Kendrew, S., Klassen, P., and Trahin, B.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The JWST has captured the sharpest IR images ever taken of the Horsehead nebula, a prototypical moderately irradiated PDR that is fully representative of most of the UV-illuminated molecular gas in the Milky Way and star-forming galaxies. We investigate the impact of FUV radiation of a molecular cloud and constrain the structure of the edge of the PDR and its illumination conditions. We used NIRCam and MIRI to obtain 17 broadband and 6 narrowband maps from 0.7 to 28 $\mu$m. We mapped the dust emission, scattered light, and several gas phase lines. We also used HST-WFC3 maps at 1.1 and 1. 6 $\mu$m, along with HST-STIS spectroscopic observations of the H$\alpha$ line. We probed the structure of the edge of the Horsehead and resolved its spatial complexity. We detected a network of faint striated features extending perpendicularly to the PDR front into the H\,II region in filters sensitive to nano-grain emission and light scattered by larger grains. This may indeed figure as the first detection of the entrainment of dust particles in the evaporative flow. The map of the 1-0 S(1) line of H$_2$ presents sharp sub-structures on scales as small as 1.5 arcsec. The ionization and dissociation fronts appear at distances 1-2 arcsec behind the edge of the PDR and seem to spatially coincide, indicating a thickness of the neutral atomic layer below 100 au. All broadband maps present strong color variations which can be explained by dust attenuation. Deviations of the emissions in the H$\alpha$, Pa$\alpha,$ and Br$\alpha$ lines also indicate dust attenuation. With a very simple model, we derive the main features of the extinction curve. A small excess of extinction at 3 $\mu$m may be attributed to icy H$_2$O mantles onto grains. In all lines of sight crossing the inner regions of the Horsehead, it appears that dust attenuation is non-negligible over the entire spectral range., Comment: 25 pages, 17 figures

Published
2024
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2. The extremely sharp transition between molecular and ionized gas in the Horsehead nebula

Author

Hernández-Vera, C., Guzmán, V. V., Goicoechea, J. R., Maillard, V., Pety, J., Petit, F. Le, Gerin, M., Bron, E., Roueff, E., Abergel, A., Schirmer, T., Carpenter, J., Gratier, P., Gordon, K., and Misselt, K.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

(Abridged) Massive stars can determine the evolution of molecular clouds with their strong ultraviolet (UV) radiation fields. Moreover, UV radiation is relevant in setting the thermal gas pressure in star-forming clouds, whose influence can extend from the rims of molecular clouds to entire star-forming galaxies. Probing the fundamental structure of nearby molecular clouds is therefore crucial to understand how massive stars shape their surrounding medium and how fast molecular clouds are destroyed, specifically at their UV-illuminated edges, where models predict an intermediate zone of neutral atomic gas between the molecular cloud and the surrounding ionized gas whose size is directly related to the exposed physical conditions. We present the highest angular resolution (~$0.5$", corresponding to $207$ au) and velocity-resolved images of the molecular gas emission in the Horsehead nebula, using CO J=3-2 and HCO$^+$ J=4-3 observations with ALMA. We find that CO and HCO$^+$ are present at the edge of the cloud, very close to the ionization (H$^+$/H) and dissociation fronts (H/H$_2$), suggesting a very thin layer of neutral atomic gas (<$650$ au) and a small amount of CO-dark gas ($A_V=0.006-0.26$ mag) for stellar UV illumination conditions typical of molecular clouds in the Milky Way. The new ALMA observations reveal a web of molecular gas filaments with an estimated thermal gas pressure of $P_{\mathrm{th}} = (2.3 - 4.0) \times 10^6$ K cm$^{-3}$, and the presence of a steep density gradient at the cloud edge that can be well explained by stationary isobaric PDR models with pressures consistent with our estimations. However, in the HII region and PDR interface, we find $P_{\mathrm{th,PDR}} > P_{\mathrm{th,HII}}$, suggesting the gas is slightly compressed. Therefore, dynamical effects cannot be completely ruled out and even higher angular observations will be needed to unveil their role., Comment: 15 pages, 1 table, 9 figures; Accepted for publication in A&A

