# PANORAMIC: Discovery of an ultra-massive grand-design spiral galaxy at $z \sim 5.2$

Mengyuan Xiao, Christina Williams, Pascal Oesch, David Elbaz, Miroslava Dessauges-Zavadsky, Rui Marques-Chaves, Longji Bing, Zhiyuan Ji, Andrea Weibel, Rachel Bezanson, et al.

► To cite this version:

Mengyuan Xiao, Christina Williams, Pascal Oesch, David Elbaz, Miroslava Dessauges-Zavadsky, et al.. PANORAMIC: Discovery of an ultra-massive grand-design spiral galaxy at $z \sim 5.2$. Astronomy & Astrophysics - A&A, 2025, 696, pp.A156. 10.1051/0004-6361/202453487. hal-05486971

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# PANORAMIC: Discovery of an ultra-massive grand-design spiral galaxy at z ~ 5.2

Mengyuan Xiao¹,*, Christina C. Williams²,³, Pascal A. Oesch¹,⁴, David Elbaz⁵,
Miroslava Dessauges-Zavadsky¹, Rui Marques-Chaves¹, Longji Bing⁶, Zhiyuan Ji³, Andrea Weibel¹,⁵,
Rachel Bezanson⁷, Gabriel Brammer⁴, Caitlin Casey⁸,⁹,⁴, Aidan P. Cloonan¹⁰, Emanuele Daddi⁵, Pratika Dayal¹¹,
Andreas L. Faisst¹², Marijn Franx¹³, Karl Glazebrook¹⁴, Anne Hutter⁴, Jeyhan S. Kartaltepe¹⁵, Ivo Labbe¹⁴,
Guilaine Lagache¹⁶, Seunghwan Lim¹⁷,¹⁸, Benjamin Magnelli⁵, Felix Martinez¹⁵, Michael V. Maseda¹⁹,
Themiya Nanayakkara¹⁴, Daniel Schaerer¹, and Katherine E. Whitaker¹⁰

(Affiliations can be found after the references)

Received 17 December 2024 / Accepted 27 February 2025

## ABSTRACT

We report the discovery of an ultra-massive grand-design red spiral galaxy, named Zhúlóng (Torch Dragon), at $z_{phot} = 5.2_{-0.2}^{+0.3}$ in the JWST PANORAMIC survey; it is the most distant bulge+disk galaxy candidate with spiral arms known to date. Zhúlóng displays an extraordinary combination of properties: (1) a classical bulge centered in a large, face-on exponential stellar disk (half-light radius of $R_e = 3.7 \pm 0.1$ kpc) with spiral arms extending across 19 kpc; (2) a clear transition from the red, quiescent core ($F_{150W} - F_{444W} = 3.1$ mag) with a high stellar mass surface density ($\log(\Sigma M_*/M_\odot \text{ kpc}^{-2}) = 9.91_{-0.09}^{+0.11}$) to the star-forming outer regions, as revealed by spatially resolved spectral energy distribution analysis, which indicates significant inside-out galaxy growth; (3) an extremely high stellar mass for its redshift, with $\log(M_*/M_\odot) = 11.03_{-0.08}^{+0.10}$, which is comparable to the Milky Way's mass, and an implied baryon-to-star conversion efficiency ($\epsilon \sim 0.3$) that is 1.5 times higher than even the most efficient galaxies at later epochs; and (4) despite an active disk, a relatively modest overall star formation rate (SFR = $66_{-46}^{+89} M_\odot \text{ yr}^{-1}$), which is >0.5 dex below the star formation main sequence at $z \sim 5.2$ and >10 times lower than ultra-massive dusty galaxies at $z = 5-6$. Zhúlóng shows that mature galaxies emerged much earlier than previously believed, in the first billion years after the Big Bang, through rapid galaxy formation and morphological evolution. Our finding offers key constraints for models of massive galaxy formation and the origin of spiral structures in the early Universe.

**Key words.** galaxies: evolution – galaxies: formation – galaxies: high-redshift – galaxies: spiral

## 1. Introduction

A remarkable revelation from early *James Webb Space Telescope* (JWST) observations is the rapid evolution of galaxies at early cosmic times (see the review in Adamo et al. 2024). Three years into the mission (Gardner et al. 2023), evidence of faster growth and maturity among galaxies continues to accumulate. By nearly all common evolutionary metrics (stellar mass, luminosity, and stellar structure), galaxies have evolved faster than expected prior to JWST (e.g., Naidu et al. 2022; Boylan-Kolchin 2023; Donnan et al. 2023; Ferreira et al. 2023; Finkelstein et al. 2024; Casey et al. 2024; de Graaff et al. 2025; Glazebrook et al. 2024; Shapley et al. 2025). This raises questions about the physical processes that drive the inferred rapid timescales associated with the observed evolution and/or points to an earlier onset of galaxy formation.

At the forefront of these discoveries are massive galaxies. Panchromatic JWST imaging and spectroscopy from the observed optical to mid-infrared have confirmed that ultra-massive galaxies existed in the early Universe ($\log(M_*/M_\odot) > 11$ at $z > 5$); they also indicate that such galaxies may be unexpectedly abundant (e.g., Labbé et al. 2023; Xiao et al. 2024; Weibel et al. 2024a). Galaxies having near Milky Way (MW) masses ~1 Gyr after the Big Bang suggests that they form in a more efficient way than previously thought. Based on small

survey areas (typical JWST imaging campaigns from Cycle 1 targeted <100 sq. arcmin per field), these ultra-massive galaxies, like the ones reported in Xiao et al. (2024), require on average about 50% of the baryons in their dark matter halos to be converted into stars – two to three times more than even the most efficient galaxies at later times (Moster et al. 2013; Wechsler & Tinker 2018; Shuntov et al. 2022). While questions remain about incomplete data or modeling assumptions for photometric samples (e.g., Wang et al. 2024a; Williams et al. 2024; Desprez et al. 2024), cosmic variance from small fields and sample sizes also complicate interpretations. This motivates studies of known massive candidates because, if true, these findings raise new important questions about the theory of evolutionary drivers of early galaxies.

A key constraint on evolutionary drivers of rapid galaxy growth is galaxy morphology. On this front, JWST is again producing surprising revelations pointing to accelerated maturity timescales for galaxies, when compared to the morphological census based on *Hubble Space Telescope* (HST) data. HST imaging suggested that the emergence of disks and spiral galaxies (perhaps the precursors of the grand-design spirals seen locally) was a late forming phenomenon, with the backbone of the Hubble sequence appearing as late as $z \sim 2$ (e.g., Lee et al. 2013; Mortlock et al. 2013). However, with JWST, there is now accumulating evidence that stellar disks formed earlier than we expected, making up ~50% of galaxies

<footnote>* Corresponding author; mengyuan.xiao@unige.ch</footnote>
up to $z < 6$ (Ferreira et al. 2022, 2023; Vega-Ferrero et al. 2024; Robertson et al. 2023; Kartaltepe et al. 2023; Jacobs et al. 2023; Huertas-Company et al. 2024). This is a factor of 10 more stellar disks than were thought to exist at this redshift prior to JWST. In addition, a few stellar spiral galaxies have also been reported at $z > 3$ (Jain & Wadadekar 2024; Wang et al. 2024b; Umehata et al. 2024; Costantin et al. 2023; Wu et al. 2023). These new findings contrast with theoretical predictions that large stellar disks predominantly formed later in cosmic history (e.g., Dekel et al. 2020; Belokurov & Kravtsov 2022; Gurvich et al. 2023; McCluskey et al. 2024).

