JWST's PEARLS: A JWST/NIRCam View of ALMA Sources

Our sample is collected from three fields that have both ALMA archival data and new JWST/NIRCam data. ACT-CL J0102−4915 (nicknamed "El Gordo") is a high-mass (M_tot ∼ 10¹⁵ M_⊙), colliding galaxy cluster at z = 0.87 (Menanteau et al. 2010, 2012; Marriage et al. 2011; Jee et al. 2014; Lindner et al. 2014). It was selected as a PEARLS field because it is a powerful cosmic lens. Its lensing properties have been modeled based on lensed background objects detected by HST (Zitrin et al. 2013; Diego et al. 2020) and more recently by the PEARLS team (Diego et al. 2022; B. Frye et al. 2022, in preparation) using JWST data.

TN J1338 + 1942 (hereafter "TNJ1338") is a radio galaxy at z = 4.11 (De Breuck et al. 1999) and is the dominant member of a protocluster (Venemans et al. 2002; Miley et al. 2004). It was selected as a PEARLS field primarily for the study of galaxy properties in a protocluster environment.

The UKIDSS Ultra-Deep Survey field (hereafter "UDS"—Stach et al. 2018) is one of the most-studied extragalactic survey fields and is where PRIMER will carry out the majority of its JWST observations.

The El Gordo field has been observed by the ALMA programs 2013.1.01358.S (PI: A. Baker) and 2018.1.00035.L (PI: K. Kohno) in Band 6 (270 GHz = 1.1 mm) and 2013.1.01051.S (PI: P. Aguirre) in Band 7 (340 GHz = 870 μm). The ALMA data in the TNJ1338 field were obtained by program 2015.1.00530.S (PI: C. De Breuck) in Band 3 (92 GHz = 3.3 mm). The UDS has a large number of ALMA programs. In the current PRIMER UDS field, the ALMA Band 6 and/or Band 7 data were collected by astroquery in each PRIMER observation region. These archival data were reduced by the Chinese South American Center ALMA data processing program (C. Cheng et al. 2023, in preparation). Briefly, the data were calibrated by the default ALMA data reduction script ScriptForPI.py. The task tclean in casa 6.2.1 (McMullin et al. 2007) was used to clean the data to build the continuum images. For this set of data, the clean parameters were set to weighting = "briggs" and robust = 2.0, and we cleaned the images to 3σ.

The final 1.1 mm map in El Gordo has beam size 128 × 093 at PA = 88° and reaches ∼0.065 mJy beam⁻¹ (rms). This map has an area of ∼4 arcmin² overlapped with the NIRCam coverage (see below) and was used for the source detection in this field. The final 870 μm map, which covers only a portion of the 1.1 mm map, reaches 0.25 mJy beam⁻¹ with beam size 033 × 040 at PA = − 35°.

In TNJ1338, the final 3.3 mm map has beam size of 211 × 174, PA = − 82° and reaches ∼0.009 mJy beam⁻¹ rms. It covers ∼2 arcmin², centered around the radio galaxy.

In the UDS field, the final images have beam sizes of about 07 at 1.1 mm and 04 at 870 μm. The total coverage is ∼1 arcmin². Both images reach rms ∼0.05 mJy. The source detections were done in both bands, and the results were merged.

Source extraction was done by running SExtractor (Bertin & Arnouts 1996) in dual-image mode. The detection was done on the ALMA maps not corrected for the primary-beam attenuation, as these have a uniform noise distribution. The photometry was done on the primary-beam-corrected images exported from casa. The detection map was convolved using a Gaussian kernel, and we set detect_thresh = 4. flux_auto was adopted for the flux density measurements. To account for the calibration uncertainty, we added in quadrature 10% of the flux density (Fomalont et al. 2014) to the reported fluxerr_auto to obtain the final uncertainty estimate. All these detections have signal-to-noise ratios (S/Ns) higher than 3, and all but two have S/N > 5 (see Table 1).

