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Álvarez-Márquez, J., Crespo Gómez, A., Colina, L., Langeroodi, D., Marques-Chaves, R., Prieto-Jiménez, C., . . . Wright, G. (2025). Insight into the starburst nature of Galaxy GN-z11 with JWST MIRI spectroscopy. Astronomy and Astrophysics, 695, Article ID A250.
Open this publication in new window or tab >>Insight into the starburst nature of Galaxy GN-z11 with JWST MIRI spectroscopy
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2025 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 695, article id A250Article in journal (Refereed) Published
Abstract [en]

This paper presents a deep MIRI/JWST medium-resolution spectroscopy (MRS) covering the rest-frame optical spectrum of the GN-z11 galaxy. The [O III] 5008 Å and Hα emission lines are detected and spectroscopically resolved. The line profiles are well modeled by a narrow Gaussian component with intrinsic full widths at half maximum of 189 ± 25 and 231 ± 52 km s-1, respectively. We do not find any evidence of a dominant broad Hα emission line component tracing a broad-line region in a type 1 active galactic nucleus (AGN). The existence of an accreting black hole dominating the optical continuum and emission lines of GN-z11 is not compatible with the measured Hα and [O III] 5008 Å luminosities. If the well-established relations for low-z AGNs apply in GN-z11, the [O III] 5008 Å and Hα luminosities would imply extremely high super-Eddington ratios (λE > 290), and bolometric luminosities ∼20 times those derived from the UV/optical continuum. However, a broad (∼430-470 km s-1) and weak (< 20-30%) Hα line component, tracing a minor AGN contribution in the optical, cannot be completely ruled out with the sensitivity of the current data. The physical and excitation properties of the ionized gas are consistent with a low-metallicity starburst with a star formation rate of 24 ± 3 M⊙ yr-1. The electron temperature of the ionized gas is Te (O++) = 14 000 ± 2100 K, while the direct-Te gas-phase metallicity is 12 + log(O/H) = 7.91 ± 0.07 (Z = 0.17 ± 0.03 Z⊙). The optical line ratios locate GN-z11 in the starburst or AGN region, but they are more consistent with those of local low-metallicity starbursts and high-z luminous galaxies detected at redshifts similar to GN-z11. We conclude that the MRS optical spectrum of GN-z11 is consistent with that of a massive, compact, and low-metallicity starburst galaxy. Its high star formation and stellar mass surface densities are close to those of the densest stellar clusters, and we therefore speculate that GN-z11 might undergo a feedback-free, highly efficient starburst phase. Additional JWST data are needed to validate this scenario and other recently proposed alternatives to explain the existence of bright compact galaxies in the early Universe.

Keywords
Galaxies: high-redshift, Galaxies: individual: GN-z11, Galaxies: ISM, Galaxies: starburst
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-242025 (URN)10.1051/0004-6361/202451731 (DOI)001452581300019 ()2-s2.0-105001168695 (Scopus ID)
Available from: 2025-04-14 Created: 2025-04-14 Last updated: 2025-04-14Bibliographically approved
Bosman, S. E. I., Álvarez-Márquez, J., Colina, L., Walter, F., Alonso-Herrero, A., Ward, M. J., . . . Vandenbussche, B. (2024). A mature quasar at cosmic dawn revealed by JWST rest-frame infrared spectroscopy. Nature Astronomy, 8(8), 1054-1065
Open this publication in new window or tab >>A mature quasar at cosmic dawn revealed by JWST rest-frame infrared spectroscopy
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2024 (English)In: Nature Astronomy, E-ISSN 2397-3366, Vol. 8, no 8, p. 1054-1065Article in journal (Refereed) Published
Abstract [en]

The rapid assembly of the first supermassive black holes is an enduring mystery. Until now, it was not known whether quasar ‘feeding’ structures (the ‘hot torus’) could assemble as fast as the smaller-scale quasar structures. We present JWST/MRS (rest-frame infrared) spectroscopic observations of the quasar J1120+0641 at z = 7.0848 (well within the epoch of reionization). The hot torus dust was clearly detected at λrest ≃ 1.3 μm, with a black-body temperature of Tdust=1,413.5−7.4+5.7 K, slightly elevated compared to similarly luminous quasars at lower redshifts. Importantly, the supermassive black hole mass of J1120+0641 based on the Hα line (accessible only with JWST), MBH = 1.52 ± 0.17 × 109 M⊙, is in good agreement with previous ground-based rest-frame ultraviolet Mg ii measurements. Comparing the ratios of the Hα, Paα and Paβ emission lines to predictions from a simple one-phase Cloudy model, we find that they are consistent with originating from a common broad-line region with physical parameters that are consistent with lower-redshift quasars. Together, this implies that J1120+0641’s accretion structures must have assembled very quickly, as they appear fully ‘mature’ less than 760 Myr after the Big Bang.

