---
title: 'GLIMPSE JWST/NIRCam Survey: Cosmic Dawn'
url: https://www.emergentmind.com/topics/glimpse-jwst-nircam-survey
type: topic
---

# GLIMPSE JWST/NIRCam Survey: Cosmic Dawn

Searching arXiv for the GLIMPSE JWST/NIRCam Survey papers and related context.
Search query: GLIMPSE JWST NIRCam Survey Abell S1063 ultraviolet luminosity function cosmic dawn
The GLIMPSE JWST/NIRCam Survey is a lensing-assisted ultra-deep imaging program centered on the galaxy cluster Abell S1063 that uses JWST/NIRCam to probe early galaxy formation, the ultraviolet luminosity function (UVLF), and the sources of cosmic reionization across approximately \(6<z<16\). By combining long integrations with strong gravitational lensing, GLIMPSE was designed to reach intrinsic magnitudes as faint as \(M_{\mathrm UV}\simeq -12\), substantially below the regime accessible to comparable blank-field surveys, while also enabling resolved studies of compact star-forming structures and searches for rare highly magnified phenomena [2511.07542]. Early GLIMPSE analyses reported two galaxy candidates at \(15.7<z<16.4\) behind Abell S1063 and used these detections to argue that the luminosity distribution at the highest redshifts may be shifting toward fainter galaxies, with implications for the UVLF and for the link between star formation and halo growth during cosmic dawn [2411.13640]. Subsequent GLIMPSE work extended the survey’s UVLF constraints across \(z\sim 9\)–15 using 105 galaxy candidates and found a nearly constant faint-end slope together with a shallow decline in the cosmic star formation rate density (SFRD), further sharpening the tension with many pre-JWST theoretical expectations [2509.24881].

## 1. Survey definition and scientific scope

GLIMPSE was designed to push JWST’s NIRCam to its limits by combining ultra-deep imaging with strong gravitational lensing. Its stated objectives are to probe the extreme faint end of the rest-frame ultraviolet luminosity function over \(6<z<16\), quantify the abundance and ionizing output of ultra-faint galaxies relevant to cosmic reionization, and resolve star-forming substructure down to \(\sim 10\) pc scales in early galaxies while also searching for highly magnified transients [2511.07542].

The survey targets Abell S1063 (AS1063), a Frontier-Fields cluster at \(z=0.348\). The field choice was motivated by a very regular mass morphology, extensive VLT/MUSE spectroscopy with more than 70 multiple images with spectroscopic redshifts within the NIRCam module B footprint, and a large high-magnification area that can be covered by a single NIRCam module [2511.07542]. A related early-science analysis described AS1063 as one of the highest-magnification Hubble Frontier Fields clusters, emphasizing that the combination of ultra-deep NIRCam imaging and cluster lensing makes it possible to probe intrinsically fainter galaxy populations than had previously been accessible [2411.13640].

This framing is central to the survey’s scientific significance. Most pre-JWST galaxy-formation models had been calibrated primarily against relatively UV-bright systems, typically \(M_{\mathrm UV}<-17\), whereas theoretical uncertainty grows strongly at fainter magnitudes. GLIMPSE was explicitly constructed to measure this poorly constrained regime [2511.07542]. A plausible implication is that the survey’s novelty lies less in extending redshift reach alone than in jointly accessing high redshift and low intrinsic luminosity.

## 2. Observational configuration and depth

GLIMPSE obtained ultra-deep JWST/NIRCam imaging in seven broadband filters and two medium-band filters. The broad bands are F090W, F115W, F150W, F200W, F277W, F356W, and F444W; the medium bands are F410M and F480M [2411.13640; 2511.07542; 2509.24881]. One overview paper describes the program as obtaining 120 h of NIRCam imaging with exposure times ranging from 20 to 40 hours per filter, yielding a \(5\sigma\) limiting magnitude of 30.9 AB in a \(0.2\) arcsec diameter aperture [2511.07542]. An earlier analysis of the \(z\sim 16\) candidates instead reports \(\simeq 155\) h of science integration, including 19 h in F200W and 23 h in F277W, with \(5\sigma\) aperture-corrected limiting depths of 30.6 AB mag uniformly in all wide bands for \(D=0.2''\) apertures [2411.13640]. Another GLIMPSE UVLF study summarizes the point-source depths as \(\simeq 30.8\) mag (AB) in each filter [2509.24881]. These differing numerical summaries reflect distinct presentations within the GLIMPSE literature rather than a single standardized statement.

