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14 results on '"WEBB-SPACE-TELESCOPE"'

1. Closing in on the sources of cosmic reionization:First results from the GLASS-JWST program

Author

Mascia, S., Pentericci, L., Calabro, A., Treu, T., Santini, P., Yang, L., Napolitano, L., Roberts-Borsani, G., Bergamini, P., Grillo, C., Rosati, P., Vulcani, B., Castellano, M., Boyett, K., Fontana, A., Glazebrook, K., Henry, A., Mason, C., Merlin, E., Morishita, T., Nanayakkara, T., Paris, D., Roy, N., Williams, H., Wang, X., Brammer, G., Bradac, M., Chen, W., Kelly, P. L., Koekemoer, A. M., Trenti, M., Windhorst, R. A., Mascia, S., Pentericci, L., Calabro, A., Treu, T., Santini, P., Yang, L., Napolitano, L., Roberts-Borsani, G., Bergamini, P., Grillo, C., Rosati, P., Vulcani, B., Castellano, M., Boyett, K., Fontana, A., Glazebrook, K., Henry, A., Mason, C., Merlin, E., Morishita, T., Nanayakkara, T., Paris, D., Roy, N., Williams, H., Wang, X., Brammer, G., Bradac, M., Chen, W., Kelly, P. L., Koekemoer, A. M., Trenti, M., and Windhorst, R. A.

Abstract

The escape fraction of Lyman-continuum (LyC) photons (f(esc)) is a key parameter for determining the sources of cosmic reionization at z >= 6. At these redshifts, owing to the opacity of the intergalactic medium, the LyC emission cannot be measured directly. However, LyC leakers during the epoch of reionization could be identified using indirect indicators that have been extensively tested at low and intermediate redshifts. These include a high [OIII]/[OII] flux ratio, high star-formation surface density, and compact sizes. In this work, we present observations of 29 4.5 = 6 have provided a substantial contribution to cosmic reionization.

Published
2023

2. MINDS. The Detection of (CO2)-C-13 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk

Author

Grant, Sierra L, van Dishoeck, Ewine F, Tabone, Benoit, Gasman, Danny, Henning, Thomas, Kamp, Inga, Guedel, Manuel, Lagage, Pierre-Olivier, Bettoni, Giulio, Perotti, Giulia, Christiaens, Valentin, Samland, Matthias, Arabhavi, Aditya M, Argyriou, Ioannis, Abergel, Alain, Absil, Olivier, Barrado, David, Boccaletti, Anthony, Bouwman, Jeroen, Garatti, Alessio Caratti O, Geers, Vincent, Glauser, Adrian M, Guadarrama, Rodrigo, Jang, Hyerin, Kanwar, Jayatee, Lahuis, Fred, Morales-Calderon, Maria, Mueller, Michael, Nehme, Cyrine, Olofsson, Goeran, Pantin, Eric, Pawellek, Nicole, Ray, Tom P, Rodgers-Lee, Donna, Scheithauer, Silvia, Schreiber, Juergen, Schwarz, Kamber, Temmink, Milou, Vandenbussche, Bart, Vlasblom, Marissa, Waters, LBFM, Wright, Gillian, Colina, Luis, Greve, Thomas R, Justannont, Kay, and Ostlin, Goeran

Subjects
Science & Technology, SPECTROSCOPY, PLANET-FORMING REGIONS, SPITZER SURVEY, Physical Sciences, WEBB-SPACE-TELESCOPE, WATER, LINE, MIDINFRARED MOLECULAR-EMISSION, SUBSTRUCTURES, LOW-MASS STARS, Astronomy & Astrophysics, YOUNG STELLAR OBJECTS
Abstract

ispartof: ASTROPHYSICAL JOURNAL LETTERS vol:947 issue:1 status: published

Published
2023

3. The Mid-infrared Instrument for JWST and Its In-flight Performance

Author

Gillian S. Wright, George H. Rieke, Alistair Glasse, Michael Ressler, Macarena García Marín, Jonathan Aguilar, Stacey Alberts, Javier Álvarez-Márquez, Ioannis Argyriou, Kimberly Banks, Pierre Baudoz, Anthony Boccaletti, Patrice Bouchet, Jeroen Bouwman, Bernard R. Brandl, David Breda, Stacey Bright, Steven Cale, Luis Colina, Christophe Cossou, Alain Coulais, Misty Cracraft, Wim De Meester, Daniel Dicken, Michael Engesser, Mireya Etxaluze, Ori D. Fox, Scott Friedman, Henry Fu, Danny Gasman, András Gáspár, René Gastaud, Vincent Geers, Adrian Michael Glauser, Karl D. Gordon, Thomas Greene, Thomas R. Greve, Timothy Grundy, Manuel Güdel, Pierre Guillard, Peter Haderlein, Ryan Hashimoto, Thomas Henning, Dean Hines, Bryan Holler, Örs Hunor Detre, Amir Jahromi, Bryan James, Olivia C. Jones, Kay Justtanont, Patrick Kavanagh, Sarah Kendrew, Pamela Klaassen, Oliver Krause, Alvaro Labiano, Pierre-Olivier Lagage, Scott Lambros, Kirsten Larson, David Law, David Lee, Mattia Libralato, Jose Lorenzo Alverez, Margaret Meixner, Jane Morrison, Migo Mueller, Katherine Murray, Matthew Mycroft, Richard Myers, Omnarayani Nayak, Bret Naylor, Bryony Nickson, Alberto Noriega-Crespo, Göran Östlin, Brian O’Sullivan, Richard Ottens, Polychronis Patapis, Konstantin Penanen, Martin Pietraszkiewicz, Tom Ray, Michael Regan, Anthony Roteliuk, Pierre Royer, Piyal Samara-Ratna, Bridget Samuelson, Beth A. Sargent, Silvia Scheithauer, Analyn Schneider, Jürgen Schreiber, Bryan Shaughnessy, Even Sheehan, Irene Shivaei, G. C. Sloan, Laszlo Tamas, Kelly Teague, Tea Temim, Tuomo Tikkanen, Samuel Tustain, Ewine F. van Dishoeck, Bart Vandenbussche, Mark Weilert, Paul Whitehouse, and Schuyler Wolff