Table 1. ALMA Source Catalog

Name	R.A.	Decl.	S870μm	S1.1mm	S3.3mm	Redshift	$\mathrm{log}({M}_{* })$	log(SFR)	Re (NIR)	μ
	J2000	J2000	(mJy)	(mJy)	(mJy)		log(M⊙)	log(M⊙ yr−1)	(kpc)
EG-ALMA 2a	01:02:49.2	−49:15:08.7	⋯	0.32 ± 0.03	⋯	3.58 ± 0.38 a	⋯	⋯	⋯	4.6
EG-ALMA 2b	01:02:49.4	−49:15:05.3	1.62 ± 0.12	0.65 ± 0.07	⋯	3.58 ± 0.38 a	⋯	⋯	⋯	5.5
EG-ALMA 3	01:02:49.3	−49:14:38.1	⋯	0.75 ± 0.08	⋯	2.34 ± 0.51	10.94 ± 0.11	1.94 ± 0.49	5.35 ± 0.27	2.1
EG-ALMA 5	01:02:50.5	−49:15:41.7	⋯	0.25 ± 0.03	⋯	2.49 ± 0.30	11.13 ± 0.14	1.09 ± 0.44	1.53 ± 0.30	1.8
EG-ALMA 6a	01:02:51.1	−49:15:38.8	⋯	0.90 ± 0.09	⋯	4.324 b	⋯	⋯	⋯	3.9
EG-ALMA 6b	01:02:54.9	−49:15:14.7	1.37 ± 0.15	1.24 ± 0.12	⋯	4.324 b	⋯	⋯	⋯	3.1
EG-ALMA 6 c	01:02:55.7	−49:15:09.0	1.89 ± 0.19	0.99 ± 0.10	⋯	4.324 b	10.14 ± 0.10	1.97 ± 0.14	1.80 ± 0.10	10.0
EG-ALMA 11	01:02:57.7	−49:15:20.0	⋯	0.11 ± 0.01	⋯	1.67 ± 0.21	10.96 ± 0.11	1.08 ± 0.46	2.27 ± 0.27	2.3
EG-ALMA 12	01:02:58.1	−49:14:56.2	⋯	0.63 ± 0.07	⋯	2.49 ± 0.18	10.91 ± 0.15	0.98 ± 0.58	1.63 ± 0.34	1.4
EG-ALMA 13	01:03:00.2	−49:16:03.4	⋯	0.17 ± 0.02	⋯	1.80 ± 1.08	10.48 ± 0.12	1.32 ± 0.62	1.08 ± 0.21	3.2
UDS-ALMA 1	02:17:19.6	−05:09:41.4	4.91 ± 1.54	⋯	⋯	2.10 ± 0.13	11.15 ± 0.08	2.30 ± 0.38	1.18 ± 0.42	1
UDS-ALMA 2	02:17:21.0	−05:08:37.2	⋯	0.93 ± 0.16	⋯	2.08 ± 0.06 c	⋯	⋯	< 0.80	1
UDS-ALMA 3	02:17:22.3	−05:10:38.6	⋯	1.02 ± 0.13	⋯	1.089 d	11.55 ± 0.14	1.75 ± 0.64	2.54 ± 0.39	1
UDS-ALMA 4	02:17:26.1	−05:10:58.3	3.04 ± 0.38	0.86 ± 0.09	⋯	1.74 ± 0.38	11.18 ± 0.19	2.42 ± 0.37	4.64 ± 0.42	1
UDS-ALMA 5	02:17:27.2	−05:11:57.8	6.31 ± 0.65	2.43 ± 0.57	⋯	2.154 d	11.32 ± 0.08	2.33 ± 0.22	3.78 ± 0.41	1
UDS-ALMA 6	02:17:43.9	−05:07:51.3	2.19 ± 0.26	⋯	⋯	2.51 ± 0.28	11.31 ± 0.07	2.28 ± 0.36	1.44 ± 0.40	1
TN-ALMA 1	13:38:24.9	−19:42:15.8	⋯	⋯	0.057 ± 0.006	3.17 ± 1.03	10.77 ± 0.40	2.36 ± 0.33	1.12 ± 0.42	1
TN-ALMA 2	13:38:25.7	−19:42:34.6	⋯	⋯	0.046 ± 0.005	3.39 ± 0.26	10.58 ± 0.09	2.17 ± 0.31	1.20 ± 0.39	1
TN-ALMA 6	13:38:26.9	−19:42:30.9	⋯	⋯	0.031 ± 0.003	1.47 ± 0.46	11.35 ± 0.10	2.05 ± 0.46	2.80 ± 0.41	1

Notes. The flux densities, masses, SFRs, and sizes for the El Gordo sources have been corrected for the gravitational lensing magnification μ. For most objects, their z_phot from magphys-photoz are listed in the "Redshift" column. The exceptions are (1) the objects that have z_spec, for which their z_spec are listed; and (2) the point-like source UDS-ALMA 2, for which we adopt z_phot from eazy as it was derived using AGN templates and is more plausible. R_e is for the disk component (i.e., with a point-source core subtracted for UDS-ALMA 1/3/4/5). Because R_e is measured in the rest-frame near-IR, it is equivalent to the half-mass radius.