Published
2023
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3. Early Results From GLASS-JWST. XVII: Building the First Galaxies -- Chapter 1. Star Formation Histories at 5<z < 7

Author

Dressler, A., Vulcani, B., Treu, T., Rieke, M., Burns, C., Calabro', A., Bonchi, A., Castellano, M., Fontana, A., Leethochawalit, N., Mason, C., Merlin, E., Morishita, T., Paris, D., Mercurio, A., Nanayakkara, T., Poggianti, B. M., Santini, P., Wang, X., Misselt, K., Stark, D. P., and Willmer, C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

JWST observations of high redshift galaxies are used to measure their star formation histories - the buildup of stellar mass in the earliest galaxies. Here we use a novel analysis program, SEDz*, to compare near-IR spectral energy distributions for galaxies with redshifts 5 < z < 7 to combinations of stellar population templates evolved from z = 12. We exploit NIRCam imaging in 7 wide bands covering 1-5 mu m, taken in the context of the GLASS-JWST-ERS program, and use SEDz* to solve for well-constrained star formation histories for 24 exemplary galaxies. In this first look we find a variety of histories, from long, continuous star formation over 5 < z < 12 to short but intense starbursts - sometimes repeating, and, most commonly, contiguous mass buildup lasting ~ 0.5 Myr,possibly the seeds of today's typical, M* galaxies., Comment: ApJL in press (accepted on October 30, 2022)

Published
2022
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4. TRUST I: A 3D externally illuminated slab benchmark for dust radiative transfer

Author

Gordon, K. D., Baes, M., Bianchi, S., Camps, P., Juvela, M., Kuiper, R., Lunttila, T., Misselt, K. A., Natale, G., Robitaille, T., and Steinacker, J.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The radiative transport of photons through arbitrary three-dimensional (3D) structures of dust is a challenging problem due to the anisotropic scattering of dust grains and strong coupling between different spatial regions. The radiative transfer problem in 3D is solved using Monte Carlo or Ray Tracing techniques as no full analytic solution exists for the true 3D structures. We provide the first 3D dust radiative transfer benchmark composed of a slab of dust with uniform density externally illuminated by a star. This simple 3D benchmark is explicitly formulated to provide tests of the different components of the radiative transfer problem including dust absorption, scattering, and emission. This benchmark includes models with a range of dust optical depths fully probing cases that are optically thin at all wavelengths to optically thick at most wavelengths. This benchmark includes solutions for the full dust emission including single photon (stochastic) heating as well as two simplifying approximations: One where all grains are considered in equilibrium with the radiation field and one where the emission is from a single effective grain with size-distribution-averaged properties. A total of six Monte Carlo codes and one Ray Tracing code provide solutions to this benchmark. Comparison of the results revealed that the global SEDs are consistent on average to a few percent for all but the scattered stellar flux at very high optical depths. The image results are consistent within 10%, again except for the stellar scattered flux at very high optical depths. The lack of agreement between different codes of the scattered flux at high optical depths is quantified for the first time. We provide the first 3D dust radiative transfer benchmark and validate the accuracy of this benchmark through comparisons between multiple independent codes and detailed convergence tests., Comment: 21 pages, 18 figures, Astronomy & Astrophysics, in press

Published
2017
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5. Benchmarking the calculation of stochastic heating and emissivity of dust grains in the context of radiative transfer simulations

Author

Camps, P, Misselt, K, Bianchi, S, Lunttila, T, Pinte, C, Natale, G, Juvela, M, Fischera, J, Fitzgerald, MP, Gordon, K, Baes, M, and Steinacker, J

Subjects
radiation mechanisms: thermal, dust, extinction, infrared: ISM, radiative transfer, methods: numerical, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