Morphological constraints are of particular interest regarding ultra-massive galaxies, where the stellar structure lends important clues to the highly efficient buildup that is implied by their high masses at early times. To date, numerous extremely compact, massive quiescent galaxies have been spectroscopically confirmed with stellar absorption features at $z \ge 5$ (e.g., Carnall et al. 2023; Weibel et al. 2024b; de Graaff et al. 2025). These findings mirror the established compact sizes of quiescent galaxies at cosmic noon, which are typically a factor of >3 smaller in size at fixed mass compared to star-forming galaxies (SFGs; e.g., van Dokkum et al. 2008; van der Wel et al. 2014; Faisst et al. 2017; Kawinwanichakij et al. 2021; Mowla et al. 2019a; Cutler et al. 2022). However, their compact structures are not a universal feature: three extreme star-forming ultra-massive galaxies presented in Xiao et al. (2024) exhibit larger and irregular morphologies, raising the question of whether dust obfuscates the stellar morphology or if there is diversity in the population. With relatively few ultra-massive galaxies known (identified from relatively small NIRCam blank-field areas), a systematic study to characterize the morphologies of representative samples has not yet been carried out, preventing general conclusions about formation pathways using morphology.

Here we report on the serendipitous discovery of a unique ultra-massive galaxy at $z_{phot} \sim 5.2$ in the PANORAMIC<fnref n="1" /> survey (Williams et al. 2025). Unlike the other ultra-massive candidates described above, it has a striking evolved morphology; a quiescent-like classical bulge, a star-forming stellar disk, and grand-design spiral arms (defined as spiral structures spanning the whole galaxy, from the nucleus to outskirts, with spiral arms starting at diametrically opposite points; e.g., Binney & Tremaine 2008; Dobbs & Baba 2014; Sellwood & Masters 2022) only 1 billion years after the Big Bang. More interestingly, it is very large in stellar size (19 kpc in diameter) and extremely massive ($\log(M_\star/M_\odot) > 11$, indicating high baryon-to-star formation efficiency), with a modest star formation rate with red color (SFR = $66_{-89}^{+46} M_\odot \text{ yr}^{-1}$; $F150W - F444W \sim 2.7$ mag). Of the few stellar spiral galaxies that have thus far been identified at $z > 3$ (Jain & Wadadekar 2024; Wang et al. 2024b; Umehata et al. 2024; Costantin et al. 2023; Wu et al. 2023), this source is the most distant, providing direct empirical evidence of the rapid dynamical evolution of massive galaxies at $z > 5$. Given its unique red color, morphology, and stellar properties, we name it Zhúlóng<fnref n="2" />.

This paper is organized as follows: In Sect. 2 we present the datasets used to measure photometry and photometric redshift methods. In Sect. 3 we present our methodology for measuring morphologies and spectral energy distribution (SED) mod-

eling. In Sect. 4 we interpret the properties of this remarkable galaxy both in the context of the formation pathway of ultra-massive galaxies and as the highest redshift example of a large, spiral galaxy. Throughout this paper, we adopt a Chabrier initial mass function (IMF; Chabrier 2003) to estimate the star formation rate (SFR) and stellar mass. We assume Planck cosmology (Planck Collaboration VI 2020) with ($\Omega_m, \Omega_\Lambda, h, \sigma_8$) = (0.3, 0.7, 0.7, 0.81). When necessary, data from the literature are converted using a conversion factor of $M_\star$ (Salpeter 1955 IMF) = $1.7 \times M_\star$ (Chabrier 2003 IMF). All magnitudes are in the AB system (Oke & Gunn 1983) such that $m_{AB} = 23.9 - 2.5 \times \log(S_v$ [µJy]).

## 2. Observational data

Zhúlóng ($\alpha, \delta$ [J2000] = 150.124874, 2.092919) was serendipitously discovered in the field (association) and was named j100024p0208 in the recent data release of the JWST PANORAMIC survey (GO-2514; PIs: C. Williams & P. Oesch; Williams et al. 2025), a pure parallel extragalactic NIRCam imaging program. The source was originally identified by chance during a search for massive galaxy candidates that were color-selected to exhibit a strong Balmer break at $z > 3$ (Long et al. 2024). Its spiral structure was identified during visual inspection of those candidates, and was unique among the sample. Zhúlóng lies within the NIRCam imaging footprint of the COSMOS-Web field (Casey et al. 2023), but is not covered by the COSMOS-PRIMER program (Dunlop et al. 2021).

### 2.1. HST and JWST NIRCam observations

We utilized imaging data from archival HST observations, including F606W and F814W from HST/ACS (Koekemoer et al. 2007, 2011; Grogin et al. 2011), and F160W from HST/WFC3 (Momcheva et al. 2017; Mowla et al. 2019b). The spiral galaxy is not detected in any HST images, and was discovered in JWST/NIRCam (Rieke et al. 2023) images with filters F115W, F150W, F200W, F277W, F356W, and F444W obtained as part of the PANORAMIC survey. For the four filters obtained by COSMOS-Web (F115W, F150W, F277W, and F444W), we combine the imaging from the two surveys. The typical $5\sigma$ depths, measured within a circular aperture of 0.16" radius, are 27.5, 27.7, 28.2, 28.4, 28.8, and 28.3 mags for F115W, F150W, F200W, F277W, F356W, and F444W, respectively.

Multiwavelength photometric measurements are derived following the same procedure as outlined in Weibel et al. (2024a). Briefly, we use SExtractor (Bertin & Arnouts 1996) in dual image mode with an inverse-variance weighted stack of the longest wavelength NIRCam wide filters, F277W+F356W+F444W, as the detection image. In this study, fluxes are measured in 0.′16, 0.′35, 0.′5, and 0.′7 radius circular apertures in images that are point spread function (PSF)-matched to the F444W band. Total fluxes are derived from the Kron AUTO aperture provided by SExtractor in the F444W band, in addition to a correction based on the encircled energy of the Kron aperture on the F444W PSF. Detailed descriptions of data reduction and photometric measurements are provided in Williams et al. (2025).

