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2023
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Astrophysical processes
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Your conditions: Micaela B. Bagley

1. ChinaXiv:202303.05800
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First Look at z > 1 Bars in the Rest-Frame Near-Infrared with JWST Early CEERS Imaging

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Yuchen Guo Shardha Jogee Steven L. Finkelstein Zilei Chen Eden Wise Micaela B. Bagley Guillermo Barro Stijn Wuyts Dale D. Kocevski Jeyhan S. Kartaltepe Elizabeth J. McGrath Henry C. Ferguson Bahram Mobasher Mauro Giavalisco Ray A. Lucas Jorge A. Zavala Jennifer M. Lotz Norman A. Grogin Marc Huertas-Company Jesús Vega-Ferrero

Abstract： Stellar bars are key drivers of secular evolution in galaxies and can be effectively studied using rest-frame near-infrared (NIR) images, which trace the underlying stellar mass and are less impacted by dust and star formation than rest-frame UV or optical images. We leverage the power of {\it{JWST}} CEERS NIRCam images to present the first quantitative identification and characterization of stellar bars at $z>1$ based on rest-frame NIR F444W images of high resolution (~1.3 kpc at z ~ 1-3). We identify stellar bars in these images using quantitative criteria based on ellipse fits. For this pilot study, we present six examples of robustly identified bars at $z>1$ with spectroscopic redshifts, including the two highest redshift bars at ~2.136 and 2.312 quantitatively identified and characterized to date. The stellar bars at $z$ ~ 1.1-2.3 presented in our study have projected semi-major axes of ~2.9-4.3 kpc and projected ellipticities of ~0.41-0.53 in the rest-frame NIR. The barred host galaxies have stellar masses ~ $ 1 \times 10^{10}$ to $2 \times 10^{11}$ $M_{\odot}$, star formation rates of ~ 21-295 $M_{\odot}$ yr$^{-1}$, and several have potential nearby companions. Our finding of bars at $z$ ~1.1-2.3 demonstrates the early onset of such instabilities and supports simulations where bars form early in massive dynamically cold disks. It also suggests that if these bars at lookback times of 8-10 Gyr survive out to present epochs, bar-driven secular processes may operate over a long time and have a significant impact on some galaxies by z ~ 0.

Peer Review Status:Awaiting Review

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2. ChinaXiv:202303.03091
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Hidden Little Monsters: Spectroscopic Identification of Low-Mass, Broad-Line AGN at $z>5$ with CEERS

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Dale D. Kocevski Masafusa Onoue Kohei Inayoshi Jonathan R. Trump Pablo Arrabal Haro Andrea Grazian Mark Dickinson Steven L. Finkelstein Jeyhan S. Kartaltepe Michaela Hirschmann Seiji Fujimoto Stephanie Juneau Ricardo O. Amorin Micaela B. Bagley Guillermo Barro Eric F. Bell Laura Bisigello Antonello Calabro Nikko J. Cleri M. C. Cooper

Abstract： We report on the discovery of two low-luminosity, broad-line AGN at $z>5$ identified using JWST NIRSpec spectroscopy from the CEERS Survey. We detect broad H$\alpha$ emission from both sources, with FWHM of $2038\pm286$ and $1807\pm207$ km s$^{-1}$, resulting in black hole (BH) masses that are 1-2 dex below that of existing samples of luminous quasars at $z>5$. The first source, CEERS 1670 at $z=5.242$, is 2-3 dex fainter than known quasars at similar redshifts and was previously identified as a candidate low-luminosity AGN based on its rest-frame optical SED. We measure a BH mass of $M_{\rm BH}=1.3\pm0.4\times 10^{7}~M_{\odot}$, confirming that this AGN is powered by the least-massive BH known in the universe at the end of cosmic reionization. The second source, CEERS 3210 at $z=5.624$, is inferred to be a heavily obscured, broad-line AGN caught in a transition phase between a dust-obscured starburst and an unobscured quasar. We estimate its BH mass to be $M_{\rm BH}\simeq 0.9-4.7 \times 10^{7}~M_{\odot}$, depending on the level of dust obscuration assumed. We derive host stellar masses, $M_\star$, allowing us to place constraints on the BH-galaxy mass relationship in the lowest mass range yet probed in the early universe. The $M_{\rm BH}/M_\star$ ratio for CEERS 1670, in particular, is consistent with or higher than the empirical relationship seen in massive galaxies at $z=0$. We examine the emission-line ratios of both sources and find that their location on the BPT and OHNO diagrams is consistent with model predictions for low-metallicity AGN with $Z/Z_\odot \simeq 0.2-0.4$. The spectroscopic identification of low-luminosity, broad-line AGN at $z>5$ with $M_{\rm BH}\simeq 10^{7}~M_{\odot}$ demonstrates the capability of JWST to push BH masses closer to the range predicted for the BH seed population and provides a unique opportunity to study the early stages of BH-galaxy assembly.