Context. Thermal emission by stochastically heated dust grains (SHGs) plays an important role in the radiative transfer (RT) problem for a dusty medium. It is therefore essential to verify that RT codes properly calculate the dust emission before studying the effects of spatial distribution and other model parameters on the simulated observables. Aims. We define an appropriate problem for benchmarking dust emissivity calculations in the context of RT simulations, specifically including the emission from SHGs. Our aim is to provide a self-contained guide for implementors of such functionality and to offer insight into the effects of the various approximations and heuristics implemented by the participating codes to accelerate the calculations. Methods. The benchmark problem definition includes the optical and calorimetric material properties and the grain size distributions for a typical astronomical dust mixture with silicate, graphite, and PAH components. It also includes a series of analytically defined radiation fields to which the dust population is to be exposed and instructions for the desired output. We processed this problem using six RT codes participating in this benchmark effort and compared the results to a reference solution computed with the publicly available dust emission code DustEM. Results. The participating codes implement different heuristics to keep the calculation time at an acceptable level.We study the effects of these mechanisms on the calculated solutions and report on the level of (dis)agreement between the participating codes. For all but the most extreme input fields, we find agreement within 10% across the important wavelength range 3 μm ≤1000 μm. Conclusions. We conclude that the relevant modules in RT codes can and do produce fairly consistent results for the emissivity spectra of SHGs. This work can serve as a reference for implementors of dust RT codes, and it will pave the way for a more extensive benchmark effort focusing on the RT aspects of the various codes.

Published
2015

6. The extremely sharp transition between molecular and ionized gas in the Horsehead nebula

Author

Hernández-Vera, C., primary, Guzmán, V. V., additional, Goicoechea, J. R., additional, Maillard, V., additional, Pety, J., additional, Le Petit, F., additional, Gerin, M., additional, Bron, E., additional, Roueff, E., additional, Abergel, A., additional, Schirmer, T., additional, Carpenter, J., additional, Gratier, P., additional, Gordon, K., additional, and Misselt, K., additional

Published
2023
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8. The extremely sharp transition between molecular and ionized gas in the Horsehead nebula

Author

Agencia Nacional de Investigación y Desarrollo (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Ministerio de Ciencia e Innovación (España), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Hernández-Vera, C. [0009-0009-2320-7243], Guzmán, V. V. [0000-0003-4784-3040], Goicoechea, Javier R. [0000-0001-7046-4319], #NODATA#, Le Petit, F. [0000-0001-8738-6724], Gerin, M. [0000-0002-2418-7952], Bron, E. [0000-0003-1532-7818], Roueff, E. [0000-0002-4949-8562], Schirmer, T. [0000-0002-8086-4890], Carpenter, J. [0000-0003-2251-0602], Gratier, P. [0000-0002-6636-4304], Hernández-Vera, C., Guzmán, V. V., Goicoechea, Javier R., Maillard, V., Pety, J., Le Petit, F., Gerin, M., Bron, E., Roueff, E., Abergel, A., Schirmer, T., Carpenter, J., Gratier, P., Gordon, K., Misselt, K., Agencia Nacional de Investigación y Desarrollo (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Ministerio de Ciencia e Innovación (España), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Hernández-Vera, C. [0009-0009-2320-7243], Guzmán, V. V. [0000-0003-4784-3040], Goicoechea, Javier R. [0000-0001-7046-4319], #NODATA#, Le Petit, F. [0000-0001-8738-6724], Gerin, M. [0000-0002-2418-7952], Bron, E. [0000-0003-1532-7818], Roueff, E. [0000-0002-4949-8562], Schirmer, T. [0000-0002-8086-4890], Carpenter, J. [0000-0003-2251-0602], Gratier, P. [0000-0002-6636-4304], Hernández-Vera, C., Guzmán, V. V., Goicoechea, Javier R., Maillard, V., Pety, J., Le Petit, F., Gerin, M., Bron, E., Roueff, E., Abergel, A., Schirmer, T., Carpenter, J., Gratier, P., Gordon, K., and Misselt, K.

