{"has_accepted_license":"1","year":"2024","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A89","publication":"Astronomy and Astrophysics","day":"01","file_date_updated":"2024-10-21T11:52:29Z","title":"A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI","publisher":"EDP Sciences","volume":690,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_published":"2024-10-01T00:00:00Z","author":[{"last_name":"Shivaei","full_name":"Shivaei, Irene","first_name":"Irene"},{"full_name":"Alberts, Stacey","first_name":"Stacey","last_name":"Alberts"},{"last_name":"Florian","first_name":"Michael","full_name":"Florian, Michael"},{"first_name":"George","full_name":"Rieke, George","last_name":"Rieke"},{"first_name":"Stijn","full_name":"Wuyts, Stijn","last_name":"Wuyts"},{"last_name":"Bodansky","full_name":"Bodansky, Sarah","first_name":"Sarah"},{"first_name":"Andrew J.","full_name":"Bunker, Andrew J.","last_name":"Bunker"},{"full_name":"Cameron, Alex J.","first_name":"Alex J.","last_name":"Cameron"},{"first_name":"Mirko","full_name":"Curti, Mirko","last_name":"Curti"},{"last_name":"Da'Eugenio","full_name":"Da'Eugenio, Francesco","first_name":"Francesco"},{"last_name":"Dudzevičiūte","full_name":"Dudzevičiūte, Ugne","first_name":"Ugne"},{"first_name":"Zhiyuan","full_name":"Ji, Zhiyuan","last_name":"Ji"},{"last_name":"Johnson","first_name":"Benjamin D.","full_name":"Johnson, Benjamin D."},{"first_name":"Ivan","full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048","last_name":"Kramarenko"},{"last_name":"Lyu","first_name":"Jianwei","full_name":"Lyu, Jianwei"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Morrison","full_name":"Morrison, Jane","first_name":"Jane"},{"last_name":"Naidu","first_name":"Rohan","full_name":"Naidu, Rohan"},{"last_name":"Pérez-González","full_name":"Pérez-González, Pablo G.","first_name":"Pablo G."},{"last_name":"Reddy","first_name":"Naveen","full_name":"Reddy, Naveen"},{"first_name":"Brant","full_name":"Robertson, Brant","last_name":"Robertson"},{"first_name":"Yang","full_name":"Sun, Yang","last_name":"Sun"},{"last_name":"Tacchella","full_name":"Tacchella, Sandro","first_name":"Sandro"},{"first_name":"Katherine","full_name":"Whitaker, Katherine","last_name":"Whitaker"},{"last_name":"Williams","first_name":"Christina C.","full_name":"Williams, Christina C."},{"first_name":"Christopher N.A.","full_name":"Willmer, Christopher N.A.","last_name":"Willmer"},{"last_name":"Witstok","first_name":"Joris","full_name":"Witstok, Joris"},{"last_name":"Xiao","full_name":"Xiao, Mengyuan","first_name":"Mengyuan"},{"first_name":"Yongda","full_name":"Zhu, Yongda","last_name":"Zhu"}],"month":"10","article_type":"original","OA_place":"publisher","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"doi":"10.1051/0004-6361/202449579","publication_status":"published","ddc":["520"],"acknowledgement":"IS thanks the members of the JWST/MIRI instrument team for their exceptional efforts and for providing an outstanding experience during the commissioning period of JWST, which fostered numerous fruitful discussions and significantly enhanced the quality of data reduction in this study. IS also thanks Karin Sandstrom and Joel Leja for their insightful discussions during the scientific development of this work. Additionally, IS acknowledges the contribution of Andras Gáspar to the construction of the F560W PSF utilised in this research. This work was supported in part by NASA grant NNX13AD82G. Part of this research has been funded by Atraccíon de Talento Grant No. 2022-T1/TIC-20472 of the Comunidad de Madrid, Spain. AJB and AC acknowledges funding from the ‘FirstGalaxies’ Advanced Grant from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (Grant agreement No. 789056). The work of CCW is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. PGP-G acknowledges support from grant PID2022-139567NB-I00 funded by Spanish Ministerio de Ciencia e Innovación CIN/AEI/10.13039/501100011033, FEDER Una manera de hacer Europa. SA acknowledges support from the JWST Mid-Infrared Instrument (MIRI) Science Team Lead, grant 80NSSC18K0555, from NASA Goddard Space Flight Center to the University of Arizona. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program PID 1207, 1080, 1081, 1895, 1220, 1286, 1287, 1963. Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESAC/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA).","type":"journal_article","oa_version":"Published Version","OA_type":"hybrid","quality_controlled":"1","abstract":[{"text":"Aims. This paper utilises the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) to extend the observational studies of dust and polycyclic aromatic hydrocarbon (PAH) emission to a new mass and star formation rate (SFR) parameter space beyond our local Universe. The combination of fully sampled spectral energy distributions (SEDs) with multiple mid-infrared (mid-IR) bands and the unprecedented sensitivity of MIRI allows us to investigate dust obscuration and PAH behaviour from z = 0.7 up to z = 2 in typical main-sequence galaxies. Our focus is on constraining the evolution of PAH strength and the dust-obscured luminosity fraction before and during cosmic noon, the epoch of peak star formation activity in the Universe.