Subjects
CALIBRATION, 4-QUADRANT PHASE MASK, Science & Technology, Space and Planetary Science, Physical Sciences, WEBB-SPACE-TELESCOPE, Astronomy and Astrophysics, Astronomy & Astrophysics
Abstract

The Mid-Infrared Instrument (MIRI) extends the reach of the James Webb Space Telescope (JWST) to 28.5 μm. It provides subarcsecond-resolution imaging, high sensitivity coronagraphy, and spectroscopy at resolutions of λ/Δλ ∼ 100–3500, with the high-resolution mode employing an integral field unit to provide spatial data cubes. The resulting broad suite of capabilities will enable huge advances in studies over this wavelength range. This overview describes the history of acquiring this capability for JWST. It discusses the basic attributes of the instrument optics, the detector arrays, and the cryocooler that keeps everything at approximately 7 K. It gives a short description of the data pipeline and of the instrument performance demonstrated during JWST commissioning. The bottom line is that the telescope and MIRI are both operating to the standards set by pre-launch predictions, and all of the MIRI capabilities are operating at, or even a bit better than, the level that had been expected. The paper is also designed to act as a roadmap to more detailed papers on different aspects of MIRI.

Published
2023
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4. Closing in on the sources of cosmic reionization: first results from the GLASS-JWST program

Author

S. Mascia, L. Pentericci, A. Calabrò, T. Treu, P. Santini, L. Yang, L. Napolitano, G. Roberts-Borsani, P. Bergamini, C. Grillo, P. Rosati, B. Vulcani, M. Castellano, K. Boyett, A. Fontana, K. Glazebrook, A. Henry, C. Mason, E. Merlin, T. Morishita, T. Nanayakkara, D. Paris, N. Roy, H. Williams, X. Wang, G. Brammer, M. Bradač, W. Chen, P. L. Kelly, A. M. Koekemoer, M. Trenti, and R. A. Windhorst

Subjects
CONTINUUM EMISSION, formation [galaxies], SPECTRAL SIGNATURES, WEBB-SPACE-TELESCOPE, FOS: Physical sciences, Astronomy and Astrophysics, early Universe, Astrophysics - Astrophysics of Galaxies, HIGH-REDSHIFT GALAXIES, LYMAN-BREAK GALAXIES, clusters: intracluster medium [galaxies], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), STAR-FORMING GALAXIES, IONIZING-RADIATION, C IV EMISSION, evolution [galaxies], STELLAR POPULATION, LY-ALPHA EMISSION
Abstract

The escape fraction of Lyman-continuum (LyC) photons ($f_{esc}$) is a key parameter for determining the sources of cosmic reionization at $z\geq 6$. At these redshifts, owing to the opacity of the intergalactic medium, the LyC emission cannot be measured directly. However, LyC leakers during the epoch of reionization could be identified using indirect indicators that have been extensively tested at low and intermediate redshifts. These include a high [OIII]/[OII] flux ratio, high star-formation surface density, and compact sizes. In this work, we present observations of 29 $4.5 \leq z \leq 8$ gravitationally lensed galaxies in the Abell 2744 cluster field. From a combined analysis of JWST-NIRSpec and NIRCam data, we accurately derived their physical and spectroscopic properties: our galaxies have low masses $(\log(M_\star)\sim 8.5)$, blue UV spectral slopes ($\beta \sim -2.1$), compact sizes ($r_e \sim 0.3-0.5$ kpc), and high [OIII]/[OII] flux ratios. We confirm that these properties are similar to those characterizing low-redshift LyC leakers. Indirectly inferring the fraction of escaping ionizing photons, we find that more than 80% of our galaxies have predicted $f_{esc}$ values larger than 0.05, indicating that they would be considered leakers. The average predicted $f_{esc}$ value of our sample is 0.12, suggesting that similar galaxies at $z\geq 6$ have provided a substantial contribution to cosmic reionization., Comment: Accepted for publication in the 4. Extragalactic astronomy section of A&A, 12 pages, 8 figures

Published
2023
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5. First JWST observations of a gravitational lens Mass model from new multiple images with near-infrared observations of SMACS J0723.3-7327

Author

Caminha, G. B., Suyu, S. H., Mercurio, A., Brammer, G., Bergamini, P., Acebron, A., Vanzella, E., Caminha, G. B., Suyu, S. H., Mercurio, A., Brammer, G., Bergamini, P., Acebron, A., and Vanzella, E.