Abstract

(Abridged) Massive stars can determine the evolution of molecular clouds with their strong ultraviolet (UV) radiation fields. Moreover, UV radiation is relevant in setting the thermal gas pressure in star-forming clouds, whose influence can extend from the rims of molecular clouds to entire star-forming galaxies. Probing the fundamental structure of nearby molecular clouds is therefore crucial to understand how massive stars shape their surrounding medium and how fast molecular clouds are destroyed, specifically at their UV-illuminated edges, where models predict an intermediate zone of neutral atomic gas between the molecular cloud and the surrounding ionized gas whose size is directly related to the exposed physical conditions. We present the highest angular resolution (~$0.5$", corresponding to $207$ au) and velocity-resolved images of the molecular gas emission in the Horsehead nebula, using CO J=3-2 and HCO$^+$ J=4-3 observations with ALMA. We find that CO and HCO$^+$ are present at the edge of the cloud, very close to the ionization (H$^+$/H) and dissociation fronts (H/H$_2$), suggesting a very thin layer of neutral atomic gas (<$650$ au) and a small amount of CO-dark gas ($A_V=0.006-0.26$ mag) for stellar UV illumination conditions typical of molecular clouds in the Milky Way. The new ALMA observations reveal a web of molecular gas filaments with an estimated thermal gas pressure of $P_{\mathrm{th}} = (2.3 - 4.0) \times 10^6$ K cm$^{-3}$, and the presence of a steep density gradient at the cloud edge that can be well explained by stationary isobaric PDR models with pressures consistent with our estimations. However, in the HII region and PDR interface, we find $P_{\mathrm{th,PDR}} > P_{\mathrm{th,HII}}$, suggesting the gas is slightly compressed. Therefore, dynamical effects cannot be completely ruled out and even higher angular observations will be needed to unveil their role.

Published
2023

9. Early Results From GLASS-JWST. XVII: Building the First Galaxies -- Chapter 1. Star Formation Histories at 5

Author

Dressler, A., Vulcani, B., Treu, T., Rieke, M., Burns, C., Calabro', A., Bonchi, A., Castellano, M., Fontana, A., Leethochawalit, N., Mason, C., Merlin, E., Morishita, T., Paris, D., Mercurio, A., Nanayakkara, T., Poggianti, B. M., Santini, P., Wang, X., Misselt, K., Stark, D. P., and Willmer, C.

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

JWST observations of high redshift galaxies are used to measure their star formation histories - the buildup of stellar mass in the earliest galaxies. Here we use a novel analysis program, SEDz*, to compare near-IR spectral energy distributions for galaxies with redshifts 5 < z < 7 to combinations of stellar population templates evolved from z = 12. We exploit NIRCam imaging in 7 wide bands covering 1-5 mu m, taken in the context of the GLASS-JWST-ERS program, and use SEDz* to solve for well-constrained star formation histories for 24 exemplary galaxies. In this first look we find a variety of histories, from long, continuous star formation over 5 < z < 12 to short but intense starbursts - sometimes repeating, and, most commonly, contiguous mass buildup lasting ~ 0.5 Myr,possibly the seeds of today's typical, M* galaxies., ApJL in press (accepted on October 30, 2022)

Published
2022
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10. Identification of luminous infrared galaxies at 1

Author

Floc'h, E, Perez-Gonzalez, P, Rieke, G, Papovich, C, Huang, J, Barmby, P, Dole, H, Egami, E, Alonso-Herrero, A, Wilson, G, Miyazaki, S, Rigby, JR, Bei, L, Blaylock, M, Engelbracht, C, Fazio, G, Frayer, D, Gordon, K, Hines, D, Misselt, K, Morrison, J, Muzerolle, J, Rieke, M, Rigopoulou, D, and Su, K