National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-235577 (URN)10.1038/s41550-024-02273-0 (DOI)001248575600002 ()2-s2.0-85196053342 (Scopus ID)
Available from: 2024-11-18 Created: 2024-11-18 Last updated: 2024-11-18Bibliographically approved
Pérez-González, P. G., Rinaldi, P., Caputi, K. I., Álvarez-Márquez, J., Annunziatella, M., Langeroodi, D., . . . van der Werf, P. P. (2024). A NIRCam-dark Galaxy Detected with the MIRI/F1000W Filter in the MIDIS/JADES Hubble Ultra Deep Field. Astrophysical Journal Letters, 969(1), Article ID L10.
Open this publication in new window or tab >>A NIRCam-dark Galaxy Detected with the MIRI/F1000W Filter in the MIDIS/JADES Hubble Ultra Deep Field
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2024 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 969, no 1, article id L10Article in journal (Refereed) Published
Abstract [en]

We report the discovery of Cerberus, an extremely red object detected with the MIRI Deep Imaging Survey (MIDIS) observations in the F1000W filter of the Hubble Ultra Deep Field. The object is detected at signal-to-noise ratio (S/N) ∼ 6, with F1000W ∼ 27 mag, and undetected in the NIRCam data gathered by the JWST Advanced Deep Extragalactic Survey (JADES), fainter than the 30.0-30.5 mag 5σ detection limits in individual bands, as well as in the MIDIS F560W ultradeep data (∼29 mag, 5σ). Analyzing the spectral energy distribution built with low-S/N (<5) measurements in individual optical-to-mid-infrared filters and higher-S/N (≳5) measurements in stacked NIRCam data, we discuss the possible nature of this red NIRCam-dark source using a battery of codes. We discard the possibility of Cerberus being a solar system body based on the <0.″016 proper motion in the 1 yr apart JADES and MIDIS observations. A substellar Galactic nature is deemed unlikely, given that the Cerberus’s relatively flat NIRCam-to-NIRCam and very red NIRCam-to-MIRI flux ratios are not consistent with any brown dwarf model. The extragalactic nature of Cerberus offers three possibilities: (1) a z ∼ 0.4 galaxy with strong emission from polycyclic aromatic hydrocarbons—the very low inferred stellar mass, M ⋆ = 105-106 M ⊙, makes this possibility highly improbable; (2) a dusty galaxy at z ∼ 4 with an inferred stellar mass M ⋆ ∼ 108 M ⊙; and (3) a galaxy with observational properties similar to those of the reddest little red dots discovered around z ∼ 7, but Cerberus lying at z ∼ 15, with the rest-frame optical dominated by emission from a dusty torus or a dusty starburst.

National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-238556 (URN)10.3847/2041-8213/ad517b (DOI)2-s2.0-85198751910 (Scopus ID)
Available from: 2025-01-28 Created: 2025-01-28 Last updated: 2025-01-28Bibliographically approved
Marconi, A., Bik, A., Brandeker, A., Östlin, G. & Zimara, J. (2024). ANDES, the high resolution spectrograph for the ELT: science goals, project overview and future developments. In: Julia J. Bryant; Kentaro Motohara; Joël R. D. Vernet (Ed.), PROCEEDINGS VOLUME 13096: Ground-based and Airborne Instrumentation for Astronomy X. Paper presented at SPIE Astronomical Telescopes + Instrumentation, Yokohama, Japan, 2024. SPIE, Article ID 1309613.
Open this publication in new window or tab >>ANDES, the high resolution spectrograph for the ELT: science goals, project overview and future developments
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2024 (English)In: PROCEEDINGS VOLUME 13096: Ground-based and Airborne Instrumentation for Astronomy X / [ed] Julia J. Bryant; Kentaro Motohara; Joël R. D. Vernet, SPIE , 2024, article id 1309613Conference paper, Published paper (Refereed)
Abstract [en]