Abstract

We present our lens mass model of SMACS J0723.3-7327, the first strong gravitational lens observed by the James Webb Space Telescope (JWST). We use data from the Hubble Space Telescope and the Multi Unit Spectroscopic Explorer (MUSE) to build our 'pre-JWST' lens model and then refine it with newly available JWST near-infrared imaging in our JWST model. To reproduce the positions of all multiple lensed images with good accuracy, the adopted mass parameterisation consists of one cluster-scale component, accounting mainly for the dark matter distribution, the galaxy cluster members, and an external shear component. The pre-JWST model has, as constraints, 19 multiple images from six background sources, of which four have secure spectroscopic redshift measurements from this work. The JWST model has more than twice the number of constraints: 30 additional multiple images from another 11 lensed sources. Both models can reproduce the multiple image positions very well, with a delta(rms) of 0 ''.39 and 0 ''.51 for the pre-JWST and JWST models, respectively. The total mass estimates within a radius of 128 kpc (roughly the Einstein radius) are 7.9(-0.2)(+0,3) x 10(13) M-circle dot and 8.7(-0.2)(+0.2) x 10(13) M-circle dot for the pre-JWST and JWST models, respectively. We predict with our mass models the redshifts of the newly detected JWST sources, which is crucial information, especially for systems without spectroscopic measurements, for further studies and follow-up observations. Interestingly, one family detected with JWST is found to be at a very high redshift, z > 7.5 (68% confidence level), and with one image that has a lensing magnification of vertical bar mu vertical bar = 9.5(-0.8)(+0.9), making it an interesting case for future studies. The lens models, including magnification maps and redshifts estimated from the model, are made publicly available, along with the full spectroscopic redshift catalogue from MUSE.

Published
2022

6. First JWST observations of a gravitational lens: Mass model from new multiple images with near-infrared observations of SMACS J0723.3-7327

Author

Caminha, G.B., Suyu, S.H., Mercurio, A., Brammer, G., Bergamini, P., Vanzella, E., and Acebron Munoz, A.

Subjects
COSMOLOGICAL CONSTRAINTS, SAMPLE, Strong Gravitational lensing, WEBB-SPACE-TELESCOPE, FOS: Physical sciences, Galaxy clusters, clusters: individual: SMACS J0723.3-7327 [galaxies], Astronomy and Astrophysics, MIDINFRARED INSTRUMENT, Astrophysics - Astrophysics of Galaxies, dark matter, PRECISE, Settore FIS/05 - Astronomia e Astrofisica, SMACSJ0723.3−7327, Space and Planetary Science, strong [gravitational lensing], Astrophysics of Galaxies (astro-ph.GA), MACS, GALAXY CLUSTERS, HUBBLE CONSTANT
Abstract

We present our lens mass model of SMACS J0723, the first strong gravitational lens observed by the James Webb Space Telescope (JWST). We use data from the Hubble Space Telescope and Multi Unit Spectroscopic Explorer (MUSE) to build our 'pre-JWST' lens model, and refine it with newly available JWST near-infrared imaging in our JWST model. To reproduce the positions of all multiple lensed images with good accuracy, the adopted mass parameterization consists of one cluster-scale component, accounting mainly for the dark matter distribution, the galaxy cluster members and an external shear component. The pre-JWST model has, as constraints, 19 multiple images from six background sources, of which four have secure spectroscopic redshift measurements from this work. The JWST model has more than twice the number of constraints, 30 additional multiple images from another eleven lensed sources. Both models can reproduce very well the multiple image positions with a $\delta_{rms}$ of $0.39''$ and $0.51''$, for the pre-JWST and JWST models, respectively. The total mass estimates within a radius of 128~kpc (~ the Einstein radius) are $7.9_{-0.2}^{+0.3}\times 10^{13}\rm M_{\odot}$ and $8.7_{-0.2}^{+0.2}\times 10^{13}\rm M_{\odot}$, for the pre-JWST and JWST models, respectively. We predict with our mass models the redshifts of the newly detected JWST sources, which are crucial information for systems without spectroscopic measurements for further studies and follow-up observations. Interestingly, one family detected with JWST is found to be at a very high redshift, $z>7.5$ (68% confidence level) and with one image having lensing magnification of $|\mu|=9.5_{-0.8}^{+0.9}$, making it an interesting case for future studies. The lens models, including magnification maps and redshifts estimated from the model are made publicly available, along with the full spectroscopic redshift catalogue from MUSE., Comment: 5 pages, 2 figures, 1 table, plus appendix. Published in A&A Letters. Lens model and redshift catalogue available at: http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/666/L9

Published
2022
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7. Nuclear high-ionisation outflow in the Compton-thick AGN NGC 6552 as seen by the JWST mid-infrared instrument

Author

Álvarez-Márquez, J., Labiano, A., Guillard, P., Dicken, D., Argyriou, I., Patapis, P., Law, D. R., Kavanagh, P. J., Larson, K. L., Gasman, D., Mueller, M., Alberts, A., Brandl, B. R., Colina, L., García-Marín, M., Jones, O. C., Noriega-Crespo, A., Shivaei, I., Temim, T., and Wright, G. S.

Subjects
ACTIVE GALACTIC NUCLEI, galaxies: active, FOS: Physical sciences, LINES, Astronomy & Astrophysics, IONIZED-GAS, instrumentation: high angular resolution, Seyfert [galaxies], kinematics and dynamics [galaxies], ABSORPTION, KINEMATICS, Instrumentation and Methods for Astrophysics (astro-ph.IM), galaxies: kinematics and dynamics, instrumentation: spectrographs, MOLECULAR-HYDROGEN EMISSION, Science & Technology, ISM [galaxies], spectrographs, galaxies: Seyfert, galaxies: ISM, galaxies: kinematics and dynamics [instrumentation], WEBB-SPACE-TELESCOPE, Astronomy and Astrophysics, SUPERMASSIVE BLACK-HOLE, Astrophysics - Astrophysics of Galaxies, GALAXIES, EXTINCTION, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, active [galaxies], Astrophysics - Instrumentation and Methods for Astrophysics, high angular resolution [instrumentation], spectrographs [instrumentation]
Abstract