### 2.2. Longer-wavelength observations

Although Zhúlóng lies within the COSMOS-Web field, it falls in a gap in the MIRI F770W footprints. Observations

<footnote n="1">¹ Parallel wide-Area Nircam Observations to Reveal And Measure the Invisible Cosmos (PANORAMIC).</footnote>

<footnote n="2">² Zhúlóng (烛龙, or Torch Dragon), which is a giant red solar dragon and god in Chinese mythology. It has a human's face and a snake's body, created day and night by opening and closing its eyes, and created seasonal winds by breathing.</footnote>
<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Morphology and photo-z of Zhúlóng. The left panel shows a 4" × 4" stacked image (F277W+F356W+F444W) with contour maps (start from 3σ). The top right panels show these same stamps in different filters. The central core's SED (circled in red; measured in 0.16" radius) has a clear post-starburst shape, which is shown in the middle right panels. In the middle right panels, the left one shows the EAZY SED fit together with the photometric points, and the right one shows the photometric redshift likelihood distribution, which has a single peak consistent with $z_{phot} = 5.2_{-0.2}^{+0.3}$. A neighboring star-forming clump (circled in blue) has a very robust redshift of $z_{phot} = 5.15_{-0.03}^{+0.04}$ from photometry due to strong emission lines.</figcaption></figure>

at longer wavelengths cover the location of Zhúlóng, but none return a detection, including Spitzer MIPS 24 µm (Le Floc'h et al. 2009), Herschel PACS (Lutz et al. 2011) and SPIRE (Oliver et al. 2012), and NIKAS Cosmological Legacy Survey at 1.2 mm and 2.0 mm (rms of 0.3 and 0.09 mJy beam⁻¹, respectively; Bing et al. 2023; Carvajal Bohorquez et al., in prep.), ALMA 2.0 mm (rms of 0.12 mJy beam⁻¹; Project ID: 2021.1.00705.S), ALMA 3.0 mm (rms of 0.06 mJy beam⁻¹; Project ID: 2021.1.01005.S), and VLA 3 GHz (Smolčić et al. 2017) and 1.4 GHz (Schinnerer et al. 2010). More recently, the ALMA large program CHAMPS (PI: A. Faisst, private comm.; Faisst et al., in prep.) also covers Zhúlóng at 1.2 mm, but again it remains undetected. The local rms level is ~0.2 mJy beam⁻¹ in the 1.2 mm map of 0.959" × 0.799" spatial resolution. The 3σ upper limit at 1.2 mm is 0.6 mJy, assuming the dust distribution is unresolved, indicating that Zhúlóng has low far-infrared (FIR) luminosity.

We note that, with the exception of the ALMA 1.2 mm observations, the remaining long-wavelength observations are too shallow to significantly constrain the FIR SED shape of Zhúlóng (see Sect. 3.3). Therefore, in this work, we only use data points from HST, JWST, and ALMA 1.2 mm.

## 2.3. Zhúlóng with a robust photometric redshift: $z_{phot} = 5.2_{-0.2}^{+0.3}$

The photometric redshift of Zhúlóng was estimated using the SED-fitting code EAZY (Brammer et al. 2008) and with the blue_sfhz_13 template set, which imposes redshift-dependent star formation histories (SFHs), excluding SFHs that start earlier than the age of the Universe at a given redshift<fnref n="3" />. We applied an error floor of 5% prior to running EAZY to account for possible remaining systematic uncertainties in the photometry and to enable more flexibility in the SED fitting. The redshift range for

fitting was set to $z \in (0.01, 20)$. Additional details on the photometric redshift modeling are presented in Williams et al. (2025).

The EAZY best-fit results are shown in Fig. 1. The redshift probability distribution $P(z)$ for Zhúlóng is strongly constrained by a prominent Balmer/4000 Å break observed in the central region (0.16" radius), resulting in narrow uncertainties with a single redshift solution $z_{phot} = 5.2_{-0.2}^{+0.3}$. In addition, the neighboring southwest clump has evidence of strong emission lines, which boost the photometry in the F277W and F444W bands, leading to an even better constrained photometric redshift: $z_{phot} = 5.15_{-0.03}^{+0.04}$. This consistency illustrates the $z_{phot}$ reliability of Zhúlóng. Further tests and a detailed discussion of the robustness of the redshift are presented in Appendix A. Nevertheless, we underline that this is still a photometric redshift. It will be important to confirm the redshift through spectroscopy in the future, such as with the upcoming COSMOS-3D grism observations (GO-5893; Kakiichi et al. 2024) or with NIRSpec spectra.

# 3. Physical properties of Zhúlóng

## 3.1. Appearance of bulge, disk, and spiral structures

We investigated the morphology of Zhúlóng with three deep JWST long-wavelength filters, F277W, F356W, and F444W, and their inverse-variance weighted stacked image. We fit our source with PySersic (Pasha & Miller 2023) using two different strategies: (1) a single Sérsic profile and (2) double Sérsic profiles. In both cases, we used PSFs for fitting that were derived from the WebbPSF software (Perrin et al. 2014) and rotated to match the position angle of the observations. The single Sérsic fit returns the best-fit half-light radius ($R_e$), which is used to quantify the galaxy size. The double Sérsic fit helps us distinguish between the contributions of the bulge and disk. In addition, comparing the best-fit results from single and double Sérsic profiles enables an inspection of the underlying bulge in the core.

<footnote n="3">³ https://github.com/gbrammer/eazy-photoz/tree/master/templates/sfhz</footnote>
<figure><img src="image_3.png" /><figcaption>**Fig. 2.** Morphological modeling of Zhúlóng. The stacked image (4'' × 4''; F277W+F356W+F444W) was modeled using PySersic with: (1) a single Sérsic profile (top row) and (2) double Sérsic profiles (bottom row). Panels from left to right show: the stacked image, the best-fit model, the model-subtracted residuals, and the surface brightness profile. The gray-shaded area in the profile indicates the 1σ noise level of the image. Notably, after subtracting the major component(s) of Zhúlóng, the spiral arms appear prominently in the residual maps. For the morphological analysis of individual images of F277W, F356W, and F444W, see Appendix B.</figcaption></figure>

The fitting process is performed on 4'' × 4'' background-subtracted cutouts centered on Zhúlóng. The bright neighboring foreground galaxy at $z \sim 1.59$ is masked during the fitting. Additionally, we conducted tests comparing the results when masking the spiral arms versus not masking them. We find that no matter whether masking them or not during the fitting process, for both single and double Sérsic fits, the best-fit results ($R_e$, Sérsic index $n$, minor-to-major axis ratio $b/a$) remain consistent within the 1σ error. In this analysis, we focused on the results where the spiral arms are also masked during the fitting as this approach enhances the visibility of the spiral arm structure in the residual plots, allowing us to more distinctly separate the disk, spiral arms, and the underlying bulge structure.

Figure 2 shows the best-fit results of the stacked image. From the residual maps, Zhúlóng shows evidence of a grand-design spiral arm structure, with high contrast primary arms extending from the bulge pointing north and south (e.g., Dobbs & Baba 2014; Sellwood & Masters 2022). The presence of the spiral arms is also indicated in the surface brightness profiles, which show the discrepancy between the observed points and the best-fit model. The single Sérsic fit yields $R_e = 2.9 \pm 0.1$ kpc, suggesting that Zhúlóng has a large stellar size. The large $n = 4.9 \pm 0.1$ reveals that the stellar light is more concentrated at the galaxy center, indicating the potential existence of a bulge structure. Meanwhile, the significant inhomogeneity in the core of the residual map also suggests the need for an additional bulge component in the fitting process, which is mitigated in the residual map of the double Sérsic fit. On the other hand, the double Sérsic fit yields evidence of both bulge and disk structures, with spiral arms shown in the residual map. The bulge component has $n = 3.7 \pm 0.2$, close to the shape of classical bulges in the local Universe ($n \sim 4$), suggesting the existence of a well-evolved bulge already in the first gigayear after the Big Bang. The bulge-to-total (light) ratio is $B/T = 0.44$. The disk component has $n = 1.2 \pm 0.1$, $R_e = 3.7 \pm 0.1$ kpc, and $b/a = 0.99 \pm 0.01$, indicating the existence of a large face-on exponential stellar disk. In addition, we note that both of the residual maps show clear evidence of stellar clumps along the spiral arms, as observed

in galaxies at cosmic noon (e.g., Rujopakarn et al. 2016; Claeyssens et al. 2023, 2025) and as also found in numerical simulations (e.g., Tamburello et al. 2015; Mandelker et al. 2017; Fensch & Bournaud 2021; Ceverino et al. 2023; Renaud et al. 2024). Furthermore, we also performed the morphological analysis for individual images, and the results remain the same (see Appendix B).

