First Batch of z ≈ 11–20 Candidate Objects Revealed by the James Webb Space Telescope Early Release Observations on SMACS 0723-73

Over the past decade, the search for high-redshift (high-z) galaxies using deep Hubble Space Telescope (HST) images in fields on both “blank sky” and lensing clusters seems to suggest that the number density of galaxies at z > 6 sharply decreases toward higher and higher redshifts (Oesch et al. 2012a, 2012b; Finkelstein et al. 2012; Yan et al. 2012; Zheng et al. 2012; Coe et al. 2013; McLure et al. 2013; Bradley et al. 2014; Bouwens et al. 2015; McLeod et al. 2016; Ishigaki et al. 2018) and even a dearth of galaxies at z > 10 (Oesch et al. 2018). This, if true, would create a severe problem for our understanding of the cosmic hydrogen reionization. There has been a consensus that the reionization ended at z ≈ 6.2 (Fan et al. 2006; Planck Collaboration et al. 2016). There is also a piece of evidence from the detection of 1.420 GHz (21 cm) H i absorption of the cosmic microwave background that the first stars came into being at z ≈ 17.2 (spanning z = 13.7–22.9; Bowman et al. 2018), which is to say that the reionization should begin at the same redshift. While this result is still under debate, an independent line of evidence also points to a similar redshift as the epoch of the first stars. One example is the gravitationally lensed galaxy MACS 1149-JD1 (Zheng et al. 2012), which is at z = 9.1096 based on the Atacama Large Millimeter/submillimeter Array (ALMA) detection of its [O iii] 88 μm line (Hashimoto et al. 2018). The very existence of oxygen ⁴ means that the galaxy has already been polluted by the previous generation of stars. To reproduce its spectral energy distribution (SED), especially its Balmer break, these authors found that the onset of the galaxy must be ∼290 Myr earlier, i.e., at the formation redshift z_f ≈ 15. It is therefore conceivable that first stars should be formed at an even earlier time (by a few tens of Myr), and so should the beginning of the reionization. All this, however, is inconsistent with the suggestion that the number of galaxies diminishes at z > 10 because this would imply that the reionization could not have happened.

HST cuts off at around 1.7 μm at the red end, which limits the highest possible redshift that it could probe to z ≈ 11. The task of exploring higher redshifts is now transferred to the James Webb Space Telescope (JWST), which just demonstrated its superb performance through the revelation of its Early Release Observations (ERO) on 2022 July 12 (Pontoppidan et al. 2022). The most relevant ERO observations to high-z studies were the NIRCam imaging on the lensing cluster SMACS 0723-73, which was one of the 41 clusters previously observed by HST in the Reionization Lensing Cluster Survey (RELICS; Coe et al. 2019). This field was observed by the NIRCam instrument (among others) in six bands, and the data were made available worldwide on July 13. These were among the very first set of JWST data suitable for high-z studies. Taking advantage of this opportunity, we report in this Letter our initial search of z > 11 objects in this field, using the now-standard “dropout” technique to identify the characteristic Lyman-break signature in the SEDs of high-z objects (e.g., Steidel et al. 1995; Bouwens et al. 2004; Stanway et al. 2004; Yan & Windhorst 2004). We briefly describe the data and the photometry in Sections 2 and 3, respectively. The selection of z > 11 candidate objects is presented in Section 4. We conclude with a discussion of the results in Section 5. All magnitudes quoted are in the AB system. All coordinates are of J2000.0 Equinox. We adopt the following cosmological parameters: Ω_M = 0.27, Ω_Λ = 0.73, and H₀ = 71 km s⁻¹ Mpc⁻¹.