The observational strategy employed the MEDIUM8 read pattern and a dither scheme intended both to fill detector gaps and improve sampling. One description gives a 6-point primary dither to fill SW gaps plus a 4-point subpixel dither for PSF sampling [2411.13640]. The later overview describes a 6-point intramodule dither plus a 4-point subpixel dither, placing MODULE B on the cluster core and MODULE A on a modestly lensed blank field [2511.07542].

A concise summary of the filter configuration as reported in the overview paper is given below.

| Filter | Exposure (h) | \(5\sigma\) depth (AB, \(0.2''\)) |
|---|---:|---:|
| F090W | 39.1 | 30.85 |
| F115W | 39.1 | 30.87 |
| F150W | 22.3 | 30.77 |
| F200W | 19.5 | 30.82 |
| F277W | 22.3 | 30.82 |
| F356W | 19.5 | 30.77 |
| F410M | 16.7 | 30.07 |
| F444W | 39.1 | 30.68 |
| F480M | 22.3 | 29.24 |

In that same presentation, the limiting magnitude is computed as
\[
m_{5\sigma} = -2.5\,\log_{10}(5\times \mathrm{noise}) + m_{\mathrm zp},
\]
where the noise is the aperture-to-aperture background RMS and \(m_{\mathrm zp}\) is the filter zero point [2511.07542].

The role of lensing is quantitatively important. For the \(z\sim 16\) search, typical magnifications of \(\mu\approx 1.25\)–1.96 were reported to boost sensitivity by \(\sim 0.3\)–0.7 mag, enabling detection down to intrinsic \(M_{\mathrm UV}\approx -17.5\) at \(z\sim 17\) in a single NIRCam pointing [2411.13640]. In the broader survey overview, GLIMPSE is described as probing intrinsic depths beyond 33 AB magnitudes and covering an effective source-plane area of approximately \(4.4\) arcmin\(^2\) at \(z\sim 6\), with the source-plane area remaining above \(3\) arcmin\(^2\) even at \(z\approx 12\) for \(\mu>1\) [2511.07542].

## 3. Lensing model and survey geometry

A core structural component of GLIMPSE is its parametric strong-lensing reconstruction for Abell S1063. The model is described as a new parametric strong-lensing model, termed “Zitrin-analytic,” comprising two cluster-scale PIEMD dark-matter halos and 303 dual-PIEMD cluster galaxies, constrained by 75 multiple images of 28 background sources, 24 of them with spectroscopic redshifts [2511.07542]. The early \(z\sim 16\) study gives an effectively identical description in slightly different wording: two PIEMD halos corresponding to the cluster core and a northeast group, plus 303 galaxy-scale DPIEs, with \(\Delta_{\mathrm rms}\approx 0.54''\) from 75 multiple images in 28 systems, 24 with spectroscopic redshifts [2411.13640]. The final image-plane reproduction error is reported as \(\Delta \mathrm{RMS}\approx 0.54''\) [2511.07542].

The magnification map for \(z=6\) spans from \(\mu\approx 2\) in low-magnification regions to \(\mu>100\) near the critical curve, with flow lines indicating the direction of gravitational shear [2511.07542]. In a separate GLIMPSE summary focused on \(z\sim 9\)–15 galaxies, the field-wide magnification is described as ranging from \(\mu\approx 1.2\) up to \(\mu\sim 30\), with typical \(\Delta\mu\sim 15\%\) systematic uncertainty [2509.24881]. These statements are not contradictory: they describe different regions or uses of the magnification distribution.

The lens model enters directly into de-lensing and volume estimation. For the two \(z\sim 16\) candidates, magnification was computed at each candidate’s position and photometric redshift, yielding \(\mu=1.25\)–1.96, and intrinsic luminosities were inferred from the observed \(m_{277}\) and \(\mu\) [2411.13640]. The source-plane volume over \(16<z<20\) was estimated as \(V_{\rm src}\approx 17\,055\pm 71\) Mpc\(^3\), while completeness simulations through the lens map reduced this to an effective selection volume of \(V_{\rm eff}=13\,714\pm 1\,784\) Mpc\(^3\) [2411.13640].

