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JWST/MIRI reveals the true number density of massive galaxies in the early Universe
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abstract
Early JWST studies reporting an unexpected abundance of massive galaxies at $z \sim 5$--$8$ challenge galaxy formation models in the $\Lambda$CDM framework. Previous stellar mass ($M_\star$) estimates suffered from large uncertainties due to the lack of rest-frame near-infrared data. Using deep JWST/NIRCam and MIRI photometry from PRIMER, we systematically analyze massive galaxies at $z \sim 3$--$8$, leveraging rest-frame $\gtrsim 1\,\mu$m constraints. We find MIRI is critical for robust $M_\star$ measurements for massive galaxies at $z > 5$: excluding MIRI overestimates $M_\star$ by $\sim 0.4$ dex on average for $M_\star > 10^{10}\,M_\odot$ galaxies, with no significant effects at lower masses. This reduces number densities of $M_\star > 10^{10}\,M_\odot$ ($10^{10.3}\,M_\odot$) galaxies by $\sim 36\%$ ($55\%$). MIRI inclusion also reduces ``Little Red Dot'' (LRD) contamination in massive galaxy samples, lowering the LRD fraction from $\sim 32\%$ to $\sim 13\%$ at $M_\star > 10^{10.3}\,M_\odot$. Assuming pure stellar origins, LRDs exhibit $M_\star \sim 10^{9\text{--}10.5}\,M_\odot$ with MIRI constraints, rarely exceeding $10^{10.5}\,M_\odot$. Within standard $\Lambda$CDM, our results indicate a moderate increase in the baryon-to-star conversion efficiency ($\epsilon$) toward higher redshifts and masses at $z > 3$. For the most massive $z \sim 8$ galaxies, $\epsilon \sim 0.3$, compared to $\epsilon \lesssim 0.2$ for typical galaxies at $z < 3$. This result is consistent with models where high gas densities and short free-fall times suppress stellar feedback in massive high-$z$ halos.
Forward citations
Cited by 8 Pith papers
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The Cosmic Rush Hour: Rapid Formation of Bright, Massive, Disky, Star-Forming Galaxies as Signatures of Early-Universe Physics
Early dark energy in large hydrodynamic simulations reproduces JWST's excess of bright, massive, high-redshift galaxies while preserving low-redshift Lambda-CDM behavior.
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A prevalent population of normal-mass central black holes in high-redshift massive galaxies
A galaxy-based JWST search finds 13 broad-line AGNs in massive galaxies at z~3-5 with normal black hole-to-stellar mass ratios near the local value, indicating that overmassive black holes are not the only early pathway.
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MINERVA: A NIRCam Medium Band and MIRI Imaging Survey to Unlock the Hidden Gems of the Distant Universe
The MINERVA survey will expand JWST medium-band imaging area by about 7 times and is forecast to cut photometric-redshift scatter and outlier fractions by factors of 3.7 and 2.6.
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BEACON: JWST NIRCam Pure-parallel Imaging Survey. I. Survey Design and Initial Results
BEACON's first 19 pure-parallel fields yield 129 galaxy candidates at z>7, 11 at z>10, and zero at z>13, with number densities consistent with earlier JWST and HST surveys.
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Physical properties of galaxies and the UV Luminosity Function from $z\sim6$ to $z\sim14$ in COSMOS-Web
A 3,099-galaxy JWST sample at z~6-14 shows a bright-end UV luminosity function excess at z~9-12 relative to evolving Schechter-function predictions, with non-evolving blue UV slopes.
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The Stellar Populations and Rest-Frame Colors of Star-Forming Galaxies at $z \approx 8$: Exploring the Impact of Filter Choice and Star Formation History Assumption with JADES
For typical star-forming galaxies at z≈8, dense JWST/NIRCam coverage with eight or more filters can replace MIRI/F770W for measuring stellar populations and rest-frame colors in most cases.
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Need for PRIMA to understand the nature and ISM physical conditions of HST-dark galaxies
PRIMA imaging and spectroscopy could characterize HST-dark galaxies in about 50 and 100 hours respectively, closing the JWST-ALMA gap and probing their dust, gas, and AGN content.
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No evidence (yet) for increased star-formation efficiency at early times
A constant, halo-mass-dependent star-formation efficiency, combined with younger stellar populations and dust, can reproduce the observed galaxy UV luminosity function and stellar mass function at z=6-13, so no increa...
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