Abstract

We present preliminary results on 24micron detections of luminous infrared galaxies at z>1 with the Multiband Imaging Photometer for Spitzer (MIPS). Observations were performed in the Lockman Hole and the Extended Groth Strip (EGS), and were supplemented by data obtained with the Infrared Array Camera (IRAC) between 3 and 9microns. The positional accuracy of ~2arcsec for most MIPS/IRAC detections provides unambiguous identifications of their optical counterparts. Using spectroscopic redshifts from the Deep Extragalactic Evolutionary Probe survey, we identify 24micron sources at z>1 in the EGS, while the combination of the MIPS/IRAC observations with $BVRIJHK$ ancillary data in the Lockman Hole also shows very clear cases of galaxies with photometric redshifts at 1=M*) galaxy counterparts. It is the first time that this population of luminous objects is detected up to z~2.5 in the infrared. Our work demonstrates the ability of the MIPS instrument to probe the dusty Universe at very high redshift, and illustrates how the forthcoming Spitzer deep surveys will offer a unique opportunity to illuminate a dark side of cosmic history not explored by previous infrared experiments.

Published
2016

11. TRUST

Author

Gordon, K. D., primary, Baes, M., additional, Bianchi, S., additional, Camps, P., additional, Juvela, M., additional, Kuiper, R., additional, Lunttila, T., additional, Misselt, K. A., additional, Natale, G., additional, Robitaille, T., additional, and Steinacker, J., additional

Published
2017
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13. ERRATUM: “THE HERSCHEL INVENTORY OF THE AGENTS OF GALAXY EVOLUTION (HERITAGE) IN THE MAGELLANIC CLOUDS, A HERSCHEL OPEN TIME KEY PROGRAM” (2013, AJ, 146, 62)

Author

Meixner, M., primary, Panuzzo, P., additional, Roman-Duval, J., additional, Engelbracht, C., additional, Babler, B., additional, Seale, J., additional, Hony, S., additional, Montiel, E., additional, Sauvage, M., additional, Gordon, K., additional, Misselt, K., additional, Okumura, K., additional, Chanial, P., additional, Beck, T., additional, Bernard, J.-P., additional, Bolatto, A., additional, Bot, C., additional, Boyer, M. L., additional, Carlson, L. R., additional, Clayton, G. C., additional, Chen, C.-H. R., additional, Cormier, D., additional, Fukui, Y., additional, Galametz, M., additional, Galliano, F., additional, Hora, J. L., additional, Hughes, A., additional, Indebetouw, R., additional, Israel, F. P., additional, Kawamura, A., additional, Kemper, F., additional, Kim, S., additional, Kwon, E., additional, Lebouteiller, V., additional, Li, A., additional, Long, K. S., additional, Madden, S. C., additional, Matsuura, M., additional, Muller, E., additional, Oliveira, J. M., additional, Onishi, T., additional, Otsuka, M., additional, Paradis, D., additional, Poglitsch, A., additional, Reach, W. T., additional, Robitaille, T. P., additional, Rubio, M., additional, Sargent, B., additional, Sewiło, M., additional, Skibba, R., additional, Smith, L. J., additional, Srinivasan, S., additional, Tielens, A. G. G. M., additional, van Loon, J. Th., additional, and Whitney, B., additional

Published
2015
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14. Two NIRCam Channels are Better than One: How JWSTCan Do More Science with NIRCam's Short-wavelength Dispersed Hartmann Sensor

Author

Schlawin, E., Rieke, M., Leisenring, J., Walker, L. M., Fraine, J., Kelly, D., Misselt, K., Greene, T., Line, M., Lewis, N., and Stansberry, J.