The NIRCam observations were carried out on UT 2022 June 7 in six bands, namely, F090W, F150W, and F200W in the “short-wavelength” (SW) channel and F277W, F356W, and F444W in the “long wavelength” (LW) channel. ⁵ As NIRCam operates in these two channels simultaneously on the same fields of view, these SW and LW passbands were observed in pairs. The exposures were obtained using nine INTRAMODULEBOX dithers to fill the 4″–5″ gaps in between the SW detectors, which did not fill the 42″–48″ gap between the modules. This resulted in two nonoverlapping fields of ∼24 × 24 each in the SW and ∼22 × 22 each in the LW. The main part of the cluster was covered by module B in the northeastern direction, while module A observed a flanking field. The dithered positions were determined by the STANDARD subpixel dither to optimally sample the point spread functions (PSFs). For each exposure, the MEDIUM8 readout pattern was adopted in the “up-the-ramp” fitting to determine the count rate. There was one integration per exposure, and each integration contained nine groups. In total, the effective exposure time in each band is 7537.2 seconds. The passband response curves are shown in Figure 1, together with the spectra of three model galaxies redshifted to z = 11 and z = 15, which we will explain in Section 4.

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As it turned out, the fully processed “Stage 3” data made available through the ERO release on July 13 were not suitable for this study due to a number of reasons. Most critically, the astrometric calibrations of different bands have small but notable inconsistencies, which makes photometry difficult. We therefore opted to reprocess these data. We retrieved the products from the Mikulski Archive for Space Telescopes (MAST), which are the calibrated single exposures from the standard JWST data reduction pipeline after the “Level 2b” processing. We then used calwebb_image3 (version 1.6.1 ⁶ ) the “Level 3” pipeline module for imaging data, to combine the single exposures in each band. As the two modules produced two nonoverlapping fields, we processed their data separately. To obtain internally the consistent world coordinate system, we aligned the individual module B images using the RELICS catalog ⁷ as the reference. For the module A images, we performed the alignment using the first image in F150W as the reference. The pixel scale and the image dimensions were set to 006 pix⁻¹ and 5000 × 5000 pixels, respectively, in all bands. The internal alignment among the six mosaics is consistent to ≲0.3 pixel. The absolute astrometric calibration of the final mosaics in both fields were tied to the second data release of Gaia. The astrometry thus determined is accurate to ∼003 and 009 (rms) in modules B and A, respectively, in both R.A. and decl. directions. The accuracy in module A is worse because there is no external source catalog comparable to the RELICS catalog used as the intermediate in the calibration.

The final stacks are in the surface brightness units of MJy sr⁻¹. At the scale of 006 pix⁻¹, this translates to the magnitude zero-point of 26.581 for all. We derive that the 5σ depths (within 02 radius aperture) in F090W, F150W, F200W, F277W, F356W, and F444W are 28.17, 28.54, 28.73, 29.67, 29.73, and 29.72 (28.16, 28.51, 28.69, 29.49, 29.69, and 29.81) mag, respectively, for module A (module B). The module B images are slightly less sensitive than the ones in module A, presumably due to the impact of the intracluster light (ICL).

We performed matched aperture photometry by running SExtractor (Bertin & Arnouts 1996) in the dual-image mode using the F356W images as the detection images. This choice was made for two reasons. First, the F356W images are about the deepest (see above). Second, the PSF in this band is nearly twice as large as in the SW bands, which makes an aperture defined in this band always sufficient to capture all the source flux in the bluer bands.

We adopted the MAG_ISO magnitudes for the color measurements. The sources of our interest are small enough in the images such that the MAG_ISO apertures include nearly all the source flux while minimizing the background noise. Hereafter we denote the magnitudes in the six bands as m₀₉₀, m₁₅₀, m₂₀₀, m₂₇₇, m₃₅₆, and m₄₄₄, respectively. We only kept the sources that have S/N ≥ 5.0 and ISOAREA_IMAGE ≥ 10 in F356W.

4.1. Selection Overview

4.2. SED Analysis

4.3. F150W Dropouts

The depths of the two bands straddling the Lyman break set the depth of the dropout selection. The nominal 2σ sensitivities (measured within 02 aperture in radius) in F150W are 29.54 and 29.50 mag in modules A and B, respectively. The criterion of m₁₅₀ − m₂₀₀ ≥ 0.8 mag for F150W dropout selection therefore implies that a valid F150W dropout should have m₂₀₀ ≤ 28.74 and 28.70 mag in these two modules, respectively. The subtlety is that the 02 aperture is only an approximation of the real MAG_ISO apertures in use. Here we ignore this difference.