Overall, from the morphological analysis, it appears that the fit may be more in favor of the double Sérsic model. However, this alone does not constitute strong enough evidence to confirm the existence of a bulge and disk in Zhúlóng. As we show in Sect. 3.2, spatially resolved SED modeling reveals significant differences in the stellar populations between the inner and outer regions of the galaxy. The combination of the morphological analysis and the SED evidence suggests that the galaxy does indeed contain separate inner and outer structural components.

Given the extended nature of Zhúlóng, and the amount of flux present in spiral arms that are not well accounted for by either Sérsic model, we also measured the size that encloses 80% of the light empirically using the azimuthally averaged light profile from the stacked image without any assumption on the parametric shape of the light distribution. Using this method, we find that these radii are larger than inferred assuming the parametric Sérsic (or double Sérsic) model. We measure $R_{80} = 9.5$ kpc for the radii enclosing 80% of the light. $R_{80}$ is extremely large compared to its half-light radius (while better reflecting the overall extent of stellar light), reflecting the fact that the spatial extent of the stars in the galaxy reaches more than 19 kpc in diameter.

## 3.2. A quiescent-like bulge and star-forming disk

We further analyzed different annular regions to explore any variation in the stellar populations across Zhúlóng. Physical properties were estimated by fitting the UV to near-infrared (NIR) SED from JWST and HST photometry using Bagpipes (Carnall et al. 2018), with the $z_{phot}$ fixed to that measured by EAZY. We considered two different SFHs: a double-power-law and a delayed SFH, using Bruzual & Charlot (2003) stellar
<figure><img src="image_4.png" /><figcaption>**Fig. 3.** Stellar population gradient from the core to the outer region. Zhúlóng has a quiescent-like galaxy core embedded in a star-forming stellar disk. The figure shows the SED shapes and photometry as measured in different annuli, from the central core (top left) to the outer region (bottom right), as indicated by the labels. The properties of different annular regions are listed in Table 1. Note that the galaxy is very extended, with spiral arms extending more than 19 kpc in diameter.</figcaption></figure>

<table><caption>**Table 1.** Properties of the entire galaxy and the different annular regions.</caption><thead><tr><th>Total</th><th>z<sub>phot</sub></th><th>log M<sub>★</sub>[M<sub>☉</sub>]</th><th>SFR [M<sub>☉</sub> yr<sup>-1</sup>]</th><th>A<sub>V</sub> [mag]</th><th></th></tr></thead><tbody><tr><td></td><td>5.2<sup>+0.3</sup><sub>-0.2</sub></td><td>11.03<sup>+0.10</sup><sub>-0.08</sub></td><td>66<sup>+89</sup><sub>-46</sub></td><td>1.1<sup>+0.2</sup><sub>-0.2</sub></td><td></td></tr><tr><th>Annulus radius</th><th>log ΣM<sub>★</sub>[M<sub>☉</sub> kpc<sup>-2</sup>]</th><th>log ΣSFR [M<sub>☉</sub> yr<sup>-1</sup> kpc<sup>-2</sup>]</th><th>log sSFR [yr<sup>-1</sup>]</th><th>A<sub>V</sub> [mag]</th><th>β<sub>UV</sub></th></tr><tr><td>&lt;0.16"</td><td>9.91<sup>+0.11</sup><sub>-0.09</sub></td><td>-5.85<sup>+5.98</sup><sub>-36.21</sub></td><td>-15.76<sup>+5.86</sup><sub>-36.12</sub></td><td>0.8<sup>+0.4</sup><sub>-0.4</sub></td><td>0.18 ± 0.48</td></tr><tr><td>0.16"-0.35"</td><td>9.52<sup>+0.07</sup><sub>-0.10</sub></td><td>0.73<sup>+0.14</sup><sub>-0.15</sub></td><td>-8.78<sup>+0.07</sup><sub>-0.06</sub></td><td>1.7<sup>+0.2</sup><sub>-0.2</sub></td><td>-0.38 ± 0.30</td></tr><tr><td>0.35"-0.5"</td><td>8.94<sup>+0.10</sup><sub>-0.08</sub></td><td>0.14<sup>+0.15</sup><sub>-0.14</sub></td><td>-8.80<sup>+0.05</sup><sub>-0.06</sub></td><td>1.2<sup>+0.2</sup><sub>-0.2</sub></td><td>-0.97 ± 0.20</td></tr><tr><td>0.5"-0.7"</td><td>8.65<sup>+0.07</sup><sub>-0.09</sub></td><td>-0.13<sup>+0.16</sup><sub>-0.15</sub></td><td>-8.78<sup>+0.09</sup><sub>-0.06</sub></td><td>1.0<sup>+0.2</sup><sub>-0.2</sub></td><td>-1.18 ± 0.19</td></tr></tbody></table>

population models and the Calzetti et al. (2000) reddening law. We adopted a broad metallicity range of 0.1 to 2.5 $Z_☉$, dust attenuation to the rest-frame V band ($A_V$) values from 0 to 5 magnitudes, and ionization parameters $logU$ ranging from -4 to -2. For the double-power-law SFH, we adopted a falling slope $\alpha = [0.01, 1000]$, a rising slope $\beta = [0.01, 1000]$, and a turnover time $\tau = [0.01, 5]$ Gyr. For the delayed SFH, we applied broad uniform priors with age (i.e., the time since star formation began) ranging from 10 Myr to 1.2 Gyr and a logarithmic $\tau$ (timescale of decrease) ranging from 10 Myr to 10 Gyr. We obtain main physical properties of $M_★$, $A_V$, and SFR that are consistent within $1\sigma$ with the results assuming the two different SFHs. As an example, the best-fit SED results assuming a double-power-law SFH are shown in Fig. 3 and Table 1.

In Fig. 3, from the central core to the outer region, the best-fit SED changes significantly from quiescent to star-forming populations. The core is dominated by old stellar populations with a red color ($F150W - F444W = 3.1$ ABmag). The best-fit SED exhibits a strong Balmer/4000 Å break, a very low specific star formation rate (sSFR) of $log(sSFR/yr^{-1}) = -15.76^{+5.86}_{-36.12}$, and a lack of emission lines. The observed colors are consistent with NIRCam-based photometric selections for $z > 3$ quiescent galaxies (Long et al. 2024). The rest-frame U-V and V-J colors as measured from EAZY are 1.4 and 1.0 mag, respectively, consistent with a quiescent/post-starburst fading stellar population (Williams et al. 2009). The rest-frame colors are also consistent

with extensions of UVJ color criteria for quiescent galaxies that have been adapted to $z > 3-6$ to accommodate younger passively evolving galaxies (Antwi-Danso et al. 2023). In contrast, the disk measured in an annulus between 0.5" and 0.7" is dominated by younger stellar populations with a relatively blue color ($F150W - F444W = 2.0$ ABmag) and, unlike the inner region, allows the presence of weak emission lines in the SED.