The first generation of ELT instruments includes an optical-infrared high resolution spectrograph, indicated as ELT-HIRES and recently christened ANDES (ArmazoNes high Dispersion Echelle Spectrograph).ANDES consists of three fibre-fed spectrographs ([U]BV, RIZ, YJH) providing a spectral resolution of ∼100,000 with a minimum simultaneous wavelength coverage of 0.4-1.8 µm with the goal of extending it to 0.35-2.4 µm with the addition of an U arm to the BV spectrograph and a separate K band spectrograph.It operates both in seeing- and diffraction-limited conditions and the fibre-feeding allows several, interchangeable observing modes including a single conjugated adaptive optics module and a small diffraction-limited integral field unit in the NIR.Modularity and fibre-feeding allows ANDES to be placed partly on the ELT Nasmyth platform and partly in the Coudé room.ANDES has a wide range of groundbreaking science cases spanning nearly all areas of research in astrophysics and even fundamental physics.Among the top science cases there are the detection of biosignatures from exoplanet atmospheres, finding the fingerprints of the first generation of stars, tests on the stability of Nature's fundamental couplings, and the direct detection of the cosmic acceleration.The ANDES project is carried forward by a large international consortium, composed of 35 Institutes from 13 countries, forming a team of almost 300 scientists and engineers which include the majority of the scientific and technical expertise in the field that can be found in ESO member states.

Place, publisher, year, edition, pages
SPIE, 2024
Series
Proceedings of SPIE - The International Society for Optical Engineering, ISSN 0277-786X, E-ISSN 1996-756X ; 13096
Keywords
cosmology, exoplanets, extremely large telescopes, fundamental physics, ground-based instruments, high resolution spectrographs, infrared spectrographs, physics and evolution of galaxies, physics and evolution of stars, stars and planets formation
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-239249 (URN)10.1117/12.3017966 (DOI)001327608100032 ()2-s2.0-85200803254 (Scopus ID)
Conference
SPIE Astronomical Telescopes + Instrumentation, Yokohama, Japan, 2024
Available from: 2025-02-10 Created: 2025-02-10 Last updated: 2025-02-10Bibliographically approved
Bik, A., Alvarez-Marquez, J., Colina, L., Crespo Gomez, A., Peissker, F., Walter, F., . . . Van Dishoeck, E. F. (2024). Clumpy star formation and an obscured nuclear starburst in the luminous dusty z = 4 galaxy GN20 seen by MIRI/JWST. Astronomy and Astrophysics, 686, Article ID A3.
Open this publication in new window or tab >>Clumpy star formation and an obscured nuclear starburst in the luminous dusty z = 4 galaxy GN20 seen by MIRI/JWST
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2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 686, article id A3Article in journal (Refereed) Published
Abstract [en]

Dusty star-forming galaxies emit most of their light at far-infrared to millimeter wavelengths as their star formation is highly obscured. Far-infrared and millimeter observations have revealed their dust, neutral and molecular gas properties. The sensitivity of JWST at rest-frame optical and near-infrared wavelengths now allows the study of the stellar and ionized gas content. We investigate the spatially resolved distribution and kinematics of the ionized gas in GN20, a dusty star-forming galaxy at z= 4.0548. We present deep MIRI/MRS integral field spectroscopy of the near-infrared rest-frame emission of GN20. We detect spatially resolved Paα, out to a radius of 6 kpc, distributed in a clumpy morphology. The star formation rate derived from Paα (144 ± 9 M yr1) is only 7.7 ± 0.5% of the infrared star formation rate (1860 ± 90 M yr1). We attribute this to very high extinction (AV = 17.2 ± 0.4 mag, or AV, mixed = 44 ± 3 mag), especially in the nucleus of GN20, where only faint Paα is detected, suggesting a deeply buried starburst. We identify four, spatially unresolved, clumps in the Paα emission. Based on the double peaked Paα profile, we find that each clump consists of at least two sub-clumps. We find mass upper limits consistent with them being formed in a gravitationally unstable gaseous disk. The ultraviolet bright region of GN20 does not have any detected Paα emission, suggesting an age of more than 10 Myr for this region of the galaxy. From the rotation profile of Paα, we conclude that the gas kinematics are rotationally dominated and the vrot/I m = 3.8 ± 1.4 is similar to low-redshift luminous infrared galaxies. From the Paα kinematics, we cannot distinguish between a rotational profile of a large disk and a late stage merger mimicking a disk. We speculate that GN20 is in the late stage of a major merger, where the clumps in a large gas-rich disk are created by the major merger, while the central starburst is driven by the merger event.