Peer Review Status:Awaiting Review

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3. ChinaXiv:202303.04807
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CEERS Key Paper I: An Early Look into the First 500 Myr of Galaxy Formation with JWST

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Steven L. Finkelstein Micaela B. Bagley Henry C. Ferguson Stephen M. Wilkins Jeyhan S. Kartaltepe Casey Papovich L. Y. Aaron Yung Pablo Arrabal Haro Peter Behroozi Mark Dickinson Dale D. Kocevski Anton M. Koekemoer Rebecca L. Larson Aurelien Le Bail Alexa M. Morales Pablo G. Perez-Gonzalez Denis Burgarella Romeel Dave Michaela Hirschmann Rachel S. Somerville

Abstract： We present an investigation into the first 500 Myr of galaxy evolution from the Cosmic Evolution Early Release Science (CEERS) survey. CEERS, one of 13 JWST ERS programs, targets galaxy formation from z~0.5 to z>10 using several imaging and spectroscopic modes. We make use of the first epoch of CEERS NIRCam imaging, spanning 35.5 sq. arcmin, to search for candidate galaxies at z>9. Following a detailed data reduction process implementing several custom steps to produce high-quality reduced images, we perform multi-band photometry across seven NIRCam broad and medium-band (and six Hubble broadband) filters focusing on robust colors and accurate total fluxes. We measure photometric redshifts and devise a robust set of selection criteria to identify a sample of 26 galaxy candidates at z~9-16. These objects are compact with a median half-light radius of ~0.5 kpc. We present an early estimate of the z~11 rest-frame ultraviolet (UV) luminosity function, finding that the number density of galaxies at M_UV ~ -20 appears to evolve very little from z~9 to z~11. We also find that the abundance (surface density [arcmin^-2]) of our candidates exceeds nearly all theoretical predictions. We explore potential implications, including that at z>10 star formation may be dominated by top-heavy initial mass functions, which would result in an increased ratio of UV light per unit halo mass, though a complete lack of dust attenuation and/or changing star-formation physics may also play a role. While spectroscopic confirmation of these sources is urgently required, our results suggest that the deeper views to come with JWST should yield prolific samples of ultra-high-redshift galaxies with which to further explore these conclusions.

Peer Review Status:Awaiting Review

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4. ChinaXiv:202303.03219
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Dusty Starbursts Masquerading as Ultra-high Redshift Galaxies in JWST CEERS Observations

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Jorge A. Zavala Veronique Buat Caitlin M. Casey Denis Burgarella Steven L. Finkelstein Micaela B. Bagley Laure Ciesla Emanuele Daddi Mark Dickinson Henry C. Ferguson Maximilien Franco E. F. Jim'enez-Andrade Jeyhan S. Kartaltepe Anton M. Koekemoer Aurélien Le Bail E. J. Murphy Casey Papovich Sandro Tacchella Stephen M. Wilkins Itziar Aretxaga

Abstract： Lyman Break Galaxy (LBG) candidates at z>10 are rapidly being identified in JWST/NIRCam observations. Due to the (redshifted) break produced by neutral hydrogen absorption of rest-frame UV photons, these sources are expected to drop out in the bluer filters while being well detected in redder filters. However, here we show that dust-enshrouded star-forming galaxies at lower redshifts (z<7) may also mimic the near-infrared (near-IR) colors of z>10 LBGs, representing potential contaminants in LBG candidate samples. First, we analyze CEERS-DSFG-1, a NIRCam dropout undetected in the F115W and F150W filters but detected at longer wavelengths. Combining the JWST data with (sub)millimeter constraints, including deep NOEMA interferometric observations, we show that this source is a dusty star-forming galaxy (DSFG) at z~5.1. We also present a tentative 2.6sigma SCUBA-2 detection at 850um around a recently identified z~16 LBG candidate in the same field and show that, if the emission is real and associated with this candidate, the available photometry is consistent with a z~5 dusty galaxy with strong nebular emission lines despite its blue near-IR colors. Further observations on this candidate are imperative to mitigate the low confidence of this tentative submillimeter emission and its positional uncertainty. Our analysis shows that robust (sub)millimeter detections of NIRCam dropout galaxies likely imply z=4-6 redshift solutions, where the observed near-IR break would be the result of a strong rest-frame optical Balmer break combined with high dust attenuation and strong nebular line emission, rather than the rest-frame UV Lyman break. This provides evidence that DSFGs may contaminate searches for ultra high-redshift LBG candidates from JWST observations.