This lensing strategy defines GLIMPSE’s position relative to blank-field JWST programs. Whereas blank fields constrain the brighter end with cleaner survey geometry, GLIMPSE explicitly sacrifices simplicity in favor of intrinsic depth. A plausible implication is that its strongest leverage lies in the faint-end UVLF and in magnified substructure studies rather than in bright-end number counts.

## 4. Source detection, photometry, and redshift selection

GLIMPSE high-redshift candidate selection combines dropout criteria with photometric-redshift fitting. In the survey overview, candidates were selected through Lyman-break criteria together with photometric redshift estimates from EAZY, using dual detection in a short-wavelength stack (F090W–F200W) and a long-wavelength stack (F277W+F356W+F444W) to maximize sensitivity to both blue and red sources [2511.07542]. Aperture photometry was measured in circular apertures from \(0.1''\) to \(1.2''\), aperture-corrected to total using the F480M PSF curve of growth, with empirical noise estimates derived from 2000 empty apertures around each source. Stringent flags were used to remove detections affected by edges, diffraction spikes, or proximity to the brightest cluster galaxy [2511.07542].

The final “use_phot=1” catalog contains 64,828 reliable detections, from which approximately 540 galaxy candidates at \(z>6\) were isolated. The redshift distribution reported in the overview is 411 sources at \(6<z<9\), 114 at \(9<z<11\), 11 at \(11<z<15\), and two remarkable candidates at \(z\approx 16\) with \(M_{\mathrm UV}\approx -17\) [2511.07542].

For the earliest-redshift subsample, the selection was more specific. The \(F200W\)-dropout criteria were
\[
m_{200}-m_{277}>1.0,
\]
\[
m_{200}-m_{277}>1.2 + 2.0(m_{277}-m_{356}),
\]
\[
m_{277}-m_{356}<0.5,
\]
with detection requirements of \(S/N>3\) in F277W, F356W, and F444W, \(S/N>4\) in at least one of these bands, and non-detection at \(S/N<2\) in the blue bands F090W, F115W, and F150W [2411.13640]. These cuts initially yielded \(\sim 40\) color-selected candidates. Photometric redshifts were then estimated with EAZY using the blue_sfhz_13 template set over \(z=0.01\)–30, requiring \(S/N>3\) in at least three bands, \(p(z)\) FWHM \(<2.5\), and no strong low-\(z\) peak, with a BEAGLE cross-check including nebular emission [2411.13640]. Of 15 initial F200W dropouts with robust \(z\approx 15.5\)–19.2 solutions, seven were removed as low-\(z\) interlopers through a \(\Delta\)BIC \(>5\) criterion using additional dusty templates, leaving a final sample of five sources with at least one \(\geq 5\sigma\) detection [2411.13640].

For the \(z\sim 9\)–15 UVLF analysis, the dropout selections were formulated differently because the target redshift range was lower. The \(z\sim 9\)–11 F115W-dropout criterion required
\[
m_{115}-m_{150}>0.8
\]
and
\[
(m_{150}-m_{200}<0.8 \ \mathrm{OR}\ m_{200}-m_{277}<0.8),
\]
while the \(z\sim 11\)–15 F150W-dropout criterion required
\[
m_{150}-m_{200}>0.8
\]
and
\[
(m_{200}-m_{277}<0.8 \ \mathrm{OR}\ m_{277}-m_{356}<0.8).
\]
These selections further required \(\geq 3\sigma\) detections in all bands redward of the break, \(\geq 5\sigma\) in at least one redward band, no detection above \(2\sigma\) in any filter blueward of the break, visual inspection for artifacts, and morphological cuts to exclude unresolved point-like brown dwarfs [2509.24881].

Completeness was quantified with extensive mock-source insertion. Approximately 200,000 mock galaxies were inserted in the source plane over \(z=8.5\)–15 and \(M_{\mathrm UV}=-20\) to \(-10\), with sizes drawn from the Shibuya+15 and Yang+22 size-luminosity relations. Recovery peaks at approximately 80% for \(M_{\mathrm UV}\gtrsim -18\) and falls to \(\lesssim 10\%\) by \(M_{\mathrm UV}\sim -13\) [2509.24881].