Abstract

The James Webb Space Telescope(JWST) offers unprecedented sensitivity, stability, and wavelength coverage for transiting exoplanet studies, opening up new avenues for measuring atmospheric abundances, structure, and temperature profiles. Taking full advantage of JWSTspectroscopy of planets from 0.6 to 28 ?m, however, will require many observations with a combination of the NIRISS, NIRCam, NIRSpec, and MIRI instruments. In this white paper, we discuss a new NIRCam mode (not yet approved or implemented) that can reduce the number of necessary observations to cover the 1.0-5.0 ?m wavelength range. Even though NIRCam was designed primarily as an imager, it also includes several grisms for phasing and aligning JWST's 18 hexagonal mirror segments. NIRCam's long-wavelength channel includes grisms that cover 2.4-5.0 ?m with a resolving power of R= 1200-1550 using two separate configurations. The long-wavelength grisms have already been approved for science operations, including wide field and single object (time series) slitless spectroscopy. We propose a new mode that will simultaneously measure spectra for science targets in the 1.0-2.0 ?m range using NIRCam's short-wavelength channel. This mode, if approved, would take advantage of NIRCam's Dispersed Hartmann Sensor (DHS), which produces 10 spatially separated spectra per source at R? 300. We discuss the added benefit of the DHS in constraining abundances in exoplanet atmospheres as well as its ability to observe the brightest systems. The DHS essentially comes for free (at no time cost) with any NIRCam long-wavelength grism observation, but the detector integration parameters have to be selected to ensure that the long-wavelength grism observations do not saturate and that JWSTdata volume downlink constraints are not violated. Combining both of NIRCam's channels will maximize the science potential of JWST, which is a limited life observatory.

Published
2017
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15. The Science Performance of JWST as Characterized in Commissioning