Furthermore, among all annular regions, the central core ($r < 0.16''$) has the highest stellar mass surface density, with $log(\Sigma M_★/M_☉ kpc^{-2}) = 9.91^{+0.11}_{-0.09}$ (see Table 1), revealing the build-up of a dense stellar bulge. The absence of star formation activity in the core is consistent with the expectations of inside-out galaxy growth and quenching (e.g., Tacchella et al. 2015).

Finally, we also calculated the stellar mass and stellar mass surface density of the bulge. Assuming the core is dominated by the bulge, with the mass-to-light ratio in the core and the best-fit bulge light profile (Fig. 2), we derived $log(M_{★,bulge}/M_☉) = 10.71^{+0.10}_{-0.09}$ and $log(\Sigma M_{★,bulge}/M_☉ kpc^{-2}) = 10.00^{+0.09}_{-0.11}$. Given the total mass of Zhúlóng (see Sect. 3.3), its bulge-to-total mass ratio is $B/T = 0.5$.

### 3.3. Ultra-massive spiral galaxy with accelerated formation

Here we focus on the integrated properties of Zhúlóng. The total $M_★$, $A_V$, and SFR are derived by fitting the UV-to-FIR SED from the JWST+HST+ALMA photometry, using Bagpipes. Similar
to the procedure derived in Sect. 3.2, we used the Calzetti et al. (2000) reddening law, the Bruzual & Charlot (2003) stellar population models, and the Draine & Li (2007) dust emission model (with energy balance), assuming different SFH (double-power-law SFH and delayed SFH) and free metallicity. The derived main properties with delayed SFH are listed in Table 1. To test the result, we also performed SED fitting with CIGALE (Boquien et al. 2019), which produced very consistent values within the errors. The total stellar mass is also consistent with the sum of the individual masses obtained from the different annuli ($\log(M_*/M_\odot) = 10.96_{-0.06}^{+0.05}$; see Sect. 3.2). In general, we find that Zhúlóng is extremely massive with $\log(M_*/M_\odot) = 11.03_{-0.08}^{+0.10}$.

Such a high stellar mass at $z \sim 5.2$ indicates that Zhúlóng must have been forming stars very efficiently. In Fig. 4 we compare its stellar mass to the maximum mass at which one would expect to find a galaxy within the PANORAMIC survey volume, given the prevailing halo mass function and cosmic baryon fraction (Boylan-Kolchin 2023; Lovell et al. 2023). Instead of taking the small coverage of PANORAMIC in the COSMOS field only, to be conservative, we considered the total PANORAMIC survey area of ~432 arcmin². Under this paradigm, we derive the most massive dark matter halo mass ($M_{\text{halo}}^{\text{max}}$) at different redshifts within the corresponding survey volume ($\Delta z = 1$; e.g., ~1.2 × 10⁶ Mpc³ at $z = 4.7–5.7$) according to the halo mass function. The derived $M_{\text{halo}}^{\text{max}}$ at $z = 5.2$ is $\log(M_{\text{halo}}/M_\odot) = 12.38$.

The maximum stellar mass is inferred from the maximum dark matter halo mass, based on $M_{\star}^{\text{max}} = \epsilon f_b M_{\text{halo}}^{\text{max}}$, with a cosmic baryon fraction $f_b = \Omega_b/\Omega_m = 0.158$ (Planck Collaboration VI 2020), and the maximum theoretical efficiency ($\epsilon$) of converting baryons into stars. Here, we considered two possible cases of $\epsilon$ in the PANORAMIC survey volume, as shown in Fig. 4: the highest efficiency from observation-based phenomenological modeling, such as abundance matching and halo occupation distribution models ($\epsilon_{\text{max,obs}} = 0.2$; dotted line; Moster et al. 2013, 2018; Tacchella et al. 2018; Pillepich et al. 2018; Wechsler & Tinker 2018; Shuntov et al. 2022) and the maximum efficiency logically allowed ($\epsilon = 1$; dashed line). As a reference, we also overplot the most extreme case of $\epsilon = 1$ in the full sky (solid line).

By comparing the stellar mass of Zhúlóng with the predictions in Fig. 4, it is clear that Zhúlóng requires an extremely efficient conversion of available baryons to stars of $\epsilon \sim 0.3$ – about 1.5 times the highest efficiency observed at lower redshifts ($\epsilon_{\text{max,obs}} \approx 0.2$). The ultra-massive properties and high efficiency make Zhúlóng another extreme source in addition to recently discovered massive galaxies (e.g., Xiao et al. 2024; Glazebrook et al. 2017, 2024; Carnall et al. 2023; Weibel et al. 2024b; de Graaff et al. 2025). In Fig. 4 we show a direct comparison of Zhúlóng and three red monster galaxies at $z_{\text{spec}} \sim 5–6$ (red points; i.e., S1, S2, and S3 in Xiao et al. 2024) as their efficiency is calculated within the similar survey volume. Together, these findings demonstrate the existence of ultra-massive galaxies that challenge our galaxy assembly models in the first billion years of the Universe (White & Rees 1978; Boylan-Kolchin 2023; Labbé et al. 2023).

In addition, in Fig. 4 we compile all currently known examples from the literature of galaxies whose stellar structures are consistent with spiral arms at $z > 3$, the highest redshift at which spiral structure has been detected in stars (rather than just gas) to date (Jain & Wadadekar 2024; Wang et al. 2024b; Umehata et al. 2024; Costantin et al. 2023; Wu et al. 2023). We note that while some other galaxies have been reported to show potential spiral-like structures in JWST images, they are not included in our figure due to the lack of comparable analy-

<figure><img src="image_5.png" /></figure>

**Fig. 4.** Stellar mass of Zhúlóng (orange star) compared to other representative galaxies and the model expectations. The red-filled circles show three spectroscopically confirmed ultra-massive galaxies (so-called red monsters; Xiao et al. 2024). The blue squares show $z > 3$ galaxies reported to have clear stellar spiral structures (Jain & Wadadekar 2024; Wang et al. 2024b; Umehata et al. 2024; Costantin et al. 2023; Wu et al. 2023). Note that there is no error bar of $M_\star$ given in Wu et al. (2023). The dashed and dotted gray lines indicate the maximum stellar mass calculated from the maximum halo mass ($M_{\text{halo}}^{\text{max}}$) given the PANORAMIC survey volume, based on $M_\star^{\text{max}} = \epsilon f_b M_{\text{halo}}^{\text{max}}$, the cosmic baryon fraction $f_b = \Omega_b/\Omega_m = 0.158$, and assuming a baryon-to-star conversion efficiency of $\epsilon = 1$ and 0.2. As a reference, we also show $\epsilon = 1$ with the full sky coverage as the black line. The gray regions indicate the stellar mass prohibited by the standard $\Lambda$ cold dark matter cosmology.

ses and stellar mass estimates (e.g., Ferreira et al. 2023). Thus, we caution that there may be more spiral galaxies at $z > 3$ than those currently identified, and a systematic study of high-redshift spiral galaxies is necessary to confirm this. In addition, sources showing only stellar disks but without clear spiral arms are also not in our plot (e.g., Yan et al. 2024). Compared with the literature-reported spiral galaxies, Zhúlóng appears to be the most distant spiral galaxy discovered so far.