^a Lensed double images of a single source (see Diego et al. 2022). ^b Lensed triple images of a single source. Its z_spec is based on CO J = 4–3 emission line (see Appendix B) and has uncertainty 0.001. ^c z_phot derived by eazy using AGN templates. ^d z_spec from Lang et al. (2019), Bourne et al. (2019). The typical z_spec uncertainty is 0.001.

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The PEARLS NIRCam data in the TNJ1338 field and the El Gordo field were taken on 2022 July 1 and 29, respectively, and these observations are described by Windhorst et al. (2023). Briefly, the observations of El Gordo were done in F090W, F115W, F150W, F200W, F277W, F356W, F410M, and F444W, and the total integration times were 2491, 2491, 1890, 2104, 2104, 1890, 2491, and 2491 s, respectively. The observations in TNJ1338 were done in F150W, F182M, F210M, F300M, F335M, and F360M with a uniform total integration time of 1031 s in each band. In both fields, the areas where the ALMA data reside are covered by one NIRCam module (module B).

As of this writing, only a small fraction of the PRIMER observations in UDS were executed, all on 2022 July 29. The NIRCam data were taken in three pointings as the parallels to the primary MIRI observations. One pointing is isolated, while the other two overlap and fill the wide gaps between the two NIRCam modules. The passbands used were the same as for El Gordo, but integration times were 837 s in each band.

All data were reduced using the JWST data reduction pipeline version 1.6.1dev3+gad99335d in the context of jwst_0944.pmap, starting from the Stage 1 "uncal" products. A few changes and augmentations were made to the pipeline to improve the reduction quality (Yan et al. 2022). In the El Gordo field, the final stacked images were created at a pixel scale 006 and were aligned to the existing HST images of the same scale produced by the Reionization Lensing Cluster Survey (Coe et al. 2019). The final stacks in the TNJ1338 field were also aligned to the existing HST images, which are available from the High Level Science Products provided by the Mikulski Archive for Space Telescopes. These HST images have pixel scale of 004, and the NIRCam images were created at the same scale. In the UDS field, the final stacks were created at 006 pixel⁻¹ and were aligned to the existing HST images of the same scale from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS; Grogin et al. 2011; Koekemoer et al. 2011).

In total, we identified 10, 4, and 6 NIRCam counterparts of our ALMA sources in the El Gordo, TNJ1338, and UDS fields, respectively. One of the TNJ1338 sources is the central radio galaxy, which is studied by Duncan et al. (2022) and not discussed further here. Table 1 lists the remaining 19 sources. Figure 1 shows the HST/Advanced Camera for Surveys (ACS) and NIRCam stamp images for each. The sources in the El Gordo field are affected by gravitational lensing to various degrees. In particular, EG-ALMA 6a/6b/6 c are the triple images of a single galaxy that is believed to be associated with the z = 4.32 galaxy group (Caputi et al. 2021). EG-ALMA 2a/2b are two images of another single galaxy lensed by two cluster-member galaxies as well as the cluster as a whole. Therefore, the 10 sources in this field correspond to seven unique galaxies; and so our final sample consists of 16 galaxies.

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For the targets in the El Gordo field, we did not use the HST data because the JWST NIRCam data alone sufficiently sample the rest-frame visible-to-near-IR range. In the UDS field, UDS-ALMA 4 has no NIRCam data in the short wavelength bands because it falls in the gap in between the modules. Therefore, we used the HST data in F606W, F814W, F125W, and F160W. For homogeneity, these HST images were also used for the other UDS targets. In TNJ1338, the bluest NIRCam band is F150W, and therefore we added HST F775W and F850LP data to extend the wavelength sampling to visible wavelengths.

We used SExtractor in dual-image mode for photometry. For the sources in El Gordo and UDS, the detection band was set to F444W; in TNJ1338, it was set to F360M. In most cases, we adopted mag_iso to optimize the S/N for the best color measurement. The exceptions were the two multiply imaged systems EG-ALMA 2a/2b and EG-ALMA 6a/6b/6 c. The former is blended with two cluster-member galaxies, which contribute the major part of the lensing effect that creates this system. The latter has a close neighbor that might be associated with the source but is not the counterpart. In both cases, their mag_iso apertures are severely contaminated by the light from these neighbors. To minimize the contamination, we had to derive colors using a circular aperture of 06 in diameter centered on the position of the brightest pixel in the F444W image.