Peer Review Status:Awaiting Review

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5. ChinaXiv:202303.05629
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CEERS Epoch 1 NIRCam Imaging: Reduction Methods and Simulations Enabling Early JWST Science Results

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Micaela B. Bagley Steven L. Finkelstein Anton M. Koekemoer Henry C. Ferguson Pablo Arrabal Haro Mark Dickinson Jeyhan S. Kartaltepe Casey Papovich Pablo G. Pérez-González Nor Pirzkal Rachel S. Somerville Christopher N. A. Willmer Guang Yang L. Y. Aaron Yung Adriano Fontana Andrea Grazian Norman A. Grogin Michaela Hirschmann Lisa J. Kewley Allison Kirkpatrick

Abstract： We present the data release and data reduction process for the Epoch 1 NIRCam observations for the Cosmic Evolution Early Release Science Survey (CEERS). These data consist of NIRCam imaging in six broadband filters (F115W, F150W, F200W, F277W, F356W and F444W) and one medium band filter (F410M) over four pointings, obtained in parallel with primary CEERS MIRI observations (Yang et al. in prep). We reduced the NIRCam imaging with the JWST Calibration Pipeline, with custom modifications and reduction steps designed to address additional features and challenges with the data. Here we provide a detailed description of each step in our reduction and a discussion of future expected improvements. Our reduction process includes corrections for known pre-launch issues such as 1/f noise, as well as in-flight issues including snowballs, wisps, and astrometric alignment. Many of our custom reduction processes were first developed with pre-launch simulated NIRCam imaging over the full 10 CEERS NIRCam pointings. We present a description of the creation and reduction of this simulated dataset in the Appendix. We provide mosaics of the real images in a public release, as well as our reduction scripts with detailed explanations to allow users to reproduce our final data products. These represent one of the first official public datasets released from the Directors Discretionary Early Release Science (DD-ERS) program.

Peer Review Status:Awaiting Review

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6. ChinaXiv:202303.03680
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The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Micaela B. Bagley Nor Pirzkal Steven L. Finkelstein Casey Papovich Danielle A. Berg Jennifer M. Lotz Gene C. K. Leung Henry C. Ferguson Anton M. Koekemoer Mark Dickinson Jeyhan S. Kartaltepe Dale D. Kocevski Rachel S. Somerville L. Y. Aaron Yung Bren E. Backhaus Caitlin M. Casey Marco Castellano Óscar A. Chávez Ortiz Katherine Chworowsky Isabella G. Cox

Abstract： We present the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey, a deep slitless spectroscopic and imaging Cycle 1 JWST treasury survey designed to constrain feedback mechanisms in low-mass galaxies across cosmic time. NGDEEP targets the Hubble Ultra Deep Field (HUDF) with NIRISS slitless spectroscopy (f~1.2e-18 erg/s/cm^2, 5sigma) to measure metallicities and star-formation rates (SFRs) for low-mass galaxies through the peak of the cosmic SFR density (0.512, constraining the slope of the faint-end of the rest-ultraviolet luminosity function. NGDEEP overlaps with the deepest HST ACS optical imaging in the sky: F435W in the HUDF (m=29.6), and F814W in HUDF-Par2 (m=30), making this a premier HST+JWST Deep Field. As a treasury survey, NGDEEP data is public immediately, and we will rapidly release data products and catalogs in the spirit of previous deep field initiatives. In this paper we present the NGDEEP survey design, summarize the science goals, and detail plans for the public release of NGDEEP reduced data products.

Peer Review Status:Awaiting Review

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7. ChinaXiv:202303.03570
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ALMA FIR View of Ultra High-redshift Galaxy Candidates at $z\sim$ 11-17: Blue Monsters or Low-$z$ Red Interlopers?