### 3.4. The location on the main sequence

Given the red, quiescent-like bulge, we investigated the location of our galaxy with respect to the star formation main sequence (SFMS) at $z \sim 5$. While previous ultra-massive galaxies are found to be in a rapid star-formation phase, Zhúlóng's SFR is significantly low. For example, the three sources from Xiao et al. (2024) S1, S2, and S3 are ultra-massive, dusty star-forming, sub-millimeter galaxies. They have SFRs of ~1000 $M_\odot$ yr$^{-1}$, large dust contents ($A_V > 3$ mag and detected by SCUBA2 observations), half-light radii of $R_{e,F448W} \sim 1–2$ kpc. Due to heavy dust obscuration, they are barely detectable in the optical wavelength bands, and hence they are also called optically dark galaxies (or HST-dark galaxies; e.g., Wang et al. 2019; Williams et al. 2019, 2024; Xiao et al. 2023). By contrast, as shown in Fig. 5, the SFR of Zhúlóng is $66_{-46}^{+89} M_\odot$ yr$^{-1}$ (also in Table 1), more than 10 times
<figure><img src="image_6.png" /></figure>

**Fig. 5.** Location of Zhúlóng (orange star) compared to the SFMS in the SFR–M* plane. The red-filled circles show three spectroscopically confirmed ultra-massive galaxies (Xiao et al. 2024). Error bars correspond to 1σ uncertainties. The extrapolated Schreiber et al. (2015) SFMS at z = 5.2, 1σ scatter (~0.3 dex), and a more extended typical scatter of 0.5 dex are highlighted with a gray line, a dark gray-shaded area, and a light gray-shaded area, respectively. We also plot the Popesso et al. (2023) SFMS at z = 5.2 with a dashed line.

lower than S1, S2, and S3. It is not detected in the deep ALMA observations at 1.2 mm (3σ upper limit of 0.6 mJy beam⁻¹) and other FIR observations, consistent with its low measured SFR (see Sect. 2.2). With these properties, the galaxy is about 1 dex below the main sequence as characterized by Schreiber et al. (2015), and 0.5 dex below the relation of Popesso et al. (2023).

# 4. Implications of the emergence of an ultra-massive grand-design spiral galaxy at 1 Gyr

## 4.1. An outlier among massive galaxies at z ~ 5

As discussed in Sect. 3.1, the galaxy is large, extending over 19 kpc (based on the size enclosing 80% of the light). We also measured its half-light size based on one- and two-component Sérsic profiles, finding ~3 and 3.9 kpc, respectively. By all metrics, Zhúlóng is large relative to comparable galaxies at similar redshifts. The typical average half-light size at z ~ 5 at log M*/M☉ ~ 10.7 from recent studies range between 0.4 and 2 kpc (e.g., Allen et al. 2024; Ito et al. 2024; Ormerod et al. 2024; Varadaraj et al. 2024; Ward et al. 2024), as estimated based on single-Sérsic models. These findings are in line with the expectation that galaxy size scales with dark matter halo size, which decreases with increasing redshift (e.g., Mo et al. 1998).

Unfortunately, JWST-derived mass-size relations, to date, are based almost entirely on galaxies one order of magnitude lower in mass, complicating direct comparison with this source. Compared to an extrapolation to the size-mass relation of SFGs at similar redshift, the half-light radius of Zhúlóng (Re ~ 3 kpc; single-Sérsic) does fall within the extrapolated scatter from lower masses (e.g., Allen et al. 2024; Miller et al. 2024).

However, in light of its low integrated sSFR (log sSFR ~ -9.2 yr⁻¹; >0.5 dex below the SFMS at these redshifts; see Fig. 5), such a large size is quite remarkable. Its red rest-frame U-V versus V-J colors in the core (see Sect. 3.2) are consistent with quiescent systems, perhaps making a

comparison to that population more appropriate. Typically, UVJ-red galaxies follow a steeper mass-size relation leading to much smaller sizes at fixed stellar mass than SFGs (e.g., van der Wel et al. 2014; Ito et al. 2024; Ji et al. 2024a). Quiescent galaxies with similarly high mass (log M*/M☉ > 10.3–11) at comparable redshifts (z > 4–7; e.g., Carnall et al. 2023; de Graaff et al. 2025; Weibel et al. 2024b; Ji et al. 2024b; Ito et al. 2024), have Re ~ 0.4–0.7 kpc, a factor of >4 smaller than what we find here (using our single-Sérsic measurement for Zhúlóng, for consistency with other studies). Unfortunately, sample sizes of comparable galaxies at log M*/M☉ ~ 11 at z ~ 5 remain small, regardless of the sSFR, and preclude a robust conclusion in comparison to the population scatter.

Thus, we also compared the R₈₀ size of Zhúlóng to the R₈₀ sizes of very massive log M*/M☉ ~ 11 galaxies (across all sSFRs) from larger-area HST surveys at z ~ 3 (Mowla et al. 2019b). We find that R₈₀ for this galaxy is still 50% larger than the average R₈₀ among comparable mass galaxies that appear more than 1 Gyr later (z ~ 2.75; Mowla et al. 2019a). While a definitive comparison to typical coeval massive galaxies is not possible without a more detailed analysis and data from larger JWST-based samples, collectively these first comparisons imply that Zhúlóng could be a notable outlier among massive galaxies, regardless of its location relative to the MS at z > 4.

While it is a likely outlier due to its large size, its properties as a massive spiral galaxy at z ~ 5.2 are also unexpected. The fraction of visibly spiral galaxies is already known to drop down to 4% at z ~ 3, in part due to surface brightness dimming that impacts visibility as (1 + z)⁴ (Kuhn et al. 2024), but remain rare even at cosmic noon (Law et al. 2012; Yuan et al. 2017). The entire spiral disk is also quite red; even at z ~ 2, where spirals are more prevalent (Conselice 2014), those with similarly red color (rest frame 0.3–0.5 µm ≥2 ABmag; Fudamoto et al. 2022) are rare, only making up 2% of the galaxy population (Shimakawa et al. 2022). The rarity of similar sources later in cosmic time makes the existence of Zhúlóng at z ~ 5.2 remarkable.