## 5. Galaxy properties and the \(z\approx 16\) candidates

The first GLIMPSE paper reported the discovery of two robust galaxy candidates at \(15.7<z<16.4\), identified through the combination of Lyman-break selection and photometric-redshift estimates [2411.13640]. Their absolute magnitudes are given as \(M_{\mathrm UV}=-17.0\) to \(-17.2\) mag, placing them in a faint intrinsic regime relative to many earlier high-\(z\) JWST detections [2411.13640].

In that analysis, the rest-frame UV absolute magnitude at approximately 1500 Å was computed from observed F277W photometry as
\[
M_{\mathrm UV}=m_{\mathrm obs}-5\log_{10}(D_L/10\,\mathrm{pc})+2.5\log_{10}(1+z).
\]
The UV continuum slope \(\beta\) was fit under the assumption \(f_\lambda\propto \lambda^\beta\) over 1260–2500 Å using F277W–F356W colors [2411.13640]. The measured \(\beta\) values span approximately \(-3.0\) to \(-2.3\), with median \(-2.81\pm 0.16\), and the abstract describes the sources as having blue UV slopes around \(\beta\simeq -2.87\), consistent with young, dust-free stellar populations [2411.13640].

The same work gives the UV luminosity as
\[
L_{\mathrm UV}=10^{0.4(51.63-M_{\mathrm UV})}\ \mathrm{erg\ s^{-1}\ Hz^{-1}}
\]
and adopts
\[
\mathrm{SFR}\ (M_\odot\,\mathrm{yr}^{-1})\simeq k_{\mathrm UV}\times L_{\mathrm UV}
\]
following Kennicutt (2012), with negligible dust correction because \(\beta<-2.3\). The resulting UV-based star formation rates are \(\mathrm{SFR}_{\mathrm UV}\simeq 0.7\)–1.0 \(M_\odot\,\mathrm{yr}^{-1}\) [2411.13640].

The paper further argues that these sources are plausible progenitors of the unusually UV-bright galaxies observed by JWST at \(z=10\)–14. Specifically, a constant SFR of approximately \(1\,M_\odot\,\mathrm{yr}^{-1}\) beginning near \(z\approx 17\) yields growth to \(M_{\mathrm UV}\sim -20\) by \(z\approx 11\)–14, while maximal \(\Lambda\)CDM-limited accretion following Dekel 13 gives an exponential star-formation history that also connects \(z\sim 17\) faint galaxies to UV-bright \(z<14\) systems [2411.13640]. This suggests continuity between faint cosmic-dawn galaxies and later bright JWST sources without invoking exotic physics, though the paper itself frames these as results of toy or tested star-formation histories rather than direct empirical demonstration.

## 6. Ultraviolet luminosity function and cosmic star formation density

A central GLIMPSE product is the measurement of the UV luminosity function at very faint intrinsic luminosities. In the \(z\sim 16\) candidate study, the number-density estimator is
\[
\phi(M_{\mathrm UV})=\frac{N_{\mathrm gal}/\Delta M}{V_{\mathrm eff}(M)},
\]
with \(\Delta M=1\) mag around \(M_{\mathrm UV}=-18.0\) [2411.13640]. For \(16<z<20\) at \(M_{\mathrm UV}=-18\pm 0.5\), the measured number density is
\[
\log_{10}\phi=-3.43^{+0.28}_{-0.64}\ \mathrm{Mpc^{-3}\ mag^{-1}},
\]
while the abstract reports the corresponding density at \(M_{\mathrm UV}=-17\) as
\[
\log_{10}(\phi/[\mathrm{Mpc}^{-3}\ \mathrm{mag}^{-1}])=-3.47^{+0.13}_{-0.10}.
\]
The same study states that this result is in clear tension with pre-JWST theoretical predictions and extends the over-abundance of galaxies previously inferred at \(z\sim 10\) out to \(z\sim 17\) [2411.13640].

