CEERS: Spatially Resolved UV and Mid-infrared Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

Lu Shen; Casey Papovich; Guang Yang; Jasleen Matharu; Xin Wang; Benjamin Magnelli; David Elbaz; Shardha Jogee; Anahita Alavi; Pablo Arrabal Haro; Bren E. Backhaus; Micaela B. Bagley; Eric F. Bell; Laura Bisigello; Antonello Calabrò; M. C. Cooper; Luca Costantin; Emanuele Daddi; Mark Dickinson; Steven L. Finkelstein; Seiji Fujimoto; Mauro Giavalisco; Norman A. Grogin; Yuchen Guo; Benne W. Holwerda; Jeyhan S. Kartaltepe; Anton M. Koekemoer; Peter Kurczynski; Ray A. Lucas; Pablo G. Pérez-González; Nor Pirzkal; Laura Prichard; Marc Rafelski; Kaila Ronayne; Raymond C. Simons; Ben Sunnquist; Harry I. Teplitz; Jonathan R. Trump; Benjamin J. Weiner; Rogier A. Windhorst; L. Y.Aaron Yung

doi:10.3847/1538-4357/acc944

CEERS: Spatially Resolved UV and Mid-infrared Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

Lu Shen, Casey Papovich, Guang Yang, Jasleen Matharu, Xin Wang, Benjamin Magnelli, David Elbaz, Shardha Jogee, Anahita Alavi, Pablo Arrabal Haro, Bren E. Backhaus, Micaela B. Bagley, Eric F. Bell, Laura Bisigello, Antonello Calabrò, M. C. Cooper, Luca Costantin, Emanuele Daddi, Mark Dickinson, Steven L. FinkelsteinSeiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Yuchen Guo, Benne W. Holwerda, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Peter Kurczynski, Ray A. Lucas, Pablo G. Pérez-González, Nor Pirzkal, Laura Prichard, Marc Rafelski, Kaila Ronayne, Raymond C. Simons, Ben Sunnquist, Harry I. Teplitz, Jonathan R. Trump, Benjamin J. Weiner, Rogier A. Windhorst, L. Y.Aaron Yung

Earth and Space Exploration, School of (SESE)

Research output: Contribution to journal › Article › peer-review

10 Scopus citations

Abstract

We present the mid-infrared (MIR) morphologies for 64 star-forming galaxies (SFGs) at 0.2 < z < 2.5 with stellar mass M _* > 10⁹ M _⊙ using James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) observations from the Cosmic Evolution Early Release Science survey. The MIRI bands span the MIR (7.7-21 μm), enabling us to measure the effective radii (R _eff) and Sérsic indexes of these SFGs at rest-frame 6.2 and 7.7 μm, which contains strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We define a “PAH band” as the MIRI bandpass that contains these features at the redshift of the galaxy. We then compare the galaxy morphologies in the PAH bands to those in the rest-frame near-ultraviolet (NUV) using Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS)/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging from UVCANDELS and CANDELS. The R _eff of galaxies in the PAH band are slightly smaller (∼10%) than those in F160W for galaxies with M _* ≳ 10^9.5 M _⊙ at z ≤ 1.2, but the PAH band and F160W have similar fractions of light within 1 kpc. In contrast, the R _eff of galaxies in the NUV band are larger, with lower fractions of light within 1 kpc compared to F160W for galaxies at z ≤ 1.2. Using the MIRI data to estimate the SFR_IR surface density, we find that the correlation between the SFR_IR surface density and stellar mass has a steeper slope than that of the SFR_UV surface density and stellar mass, suggesting more massive galaxies having increasing amounts of obscured fraction of star formation in their inner regions. This paper demonstrates how the high-angular resolution data from JWST/MIRI can reveal new information about the morphology of obscured star formation.