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Seiji Fujimoto Steven L. Finkelstein Denis Burgarella Chris L. Carilli Véronique Buat Caitlin M. Casey Laure Ciesla Sandro Tacchella Jorge A. Zavala Gabriel Brammer Yoshinobu Fudamoto Masami Ouchi Francesco Valentino M. C. Cooper Mark Dickinson Maximilien Franco Mauro Giavalisco Taylor A. Hutchison Jeyhan S. Kartaltepe Anton M. Koekemoer

Abstract： We present ALMA Band 7 observations of a remarkably bright galaxy candidate at $z_{\rm phot}$=$16.7^{+1.9}_{-0.3}$ ($M_{\rm UV}$=$-21.6$), S5-z17-1, identified in JWST Early Release Observation data of Stephen's Quintet. We do not detect the dust continuum at 866 $\mu$m, ruling out the possibility that S5-z17-1 is a low-$z$ dusty starburst with a star-formation rate (SFR) of $\gtrsim 30\,M_{\odot}$ yr$^{-1}$. We detect a 5.1$\sigma$ line feature at $338.726\pm0.007$ GHz exactly coinciding with the JWST source position, with a 2% likelihood of the signal being spurious. The most likely line identification would be [OIII]52$\mu$m at $z=16.01$ or [CII]158$\mu$m at $z=4.61$, whose line luminosities do not violate the non-detection of the dust continuum in both cases. Together with three other $z\gtrsim$ 11-13 candidate galaxies recently observed with ALMA, we conduct a joint ALMA and JWST spectral energy distribution (SED) analysis and find that the high-$z$ solution at $z\sim$11-17 is favored in every candidate as a very blue (UV continuum slope of $\approx-2.3$) and luminous ($M_{\rm UV}$ $\approx$ [$-$24:$-$21]) system. Still, we find in some candidates that reasonable SED fits ($\Delta$ $\chi^{2}\lesssim4$) are reproduced by type-II quasar and/or quiescent galaxy templates with strong emission lines at $z\sim3$-5, where such populations predicted from their luminosity functions and EW([OIII]+H$\beta$) distributions are abundant in survey volumes used for the $z\sim$11-17 candidates. While these recent ALMA observation results have strengthened the likelihood of the high-$z$ solutions, lower-$z$ possibilities are not completely ruled out in some of the $z\sim$11-17 candidates.

Peer Review Status:Awaiting Review

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8. ChinaXiv:202303.03693
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New $z > 7$ Lyman-alpha Emitters in EGS: Evidence of an Extended Ionized Structure at $z \sim 7.7$

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Intae Jung Steven L. Finkelstein Rebecca L. Larson Taylor A. Hutchison Amber N. Straughn Micaela B. Bagley Marco Castellano Nikko J. Cleri M. C. Cooper Mark Dickinson Henry C. Ferguson Benne W. Holwerda Jeyhan S. Kartaltepe Seonwoo Kim Anton M. Koekemoer Casey Papovich Hyunbae Park Laura Pentericci Pablo G. Perez-Gonzalez Mimi Song

Abstract： We perform a ground-based near-infrared spectroscopic survey using the Keck/MOSFIRE spectrograph to target Ly$\alpha$ emission at $7.0$4$\sigma$ level in eight $z>7$ galaxies, which include additional members of the known $z\sim7.7$ Ly$\alpha$-emitter (LAE) cluster (Tilvi et al. 2020). With the addition of these newly-discovered $z\sim7.7$ LAEs, this is currently the largest measured LAE cluster at $z>7$. The unusually-high Ly$\alpha$ detection rate at $z\sim7.7$ in this field suggests significantly stronger Ly$\alpha$ emission from the clustered LAEs than from the rest of our targets. We estimate the ionized bubble sizes around these LAEs and conclude that the LAEs are clustered within an extended ionized structure created by overlapping ionized bubbles which allow the easier escape of Ly$\alpha$ from galaxies. It is remarkable that the brightest object in the cluster has the lowest measured redshift of the Ly$\alpha$ line, being placed in front of the other LAEs in the line-of-sight direction. This suggests that we are witnessing the enhanced IGM transmission of Ly$\alpha$ from galaxies on the rear side of an ionized area. This could be a consequence of Ly$\alpha$ radiative transfer: Ly$\alpha$ close to the central velocity is substantially scattered by the IGM while Ly$\alpha$ from the rear-side galaxies is significantly redshifted to where it has a clear path.