For the larger GLIMPSE sample at \(z\approx 6\)–12, the survey overview reports binned number densities corrected for completeness and delensed effective volume and fits a Schechter function,
\[
\Phi(M)=0.4\,\ln(10)\,\Phi^*\,10^{0.4(\alpha+1)(M^*-M)}\exp[-10^{0.4(M^*-M)}].
\]
At \(z\approx 6\)–9 the best-fit parameters are
\[
\Phi^*=(1.5\pm 0.4)\times 10^{-3}\ \mathrm{Mpc^{-3}\ mag^{-1}},\quad
M^*=-20.6\pm 0.3,\quad
\alpha=-2.02\pm 0.12,
\]
and at \(z\approx 10\)–12
\[
\Phi^*=(0.6\pm 0.3)\times 10^{-3},\quad
M^*=-20.1\pm 0.5,\quad
\alpha=-2.1\pm 0.3.
\]
The steep \(\alpha<-2\) at \(z>8\) is reported to imply that galaxies fainter than \(M_{\mathrm UV}=-16\) can contribute 50–60% of the total UV luminosity density, whereas a shallower \(\alpha\approx -1.8\) would imply \(\lesssim 40\%\) [2511.07542].

The dedicated \(z\sim 9\)–15 GLIMPSE UVLF analysis instead combined GLIMPSE counts with literature bright-end data and fitted a double-power law,
\[
\phi(M)=\frac{\phi^*}{10^{0.4(M-M^*)(\alpha+1)}+10^{0.4(M-M^*)(\beta+1)}}.
\]
Its best-fit parameters are reported in four redshift bins:

| Redshift bin | \(\log \phi^*\) | \(M^*\) | \(\alpha\) | \(\beta\) |
|---|---:|---:|---:|---:|
| \(z\simeq 9\) | \(-4.01\pm 0.04\) | \(-20.30\pm 0.20\) | \(-2.01\pm 0.20\) | \(-4.30\pm 0.21\) |
| \(z\simeq 10\) | \(-4.19\pm 0.06\) | \(-20.20\pm 0.19\) | \(-2.07\pm 0.19\) | \(-4.31\pm 0.19\) |
| \(z\simeq 11\) | \(-4.53\pm 0.01\) | \(-20.80\pm 0.19\) | \(-2.10\pm 0.19\) | \(-4.35\pm 0.19\) |
| \(z\simeq 13\) | \(-4.70\pm 0.20\) | \(-20.60\pm 0.18\) | \(-2.10\pm 0.19\) | \(-4.00\pm 0.20\) |

The reported evolution of the faint-end slope from \(\alpha=-2.01\pm 0.20\) at \(z=9\) to \(\alpha=-2.10\pm 0.19\) at \(z=13\) is described as minimal, in contrast to the stronger redshift evolution inferred at lower redshift [2509.24881].

The same paper converts UV luminosity to SFR with the standard calibration for a Salpeter IMF,
\[
\kappa_{\rm UV}=1.15\times 10^{-28}\ \bigl[M_\odot\,\mathrm{yr}^{-1}/(\mathrm{erg\ s^{-1}\ Hz^{-1}})\bigr],
\]
and no dust correction, citing UV slopes \(\beta\sim -2.3\) that imply low attenuation [2509.24881]. The SFRD is written as
\[
\mathrm{SFRD}(z)=\int_{M_{\rm lim}}^{\infty}\phi(M)\,\kappa_{\rm UV}\,10^{-0.4(M+48.6)}\,dM.
\]
Integrated to \(M_{\mathrm UV}=-16\), the derived values are \(\log \rho_{\mathrm SFR}=-2.57\pm 0.44\) at \(z\simeq 9\), \(-2.74\pm 0.44\) at \(z\simeq 10\), \(-2.75\pm 0.44\) at \(z\simeq 11\), and \(-3.02\pm 0.43\) at \(z\simeq 13\), with best-fit redshift evolution
\[
\rho_{\mathrm SFR}\propto (1+z)^{-2.94^{+0.06}_{-0.10}}.
\]
When the integration limit is extended to \(M_{\mathrm UV}=-13\), galaxies with \(-16<M_{\mathrm UV}<-13\) provide more than 50% of the total cosmic SFR density out to \(z\approx 13\) [2509.24881].

## 7. Theoretical tension, ancillary science, and public release

GLIMPSE papers emphasize a persistent mismatch between observed galaxy abundances and many pre-JWST models. For the \(z\sim 16\) detections, pre-JWST semi-analytic models such as Mason 15 and Dayal 14 and hydrodynamic models such as Behroozi 19 and Wilkins 23 underpredict the observed abundance by \(3\)–\(5\sigma\), whereas post-JWST-tuned models including Muñoz 23, the FFB scenario of Li 24, and FIREbox Feldmann 24 align within \(1\)–\(2\sigma\), especially near the upper envelope [2411.13640]. That work further states that the bright end of the UVLF at \(z\sim 16\) appears to decline steeply, with no detections in blank fields such as CEERS, JADES, PRIMER, and NGDEEP, while lensing reveals abundant faint galaxies near \(M_{\mathrm UV}\approx -18\) [2411.13640]. A toy model in which a constant 30% star-formation efficiency of halo accretion persists over 100 Myr is said to reproduce a steep UVLF that tracks the halo mass function [2411.13640].