Author

Jane Rigby, Marshall Perrin, Michael McElwain, Randy Kimble, Scott Friedman, Matt Lallo, René Doyon, Lee Feinberg, Pierre Ferruit, Alistair Glasse, Marcia Rieke, George Rieke, Gillian Wright, Chris Willott, Knicole Colon, Stefanie Milam, Susan Neff, Christopher Stark, Jeff Valenti, Jim Abell, Faith Abney, Yasin Abul-Huda, D. Scott Acton, Evan Adams, David Adler, Jonathan Aguilar, Nasif Ahmed, Loïc Albert, Stacey Alberts, David Aldridge, Marsha Allen, Martin Altenburg, Javier Álvarez-Márquez, Catarina Alves de Oliveira, Greg Andersen, Harry Anderson, Sara Anderson, Ioannis Argyriou, Amber Armstrong, Santiago Arribas, Etienne Artigau, Amanda Arvai, Charles Atkinson, Gregory Bacon, Thomas Bair, Kimberly Banks, Jaclyn Barrientes, Bruce Barringer, Peter Bartosik, William Bast, Pierre Baudoz, Thomas Beatty, Katie Bechtold, Tracy Beck, Eddie Bergeron, Matthew Bergkoetter, Rachana Bhatawdekar, Stephan Birkmann, Ronald Blazek, Claire Blome, Anthony Boccaletti, Torsten Böker, John Boia, Nina Bonaventura, Nicholas Bond, Kari Bosley, Ray Boucarut, Matthew Bourque, Jeroen Bouwman, Gary Bower, Charles Bowers, Martha Boyer, Larry Bradley, Greg Brady, Hannah Braun, David Breda, Pamela Bresnahan, Stacey Bright, Christopher Britt, Asa Bromenschenkel, Brian Brooks, Keira Brooks, Bob Brown, Matthew Brown, Patricia Brown, Andy Bunker, Matthew Burger, Howard Bushouse, Steven Cale, Alex Cameron, Peter Cameron, Alicia Canipe, James Caplinger, Francis Caputo, Mihai Cara, Larkin Carey, Stefano Carniani, Maria Carrasquilla, Margaret Carruthers, Michael Case, Riggs Catherine, Don Chance, George Chapman, Stéphane Charlot, Brian Charlow, Pierre Chayer, Bin Chen, Brian Cherinka, Sarah Chichester, Zack Chilton, Taylor Chonis, Mark Clampin, Charles Clark, Kerry Clark, Dan Coe, Benee Coleman, Brian Comber, Tom Comeau, Dennis Connolly, James Cooper, Rachel Cooper, Eric Coppock, Matteo Correnti, Christophe Cossou, Alain Coulais, Laura Coyle, Misty Cracraft, Mirko Curti, Steven Cuturic, Katherine Davis, Michael Davis, Bruce Dean, Amy DeLisa, Wim deMeester, Nadia Dencheva, Nadezhda Dencheva, Joseph DePasquale, Jeremy Deschenes, Örs Hunor Detre, Rosa Diaz, Dan Dicken, Audrey DiFelice, Matthew Dillman, William Dixon, Jesse Doggett, Tom Donaldson, Rob Douglas, Kimberly DuPrie, Jean Dupuis, John Durning, Nilufar Easmin, Weston Eck, Chinwe Edeani, Eiichi Egami, Ralf Ehrenwinkler, Jonathan Eisenhamer, Michael Eisenhower, Michelle Elie, James Elliott, Kyle Elliott, Tracy Ellis, Michael Engesser, Nestor Espinoza, Odessa Etienne, Mireya Etxaluze, Patrick Falini, Matthew Feeney, Malcolm Ferry, Joseph Filippazzo, Brian Fincham, Mees Fix, Nicolas Flagey, Michael Florian, Jim Flynn, Erin Fontanella, Terrance Ford, Peter Forshay, Ori Fox, David Franz, Henry Fu, Alexander Fullerton, Sergey Galkin, Anthony Galyer, Macarena García Marín, Jonathan P. Gardner, Lisa Gardner, Dennis Garland, Bruce Garrett, Danny Gasman, Andras Gaspar, Daniel Gaudreau, Peter Gauthier, Vincent Geers, Paul Geithner, Mario Gennaro, Giovanna Giardino, Julien Girard, Mark Giuliano, Kirk Glassmire, Adrian Glauser, Stuart Glazer, John Godfrey, David Golimowski, David Gollnitz, Fan Gong, Shireen Gonzaga, Michael Gordon, Karl Gordon, Paul Goudfrooij, Thomas Greene, Matthew Greenhouse, Stefano Grimaldi, Andrew Groebner, Timothy Grundy, Pierre Guillard, Irvin Gutman, Kong Q. Ha, Peter Haderlein, Andria Hagedorn, Kevin Hainline, Craig Haley, Maryam Hami, Forrest Hamilton, Heidi Hammel, Carl Hansen, Tom Harkins, Michael Harr, Jessica Hart, Quyen Hart, George Hartig, Ryan Hashimoto, Sujee Haskins, William Hathaway, Keith Havey, Brian Hayden, Karen Hecht, Chris Heller-Boyer, Caroline Henriques, Alaina Henry, Karl Hermann, Scarlin Hernandez, Brigette Hesman, Brian Hicks, Bryan Hilbert, Dean Hines, Melissa Hoffman, Sherie Holfeltz, Bryan J. Holler, Jennifer Hoppa, Kyle Hott, Joseph M. Howard, Rick Howard, Alexander Hunter, David Hunter, Brendan Hurst, Bernd Husemann, Leah Hustak, Luminita Ilinca Ignat, Garth Illingworth, Sandra Irish, Wallace Jackson, Amir Jahromi, Peter Jakobsen, LeAndrea James, Bryan James, William Januszewski, Ann Jenkins, Hussein Jirdeh, Phillip Johnson, Timothy Johnson, Vicki Jones, Ron Jones, Danny