Figure 2 shows the full SEDs, combining rest-frame visible-to-near-IR photometry with the ALMA photometry. We used magphys+photoz (da Cunha et al. 2008; Battisti et al. 2019) to fit these SEDs to obtain physical properties of the hosts, most importantly the photometric redshift (z_phot), the star formation rate (SFR), and the stellar mass (M_*). The best-fit results are shown in Figure 2, and the derived values are presented in Table 1. The SFR and M_* values for the El Gordo sources have been corrected for the magnification factors (μ) at the corresponding redshifts. Two sources, UDS-ALMA 3 and 5, have spectroscopic redshifts (z_spec), which are quoted in Table 1; their M_* and SFR listed in the table were derived at their z_spec, while Figure 2 still shows their SED-fitting results when treating redshift as a free parameter.

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magphys+photoz is designed to fit panchromatic SEDs based on the "energy-balance" premise, which argues that the UV-to-near-IR energy absorbed by dust in a system should roughly equal the far-IR-to-millimeter light reemitted by dust. This approach provides a good constraint on the amount of dust extinction, and propagates the uncertainty of z_phot to the uncertainties in other derived parameters. However, the energy-balance premise might not hold if the dust component is not well mixed with stars in the host galaxy. In addition, we have only one or two ALMA bands constraining the dust emission. To check the robustness of the z_phot derived by magphys+photoz, we also fitted the visible-to-near-IR SEDs using eazy (Brammer et al. 2008) with eazy_v1.1_lines.spectra.param templates to derive z_phot independently. The best-fit results are summarized in Figure 3. For most sources, these two sets of z_phot are consistent with each other (see Appendix A), which gives us confidence in the results obtained by magphys+photoz.

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EG-ALMA 2a/2b and EG-ALMA 6a/6b/6 c are two multiply imaged systems. (The latter has z_spec from the ALMA spectroscopy; see Appendix B.) It is difficult to obtain reliable photometry for them because the images are highly distorted. This is reflected in the disagreement in z_phot values for the individual images and for the same image as measured by the two different methods. We have therefore excluded these objects from the later discussion. We also exclude UDS-ALMA 2, which is likely a quasar, for most purposes.

Figure 4 (left) compares these ALMA source hosts to the "star formation main sequence" from Speagle et al. (2014). Excluding EG-ALMA 2a/2b, EG-ALMA 6a/6b/6 c, and UDS-ALMA 2, all other sources have M_* ≥ 10^10.5 M_⊙, in line with the general SMG population. However, three objects have SFR ≤ 16 M_⊙ yr⁻¹, which puts them well below the main sequence. This is more clearly seen in Figure 4 (middle). The mean ratio of specific SFR (sSFR) to main sequence is 0.24; the aforementioned three sources are below 0.10, which places them in the realm of quiescent galaxies. In other words, their host galaxies have already built up the bulk of their stellar masses, and their ongoing star formation, while detectable from the submillimeter/millimeter emission, is not significantly increasing the host's stellar mass. The usual UVJ diagnostic (Figure 4 right) shows that the three quiescent hosts are indeed in the conventional quiescent-galaxy region (Labbe et al. 2005; Williams et al. 2009), verifying the low sSFR.

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The NIRCam images (Figure 1) allow morphologies to be determined for 13 of the ALMA source hosts. ²⁷ By our visual classification, all 13 show nondisturbed (or weakly disturbed) disks even though some of them (e.g., UDS-ALMA 4) might have features indicative of a recent minor merger. ²⁸

To further study the morphologies, we ran galfit (Peng et al. 2002) to fit Sérsic profiles to the galaxies' F444W or F360M images (the latter only for the three TNJ1338 sources). The results are shown in Figure 5 and detailed in Appendix B. Briefly, the fitted Sérsic indices n are near 1 (median 〈n〉 = 1.1 ± 0.8), consistent with disky galaxies. The galfit run also computed half-light radii (R_e ) based on the best-fit profile and excluding a central point source when one was present. At the source redshifts, F444W or F360M samples the rest-frame visible-to-near-IR range, and therefore this R_e reflects the stellar mass distribution. In other words, R_e is a proxy for the half-mass radius. The median R_e of our sample is 1.6 kpc with bootstrap uncertainty 0.4 kpc. The dispersion of the whole sample is 1.4 kpc. For comparison, the median R_e of the disk galaxies among the far-IR/SMG sample (0.5 ≲ z ≲ 3) of Ling & Yan (2022) is 3.6 kpc. Figure 6 shows the mass–size distributions of our ALMA sources as well as those of the few recently published NIRCam results in other fields. The mass–size relations of star-forming and quiescent galaxies fromSuess et al. (2019, their Figure 7) are also shown for comparison. Qualitatively, most of our sources fall below the relation for star-forming galaxies and are more in line with that of quiescent galaxies, despite the fact that most of our sources are not quiescent. In contrast, the ultrared, flattened, disky galaxies recently found by Nelson et al. (2022) have larger R_e and follow more closely the relation for star-forming galaxies. A larger sample will be needed to further investigate this problem.