Context. During the commissioning of the James Webb Space Telescope (JWST), the mid-infrared instrument (MIRI) observed NGC 6552 with the MIRI Imager and the Medium-Resolution Spectrograph (MRS). NGC 6552 is an active galactic nucleus (AGN) at a redshift of 0.0266 (DL = 120 Mpc) classified as a Seyfert 2 nucleus in the optical and Compton-thick AGN in the X-ray. Aims. This work exemplifies and demonstrates the MRS capabilities to study the mid-infrared (mid-IR) spectra and characterise the physical conditions and kinematics of the ionised and molecular gas in the nuclear regions of nearby galaxies. Methods. MIRI Imager observations covers the full NGC 6552 galaxy at 5.6 μm. MRS observations covers its nuclear region (3.6 × 4.3 kpc at 17.7-27.9 μm) in a wavelength range between 4.9 and 27.9 μm. These observations were obtained with the aim to investigate the persistence of the MIRI detectors (residual signal left from previous bright source observations). However, NGC 6552 observations demonstrate the performance and power of the MIRI instrument even with a non-optimal observational strategy. Results. We obtained the nuclear, circumnuclear, and central mid-IR spectra of NGC 6552. They provide the first clear observational evidence for a nuclear outflow in NGC 6552. The outflow contributes to 67±7% of the total line flux independent of the ionisation potential (27-187 eV) and critical densities (104-4 × 106 cm-3), showing an average blue-shifted peak velocity of -127±45 km s-1 and an outflow maximal velocity of 698±80 km s-1. Since the mid-IR photons penetrate dusty regions as efficiently as X-ray keV photons, we interpret these results as the evidence for a highly ionised, non-stratified, AGN-powered, and fast outflowing gas in a low density environment (few 103 cm-3) located very close (< 0.2 kpc) to the Compton-thick AGN. Nine pure rotational molecular Hydrogen lines are detected and spectrally resolved, and exhibit symmetric Gaussian profiles, consistent with the galactic rotation, and with no evidence of outflowing H2 material. We detect a warm H2 mass of 1.9 ± 1.1 × 107 M⊙ in the central region (1.8 kpc in diameter) of the galaxy, with almost 30% of that mass in the circumnuclear region. Line ratios confirm that NGC 6552 has a Seyfert nucleus with a black hole mass estimated in the range of 0.6-6 million solar masses. Conclusions. This work demonstrates the power of the newly commissioned MIRI Medium Resolution Spectrograph to reveal new insights in the kinematics and ionisation state of the interstellar medium around the dusty nuclear regions of nearby active galaxies., Astronomy & Astrophysics, 672, ISSN:0004-6361, ISSN:1432-0746

Published
2023
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8. Direct emission spectroscopy of exoplanets with the medium resolution imaging spectrometer on board JWST MIRI

Author

N. P. Whiteford, P. Mollière, E. Nasedkin, I. Argyriou, Adrian Glauser, Sascha P. Quanz, Alistair Glasse, G. Cugno, and Polychronis Patapis

Subjects
Point spread function, planets and satellites, BROWN DWARFS, data analysis, MU-M, Imaging spectrometer, FOS: Physical sciences, MIDINFRARED INSTRUMENT, Astrophysics, Astronomy & Astrophysics, imaging spectroscopy, Computer Science::Digital Libraries, 51 ERI B, Spectral line, methods, PLANETARY-MASS COMPANION, gaseous planets, Planet, ATMOSPHERIC CHARACTERIZATION, Radiative transfer, Emission spectrum, Instrumentation and Methods for Astrophysics (astro-ph.IM), planetary systems, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Science & Technology, Spectrometer, HR 8799 B, Astrophysics::Instrumentation and Methods for Astrophysics, WEBB-SPACE-TELESCOPE, Astronomy and Astrophysics, Physics::History of Physics, Exoplanet, GIANT PLANETS, Space and Planetary Science, Physical Sciences, infrared, atmospheres, 1ST LIGHT, Astrophysics::Earth and Planetary Astrophysics, techniques, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Medium Resolution Spectrometer on board JWST/MIRI will give access to mid-IR spectra while retaining spatial information. With the unparalleled sensitivity of JWST and the MIRI detectors, the MRS has the potential to revolutionise our understanding of giant exoplanet atmospheres. Molecular mapping is a promising detection and characterisation technique used to study the spectra of directly imaged exoplanets. We aim to examine the feasibility and application of this technique to MRS observations. We used the instrument simulator MIRISIM to create mock observations of resolved star and exoplanet systems. As an input for the simulator, we used stellar and planet parameters from literature, with the planet spectrum being modelled with the radiative transfer code petitRADTRANS. After processing the raw data with the JWST pipeline, we high pass filter the data to account for the stellar point spread function, and used a forward modelling approach to detect the companions and constrain the chemical composition of their atmospheres through their molecular signatures. We identified limiting factors in spectroscopic characterisation of directly imaged exoplanets with the MRS and simulated observations of two representative systems, HR8799 and GJ504. In both systems, we could detect the presence of multiple molecules that were present in the input model of their atmospheres. We used two different approaches with single molecule forward models, used in literature, that are sensitive to detecting mainly H$_2$O, CO, CH$_4$, and NH$_3$, and a log-likelihood ratio test that uses full atmosphere forward models and is sensitive to a larger number of less dominant molecular species. We show that the MIRI MRS can be used to characterise widely separated giant exoplanets in the mid-IR using molecular mapping., 18 pages, 10 figures. Accepted for publication in Astronomy & Astrophysics

Published
2022
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9. Wavelength calibration and resolving power of the JWST MIRI Medium Resolution Spectrometer