Peer Review Status:Awaiting Review

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9. ChinaXiv:202303.03324
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CEERS Key Paper V: A triality on the nature of HST-dark galaxies

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Pablo G. Pérez-González Guillermo Barro Marianna Annunziatella Luca Costantin Ángela García-Argumánez Elizabeth J. McGrath Rosa M. Mérida Jorge A. Zavala Pablo Arrabal Haro Micaela B. Bagley Bren E. Backhaus Peter Behroozi Eric F. Bell Véronique Buat Antonello Calabrò Caitlin M. Casey Nikko J. Cleri Rosemary T. Coogan M. C. Cooper Asantha R. Cooray

Abstract： The new capabilities that JWST offers in the near- and mid-infrared (IR) are used to investigate in unprecedented detail the nature of optical/near-IR faint, mid-IR bright sources, HST-dark galaxies among them. We gather JWST data from the CEERS survey in the EGS, jointly with HST data, and analyze spatially resolved optical-to-mid-IR spectral energy distributions (SEDs) to estimate both photometric redshifts in 2 dimensions and stellar populations properties in a pixel-by-pixel basis. We select 138 galaxies with F150W-F356W>1.5 mag, F356W<27.5 mag. The nature of these sources is threefold: (1) 71% are dusty star-forming galaxies at 2100 Gyr^-1); (2) 18% are quiescent/dormant (i.e., subject to reignition and rejuvenation) galaxies at 3展开 -->

Peer Review Status:Awaiting Review

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10. ChinaXiv:202303.06070
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COSMOS-Web: An Overview of the JWST Cosmic Origins Survey

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Caitlin M. Casey Jeyhan S. Kartaltepe Nicole E. Drakos Maximilien Franco Santosh Harish Louise Paquereau Olivier Ilbert Caitlin Rose Isabella G. Cox James W. Nightingale Brant E. Robertson John D. Silverman Anton M. Koekemoer Richard Massey Henry Joy McCracken Jason Rhodes Hollis B. Akins Aristeidis Amvrosiadis Rafael C. Arango-Toro Micaela B. Bagley

Abstract： We present the survey design, implementation, and outlook for COSMOS-Web, a 255 hour treasury program conducted by the James Webb Space Telescope in its first cycle of observations. COSMOS-Web is a contiguous 0.54 deg$^2$ NIRCam imaging survey in four filters (F115W, F150W, F277W, and F444W) that will reach 5$\sigma$ point source depths ranging $\sim$27.5-28.2 magnitudes. In parallel, we will obtain 0.19 deg$^2$ of MIRI imaging in one filter (F770W) reaching 5$\sigma$ point source depths of $\sim$25.3-26.0 magnitudes. COSMOS-Web will build on the rich heritage of multiwavelength observations and data products available in the COSMOS field. The design of COSMOS-Web is motivated by three primary science goals: (1) to discover thousands of galaxies in the Epoch of Reionization ($64$ and place constraints on the formation of the Universe's most massive galaxies ($M_\star>10^{10}$\,M$_\odot$), and (3) directly measure the evolution of the stellar mass to halo mass relation using weak gravitational lensing out to $z\sim2.5$ and measure its variance with galaxies' star formation histories and morphologies. In addition, we anticipate COSMOS-Web's legacy value to reach far beyond these scientific goals, touching many other areas of astrophysics, such as the identification of the first direct collapse black hole candidates, ultracool sub-dwarf stars in the Galactic halo, and possibly the identification of $z>10$ pair-instability supernovae. In this paper we provide an overview of the survey's key measurements, specifications, goals, and prospects for new discovery.