Original language	English (US)
Article number	7
Journal	Astrophysical Journal
Volume	950
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/acc944
State	Published - Jun 1 2023

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/acc944

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Shen, L., Papovich, C., Yang, G., Matharu, J., Wang, X., Magnelli, B., Elbaz, D., Jogee, S., Alavi, A., Arrabal Haro, P., Backhaus, B. E., Bagley, M. B., Bell, E. F., Bisigello, L., Calabrò, A., Cooper, M. C., Costantin, L., Daddi, E., Dickinson, M., ... Yung, L. Y. A. (2023). CEERS: Spatially Resolved UV and Mid-infrared Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes. Astrophysical Journal, 950(1), Article 7. https://doi.org/10.3847/1538-4357/acc944

Shen, L, Papovich, C, Yang, G, Matharu, J, Wang, X, Magnelli, B, Elbaz, D, Jogee, S, Alavi, A, Arrabal Haro, P, Backhaus, BE, Bagley, MB, Bell, EF, Bisigello, L, Calabrò, A, Cooper, MC, Costantin, L, Daddi, E, Dickinson, M, Finkelstein, SL, Fujimoto, S, Giavalisco, M, Grogin, NA, Guo, Y, Holwerda, BW, Kartaltepe, JS, Koekemoer, AM, Kurczynski, P, Lucas, RA, Pérez-González, PG, Pirzkal, N, Prichard, L, Rafelski, M, Ronayne, K, Simons, RC, Sunnquist, B, Teplitz, HI, Trump, JR, Weiner, BJ, Windhorst, RA & Yung, LYA 2023, 'CEERS: Spatially Resolved UV and Mid-infrared Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes', Astrophysical Journal, vol. 950, no. 1, 7. https://doi.org/10.3847/1538-4357/acc944

@article{0237736df0fe42b089aed1d289efdd4a,

title = "CEERS: Spatially Resolved UV and Mid-infrared Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes",

abstract = "We present the mid-infrared (MIR) morphologies for 64 star-forming galaxies (SFGs) at 0.2 < z < 2.5 with stellar mass M * > 109 M ⊙ using James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) observations from the Cosmic Evolution Early Release Science survey. The MIRI bands span the MIR (7.7-21 μm), enabling us to measure the effective radii (R eff) and S{\'e}rsic indexes of these SFGs at rest-frame 6.2 and 7.7 μm, which contains strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We define a “PAH band” as the MIRI bandpass that contains these features at the redshift of the galaxy. We then compare the galaxy morphologies in the PAH bands to those in the rest-frame near-ultraviolet (NUV) using Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS)/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging from UVCANDELS and CANDELS. The R eff of galaxies in the PAH band are slightly smaller (∼10%) than those in F160W for galaxies with M * ≳ 109.5 M ⊙ at z ≤ 1.2, but the PAH band and F160W have similar fractions of light within 1 kpc. In contrast, the R eff of galaxies in the NUV band are larger, with lower fractions of light within 1 kpc compared to F160W for galaxies at z ≤ 1.2. Using the MIRI data to estimate the SFRIR surface density, we find that the correlation between the SFRIR surface density and stellar mass has a steeper slope than that of the SFRUV surface density and stellar mass, suggesting more massive galaxies having increasing amounts of obscured fraction of star formation in their inner regions. This paper demonstrates how the high-angular resolution data from JWST/MIRI can reveal new information about the morphology of obscured star formation.",

author = "Lu Shen and Casey Papovich and Guang Yang and Jasleen Matharu and Xin Wang and Benjamin Magnelli and David Elbaz and Shardha Jogee and Anahita Alavi and {Arrabal Haro}, Pablo and Backhaus, {Bren E.} and Bagley, {Micaela B.} and Bell, {Eric F.} and Laura Bisigello and Antonello Calabr{\`o} and Cooper, {M. C.} and Luca Costantin and Emanuele Daddi and Mark Dickinson and Finkelstein, {Steven L.} and Seiji Fujimoto and Mauro Giavalisco and Grogin, {Norman A.} and Yuchen Guo and Holwerda, {Benne W.} and Kartaltepe, {Jeyhan S.} and Koekemoer, {Anton M.} and Peter Kurczynski and Lucas, {Ray A.} and P{\'e}rez-Gonz{\'a}lez, {Pablo G.} and Nor Pirzkal and Laura Prichard and Marc Rafelski and Kaila Ronayne and Simons, {Raymond C.} and Ben Sunnquist and Teplitz, {Harry I.} and Trump, {Jonathan R.} and Weiner, {Benjamin J.} and Windhorst, {Rogier A.} and Yung, {L. Y.Aaron}",

note = "Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = jun,

day = "1",

doi = "10.3847/1538-4357/acc944",

language = "English (US)",

volume = "950",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "1",

}

TY - JOUR

T1 - CEERS

T2 - Spatially Resolved UV and Mid-infrared Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

AU - Shen, Lu

AU - Papovich, Casey

AU - Yang, Guang

AU - Matharu, Jasleen

AU - Wang, Xin

AU - Magnelli, Benjamin

AU - Elbaz, David

AU - Jogee, Shardha

AU - Alavi, Anahita

AU - Arrabal Haro, Pablo

AU - Backhaus, Bren E.