Author

Adrian Glauser, J. Alvarez-Marquez, David R. Law, Bart Vandenbussche, Bernhard R. Brandl, Polychronis Patapis, B. Shaughnessy, Alistair Glasse, Alvaro Labiano, Fred Lahuis, Michael Mueller, Pierre Royer, Kay Justtanont, Alberto Noriega-Crespo, Juan Rafael Martínez-Galarza, and Ioannis Argyriou

Subjects
Physics::Instrumentation and Detectors, FOS: Physical sciences, Instrumentation: spectrographs, MIDINFRARED INSTRUMENT, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, Spectral line, Infrared: general, THERMAL-EXPANSION MEASUREMENTS, Integral field spectrograph, Optics, Methods: data analysis, data analysis [methods], Instrumentation: detectors, Spectral resolution, Spectroscopy, Instrumentation and Methods for Astrophysics (astro-ph.IM), general [infrared], TEMPERATURE, Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), Physics, Science & Technology, detectors [instrumentation], Spectrometer, Pixel, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, WEBB-SPACE-TELESCOPE, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Physics::History of Physics, Wavelength, IV, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, Astrophysics - Instrumentation and Methods for Astrophysics, business, Fabry–Pérot interferometer, spectrographs [instrumentation], Astrophysics - Earth and Planetary Astrophysics
Abstract

The Mid-Infrared Instrument (MIRI) on-board JWST will provide imaging, coronagraphy, low-resolution spectroscopy and medium-resolution spectroscopy at unprecedented sensitivity levels in the mid-infrared wavelength range. The Medium-Resolution Spectrometer (MRS) of MIRI is an integral field spectrograph that provides diffraction-limited spectroscopy between 4.9 and 28.3 um, within a FOV varying from 13 to 56" square. From ground testing, we calculate the physical parameters essential to general observers and calibrating the wavelength solution and resolving power of the MRS is critical for maximising the scientific performance of the instrument. We have used ground-based observations of discrete spectral features in combination with Fabry-Perot etalon spectra to characterize the wavelength solution and spectral resolving power of the MRS. We present the methodology used to derive the MRS spectral characterisation, which includes the precise wavelength coverage of each MRS sub-band, computation of the resolving power as a function of wavelength, and measuring slice-dependent spectral distortions. The resolving power varies from R3500 in channel 1 to R1500 in channel 4. Based on the ground test data, the wavelength calibration accuracy is estimated to be below one tenth of a pixel, with small systematic shifts due to the target position within a slice for unresolved sources, that have a maximum amplitude of about 0.25 spectral resolution elements. Based on ground test data, the MRS complies with the spectral requirements for both the R and wavelength accuracy for which it was designed. We also present the commissioning strategies and targets that will be followed to update the spectral characterisation of the MRS., 13 pages. Accepted for publication in A&A

Published
2021
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10. mirisim : a simulator for the Mid-Infrared Instrument on JWST

Author

Olivia Jones, Vincent Geers, Adrian M. Glauser, A. Coulais, A. D. O'Brien, David R. Law, Benjamin A. Sargent, Kristen Murray, C. Cossou, Steven Beard, W. De Meester, G. S. Wright, Alistair Glasse, Jeroen Bouwman, R. Gastaud, Ruyman Azzollini, J. Schreiber, Misty Cracraft, M. Topinka, Pamela Klaassen, Patrick J. Kavanagh, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)

Subjects
instruments [space vehicles], Mid infrared, FOS: Physical sciences, Astronomy & Astrophysics, 01 natural sciences, law.invention, 010309 optics, Telescope, Software, law, 0103 physical sciences, space vehicles: instruments, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Simulation, computer.programming_language, Physics, [PHYS]Physics [physics], Science & Technology, Spectrometer, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, James Webb Space Telescope, Detector, WEBB-SPACE-TELESCOPE, Astronomy and Astrophysics, Python (programming language), Metadata, Space and Planetary Science, Physical Sciences, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, computer
Abstract

The Mid-Infrared Instrument (MIRI) on the James Webb Space Telescope (JWST), has imaging, four coronagraphs and both low and medium resolution spectroscopic modes . Being able to simulate MIRI observations will help commissioning of the instrument, as well as get users familiar with representative data. We designed the MIRI instrument simulator (MIRISim) to mimic the on-orbit performance of the MIRI imager and spectrometers using the Calibration Data Products (CDPs) developed by the MIRI instrument team. The software encorporates accurate representations of the detectors, slicers, distortions, and noise sources along the light path including the telescope's radiative background and cosmic rays. The software also includes a module which enables users to create astronomical scenes to simulate. MIRISim is a publicly available Python package that can be run at the command line, or from within Python. The outputs of MIRISim are detector images in the same uncalibrated data format that will be delivered to MIRI users. These contain the necessary metadata for ingestion by the JWST calibration pipeline., 10 pages, 8 figures. Accepted for publication by MNRAS

Published
2020
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11. A Framework for Prioritizing the TESS Planetary Candidates Most Amenable to Atmospheric Characterization

