Investigating the physical properties of galaxies in the Epoch of Reionization with MIRI/JWST spectroscopy

Álvarez-Márquez, J.; Colina, L.; Marques-Chaves, R.; Ceverino, Daniel; Alonso‐Herrero, A.; Caputi, K.; García-Marín, M.; Labiano, Á.; Fèvre, O. Le; Nørgaard-Nielsen, H. U.; Östlin, Göran; Pérez‐González, Pablo G.; Pye, J. P.; Tikkanen, Tuomo; Werf, P. P. van der; Walter, Fabian; Wright, Gillian

doi:10.1051/0004-6361/201935594

Cited by 18 publications

(15 citation statements)

References 73 publications

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“…Large spectro-photometric surveys on 8-meter telescopes will provide thousands to millions of spectra in the deepest photometric fields, such as with the Multi-Object Optical and Near-infrared Spectrograph (MOONS) for the Very Large Telescope (VLT) and the Subaru Prime Focus Spectrograph (PFS), and larger facilities (e.g., Extremely Large Telescope) such as the Multi-Object Spectrograph for Astrophysics, Intergalacticmedium studies, and Cosmology (MOSAIC) . The James Webb Space Telescope (JWST) will push the observations of both restframe UV-optical continuum and emission lines to very high redshift in particular the Hα and [OIII]λ5007 emission lines for which different physical conditions and configurations will need to be taken into account in their modeling (Schaerer & de Barros 2009;Wright et al 2015;Wells et al 2015;Álvarez-Márquez et al 2019;Chevallard et al 2019). While treating both photometric and emission line information simultaneously, it is important to account for the potential contribution of emission lines in photometric bands, which can substantially modify the observed fluxes increasing the uncertainties in the parameter estimations (Schaerer & de Barros 2010;Stark et al 2013;Tang et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Fitting spectral energy distributions of FMOS-COSMOS emission-line galaxies atz∼ 1.6: Star formation rates, dust attenuation, and [OIII]λ5007 emission-line luminosities

Villa-Vélez

Buat

Theulé

et al. 2021

A&A

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We perform a spectral energy distribution fitting analysis on a COSMOS photometric sample covering the ultra-violet up to the farinfrared wavelengths and including emission lines from the Fiber Multi-Object Spectrograph (FMOS) survey. The sample consists of 182 objects with Hα and [OIII]λ5007 emission line measurements lying in a redshift range of 1.40 < z < 1.68. We obtain robust estimates of the stellar mass and star-formation rate spanning over a range of 10 9.5 −10 11.5 M and 10 1 −10 3 M yr −1 from the Bayesian analysis performed with CIGALE and using continuum photometry and Hα fluxes. Combining photometry and spectroscopy gives secure estimations of the amount of dust attenuation for both continuum and line emissions. We obtain a median attenuation of A Hα = 1.16 ± 0.19 mag and A [OIII] = 1.41 ± 0.22 mag. Hα and [OIII]λ5007 attenuations are found to increase with stellar mass, confirming previous findings with Hα. A difference of 57% in the attenuation experienced by emission lines and continuum is found to be in agreement with the emission lines being more attenuated than the continuum emission. Implementation of new CLOUDY HII-region models in CIGALE enables good fits of the Hα, Hβ, [OIII]λ5007 emission lines with discrepancies smaller than 0.2 dex in the predicted fluxes. Fitting the [NII]λ6584 line is found challenging due to well-known discrepancies in the locus of galaxies in the [NII]-BPT diagram at intermediate and high redshifts. We find a positive correlation between SFR and L [OIII]λ5007 after correcting for dust attenuation and we derive the linear relation log 10 (SFR/M yr −1 ) = log 10 (L [OIII] /ergs s −1 ) − (41.20 ± 0.02). Leaving the slope as a free parameter leads to log 10 (SFR/M yr −1 ) = (0.83 ± 0.06) log 10 (L [OIII] /ergs s −1 ) − (34.01 ± 2.63). The spread in the relation is driven by differences in the gas-phase metallicity and ionization parameter accounting for a 0.24 dex and 1.1 dex of the dispersion, respectively. We report an average value of log U ≈ −2.85 for this sample of galaxies. Including HII-region models to fit simultaneously photometric data and emission line fluxes is paramount to analyses of upcoming data sets from large spectroscopic surveys of the future, such as MOONS and PFS.