There are 32 (28) validated F150W dropouts in module A (B), and the median brightness is m₂₀₀ = 28.23 (28.13) mag. There are three and four bright objects with m₂₀₀ ≤ 27.5 mag in modules A and B, respectively. ⁸ Figure 2 shows the image stamps of an example object in the six NIRCam bands (top), together with its SED fitting results (bottom right; z_ph = 15.0). Two color–color diagrams are also shown (bottom left and middle) to demonstrate the location of these F150W dropouts in the NIRCam color space. In the m₁₅₀ − m₂₀₀ versus m₂₀₀ − m₂₇₇ projection, which is the main diagnostic diagram for F150W dropouts, all the dropouts (filled red symbols) are far away (>0.5 mag) from the contamination region occupied by brown dwarfs (open green boxes). Four of them (fill red symbols with a blue outline) seem to be close (within 2σ of color errors) to the mid-z old galaxy contamination region (blue curve). However, only one of them is really close to this contamination region in the multidimension color space. This is demonstrated in the m₂₀₀ − m₂₇₇ versus m₂₇₇ − m₃₅₆ projection of the color space, where the other three are seen far away from the contamination. This suggests that the contamination rate is rather low (1 out of 60).

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The SED fitting results also support the high-z interpretation of the F150W dropouts; 83% of our objects have the first PDF peak at z > 10, and half of the remaining 17% still have the second PDF peak at z > 10. Taking these peak z_ph as the solutions, the high-z constituents among the F150W dropouts have z_ph = 10.2–16.0, with the median of z_ph = 11.6. The sample has median m₂₀₀ = 28.2 mag, which corresponds to rest-frame UV absolute magnitude of M_UV = −19.6 mag.

Among the F150W dropouts, one object in the module B sample is of particular interest. ⁹ Due to its complexity, we did not include it in the SED analysis. Its image is shown in Figure 3. While its structure in the LW images is not clearly resolved, this object can be discerned as a system of four separate sources. Together with a close neighbor of similar color, the five objects line up a “chain” in the sky, which we dub as “C-1” through “C-5” from east to west. To obtain better photometry, we extracted these sources using the F200W image as the detection image, as it shows all five components more clearly owing to its better resolution. Despite still suffering from severe blending, this set of photometry suggests that three components, C-2, 3, and 5, are all consistent with being F150W dropouts. C-4 actually qualifies as a F200W dropout. C-1, which is barely visible in F090W, also has a rather red color of m₁₅₀ − m₂₀₀ = 0.67 ± 0.08 suggesting its being at z ≈ 10. Combining C-2 through C-5 into a single object, it has m₃₅₆ = 23.1 mag (m₂₀₀ = 24.8 mag), which makes it the brightest system among the high-z candidates in this field. It deserves spectroscopic study in the near future to determine its redshift and to understand the relation between the individual components.

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4.4. F200W Dropouts

For F200W dropouts, we consider the 2σ sensitivity limits in F200W, which are 29.73 and 29.69 mag in modules A and B, respectively. Therefore, the brightness threshold for a valid F200W dropout is m₂₇₇ ≤ 28.93 and 28.89 mag in these two modules, respectively. There are 8 (7) validated F200W dropouts in module A (B). An example object is shown in Figure 4, together with its SED fitting results (z_ph = 20.6). Two diagnostic color–color diagrams are also shown. All these objects are far away from the brown dwarf contamination region. By coincidence, there are also four objects close to the mid-z old galaxy contamination region in the main m₂₀₀ − m₂₇₇ versus m₂₇₇ − m₃₅₆ diagram. However, only one of them is really close to the contamination region, which can be seen in the m₂₇₇ − m₃₅₆ versus m₃₅₆ − m₄₄₄ diagram. Therefore, this suggests that the contamination rate in the F200W dropout sample is also low (1 out of 15).

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The SED fitting shows that only one F200W dropout has z_ph < 10, and the others have z_ph ranging from 14.2 to 20.6, with the median of z_ph = 16.0. The sample has median m₂₇₇ = 28.6 mag, which also corresponds to M_UV = −19.6 mag. There is one bright object from module A that has m₂₇₇ = 26.85 ± 0.03 mag, whose m₂₇₇ − m₃₅₆ color is redder than the reddest mid-z old galaxy but is consistent with being a dusty galaxy at z > 11. This is the only one from the module A sample that is brighter than 27.5 mag. Interestingly, no object in the module B sample is brighter than m₂₇₇ = 27.5 mag.