Peer Review Status:Awaiting Review

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11. ChinaXiv:202303.02377
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CEERS Key Paper III: The Diversity of Galaxy Structure and Morphology at z=3-9 with JWST

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Jeyhan S. Kartaltepe Caitlin Rose Brittany N. Vanderhoof Elizabeth J. McGrath Luca Costantin Isabella G. Cox L. Y. Aaron Yung Dale D. Kocevski Stijn Wuyts Henry C. Ferguson Brett H. Andrews Micaela B. Bagley Steven L. Finkelstein Ricardo O. Amorin Pablo Arrabal Haro Bren E. Backhaus Peter Behroozi Laura Bisigello Antonello Calabro Caitlin M. Casey Rosemary T. Coogan

Abstract： We present a comprehensive analysis of the evolution of the morphological and structural properties of a large sample of galaxies at z=3-9 using early JWST CEERS NIRCam observations. Our sample consists of 850 galaxies at z>3 detected in both CANDELS HST imaging and JWST CEERS NIRCam images to enable a comparison of HST and JWST morphologies. Our team conducted a set of visual classifications, with each galaxy in the sample classified by three different individuals. We also measure quantitative morphologies using the publicly available codes across all seven NIRCam filters. Using these measurements, we present the fraction of galaxies of each morphological type as a function of redshift. Overall, we find that galaxies at z>3 have a wide diversity of morphologies. Galaxies with disks make up a total of 60\% of galaxies at z=3 and this fraction drops to ~30% at z=6-9, while galaxies with spheroids make up ~30-40% across the whole redshift range and pure spheroids with no evidence for disks or irregular features make up ~20%. The fraction of galaxies with irregular features is roughly constant at all redshifts (~40-50%), while those that are purely irregular increases from ~12% to ~20% at z>4.5. We note that these are apparent fractions as many selection effects impact the visibility of morphological features at high redshift. The distributions of S\'ersic index, size, and axis ratios show significant differences between the morphological groups. Spheroid Only galaxies have a higher S\'ersic index, smaller size, and higher axis ratio than Disk/Irregular galaxies. Across all redshifts, smaller spheroid and disk galaxies tend to be rounder. Overall, these trends suggest that galaxies with established disks and spheroids exist across the full redshift range of this study and further work with large samples at higher redshift is needed to quantify when these features first formed.

Peer Review Status:Awaiting Review

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12. ChinaXiv:202303.03385
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CEERS Key Paper IV: Galaxies at $4 < z < 9$ are Bluer than They Appear -- Characterizing Galaxy Stellar Populations from Rest-Frame $\sim 1$ micron Imaging

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Casey Papovich Justin Cole Guang Yang Steven L. Finkelstein Guillermo Barro Véronique Buat Denis Burgarella Pablo G. Pérez-González Paola Santini Lise-Marie Seillé Lu Shen Pablo Arrabal Haro Micaela B. Bagley Eric F. Bell Laura Bisigello Antonello Calabrò Caitlin M. Casey Marco Castellano Katherine Chworowsky Nikko J. Cleri

Abstract： We present results from the Cosmic Evolution Early Release Survey (CEERS) on the stellar-population parameters for 28 galaxies with redshifts $4展开 -->

Peer Review Status:Awaiting Review

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13. ChinaXiv:202303.02409
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CEERS: Spatially Resolved UV and mid-IR Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

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

Abstract： We present the mid-IR (MIR) morphologies for 70 star-forming galaxies (SFGs) at $0.210^{9}~M_\odot}$ using JWST MIRI observations from the Cosmic Evolution Early Release Science survey (CEERS). The MIRI bands span the MIR (7.7--21 $\mu$m), enabling us to measure the effective radii ($R_{\mathrm{eff}}$) and S\'{e}rsic indexes of these SFGs at rest-frame 6.2 and 7.7 $\mu$m, which contains strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We compare the PAH-band morphologies to those in rest-frame Near-UV (NUV) using HST ACS/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging from UVCANDELS and CANDELS, where the NUV-band and F160W trace the profile of (unobscured) massive stars and the stellar continuum, respectively. The $R_{\mathrm{eff}}$ of galaxies in the PAH-band are slightly smaller ($\sim$10) than those in F160W for more massive galaxies with $\mathrm{M_*\gtrsim10^{9.5}~M_\odot}$ at $z\leq1.2$ and with $\mathrm{M_*\gtrsim10^{10}~M_\odot}$ at $z\geq1.2$, but the PAH-band and F160W have a similar fractions of light within 1 kpc. In contrast, the $R_{\rm{eff}}$ of galaxies in the NUV-band are larger, with lower fractions of light within 1 kpc compared to the F160W for galaxies at $z\leq1.2$. Using the MIRI data to estimate the surface density of the IR-based SFR, we find the correlation between the IR-based SFR surface density and stellar mass has a steeper slope than that of the UV-based surface density and stellar mass, suggesting galaxies with higher stellar masses 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.

Peer Review Status:Awaiting Review

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