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Section: Introductionmentioning

confidence: 99%

Fitting spectral energy distributions of FMOS-COSMOS emission-line galaxies atz∼ 1.6: Star formation rates, dust attenuation, and [OIII]λ5007 emission-line luminosities

Villa-Vélez

Buat

Theulé

et al. 2021

A&A

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“…The cross calibration among adjacent bands should also correct for isolated shifts in the lines. Also, we are currently working on MIRISim (Klaassen et al 2021) simulations of the targets with the flight pipeline to improve the analysis strategy if needed (e.g., Álvarez-Márquez et al 2019). Taking all these into account, and based on the instrument models and extensive analysis of the data, we expect variations between the ground and on-orbit wavelength calibration below 1-5 pixels at most.…”

Section: Target Selectionmentioning

confidence: 99%

Wavelength calibration and resolving power of the JWST MIRI Medium Resolution Spectrometer

Labiano

Argyriou

Álvarez-Márquez

et al. 2021

A&A

Self Cite

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Context. The Mid-Infrared Instrument (MIRI) onboard the James Webb Space Telescope (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 µm, within a field of view (FOV) varying from ∼13 to ∼56 arcsec square. The design for MIRI MRS conforms with the goals of the JWST mission to observe high redshift galaxies and to study cosmology as well as observations of galactic objects, and stellar and planetary systems. Aims. From ground testing, we calculate the physical parameters essential for general observers and calibrating the wavelength solution and resolving power of the MRS which is critical for maximizing the scientific performance of the instrument. Methods. 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 characterization, 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. Results. The ground calibration of the MRS shows that it will cover the wavelength ranges from 4.9 to 28.3 µm, divided in 12 overlapping spectral sub-bands. The resolving power is R 3500 in channel 1, R 3000 in channel 2, R 2500 in channel 3, and R 1500 in channel 4. The MRS spectral resolution optimizes the sensitivity for detection of spectral features with a velocity width of ∼ 100 km s −1 which is characteristic of most astronomical phenomena JWST aims to study in the mid-infrared. Based on the ground test data, the wavelength calibration accuracy is estimated to be below one-tenth of a pixel (0.1 nm at 5 µm and 0.4 at 28 µm), 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. The absolute wavelength calibration is presently uncertain at the level of 0.35 nm at 5 µm and 46 nm at 28 µm, and it will be refined using in-flight commissioning observations. Conclusions. 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 characterization of the MRS.

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“…The cross calibration among adjacent bands should also correct for isolated shifts in the lines. Also, we are currently working on MIRISim (Klaassen et al 2021) simulations of the targets with the flight pipeline to improve the analysis strategy if needed (e.g., Álvarez-Márquez et al 2019). Taking all these into account, and based in the instrument models and extensive analysis of the data, we expect variations between the ground and on-orbit wavelength calibration below 1-5 pixels at most.…”

Section: Target Selectionmentioning

confidence: 99%

Wavelength Calibration and Resolving Power of the JWST MIRI Medium Resolution Spectrometer

Labiano,

Argyriou,

Alvarez-Marquez

et al. 2021

Preprint

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Context. The Mid-Infrared Instrument (MIRI) on-board the James Webb Space Telescope 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 µm, within a FOV varying from ∼13 to ∼56 arcsec square. The design for MIRI MRS conforms with the goals of the JWST mission to observe high redshift galaxies and to study cosmology as well as observations of galactic objects, stellar and planetary systems. Aims. 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 maximizing the scientific performance of the instrument. Methods. 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 characterization, 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. Results. The ground calibration of the MRS shows that it will cover the wavelength ranges from 4.9 to 28.3 µm, divided in 12 overlapping spectral sub-bands. The resolving power, is R 3500 in channel 1, R 3000 in channel 2, R 2500 in channel 3, and R 1500 in channel 4. The MRS spectral resolution optimises the sensitivity for detection of spectral features with a velocity width of ∼ 100 km s −1 which is characteristic of most astronomical phenomena JWST aims to study in the mid-IR. Based on the ground test data, the wavelength calibration accuracy is estimated to be below one tenth of a pixel (0.1 nm at 5 µm and 0.4 at 28 µm), 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. The absolute wavelength calibration is presently uncertain at the level of 0.35 nm at 5 µm and 46 nm at 28 µm, and will be refined using in-flight commissioning observations. Conclusions. 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.

show abstract

Investigating the physical properties of galaxies in the Epoch of Reionization with MIRI/JWST spectroscopy

Cited by 18 publications

References 73 publications

Fitting spectral energy distributions of FMOS-COSMOS emission-line galaxies atz∼ 1.6: Star formation rates, dust attenuation, and [OIII]λ5007 emission-line luminosities

Fitting spectral energy distributions of FMOS-COSMOS emission-line galaxies atz∼ 1.6: Star formation rates, dust attenuation, and [OIII]λ5007 emission-line luminosities

Wavelength calibration and resolving power of the JWST MIRI Medium Resolution Spectrometer

Wavelength Calibration and Resolving Power of the JWST MIRI Medium Resolution Spectrometer

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