Jones, Olivia Jones, Ian Jordan, Margaret Jordan, Sarah Jurczyk, Alden Jurling, Catherine Kaleida, Phillip Kalmanson, Jens Kammerer, Huijo Kang, Shaw-Hong Kao, Diane Karakla, Patrick Kavanagh, Doug Kelly, Sarah Kendrew, Herbert Kennedy, Deborah Kenny, Ritva Keski-kuha, Charles Keyes, Richard Kidwell, Wayne Kinzel, Jeff Kirk, Mark Kirkpatrick, Danielle Kirshenblat, Pamela Klaassen, Bryan Knapp, J. Scott Knight, Perry Knollenberg, Robert Koehler, Anton Koekemoer, Aiden Kovacs, Trey Kulp, Nimisha Kumari, Mark Kyprianou, Stephanie La Massa, Aurora Labador, Alvaro Labiano, Pierre-Olivier Lagage, Charles-Philippe Lajoie, Matthew Lallo, May Lam, Tracy Lamb, Scott Lambros, Richard Lampenfield, James Langston, Kirsten Larson, David Law, Jon Lawrence, David Lee, Jarron Leisenring, Kelly Lepo, Michael Leveille, Nancy Levenson, Marie Levine, Zena Levy, Dan Lewis, Hannah Lewis, Mattia Libralato, Paul Lightsey, Miranda Link, Lily Liu, Amy Lo, Alexandra Lockwood, Ryan Logue, Chris Long, Douglas Long, Charles Loomis, Marcos Lopez-Caniego, Jose Lorenzo Alvarez, Jennifer Love-Pruitt, Adrian Lucy, Nora Luetzgendorf, Peiman Maghami, Roberto Maiolino, Melissa Major, Sunita Malla, Eliot Malumuth, Elena Manjavacas, Crystal Mannfolk, Amanda Marrione, Anthony Marston, André Martel, Marc Maschmann, Gregory Masci, Michaela Masciarelli, Michael Maszkiewicz, John Mather, Kenny McKenzie, Brian McLean, Matthew McMaster, Katie Melbourne, Marcio Meléndez, Michael Menzel, Kaiya Merz, Michele Meyett, Luis Meza, Cherie Miskey, Karl Misselt, Christopher Moller, Jane Morrison, Ernie Morse, Harvey Moseley, Gary Mosier, Matt Mountain, Julio Mueckay, Michael Mueller, Susan Mullally, Jess Murphy, Katherine Murray, Claire Murray, David Mustelier, James Muzerolle, Matthew Mycroft, Richard Myers, Kaila Myrick, Shashvat Nanavati, Elizabeth Nance, Omnarayani Nayak, Bret Naylor, Edmund Nelan, Bryony Nickson, Alethea Nielson, Maria Nieto-Santisteban, Nikolay Nikolov, Alberto Noriega-Crespo, Brian O’Shaughnessy, Brian O’Sullivan, William Ochs, Patrick Ogle, Brenda Oleszczuk, Joseph Olmsted, Shannon Osborne, Richard Ottens, Beverly Owens, Camilla Pacifici, Alyssa Pagan, James Page, Sang Park, Keith Parrish, Polychronis Patapis, Lee Paul, Tyler Pauly, Cheryl Pavlovsky, Andrew Pedder, Matthew Peek, Maria Pena-Guerrero, Konstantin Penanen, Yesenia Perez, Michele Perna, Beth Perriello, Kevin Phillips, Martin Pietraszkiewicz, Jean-Paul Pinaud, Norbert Pirzkal, Joseph Pitman, Aidan Piwowar, Vera Platais, Danielle Player, Rachel Plesha, Joe Pollizi, Ethan Polster, Klaus Pontoppidan, Blair Porterfield, Charles Proffitt, Laurent Pueyo, Christine Pulliam, Brian Quirt, Irma Quispe Neira, Rafael Ramos Alarcon, Leah Ramsay, Greg Rapp, Robert Rapp, Bernard Rauscher, Swara Ravindranath, Timothy Rawle, Michael Regan, Timothy A. 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Subjects
Science & Technology, Observatories, Infrared astronomy, Astronomical instrumentation, INFRARED SPECTROGRAPH NIRSPEC, FOS: Physical sciences, Astronomy and Astrophysics, Astronomy & Astrophysics, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, Physical Sciences, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

This paper characterizes the actual science performance of the James Webb Space Telescope (JWST), as determined from the six month commissioning period. We summarize the performance of the spacecraft, telescope, science instruments, and ground system, with an emphasis on differences from pre-launch expectations. Commissioning has made clear that JWST is fully capable of achieving the discoveries for which it was built. Moreover, almost across the board, the science performance of JWST is better than expected; in most cases, JWST will go deeper faster than expected. The telescope and instrument suite have demonstrated the sensitivity, stability, image quality, and spectral range that are necessary to transform our understanding of the cosmos through observations spanning from near-earth asteroids to the most distant galaxies., Comment: 5th version as accepted to PASP; 31 pages, 18 figures; https://iopscience.iop.org/article/10.1088/1538-3873/acb293

Published
2022
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