## 4.2. A Milky Way analog with 1 Gyr formation time

While a potential outlier at z ~ 5, this galaxy is instead remarkably comparable to massive evolved spirals like the MW at z ~ 0. MW-like spirals are characterized by old bulges (thought to form early in the universe) but whose extended disks are thought to have built up slowly over the course of 10 Gyr (van Dokkum et al. 2013; Bovy & Rix 2013). For context, current estimates indicate that the MW has a comparably massive core (bulge + bar) to Zhúlóng with log M*/M☉ ~ 10, total stellar mass of log M*/M☉ ~ 10.8 (even slightly lower than Zhúlóng), with a comparable sSFR, consistent with our upper limit (~10⁻¹⁰.⁶ yr⁻¹; Licquia & Newman 2015). Various estimates for the half-light radius of the MW suggest a scale length for the thin disk of Rₑ = 2.6 ± 0.5 kpc (Bland-Hawthorn & Gerhard 2016, and references within, based on independent analyses ranging between 1.8 and 6 kpc). The full extent of its stellar disk (diameter ~19 kpc) is already of comparable size to mature MW-like spirals seen at z ~ 0 (~8–12 kpc in diameter; e.g., Bland-Hawthorn & Gerhard 2016; Lian et al. 2024).

Unlike typical coeval galaxies, Zhúlóng has instead developed comparable structures (bulge mass and density, disk and spiral size, spatially segregated stellar populations) and comparable stellar mass, 10× faster than MW-like galaxies at z ~ 0, demonstrating that such an advanced evolutionary stage in galaxy evolution can be reached in only 1 Gyr. Moreover, in
the Λ cold dark matter paradigm, the Universe was 6³ times denser at z ~ 5 compared to today; this makes it astonishing that Zhúlóng appears with a well-organized morphology with a size close to that of the MW at z ~ 0 despite this high merger rate in the early Universe (e.g., Duan et al. 2024). How a morphologically mature galaxy that resembles nearby massive spirals can form in this environment remains an open question, but the discovery of this source is a first step and provides an important constraint on galaxy formation models.

### 4.3. Implications for the efficient growth of massive galaxies

The ultra-massive nature of Zhúlóng indicates an efficient mass build-up and a high star formation efficiency (see Fig. 4) in the past. Multiple minor mergers and/or major mergers may have driven this rapid growth. In addition, the presence of clumps also supports efficient growth; fragmentation of gas-rich disks into star-forming clumps may increase the star formation efficiency, helping galaxies grow more quickly to reach such masses (e.g., Dessauges-Zavadsky et al. 2019, 2023; Faisst et al. 2025; Fujimoto et al. 2024).

Although the galaxies described below have all been reported with high star formation efficiencies, the structure in the stellar populations of Zhúlóng clearly distinguishes it from other ultra-massive dusty SFGs (e.g., Xiao et al. 2024) and early-forming massive quiescent galaxies (e.g., Glazebrook et al. 2017, 2024; Carnall et al. 2023; Weibel et al. 2024b; de Graaff et al. 2025). It is clear that Zhúlóng formed through an inside-out pathway (see Sect. 3.2), and only a handful of other galaxies at z > 4 have been identified to have this stellar structure (e.g., Baker et al. 2024; Ji et al. 2024b; Nelson et al. 2024).

Zhúlóng has now demonstrated that there must be broad diversity in morphology among ultra-massive galaxies. While an answer about the origin of the spiral structure awaits further spectroscopic information, it now seems clear that at least some ultra-massive galaxies exhibit large disks (in contrast to the other known examples, which are nearly all compact). This may reflect a diversity of formation pathways that must be factored into any theories about the physical processes that drive their early formation at high redshift. Larger sample sizes will be required to better understand the morphological diversity of ultra-massive galaxies, which will be enabled in the future by the continued accumulation of wide-area JWST imaging.

## 5. Conclusions

We have presented the serendipitous discovery of the most distant ultra-massive spiral galaxy candidate identified in the pure parallel imaging survey PANORAMIC (in the COSMOS field). It has $z_{phot} = 5.2_{-0.2}^{+0.3}$, which is well constrained by a strong Balmer/4000 Å break and consistent with the neighboring star-forming clump (Fig. 1). After combining the JWST/NIRCam, HST, and ALMA data, we find the following extremely intriguing properties:

1. A quiescent bulge, a large star-forming disk, and spiral arms: From the morphological analysis, Zhúlóng perfectly exhibits a classical bulge ($n = 3.7 \pm 0.2$ and $R_e = 0.9 \pm 0.1$ kpc) and a large face-on stellar disk ($n = 1.2 \pm 0.1$, $R_e = 3.7 \pm 0.1$ kpc, and $b/a = 0.99 \pm 0.01$) extending over 19 kpc, with spiral arms embedded in (Fig. 2). The SED analysis of different annular regions shows that Zhúlóng has a quiescent-like core and a star-forming stellar disk (Fig. 3). Compared to the stellar disk,

the center core is (i) red ($F150W - F444W = 3.1$ mag); (ii) has one of the highest stellar mass surface densities measured among quiescent galaxies ($\log(\Sigma M_*/M_\odot \text{kpc}^{-2}) = 9.91_{-0.09}^{+0.11}$; see Table 1), revealing the buildup of the stellar bulge; and (iii) is quiescent – indicating an inside-out galaxy growth (or quenching). For the bulge, we derive $\log(M_{*,\text{bulge}}/M_\odot) = 10.71_{-0.09}^{+0.10}$, $\log(\Sigma M_{*,\text{bulge}}/M_\odot \text{kpc}^{-2}) = 10.00_{-0.11}^{+0.09}$, and $B/T = 0.5$.

2. Extreme stellar mass: Zhúlóng is extremely massive ($\log(M_*/M_\odot) = 11.03_{-0.08}^{+0.10}$; Fig. 4) and adds to the growing list of ultra-massive galaxies discovered in the first billion years. Assuming it is located in the most massive dark matter halo expected in the whole PANORAMIC survey volume, we infer that Zhúlóng must have been forming stars very efficiently, with a baryon-to-star conversion efficiency of $\epsilon \sim 0.3$, which is about 1.5 times higher than even the most efficient galaxies at later epochs.

3. Low star formation activity: Although the disk is still forming stars, Zhúlóng has a total SFR = $66_{-46}^{+89} M_\odot \text{yr}^{-1}$ (Table 1 and Fig. 5), which is $\ge 0.5$ dex below the SFMS at z ~ 5.2 (Schreiber et al. 2015; Popesso et al. 2023). This relatively modest SFR indicates that Zhúlóng is in the transformation phase from star-forming to quiescence.

4. Most distant spiral galaxy discovered so far: Compared to other recently reported stellar spiral galaxies at z > 3, Zhúlóng appears to be the most distant spiral galaxy discovered so far. While the origin of the spiral structure is unknown, it demonstrates that MW-like galaxies could evolve earlier in the Universe than previously thought (10 times faster than locally, <1 Gyr after the Big Bang) while efficiently building enormous stellar mass.

Zhúlóng, at $z_{phot} \sim 5.2$, is potentially the highest-redshift, red, ultra-massive, grand-design spiral galaxy with a large stellar size. Overall, the galaxy sits below the main sequence, suggesting its star formation activity is ramping down. It contains a quiescent bulge, a large star-forming disk, and spiral arms. For a galaxy at z > 5, having any of these relevant properties would be enough to make it special. The presence of all of these properties makes Zhúlóng very exceptional, indicating the rapid formation and morphological evolution of massive galaxies in the early Universe. With future JWST integral field unit (IFU) observations, combined with higher-resolution and deeper ALMA data, this galaxy will provide a unique window into what triggers rapid mass assembly and early disk formation.