Author

Daniel D. B. Koll, Nicolas B. Cowan, Emily Rauscher, Jessie L. Christiansen, Dana R. Louie, Miguel de Val-Borro, David K. Sing, Keivan G. Stassun, Zach Berta-Thompson, Stephen R. Kane, Thomas G. Beatty, Diana Dragomir, Joanna K. Barstow, Natasha E. Batalha, Eliza M.-R. Kempton, Robert T. Zellem, Jeff A. Valenti, Drake Deming, Matthias Mallonn, Eric Gaidos, Kevin Heng, Valerio Nascimbeni, Laura Kreidberg, Evgenya L. Shkolnik, Sara Seager, Ian J. M. Crossfield, Jayne Birkby, Caroline V. Morley, David Charbonneau, Megan Mansfield, Carolina von Essen, Sarah Ballard, Lars A. Buchhave, Enric Palle, Elisa V. Quintana, Mercedes Lopez-Morales, Alessandro Sozzetti, René Doyon, Norio Narita, Jacob L. Bean, Thomas Barclay, Renyu Hu, Mark R. Swain, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, MIT Kavli Institute for Astrophysics and Space Research, and Low Energy Astrophysics (API, FNWI)

Subjects
JWST, 010504 meteorology & atmospheric sciences, 530 Physics, detection [planets and satellites], Computer science, FOS: Physical sciences, MIDINFRARED INSTRUMENT, 01 natural sciences, Astrobiology, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), STAR, 520 Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, WEBB-SPACE-TELESCOPE, Astronomy and Astrophysics, Thermal emission, atmospheres [planets and satellites], EXOPLANETS, Mass measurement, Exoplanet, Characterization (materials science), Rapid identification, Radial velocity, Stars, Space and Planetary Science, TEMPERATE TERRESTRIAL PLANETS, Astrophysics::Earth and Planetary Astrophysics, ROCKY, Astrophysics - Earth and Planetary Astrophysics
Abstract

A key legacy of the recently launched TESS mission will be to provide the astronomical community with many of the best transiting exoplanet targets for atmospheric characterization. However, time is of the essence to take full advantage of this opportunity. JWST, although delayed, will still complete its nominal five year mission on a timeline that motivates rapid identification, confirmation, and mass measurement of the top atmospheric characterization targets from TESS. Beyond JWST, future dedicated missions for atmospheric studies such as ARIEL require the discovery and confirmation of several hundred additional sub-Jovian size planets (R_p < 10 R_Earth) orbiting bright stars, beyond those known today, to ensure a successful statistical census of exoplanet atmospheres. Ground-based ELTs will also contribute to surveying the atmospheres of the transiting planets discovered by TESS. Here we present a set of two straightforward analytic metrics, quantifying the expected signal-to-noise in transmission and thermal emission spectroscopy for a given planet, that will allow the top atmospheric characterization targets to be readily identified among the TESS planet candidates. Targets that meet our proposed threshold values for these metrics would be encouraged for rapid follow-up and confirmation via radial velocity mass measurements. Based on the catalog of simulated TESS detections by Sullivan et al. (2015), we determine appropriate cutoff values of the metrics, such that the TESS mission will ultimately yield a sample of $\sim300$ high-quality atmospheric characterization targets across a range of planet size bins, extending down to Earth-size, potentially habitable worlds., accepted to PASP

Published
2018
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12. The Transiting Exoplanet Community Early Release Science Program for JWST