AU - Bagley, Micaela B.

AU - Bell, Eric F.

AU - Bisigello, Laura

AU - Calabrò, Antonello

AU - Cooper, M. C.

AU - Costantin, Luca

AU - Daddi, Emanuele

AU - Dickinson, Mark

AU - Finkelstein, Steven L.

AU - Fujimoto, Seiji

AU - Giavalisco, Mauro

AU - Grogin, Norman A.

AU - Guo, Yuchen

AU - Holwerda, Benne W.

AU - Kartaltepe, Jeyhan S.

AU - Koekemoer, Anton M.

AU - Kurczynski, Peter

AU - Lucas, Ray A.

AU - Pérez-González, Pablo G.

AU - Pirzkal, Nor

AU - Prichard, Laura

AU - Rafelski, Marc

AU - Ronayne, Kaila

AU - Simons, Raymond C.

AU - Sunnquist, Ben

AU - Teplitz, Harry I.

AU - Trump, Jonathan R.

AU - Weiner, Benjamin J.

AU - Windhorst, Rogier A.

AU - Yung, L. Y.Aaron

PY - 2023/6/1

Y1 - 2023/6/1

N2 - We present the mid-infrared (MIR) morphologies for 64 star-forming galaxies (SFGs) at 0.2 < z < 2.5 with stellar mass M * > 109 M ⊙ using James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) observations from the Cosmic Evolution Early Release Science survey. The MIRI bands span the MIR (7.7-21 μm), enabling us to measure the effective radii (R eff) and Sérsic indexes of these SFGs at rest-frame 6.2 and 7.7 μm, which contains strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We define a “PAH band” as the MIRI bandpass that contains these features at the redshift of the galaxy. We then compare the galaxy morphologies in the PAH bands to those in the rest-frame near-ultraviolet (NUV) using Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS)/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging from UVCANDELS and CANDELS. The R eff of galaxies in the PAH band are slightly smaller (∼10%) than those in F160W for galaxies with M * ≳ 109.5 M ⊙ at z ≤ 1.2, but the PAH band and F160W have similar fractions of light within 1 kpc. In contrast, the R eff of galaxies in the NUV band are larger, with lower fractions of light within 1 kpc compared to F160W for galaxies at z ≤ 1.2. Using the MIRI data to estimate the SFRIR surface density, we find that the correlation between the SFRIR surface density and stellar mass has a steeper slope than that of the SFRUV surface density and stellar mass, suggesting more massive galaxies having increasing amounts of obscured fraction of star formation in their inner regions. This paper demonstrates how the high-angular resolution data from JWST/MIRI can reveal new information about the morphology of obscured star formation.

AB - We present the mid-infrared (MIR) morphologies for 64 star-forming galaxies (SFGs) at 0.2 < z < 2.5 with stellar mass M * > 109 M ⊙ using James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) observations from the Cosmic Evolution Early Release Science survey. The MIRI bands span the MIR (7.7-21 μm), enabling us to measure the effective radii (R eff) and Sérsic indexes of these SFGs at rest-frame 6.2 and 7.7 μm, which contains strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We define a “PAH band” as the MIRI bandpass that contains these features at the redshift of the galaxy. We then compare the galaxy morphologies in the PAH bands to those in the rest-frame near-ultraviolet (NUV) using Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS)/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging from UVCANDELS and CANDELS. The R eff of galaxies in the PAH band are slightly smaller (∼10%) than those in F160W for galaxies with M * ≳ 109.5 M ⊙ at z ≤ 1.2, but the PAH band and F160W have similar fractions of light within 1 kpc. In contrast, the R eff of galaxies in the NUV band are larger, with lower fractions of light within 1 kpc compared to F160W for galaxies at z ≤ 1.2. Using the MIRI data to estimate the SFRIR surface density, we find that the correlation between the SFRIR surface density and stellar mass has a steeper slope than that of the SFRUV surface density and stellar mass, suggesting more massive galaxies having increasing amounts of obscured fraction of star formation in their inner regions. This paper demonstrates how the high-angular resolution data from JWST/MIRI can reveal new information about the morphology of obscured star formation.

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CEERS: Spatially Resolved UV and Mid-infrared Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

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