Keywords
Galaxies: high-redshift, Galaxies: individual, Galaxies: ISM, Galaxies: kinematics and dynamics, Galaxies: starburst
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-235657 (URN)10.1051/0004-6361/202348845 (DOI)001230620000007 ()2-s2.0-85194182446 (Scopus ID)
Available from: 2024-11-18 Created: 2024-11-18 Last updated: 2024-11-18Bibliographically approved
Sirressi, M., Adamo, A., Hayes, M. J., Rivera-Thorsen, T. E., Aloisi, A., Bik, A., . . . Wofford, A. (2024). CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback. Astronomical Journal, 167(4), Article ID 166.
Open this publication in new window or tab >>CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
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2024 (English)In: Astronomical Journal, ISSN 0004-6256, E-ISSN 1538-3881, Vol. 167, no 4, article id 166Article in journal (Refereed) Published
Abstract [en]

We analyze the far-ultraviolet (1130−1770 Å rest frame) spectroscopy of 20 young (<50 Myr) and massive (>104M) star clusters (YSCs) in 11 nearby star-forming galaxies. We probe the interstellar gas intervening along the line of sight, detecting several metal absorption lines of a wide range of ionization potentials, from 6.0 to 77.5 eV. Multiple-component Voigt fits to the absorption lines are used to study the kinematics of the gas. We find that nearly all targets in the sample feature gas outflowing from 30 up to 190 km s−1, often in both the neutral and ionized phases. The outflow velocities correlate with the underlying stellar population properties directly linked to the feedback: the mass of the YSCs, the photon production rate, and the instantaneous mechanical luminosity produced by stellar winds and supernovae. We detect a neutral inflow in four targets, which we interpret as likely not associated with the star cluster but tracing larger-scale gas kinematics. A comparison between the outflows' energy and that produced by the associated young stellar populations suggests an average coupling efficiency of 10% with a broad scatter. Our results extend the relation found in previous works between galactic outflows and the host galaxy star formation rate to smaller scales, pointing toward the key role that clustered star formation and feedback play in regulating galaxy growth.

Keywords
Observational astronomy, Ultraviolet surveys, Young star clusters, Stellar feedback, Interstellar clouds
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-228031 (URN)10.3847/1538-3881/ad29f9 (DOI)001187473700001 ()2-s2.0-85188328653 (Scopus ID)
Available from: 2024-04-11 Created: 2024-04-11 Last updated: 2024-04-11Bibliographically approved
Pedrini, A., Adamo, A., Calzetti, D., Bik, A., Gregg, B., Linden, S. T., . . . Vieira, H. F. (2024). FEAST: Feedback in Emerging extragAlactic Star ClusTers. Astrophysical Journal, 971(1), Article ID 32.
Open this publication in new window or tab >>FEAST: Feedback in Emerging extragAlactic Star ClusTers
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2024 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 971, no 1, article id 32Article in journal (Refereed) Published
Abstract [en]

We investigate the emergence phase of young star clusters in the nearby spiral galaxy NGC 628. We use JWST NIRCam and MIRI observations to create spatially resolved maps of the Paα 1.87 μm and Brα 4.05 μm hydrogen recombination lines, as well as 3.3 and 7.7 μm emission from polycyclic aromatic hydrocarbons (PAHs). We extract 953 compact H ii regions and analyze the PAH emission and morphology at ∼10 pc scales in the associated photodissociation regions. While H ii regions remain compact, radial profiles help us to define three PAH morphological classes: compact (∼42%), extended (∼34%), and open (∼24%). The majority of compact and extended PAH morphologies are associated with very young star clusters (<5 Myr), while open PAH morphologies are mainly associated with star clusters older than 3 Myr. We observe a general decrease in the 3.3 and 7.7 μm PAH band emission as a function of cluster age, while their ratio remains constant with age out to 10 Myr and morphological class. The recovered PAH3.3μm/PAH7.7μm ratio is lower than values reported in the literature for reference models that consider neutral and ionized PAH populations and analyses conducted at galactic physical scales. The 3.3 and 7.7 μm bands are typically associated with neutral and ionized PAHs, respectively. While we expected neutral PAHs to be suppressed in proximity to an ionizing source, the constant PAH3.3μm/PAH7.7μm ratio would indicate that both families of molecules disrupt at similar rates in proximity to H ii regions.