Author

Jacob L. Bean, Kevin B. Stevenson, Natalie M. Batalha, Zachory Berta-Thompson, Laura Kreidberg, Nicolas Crouzet, Björn Benneke, Michael R. Line, David K. Sing, Hannah R. Wakeford, Heather A. Knutson, Eliza M.-R. Kempton, Jean-Michel Désert, Ian Crossfield, Natasha E. Batalha, Julien de Wit, Vivien Parmentier, Joseph Harrington, Julianne I. Moses, Mercedes Lopez-Morales, Munazza K. Alam, Jasmina Blecic, Giovanni Bruno, Aarynn L. Carter, John W. Chapman, Leen Decin, Diana Dragomir, Thomas M. Evans, Jonathan J. Fortney, Jonathan D. Fraine, Peter Gao, Antonio García Muñoz, Neale P. Gibson, Jayesh M. Goyal, Kevin Heng, Renyu Hu, Sarah Kendrew, Brian M. Kilpatrick, Jessica Krick, Pierre-Olivier Lagage, Monika Lendl, Tom Louden, Nikku Madhusudhan, Avi M. Mandell, Megan Mansfield, Erin M. May, Giuseppe Morello, Caroline V. Morley, Nikolay Nikolov, Seth Redfield, Jessica E. Roberts, Everett Schlawin, Jessica J. Spake, Kamen O. Todorov, Angelos Tsiaras, Olivia Venot, William C. Waalkes, Peter J. Wheatley, Robert T. Zellem, Daniel Angerhausen, David Barrado, Ludmila Carone, Sarah L. Casewell, Patricio E. Cubillos, Mario Damiano, Miguel de Val-Borro, Benjamin Drummond, Billy Edwards, Michael Endl, Nestor Espinoza, Kevin France, John E. Gizis, Thomas P. Greene, Thomas K. Henning, Yucian Hong, James G. Ingalls, Nicolas Iro, Patrick G. J. Irwin, Tiffany Kataria, Fred Lahuis, Jérémy Leconte, Jorge Lillo-Box, Stefan Lines, Joshua D. Lothringer, Luigi Mancini, Franck Marchis, Nathan Mayne, Enric Palle, Emily Rauscher, Gaël Roudier, Evgenya L. Shkolnik, John Southworth, Mark R. Swain, Jake Taylor, Johanna Teske, Giovanna Tinetti, Pascal Tremblin, Gregory S. Tucker, Roy van Boekel, Ingo P. Waldmann, Ian C. Weaver, Tiziano Zingales, University of Chicago, Space Telescope Science Institute (STSci), NASA Ames Research Center (ARC), Department of Astrophysical and Planetary Sciences [Boulder], University of Colorado [Boulder], Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Instituto de Astrofisica de Canarias (IAC), Universidad de La Laguna [Tenerife - SP] (ULL), Département de Physique [Montréal], Université de Montréal [Montréal], School of Earth and Space Exploration [Tempe] (SESE), Arizona State University [Tempe] (ASU), University of Exeter, Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Grinnell College, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of Central Florida [Orlando], Space Science Institute [Boulder] (SSI), New York University [Abu Dhabi], NYU System (NYU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), University of California [Santa Cruz] (UCSC), University of California, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Zentrum für Astronomie und Astrophysik [Berlin] (ZAA), Technische Universität Berlin (TUB), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Center for Space and Habitability (CSH), University of Bern, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Brown University, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Austrian Academy of Sciences (OeAW), University of Warwick [Coventry], Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), GSFC Solar System Exploration Division, NASA Goddard Space Flight Center (GSFC), University of Michigan [Ann Arbor], University of Michigan System, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, The Foundation for Scientific and Industrial Research (SINTEF), College of Engineering, Mathematics and Physical Sciences [Exeter] (EMPS), Wesleyan University, Amsterdam University of Applied Sciences, Department of Physics and Astronomy [UCL London], University College of London [London] (UCL), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Blue Marble Space Institute of Science (BMSIS), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Department of Physics and Astronomy [Leicester], University of Leicester, Space Research Institute of Austrian Academy of Sciences (IWF), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Astrochemistry Laboratory [Greenbelt], Catholic University of America, McDonald Observatory, University of Texas at Austin [Austin], Center for Astrophysics and Space Astronomy [Boulder] (CASA), Department of Physics and Astronomy [Newark], University of Delaware [Newark], Cornell University, Infrared Processing and Analysis Center (IPAC), University of Vienna [Vienna], Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], SRON Netherlands Institute for Space Research (SRON), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Carl Sagan Center, SETI Institute, Department of Physics, University of Rome Tor Vergata, Maison de la Simulation (MDLS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université Paris-Sud - Paris 11 (UP11)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Ames Laboratory [Ames, USA], Iowa State University (ISU)-U.S. Department of Energy (DOE), Low Energy Astrophysics (API, FNWI), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides ( CASSIOPEE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Plasmachemistry, CNR-IMIP, Katholieke Universiteit Leuven ( KU Leuven ), University of California [Santa Cruz] ( UCSC ), Eidgenössische Technische Hochschule, Swiss Federal Institute of Technology in Zürich ( ETH Zürich ), Max-Planck-Institut für Astronomie ( MPIA ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), The Foundation for Scientific and Industrial Research ( SINTEF ), Laboratoire inter-universitaire des systèmes atmosphèriques ( LISA ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Astrophysical Sciences [Princeton], Princeton University, Center for Astrophysics and Space Astronomy [Boulder] ( CASA ), University of Colorado Boulder [Boulder], Dept of Physics, University of Florida [Gainesville], Stony Brook University [The State University of New York] ( SBU ), ECLIPSE 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), University College of London [London] ( UCL ), Maison de la Simulation ( MDLS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Recherche en Informatique et en Automatique ( Inria ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Iowa State University ( ISU ) -U.S. Department of Energy ( DOE ), Université de Montréal (UdeM), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of Central Florida [Orlando] (UCF), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Technische Universität Berlin (TU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Stiftelsen for INdustriell og TEknisk Forskning Digital [Trondheim] (SINTEF Digital), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Cornell University [New York], Università degli Studi di Roma Tor Vergata [Roma], Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut National de Recherche en Informatique et en Automatique (Inria)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Iowa State University (ISU)-U.S. Department of Energy [Washington] (DOE), Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Smithsonian Institution-Harvard University [Cambridge], Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Harvard University-Smithsonian Institution, Technical University of Berlin / Technische Universität Berlin (TU), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Agence Spatiale Européenne = European Space Agency (ESA), and University of Oxford

Subjects
MODEL ATMOSPHERES, Exclusive access, 010504 meteorology & atmospheric sciences, Computer science, Science program, observational [methods], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, MIDINFRARED INSTRUMENT, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Planets and satellites: Individual, 01 natural sciences, EXTRASOLAR GIANT PLANETS, Planets and satellites: Atmospheres, individual (WASP-79b, WASP-43b, WASP-18b) [planets and satellites], Settore FIS/05 - Astronomia e Astrofisica, Methods: Observational, Planet, 0103 physical sciences, Early release, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, LIGHT CURVES, Earth and Planetary Astrophysics (astro-ph.EP), Science & Technology, Community engagement, TIME-SERIES PHOTOMETRY, THERMAL EMISSION, James Webb Space Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, WEBB-SPACE-TELESCOPE, Astronomy and Astrophysics, HOT-JUPITER, atmospheres [planets and satellites], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Data science, Methods observational, Exoplanet, 13. Climate action, Space and Planetary Science, Physical Sciences, HD 189733B, Astrophysics::Earth and Planetary Astrophysics, ATMOSPHERIC CIRCULATION, Astrophysics - Earth and Planetary Astrophysics
Abstract