\r\n\r\nMethods. In this study, we utilise MIRI multi-band imaging data from the SMILES survey (5 to 25 μm), complemented with NIRCam photometry from the JADES survey (1 to 5 μm), available HST photometry (0.4 to 0.9 μm), and spectroscopic redshifts from the FRESCO and JADES surveys in GOODS-S for 443 star-forming (without dominant active galactic nucleus (AGN)) galaxies at z = 0.7 − 2.0. This redshift range was chosen to ensure that the MIRI data cover mid-IR dust emission. Our methodology involved employing ultraviolet (UV) to IR energy balance SED fitting to robustly constrain the fraction of dust mass in PAHs and dust-obscured luminosity. Additionally, we inferred dust sizes from MIRI 15 μm imaging data, enhancing our understanding of the physical characteristics of dust within these galaxies.\r\n\r\nResults. We find a strong correlation between the fraction of dust in PAHs (PAH fraction, qPAH) with stellar mass. Moreover, the sub-sample with robust qPAH measurements (N = 216) shows a similar behaviour between qPAH and gas-phase metallicity to that at z ∼ 0, suggesting a universal relation: qPAH is constant (∼3.4%) above a metallicity of Z ∼ 0.5 Z⊙ and decreases to < 1% at metallicities ≲0.3 Z⊙. This indicates that metallicity is a good indicator of the interstellar medium properties that affect the balance between the formation and destruction of PAHs. The lack of a redshift evolution from z ∼ 0 − 2 also implies that above Z ∼ 0.5 Z⊙ the PAH emission effectively traces obscured luminosity and the previous locally calibrated PAH-SFR calibrations remain applicable in this metallicity regime. We observe a strong correlation between the obscured UV luminosity fraction (ratio of obscured to total luminosity) and stellar mass. Above the stellar mass of M* > 5 × 109 M⊙, on average, more than half of the emitted luminosity is obscured, while there exists a non-negligible population of lower-mass galaxies with > 50% obscured fractions. At a fixed mass, the obscured fraction correlates with SFR surface density. This is a result of higher dust covering fractions in galaxies with more compact star-forming regions. Similarly, galaxies with high IRX (IR to UV luminosity) at a given mass or UV continuum slope (β) tend to have higher ΣSFR and shallower attenuation curves, owing to their higher effective dust optical depths and more compact star-forming regions.","lang":"eng"}],"article_processing_charge":"Yes (in subscription journal)","file":[{"success":1,"file_id":"18458","date_updated":"2024-10-21T11:52:29Z","checksum":"f399be98968b9ca5611c832a9b1eee2b","relation":"main_file","access_level":"open_access","file_name":"2024_AstronomyAstrophysics_Shivaei.pdf","creator":"dernst","file_size":10777358,"content_type":"application/pdf","date_created":"2024-10-21T11:52:29Z"}],"date_created":"2024-10-20T22:02:06Z","intvolume":"       690","status":"public","date_updated":"2024-10-21T11:59:29Z","_id":"18448","language":[{"iso":"eng"}],"oa":1,"external_id":{"arxiv":["2402.07989"]},"scopus_import":"1","citation":{"ista":"Shivaei I, Alberts S, Florian M, Rieke G, Wuyts S, Bodansky S, Bunker AJ, Cameron AJ, Curti M, Da’Eugenio F, Dudzevičiūte U, Ji Z, Johnson BD, Kramarenko I, Lyu J, Matthee JJ, Morrison J, Naidu R, Pérez-González PG, Reddy N, Robertson B, Sun Y, Tacchella S, Whitaker K, Williams CC, Willmer CNA, Witstok J, Xiao M, Zhu Y. 2024. A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. Astronomy and Astrophysics. 690, A89.","apa":"Shivaei, I., Alberts, S., Florian, M., Rieke, G., Wuyts, S., Bodansky, S., … Zhu, Y. (2024). A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202449579\">https://doi.org/10.1051/0004-6361/202449579</a>","short":"I. Shivaei, S. Alberts, M. Florian, G. Rieke, S. Wuyts, S. Bodansky, A.J. Bunker, A.J. Cameron, M. Curti, F. Da’Eugenio, U. Dudzevičiūte, Z. Ji, B.D. Johnson, I. Kramarenko, J. Lyu, J.J. Matthee, J. Morrison, R. Naidu, P.G. Pérez-González, N. Reddy, B. Robertson, Y. Sun, S. Tacchella, K. Whitaker, C.C. Williams, C.N.A. Willmer, J. Witstok, M. Xiao, Y. Zhu, Astronomy and Astrophysics 690 (2024).","chicago":"Shivaei, Irene, Stacey Alberts, Michael Florian, George Rieke, Stijn Wuyts, Sarah Bodansky, Andrew J. Bunker, et al. “A New Census of Dust and Polycyclic Aromatic Hydrocarbons at z = 0.7-2 with JWST MIRI.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202449579\">https://doi.org/10.1051/0004-6361/202449579</a>.","ama":"Shivaei I, Alberts S, Florian M, et al. A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. <i>Astronomy and Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202449579\">10.1051/0004-6361/202449579</a>","mla":"Shivaei, Irene, et al. “A New Census of Dust and Polycyclic Aromatic Hydrocarbons at z = 0.7-2 with JWST MIRI.” <i>Astronomy and Astrophysics</i>, vol. 690, A89, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202449579\">10.1051/0004-6361/202449579</a>.","ieee":"I. Shivaei <i>et al.</i>, “A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI,” <i>Astronomy and Astrophysics</i>, vol. 690. EDP Sciences, 2024."}}