National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-238125 (URN)10.3847/1538-4357/ad534d (DOI)001283355600001 ()2-s2.0-85200572720 (Scopus ID)
Available from: 2025-01-20 Created: 2025-01-20 Last updated: 2025-01-20Bibliographically approved
Gregg, B., Calzetti, D., Adamo, A., Bajaj, V., Ryon, J. E., Linden, S. T., . . . Faustino Vieira, H. (2024). Feedback in Emerging Extragalactic Star Clusters, FEAST: The Relation between 3.3 μm Polycyclic Aromatic Hydrocarbon Emission and Star Formation Rate Traced by Ionized Gas in NGC 628. Astrophysical Journal, 971(1), Article ID 115.
Open this publication in new window or tab >>Feedback in Emerging Extragalactic Star Clusters, FEAST: The Relation between 3.3 μm Polycyclic Aromatic Hydrocarbon Emission and Star Formation Rate Traced by Ionized Gas in NGC 628
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2024 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 971, no 1, article id 115Article in journal (Refereed) Published
Abstract [en]

We present maps of ionized gas (traced by Paα and Brα) and 3.3 μm polycyclic aromatic hydrocarbon (PAH) emission in the nearby spiral galaxy NGC 628, derived from new JWST/NIRCam data from the Feedback in Emerging extrAgalactic Star clusTers (FEAST) survey. With this data, we investigate and calibrate the relation between 3.3 μm PAH emission and star formation rate (SFR) in and around emerging young star clusters (eYSCs) on a scale of ∼40 pc. We find a tight (correlation coefficient ρ ∼ 0.9) sublinear (power-law exponent α ∼ 0.75) relation between the 3.3 μm PAH luminosity surface density and SFR traced by Brα for compact, cospatial (within 0.″16 or ∼7 pc) peaks in Paα, Brα, and 3.3 μm (eYSC-I). The scatter in the relationship does not correlate well with variations in local interstellar medium metallicity, due to a radial metallicity gradient, but rather is likely due to stochastic sampling of the stellar initial mass function (IMF) and variations in the PAH heating and age of our sources. The deviation from a linear relation may be explained by PAH destruction in more intense ionizing environments, variations in age, and IMF stochasticity at intermediate to low luminosities. We test our results with various continuum subtraction techniques using combinations of NIRCam bands and find that they remain robust with only minor differences in the derived slope and intercept. An unexpected discrepancy is identified between the relations of hydrogen recombination lines (Paα versus Brα; Hα versus Brα).

National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-238105 (URN)10.3847/1538-4357/ad54b4 (DOI)001288083500001 ()2-s2.0-85201102920 (Scopus ID)
Available from: 2025-01-20 Created: 2025-01-20 Last updated: 2025-01-20Bibliographically approved
Komarova, L., Oey, M. S., Hernandez, S., Adamo, A., Sirressi, M., Leitherer, C., . . . Rivera-Thorsen, T. E. (2024). Haro 11: The Spatially Resolved Lyman Continuum Sources. Astrophysical Journal, 967(2), Article ID 117.
Open this publication in new window or tab >>Haro 11: The Spatially Resolved Lyman Continuum Sources
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2024 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 967, no 2, article id 117Article in journal (Refereed) Published
Abstract [en]