The James Webb Space Telescope (JWST) presents the opportunity to transform our understanding of planets and the origins of life by revealing the atmospheric compositions, structures, and dynamics of transiting exoplanets in unprecedented detail. However, the high-precision, time-series observations required for such investigations have unique technical challenges, and prior experience with other facilities indicates that there will be a steep learning curve when JWST becomes operational. In this paper we describe the science objectives and detailed plans of the Transiting Exoplanet Community Early Release Science (ERS) Program, which is a recently approved program for JWST observations early in Cycle 1. The goal of this project, for which the obtained data will have no exclusive access period, is to accelerate the acquisition and diffusion of technical expertise for transiting exoplanet observations with JWST, while also providing a compelling set of representative datasets that will enable immediate scientific breakthroughs. The Transiting Exoplanet Community ERS Program will exercise the time-series modes of all four JWST instruments that have been identified as the consensus highest priorities, observe the full suite of transiting planet characterization geometries (transits, eclipses, and phase curves), and target planets with host stars that span an illustrative range of brightnesses. The observations in this program were defined through an inclusive and transparent process that had participation from JWST instrument experts and international leaders in transiting exoplanet studies. Community engagement in the project will be centered on a two-phase Data Challenge that culminates with the delivery of planetary spectra, time-series instrument performance reports, and open-source data analysis toolkits in time to inform the agenda for Cycle 2 of the JWST mission., Comment: PASP in press

Published
2018
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13. Recovering the Properties of High-redshift Galaxies with Different JWST Broadband Filters

Author

Bisigello, L., Caputi, K. I., Colina, L., Le Fevre, O., Norgaard-Nielsen, H. U., Pérez González, Pablo Guillermo, van der Werf, P., Ilbert, O., Grogin, N., Koekemoer, A., Bisigello, L., Caputi, K. I., Colina, L., Le Fevre, O., Norgaard-Nielsen, H. U., Pérez González, Pablo Guillermo, van der Werf, P., Ilbert, O., Grogin, N., and Koekemoer, A.

Abstract

© 2017. The American Astronomical Society. All rights reserved. L.B. and K.I.C. acknowledge the support of the Nederlandse Onderzoekschool voor de Astronomie (NOVA). K.I.C. also acknowledges funding from the European Research Council through the award of the Consolidator Grant ID 681627-BUILDUP. O.L.F. acknowledges funding from the European Research Council Advanced Grant ID 268107-EARLY. P.G. P.-G. acknowledges support from the Spanish Government MINECO Grants AYA2012-31277 and AYA2015-70815-ERC. L.C. acknowledges support from the Spanish Government MINECO Grants AAYA2012-32295., Imaging with the James Webb Space Telescope (JWST) will allow observations of the bulk of distant galaxies at the epoch of reionization. The recovery of their properties, such as age, color excess E(B-V), specific star formation rate (sSFR), and stellar mass, will mostly rely on spectral energy distribution fitting, based on the data provided by JWST's two imager cameras, namely the Near Infrared Camera (NIRCam) and the Mid Infrared Imager (MIRI). In this work we analyze the effect of choosing different combinations of NIRCam and MIRI broadband filters, from 0.6 to 7.7 mu m, on the recovery of these galaxy properties. We performed our tests on a sample of 1542 simulated galaxies, with known input properties, at z = 7-10. We found that, with only eight NIRCam broadbands, we can recover the galaxy age within 0.1 Gyr and the color excess within 0.06 mag for 70% of the galaxies. Additionally, the stellar masses and sSFR are recovered within 0.2 and 0.3 dex, respectively, at z = 7-9. Instead, at z = 10, no NIRCam band traces purely the lambda > 4000 angstrom regime and the percentage of outliers in stellar mass (sSFR) increases by > 20% (> 90%), in comparison to z = 9. The MIRI F560W and F770W bands are crucial to improve the stellar mass and the sSFR estimation at z = 10. When nebular emission lines are present, deriving correct galaxy properties is challenging at any redshift and with any band combination. In particular, the stellar mass is systematically overestimated in up to 0.3 dex on average with NIRCam data alone and including MIRI observations only marginally improves the estimation., Unión Europea. H2020, Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), Nederlandse Onderzoekschool voor de Astronomie (NOVA), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2017

14. The impact of JWST broad-band filter choice on photometric redshift estimation

Author

P. van der Werf, Anton M. Koekemoer, Karina Caputi, Luis Colina, L. Bisigello, Hans Ulrik Nørgaard-Nielsen, Norman A. Grogin, O. Le Fevre, John P. Pye, Pablo G. Pérez-González, O. Ilbert, Kapteyn Astronomical Institute, Astronomy, 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
GOODS-SOUTH FIELD, Astrofísica, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, MIDINFRARED INSTRUMENT, 01 natural sciences, high-redshift [Galaxies], LY-ALPHA EMITTERS, STELLAR POPULATIONS, galaxies: high-redshift, 0103 physical sciences, Broadband, distances and redshifts [Galaxies], EXTRAGALACTIC LEGACY SURVEY, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Photometric redshift, Physics, Government, business.industry, photometry [Galaxies], European research, WEBB-SPACE-TELESCOPE, Astronomy and Astrophysics, VLT DEEP SURVEY, Astrophysics - Astrophysics of Galaxies, GALAXIES, Red shift, Astronomía, galaxies: photometry, Photometry (astronomy), [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Filter (video), KECK SPECTROSCOPY, Astrophysics of Galaxies (astro-ph.GA), galaxies: distances and redshifts, Telecommunications, business, Near infrared radiation, OPTICAL SPECTROSCOPY
Abstract

The determination of galaxy redshifts in James Webb Space Telescope (JWST)'s blank-field surveys will mostly rely on photometric estimates, based on the data provided by JWST's Near-Infrared Camera (NIRCam) at 0.6-5.0 {\mu}m and Mid Infrared Instrument (MIRI) at {\lambda}>5.0 {\mu}m. In this work we analyse the impact of choosing different combinations of NIRCam and MIRI broad-band filters (F070W to F770W), as well as having ancillary data at {\lambda}=10, but the zphot quality significantly degrades at S/N, Comment: 29 pages, 27 figures, 12 tables. Accepted for publication at the ApJS

Published
2016
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