**Acknowledgements.** We are very grateful to the anonymous referee for instructive comments, which helped to improve the overall quality and strengthened the analyses of this work. We thank Boris Sindhu Kalita, Francoise Combes, and Maximilien Franco for valuable discussions and suggestions that improved this paper. This work is based in part 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 2514. Support for program JWST-GO-2514 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2023.1.00180.L. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSTC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The work of CCW is supported by NOIRLab, which is managed by the Association
of Universities for Research in Astronomy (AURA) under a cooperative agree-
ment with the National Science Foundation. The Cosmic Dawn Center (DAWN)
is funded by the Danish National Research Foundation under grant DNRF140.
PD acknowledges support from the NWO grant 016.VIDI.189.162 ("ODIN")
and warmly thanks the European Commission's and University of Groningen's
CO-FUND Rosalind Franklin program. AH acknowledges support by the VIL-
LUM FONDEN under grant 37459. MVM acknowledges support from the
National Science Foundation via AAG grant 2205519 and the Wisconsin Alumni
Research Foundation via grant MSN251397. CCW, AC, ZJ and KEW acknowl-
edge funding from program JWST-GO-2514 that was provided by NASA
through a grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS 5-03127. ZJ also acknowledges funding from JWST/NIRCam
contract to the University of Arizona NAS5-02015. I.L. acknowledges sup-
port from Australian Research Council Future Fellowship FT220100798. SL
acknowledges support by the Science and Technology Facilities Council (STFC)
and by the UKRI Frontier Research grant RISEandFALL. LB acknowledges
funding from STFC through ST/T000473/1 and ST/X001040/1. K.G. and T.N.
acknowledge support from Australian Research Council Laureate Fellowship
FL180100060.

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5 Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191 Gif-sur-Yvette, France

6 Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UK

7 Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA 15260, USA

8 Department of Physics, University of California, Santa Barbara, CA 93106, USA

9 Department of Astronomy, University of Texas at Austin, 2515 Speedway Blvd. Stop C1400, Austin, TX 78712, USA

10 Department of Astronomy, University of Massachusetts Amherst, Amherst, MA 01003, USA

11 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands

12 Caltech/IPAC, 1200 E. California Blvd., Pasadena, CA 91125, USA

13 Leiden Observatory, Leiden University, PO Box 9513, NL-2300 AA Leiden, The Netherlands

14 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn 3122, VIC, Australia

15 Laboratory for Multiwavelength Astrophysics, School of Physics and Astronomy, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623, USA

16 Aix Marseille Univ., CNRS, CNES, LAM, Marseille, France

17 Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK

18 Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge CB3 0HE, UK

19 Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison, WI 53706, USA

<footnote n="1">¹ Department of Astronomy, University of Geneva, Chemin Pegasi 51, 1290 Versoix, Switzerland</footnote>

<footnote n="2">² NSF National Optical-Infrared Astronomy Research Laboratory, 950 North Cherry Avenue, Tucson, AZ 85719, USA</footnote>

<footnote n="3">³ Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA</footnote>

<footnote n="4">⁴ Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Jagtvej 128, København N DK-2200, Denmark</footnote>
# Appendix A: Robustness of the redshift solution for Zhúlóng

In Fig. 1 we show the narrow photometric redshift distribution $P(z)$ of Zhúlóng, derived using EAZY for the galaxy core (0.16" radius aperture). To ensure the robustness of our results, we also performed SED fitting with Bagpipes, allowing the redshift to vary from 1 to 10. We assumed different SFHs, including delayed SFH and double-power-law SFH, and the same settings as described in Sect. 3.2. The resulting $P(z)$ shows a single strong peak, consistent with the EAZY results. Specifically, the photometric redshift is $z_{phot} = 5.42_{-0.45}^{+0.31}$ for delayed SFH (Fig. A.1-a) and $z_{phot} = 5.59_{-0.38}^{+0.29}$ for the double-power-law SFH.

However, when a larger aperture (e.g., 0.7" radius) is used, a second redshift solution at $z \sim 1.6$ emerges (Fig. A.1-b). To further investigate this, we reran the SED fitting for the galaxy core using EAZY with the redshift fixed to $z = 1.6$. The resulting fit, shown in Fig. A.1-c, has a large chi-square value ($\chi^2 = 46$), indicating a very poor fit.

To explore the cause of this low-redshift solution with a large aperture, we further inspected the images and find a bright clump (clump 2, thereafter; Fig. A.1-d) at F606W and F814W from HST/ACS. Clump 2 is located southeast of the $z_{phot} = 5.15_{-0.03}^{+0.04}$ clump reported in Fig. 1. The EAZY fitting results for clump 2 show a broad $P(z)$ distribution with $z_{phot} = 1.65_{-0.02}^{+2.11}$, suggesting it may be a foreground clump. Thus, the second redshift peak in Fig. A.1-b is likely due to contamination from clump 2.

We performed SED fitting on the galaxy core using both EAZY and Bagpipes, and both methods consistently indicate that Zhúlóng is a strong spiral galaxy candidate at $z > 5$. However, we identify the potential presence of foreground structure(s) that could contaminate the redshift measurements of Zhúlóng when larger apertures are used. We note here that clump 2 does not affect our main results, as the global properties of Zhúlóng are derived using the total flux measured within a 0.5" radius aperture (with aperture corrections applied), with clump 2 not included. While clump 2 is included in the SED fitting for the annular radius of 0.5" – 0.7" and may influence the fitting results (see Fig. 3), we cannot confirm whether it is a low-$z$ clump without spectroscopic observations and thus did not remove it from the analysis. In any case, the key findings of inside-out galaxy growth and a quiescent-like galaxy core embedded in a star-forming stellar disk remain consistent even when considering only the remaining annuli. In addition, it does not affect our identification of spiral features. To confirm whether Zhúlóng is indeed a distant spiral galaxy at $z > 5$, follow-up JWST NIRSpec/IFU observations are necessary.

<figure><img src="image_7.png" /><figcaption>**Fig. A.1.** (a) Photometric redshift likelihood distribution, $P(z)$, for the central core (0.16" radius aperture) derived with Bagpipes. This $P(z)$ is consistent with that shown in Fig. 1. (b) $P(z)$ derived with Bagpipes using a 0.7" radius aperture, showing a second redshift solution at $z \sim 1.6$. (c) EAZY SED fitting results for the central core (0.16" radius) with the redshift fixed at $z = 1.6$, indicating a poor fit with $\chi^2 = 46$. (d) Bright clump (clump 2, marked with a black circle) detected at $5.5\sigma$ and $7.5\sigma$ in the F606W and F814W bands, respectively. The EAZY fit for clump 2 shows a broad redshift distribution with $z_{phot} = 1.65_{-0.02}^{+2.11}$, which suggests it may be a foreground object.</figcaption></figure>
Appendix B: Morphological modeling of Zhúlóng

<figure><img src="image_8.png" /><figcaption>**Fig. B.1.** Similar to Fig. 2, but showing results for the F277W, F356W, F444W, and stacked images. Each is modeled using double Sérsic profiles to decompose the bulge and disk.</figcaption></figure>

<figure><img src="image_9.png" /><figcaption>**Fig. B.2.** Similar to Fig. 2, but showing results for the F277W, F356W, F444W, and stacked images. Each is modeled using a single Sérsic profile.</figcaption></figure>