As the nearest confirmed Lyman continuum (LyC) emitter, Haro 11 is an exceptional laboratory for studying LyC escape processes crucial to cosmic reionization. Our new Hubble Space Telescope/Cosmic Origins Spectrograph G130M/1055 observations of its three star-forming knots now reveal that the observed LyC originates in Knots B and C, with 903–912 Å luminosities of 1.9 ± 1.5 × 1040 erg s−1 and 0.9 ± 0.7 × 1040 erg s−1, respectively. We derive local escape fractions fesc,912 = 3.4% ± 2.9% and 5.1% ± 4.3% for Knots B and C, respectively. Our Starburst99 modeling shows dominant populations on the order of ∼1–4 Myr and 1–2 × 107M in each knot, with the youngest population in Knot B. Thus, the knot with the strongest LyC detection has the highest LyC production. However, LyC escape is likely less efficient in Knot B than in Knot C due to higher neutral gas covering. Our results therefore stress the importance of the intrinsic ionizing luminosity, and not just the escape fraction, for LyC detection. Similarly, the Lyα escape fraction does not consistently correlate with LyC flux, nor do narrow Lyα red peaks. High observed Lyα luminosity and low Lyα peak velocity separation, however, do correlate with higher LyC escape. Another insight comes from the undetected Knot A, which drives the Green Pea properties of Haro 11. Its density-bounded conditions suggest highly anisotropic LyC escape. Finally, both of the LyC-leaking Knots, B and C, host ultraluminous X-ray sources (ULXs). While stars strongly dominate over the ULXs in LyC emission, this intriguing coincidence underscores the importance of unveiling the role of accretors in LyC escape and reionization.

National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-231534 (URN)10.3847/1538-4357/ad3962 (DOI)001229810600001 ()2-s2.0-85194087869 (Scopus ID)
Available from: 2024-07-23 Created: 2024-07-23 Last updated: 2024-07-23Bibliographically approved
Hsiao, T.-Y. Y., Álvarez-Márquez, J., Coe, D., Crespo Gómez, A., Abdurro’uf, ., Dayal, P., . . . Zitrin, A. (2024). JWST MIRI Detections of Hα and [O III] and a Direct Metallicity Measurement of the z = 10.17 Lensed Galaxy MACS0647-JD. Astrophysical Journal, 973(2), Article ID 81.
Open this publication in new window or tab >>JWST MIRI Detections of Hα and [O III] and a Direct Metallicity Measurement of the z = 10.17 Lensed Galaxy MACS0647-JD
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2024 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 973, no 2, article id 81Article in journal (Refereed) Published
Abstract [en]

JWST spectroscopy has revolutionized our understanding of galaxies in the early Universe. Covering wavelengths up to 5.3 μm, NIRSpec can detect rest-frame optical Hα emission lines out to z = 7 and [O iii] to z = 9.5. Observing these lines in more distant galaxies requires longer wavelength spectroscopy with MIRI. Here we present MIRI Medium Resolution Spectrograph integral field unit observations of the lensed galaxy merger MACS0647-JD at z = 10.165. With exposure times of 4.2 hr in each of two bands (SHORT and LONG), we detect Hα at 9σ, [O iii] λ5008 at 11σ, and [O iii] λ4960 at 3σ. Combined with previously reported NIRSpec spectroscopy that yielded seven emission lines including the auroral line [O iii] λ4363, we present the first direct metallicity measurement of a z > 10 galaxy: 12 + log ( O / H ) = 7.79 ± 0.09 , or 0.13 − 0.03 + 0.02 Z ⊙ . This is similar to galaxies at z ∼ 4-9 with direct metallicity measurements, though higher than expected given the high specific star formation rate log(sSFR/yr−1) = −7.4 ± 0.3. We further constrain the ionization parameter log ( U ) = −1.9 ± 0.1, ionizing photon production efficiency log(ξion) = 25.3 ± 0.1, and SFR = 5.0 ± 0.6 M⊙ yr−1 within the past 10 Myr. These observations demonstrate the combined power of JWST NIRSpec and MIRI for studying galaxies in the first 500 million years.

National Category
Astronomy, Astrophysics and Cosmology Atom and Molecular Physics and Optics
Identifiers
urn:nbn:se:su:diva-237646 (URN)10.3847/1538-4357/ad6562 (DOI)001318988000001 ()2-s2.0-85205391221 (Scopus ID)
Available from: 2025-01-13 Created: 2025-01-13 Last updated: 2025-01-13Bibliographically approved
Organisations
Identifiers
ORCID iD: ORCID iD iconorcid.org/0000-0001-8068-0891

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