4.5. F277W Dropouts

For F277W dropouts, we consider the 2σ sensitivity limits in F277W, which are 30.72 and 30.69 mag in modules A and B, respectively. Therefore, the brightness threshold for a valid F277W dropout is m₃₅₆ ≤ 29.86 and 29.68 mag in these two modules, respectively. There are 10 validated objects in the module A sample but only two in the module B sample. This can be explained by the difference of ∼0.2 mag in the brightness thresholds of the two modules. Six out of the 10 module A objects are fainter than m₃₅₆ = 29.4 mag, and therefore it is conceivable that severe incompleteness at close to the selection limit in module B significantly reduces the number of detections.

As these dropouts have significant detections in only F356W and F444W, we did not attempt SED fitting. Figure 5 shows the image stamps of one object as an example, together with two color–color diagrams. In the main diagnostic diagram of m₂₇₇ − m₃₅₆ versus m₃₅₆ − m₄₄₄, half of these dropouts are far away from the contamination regions and the other half seem to have similar colors as brown dwarfs. However, these halves are in fact far away from the brown dwarf contamination region in the color space. This can be seen in the m₂₀₀ − m₄₄₄ versus m₂₀₀ − m₃₅₆ projection. If their observed m₂₇₇ − m₃₅₆ color decrements are indeed due to the Lyman break, they are at z ≈ 24.7. This suggests that the search for “first objects” probably should aim at z > 20. Lacking additional information, however, we refrain from further speculating on their nature.

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For the dropouts selected in module B, which is on the cluster field, it is necessary to consider the magnification by the cluster. Shortly before the ERO release, a lens model for this cluster was published (Golubchik et al. 2022). This is based on the Light-Traces-Mass approach (LTM; Zitrin et al. 2009) and uses the RELICS images and redshifts measured by the Multi Unit Spectroscopic Explorer at the Very Large Telescope. The ERO NIRCam data have revealed new multiply imaged systems, which allow a suite of updated lensing models being built using parametric modeling codes (Caminha et al. 2022; Pascale et al. 2022; Mahler et al. 2022). In this work, we used the LTM model of Golubchik et al. (2022) and the parametric model present in Pascale et al. (2022). The magnification factor (μ) at a given source location is the average of the results from these two models calculated based on z_ph as described in Section 4.2.

It is interesting to compare the dropouts selected in the cluster field and the flanking field to see whether and how gravitational lensing plays a role. Overall the cluster field does not produce statistically larger samples; in fact it has slightly fewer dropouts, which is caused by its slightly shallower depths due to the presence of the ICL. Nor does it produce statistically brighter samples. However, it does result in the brightest candidates: two of its F150W dropouts have m₂₀₀ < 26.5 mag, one of which is the “chain of five” system. This system has μ = 2.3, while the other has μ = 1.6.

The large number of dropouts presented in this work demands further investigations. For simplicity, we concentrate on the F150W and F200W dropouts in the rest of the discussion. As explained in Section 4, these objects cannot be fake sources because they are all secure detections in more than two bands (some are detected in five bands). In the multidimension color space, the vast majority of these sources (with the exception of one object in each sample) are far away enough from the contamination regions due to mid-z old galaxies and brown dwarfs, and therefore most of them cannot be attributed to contaminations. Recently, Zavala et al. (2022) presented a case where a z < 6 dusty starburst mimics the color of an F200W dropout. Their source is detected in millimeter continuum by NOEMA. In contrast, the deep ALMA 1.3 mm mapping in our field, which covers ∼50% of module B, does not reveal any continuum sources at our dropout positions (see Cheng et al. 2022).