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By virtue of their submillimeter/millimeter emission, the ALMA sources discussed in this work are SMGs. However, they include many sources fainter than the bulk of the SMG population previously studied in the literature. This is because of the combination of the gravitational lensing by a cluster in one of our survey fields and that most of our sources were not preselected by surveys using single-dish submillimeter/millimeter telescopes but were serendipitous discoveries in ALMA maps of various depths. The ALMA maps are deeper than any single-dish survey, and therefore most of our ALMA sources are fainter than those from the usual SMG samples. This is demonstrated in Figure 7. Specific to the El Gordo field, the median S_870μm flux density of our sample is 1.1 mJy after correcting for the lensing magnification. If we exclude the two multiply imaged systems, the median S_870μm drops to 0.5 mJy in the El Gordo field, and the median S_870μm of the whole sample is 2 mJy. In contrast, the AS2UDS sample has median S_870μm = 3.6 mJy and reaches down to 0.6 mJy. Our sample therefore includes more SMGs with low-to-moderate SFRs, which explains why most of our sources exhibit properties (e.g., their nondisturbed disky morphologies) different from those often described in the literature. On the other hand, it is not surprising that most z ≳ 2 galaxies should have some low-level, ongoing star formation. Due to the high sensitivity of ALMA, our sample is more sensitive than the single-dish-preselected SMG samples in probing such activity.

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After excluding the two multiply imaged systems (EG-ALMA 2a/2b and EG-ALMA 6a/6b/6c) and the quasar (UDS-ALMA 2), the remaining 13 ALMA source hosts in our sample are all disk galaxies, mostly showing little sign of disturbance suggestive of major mergers. The two ALMA sources of Cheng et al. (2022) that are large enough for morphological study are similar systems. This would be a surprising result in the pre-JWST era. However, recent JWST/NIRCam morphological studies of the general galaxy population have shown that disk galaxies are already common at z > 1.5 (Ferreira et al. 2022a, 2022b; Jacobs et al. 2022). If star formation at z ≈ 1–3 mostly happens in disk galaxies, it can explain why our ALMA source hosts are mostly such systems.

All these 13 disk galaxies have already acquired large stellar masses, which range from 0.3 to 3.5 × 10¹¹ M_⊙. As they have no indication of being major mergers, these galaxies most likely assembled the majority of their stars through secular growth (e.g., Guo et al. 2022), although we cannot rule out the role of minor mergers. Given their SFRs of 10–300 M_⊙ yr⁻¹, their sSFRs spread them over both the star-forming main sequence and the quiescent categories. Three of them are deemed quiescent galaxies based on their sSFRs. These same three galaxies are also in the quiescent region in the rest-frame UVJ diagram, which is to say that their UV-to-near-IR emissions show no sign of ongoing star formation. Had there not been ALMA revealing their low-level star formation hidden by dust (SFRs of 10–15 M_⊙ yr⁻¹), they would be viewed as "red-and-dead" and yet disky galaxies. These galaxies are similar to those recently reported by Nelson et al. (2022) in the sense that they are also red disky galaxies; the difference is that ours are still detected in the HST bands. Future morphological study within the same ALMA coverage will reveal whether there really are disk galaxies that have completely ceased star formation.

Another interesting result is that our galaxies have a wide range of half-light (equivalently, half-mass) radii R_e . EG-ALMA 3 has the largest R_e = 5.35 ± 0.27 kpc, while EG-ALMA 13 has the smallest R_e = 1.08 ± 0.21 kpc. EG-ALMA 3 (z_phot = 2.34, M_* = 8.7 × 10¹⁰ M_⊙, SFR = 87 M_⊙ yr⁻¹) is similar to the recently reported grand-design spiral galaxy A2744-DSG-z3 at z = 3.06 (Wu et al. 2022), which has R_e = 7.3 ± 0.8 kpc and M_* = 4.0 × 10¹⁰ M_⊙. The latter is also an ALMA source and has SFR = 85 M_⊙ yr⁻¹ based on its far-IR-to-millimeter luminosity (Sun et al. 2022). Such large disks are rare in our sample; however, the median R_e of our sample is 1.6 kpc, which means that our targets are predominantly small disks. The sizes of the general disk-galaxy population at z > 1.5 is still awaiting investigation, and therefore it is unclear whether our sample being dominated by small disks is normal or is caused by some selection bias that is still unknown to us.