The \(z\sim 9\)–15 UVLF paper broadens the theoretical comparison. It states that many pre-JWST models, including Mason+15 and Tacchella+18, predict a steep decline in \(\phi^*\) and a steepening to \(\alpha\lesssim -3\) by \(z>12\), thereby underestimating both bright and faint galaxies. Dust-free outflow models such as Ferrara+23 improve the bright end at \(z\simeq 11\)–12 but still underpredict the faint population at \(z>12\). Stochastic bursty star-formation histories in simulations such as Sun+23 and SPHINX partially alleviate the bright-end excess but do not reproduce the measured faint-end \(\phi\) or the mild evolution of \(\alpha\) and SFRD. Feedback-free starbursts as in Dekel+23 require an unphysically rising maximum star-formation efficiency from \(\epsilon_{\max}\sim 0.2\) at \(z\approx 9\) to \(\epsilon_{\max}\sim 1\) at \(z>12\) [2509.24881]. The paper concludes that none of the currently discussed scenarios—increased SFE, bursty star formation, zero dust, or an evolving IMF—fully captures the observed slowly declining UVLF normalization and nearly constant \(\alpha\) [2509.24881].

Beyond the luminosity function, GLIMPSE also supports ancillary early-science programs. By exploiting magnifications up to \(\sim 140\), one overview reports \(\sim 451\) individual stellar clumps in 61 lensed galaxies at \(0.5<z<8.2\), of which approximately 145 have de-lensed half-light radii \(\lesssim 20\) pc and inferred stellar masses \(M_\star\lesssim 10^5\,M_\odot\), consistent with young globular-cluster progenitors; some reach \(M_{\mathrm UV}\approx -8.5\) [2511.07542]. The same paper notes a handful of faint high-\(z\) active galactic nucleus candidates at \(z=6\)–8 with power-law rest-frame UV slopes, compact morphologies, and mild F480M excesses, suggesting black-hole masses \(M_{\mathrm BH}\sim 10^6\)–\(10^7\,M_\odot\), as well as two transient events at \(z\approx 1.8\) and 4.3 consistent with highly magnified asymptotic-giant-branch stars and a Pop III candidate at \(z\approx 6\) behind A2744 [2511.07542].

GLIMPSE DR1, released in December 2024, includes reduced JWST and HST mosaics, photometric catalogs, and strong-lensing model files. Specifically, it provides NIRCam mosaics at 20 mas/pix in the short wavelength channel and 40 mas/pix in the long wavelength channel across all nine filters, PSF-matched and bCG/ICL-subtracted HST ACS+WFC3 mosaics, photometric catalogs containing fluxes in \(0.1''\)–\(1.2''\) apertures together with aperture corrections, photometric redshifts, and use_phot flags, and strong-lensing model products including Zitrin-analytic parameters, MCMC chain samples, and magnification maps in FITS and Lenstool formats [2511.07542]. The data are hosted at MAST under DOI:10.17909/GLIMPSE_DR1 and mirrored at the Dawn JWST Archive; the survey documentation advises use of the provided use_phot mask and per-pixel depth and magnification maps for rigorous effective-area and volume calculations [2511.07542].

Taken together, these results position GLIMPSE as a survey optimized for the intrinsically faint galaxy population at cosmic dawn. The combined evidence from its \(z\approx 16\) candidate detections, faint-end UVLF measurements, and SFRD estimates suggests that the earliest observable star-forming population may be dominated by numerous modest-SFR systems at luminosities substantially below the bright galaxies first highlighted by JWST [2411.13640; 2509.24881]. This suggests that future observational tests of galaxy formation and reionization at the highest redshifts will depend critically on surveys that can access the same faint intrinsic regime.

Source: https://www.emergentmind.com/topics/glimpse-jwst-nircam-survey