On the other hand, the color decrements of our dropouts are consistent with the Lyman break being shifted to z ≳ 11. If they are indeed at such high redshifts, their large surface densities pose a problem for many predictions. Over the past decade, it has become a dominant view that there is a paucity of galaxies at z > 10. Almost all predictions based on theoretical models or extrapolations from the results at lower redshifts expect a rather low surface density of galaxies at z > 10 awaiting JWST (see, e.g., Behroozi et al. 2020; Vogelsberger et al. 2020). The only exception is probably the luminosity function proposed by Yan et al. (2010), which would predict ∼94 galaxies at 11.3 ≤ z ≤ 15.4 to be discovered as F150W dropouts over the 11.52 arcmin² SMACS 0723-73 NIRCam field to the selection limit of m₂₀₀ ≈ 28.7 mag as done in this work (but assuming 100% completeness).

Assuming that the F150W and F200W dropouts are indeed at high-z, Figure A1 (see the Appendix) summarizes their properties based on the SED analysis. The top panel shows the z_ph distributions of the F150W dropout sample (left) and F200W dropout sample (right). Discarding the interlopers at z_ph < 11, the median is z_ph = 11.6 and 15.8 for the F150W and F200W dropouts, respectively, which is largely consistent with the expectation. The middle and the bottom panels show the distributions of three derived quantities for the F150W and F200W dropout samples, respectively. From left to right, these are age (T), stellar mass (M), and SFR. The objects in the cluster field have been demagnified to show the intrinsic M and SFR. The median ages for both samples are ∼34 Myr, indicating that the formation processes of these galaxies had just begun. The median stellar mass is consistent with this picture, which is 14× and 8.2 × 10⁷ M_⊙ for the F150W and F200W dropouts, respectively. They have moderate median SFRs of 19–52 M_⊙ yr⁻¹, which means that they could have assembled all their existing stars at such rates over their lifetimes so far.

We note that the surface densities of the F150W and F200W dropouts differ by 4×, increasing from 2.6 arcmin⁻² for the F200W dropouts to 10.6 arcmin⁻² for the F150W dropouts. This cannot be due to any selection bias, as the selection of the F200W dropouts in fact has gone ∼0.2 mag deeper (see Section 4.4). If they are at the suggested high redshifts, both samples probe populations of similar luminosity (M_UV ∼ −19.6 mag). The SED analysis results shown in Figure A1 also support that these two samples contain similar objects. Therefore, assuming that most of these dropouts are genuine z ≳ 11 galaxies, this would suggest a rapid increase of number density over ∼ 140 Myr from z ≈ 17.3 to z ≈ 12.7.

We emphasize again that our dropouts are only candidates at z ≳ 11. Even for those that have good SED fits producing z_ph > 11, it is still possible that they could be due to some new types of contaminators that we are not familiar with. It is critical to obtain JWST spectroscopy on at least a subset of such candidates so that our future exploration of the high-z universe can be put onto a solid footing.

The authors are grateful to the JWST ERO teams and many behind them for all their hard work that led to the prompt release of the ERO data used in this study. We also thank Adi Zitrin for supplying the lensing magnification calculation. We thank the anonymous referee for the constructive comments and criticisms, which improved the quality of this Letter. H.Y. acknowledges the partial support from the University of Missouri Research Council grant URC-21-005. Z.M. is supported in-part by the National Science Foundation, grant No. 1636621. C.C. is supported by the National Natural Science Foundation of China, No. 11803044, 12173045. This project is based on observations made with the NASA/ESA/CSA James Webb Space Telescope and obtained from the Mikulski Archive for Space Telescopes, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA).

Facility: JWST (NIRCam). -

The full list of dropouts are presented in Table 1. As stated in Section 4.5, the F277W dropouts are only significantly detected in two to three bands and therefore should be used with caution. Note that the Equatorial coordinates are tied to the DR2 of GAIA, which is different from the astrometric system that the existing RELICS data were calibrated onto. We also note that the “chain of five” system is included in the F150W dropout sample; however only the C-4 component is listed in the catalog as the representative.

The Le Phare SED fitting results of our objects are detailed in Appendix C, and the key statistics are summarized in Figure A1. The statistics of T, M, and SFR are done on the subsets that retain only the objects that either the primary or the secondary solutions have z_ph ≥ 11 (rounded off to integers). If the primary solution has z_ph ≥ 11, these parameters are calculated at this solution; if only the secondary solution has z_ph ≥ 11, these parameters are calculated at the secondary solution. In total, the subset contains 39 (14) F150W (F200W) dropouts.

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The details of the EAZY SED fitting for z_ph are presented in Appendix D. Based on the z_ph estimates from these two different methods, we further group the F150W and F200W dropouts into four categories (indicated by “G_ph” in Table 1) based on whether their z_ph are at high-z (>11.0 for the F150W dropouts and >15.0 for the F200W dropouts, respectively): (i) both methods have the primary solution (corresponding to the primary peak of P(z)) at high-z; (ii) either method has the primary solution at high-z; (iii) neither method has the primary solution at high-z but at least one has the secondary solution (corresponding to the secondary peak of P(z)) at high-z; (iv) neither method has the primary nor the secondary solution at high-z. While such a grouping is not necessarily a ranking of the quality of these dropouts, it could be useful for follow-up studies in the future.

Three days after our Letter was submitted to arXiv, Atek et al. (2022) and Donnan et al. (2022) also submitted their papers to arXiv and they discussed high-z objects in SMACS 0723-73 as well. Among the nine z ≈ 11–16 candidates in Atek et al. (2022), their SMACS_z11b, SMACS_z12b, and SMACS_z11e correspond to our F150DA-63, F150DA-77, and F150DA-81, respectively. Their SMACS_z16a and SMACS_z16b were selected by us as initial F200W dropouts but were rejected in the visual inspection step because they are visible in the veto band (F150W). Their SMACS_z11a, SMACS_z11c, SMACS_z11d, and SMACS_z12a do not meet our F150W dropout selection criteria either because of the less prominent color decrement or due to not having S/N ≥ 5 in F200W. Donnan et al. (2022) also included nine z ≈ 11–16 candidates, but only four of them are in SMACS 0723-73. Their ID 6486 does not meet our F150W dropout color criterion. Their 21901, 35470, 40079 were selected by us as initial F150W dropouts in module B but were later rejected because they all have m₂₀₀ > 28.70 and are fainter than the depth threshold that we set for F150W dropout selection in module B.

Upon finishing this Letter, we came to be aware of a possible NIRCam flux calibration adjustment, which would require rescaling of the current pipeline reduced products. In the six bands relevant here, the scaling factors are 1.143, 1.028, 1.091, 0.870, 0.860, 0.815, from the bluest to the reddest, respectively. These correspond to adding the following numbers to the magnitudes derived using the original zero-point: −0.145, −0.030, −0.095, 0.151, 0.164, and 0.222, from the bluest to the reddest, respectively. As none of these scaling factors have been vetted and any of them could be evolving in the next few months, we chose not to make these changes to our photometry.

Nonetheless, we still investigate how such changes could impact our dropout samples. As it turns out, all our F150W dropouts would still survive, and the new z_ph statistics would not change. Five of the F200W dropouts would have m₂₀₀ − m₂₇₇ < 0.8 mag (ranging from 0.65 to 0.78 mag); however, the new z_ph estimates would still put them at high-z. This is understandable because this is equivalent to lowering the color decrement threshold from 0.8 to 0.65 mag, or in other words, the Lyman-break signature moves 45% instead of 50% out of the dropout band. Therefore, none of our conclusions would be changed.

Figures B1, B2, and B3 present the image cutouts of all our F150W, F200W, and F277W dropouts, respectively. The “chain of five” is already presented in Figure 3 and is not included here.

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View extended figure (6 panels)

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View extended figure (2 panels)

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Figure C1 and C2 present the SED fitting results for the F150W and F200W dropouts, using Le Phare and BC03 models as described in Section 4.2. These are similar to those shown in Figures 2 and 4. The “chain of five” are not included, as their photometry is severely affected by blending. The quoted χ² are the total values (i.e., not the “reduced χ²”).

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We also performed SED fitting using EAZY-py ¹⁰ , the latest implementation of EAZY, which incorporates templates with emission lines. Figures D1 and D2 show the results. We made a modification to the code so that flux density upper limits can be used. By design, EAZY is for z_ph derivation but is not for stellar population analysis. The black boxes with error bars are the data points, and the black curves are the best-fit models. The red circles are the synthesized flux densities based on the best-fit models. P(z) is shown next to the SED plot in each panel. The quoted χ² are the total values.

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