What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST

Faisst, Andreas L.; Chary, R.-R.; Brammer, Gabriel; Toft, Sune

doi:10.3847/2041-8213/aca1bf

Cited by 12 publications

(5 citation statements)

References 93 publications

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“…27 In addition, a correction for the effect of dust in the Milky Way is applied to the templates within EAZY-PY, pulling the Galactic dust map by Schlafly & Finkbeiner (2011) from DUSTMAPS (Green 2018). This effect is relevant for SMACS 0723 (E(B − V ) MW = 0.19; see also Faisst et al 2022) and to a lesser extent for the rest of the fields (E(B − V ) MW = 0.007-0.07). In terms of photometric redshifts, we obtain a good agreement with spectroscopic determinations from archival observations when available (G. Brammer et al 2023, in preparation).…”

Section: Modeling Of the Spectral Energy Distributionmentioning

confidence: 94%

An Atlas of Color-selected Quiescent Galaxies at z > 3 in Public JWST Fields

Valentino

Brammer

Gould

et al. 2023

ApJ

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We present the results of a systematic search for candidate quiescent galaxies in the distant universe in 11 JWST fields with publicly available observations collected during the first 3 months of operations and covering an effective sky area of ∼145 arcmin2. We homogeneously reduce the new JWST data and combine them with existing observations from the Hubble Space Telescope. We select a robust sample of ∼80 candidate quiescent and quenching galaxies at 3 < z < 5 using two methods: (1) based on their rest-frame UVJ colors, and (2) a novel quantitative approach based on Gaussian mixture modeling of the near-UV − U, U − V, and V − J rest-frame color space, which is more sensitive to recently quenched objects. We measure comoving number densities of massive (M ⋆ ≥ 1010.6 M ⊙) quiescent galaxies consistent with previous estimates relying on ground-based observations, after homogenizing the results in the literature with our mass and redshift intervals. However, we find significant field-to-field variations of the number densities up to a factor of 2–3, highlighting the effect of cosmic variance and suggesting the presence of overdensities of red quiescent galaxies at z > 3, as could be expected for highly clustered massive systems. Importantly, JWST enables the robust identification of quenching/quiescent galaxy candidates at lower masses and higher redshifts than before, challenging standard formation scenarios. All data products, including the literature compilation, are made publicly available.

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Section: Modeling Of the Spectral Energy Distributionmentioning

confidence: 94%

An Atlas of Color-selected Quiescent Galaxies at z > 3 in Public JWST Fields

Valentino

Brammer

Gould

et al. 2023

ApJ

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“…The superior sensitivity and spatial resolution of JWST allows us to detect these clusters in unprecedented detail. Preliminary results based on JWST data in SMACS0723 are presented in Lee et al (2022), Faisst et al (2022). It is interesting to compare our results with those from earlier works.…”

Section: Correlation Between Dm Icl and Gcdmentioning

confidence: 67%

“…In addition, the improved spatial resolution in the infrared bands allows for the detection of small clumps of old stellar populations in the cluster stripped from their hosts galaxies. The first image of JWST on this cluster reveals hundreds of unresolved clumps that have been interpreted as GCs (Lee et al 2022;Faisst et al 2022); however, they could also be the surviving remnants (after a close encounter with a larger galaxy in the cluster, such as the BCG) of compact galactic cores. Both the stars in the ICL and in GCs are expected to interact with the rest of the matter in the cluster mostly through gravitational forces, thus behaving similarly to DM.…”

Section: Discussionmentioning

confidence: 99%

“…The first image of JWST reveals approximately two dozen lensed system candidates, six of which have spectroscopic redshift estimations from MUSE and JWST data (Golubchik et al 2022;Sharon et al 2023;Pascale et al 2022;Mahler et al 2023;Caminha et al 2022) 2 . One of the surprises in the new data is the presence of hundreds of point-like sources near the large member galaxies in the cluster, which are possibly stripped galactic nuclei or compact globular clusters (Lee et al 2022;Faisst et al 2022). Some of the lensed galaxies also show small unresolved structures that could be compact star-forming regions, globular clusters (GCs), groups of stars, or even individual stars in cases of extreme magnification (Mowla et al 2022).…”

Section: Introductionmentioning

confidence: 98%

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Exploring the correlation between dark matter, intracluster light, and globular cluster distribution in SMACS0723

Diego,

Pascale,

Frye

et al. 2023

A&A

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We present a free-form model of SMACS0723, the first cluster observed with JWST. This model does not make any strong assumptions on the distribution of mass (mostly made up of dark matter) in the cluster and we use it to study the possible correlation between dark matter with the intracluster light and distribution of globular clusters (GCs). To explore the uncertainty in mass modeling, we derived three lens models based on spectroscopically confirmed systems and new candidate systems with redshifts predicted by the lens model derived from the spectroscopic systems. We find that beyond the radius of influence for the brightest cluster galaxy (BCG), the total mass does not trace the intracluster light (ICL), implying the need for a dark component (dark matter). Two loop-like structures observed in the intracluster light do not have any obvious correspondence with the total mass (of mostly dark matter) distribution. The radial profiles of the ICL and the distribution of GCs are similar to each other, but they are steeper than the profile of the lens model. More specifically, we find that the total mass is shallower by 1 dex in log scale than both ICL and GC profiles. This is in excellent agreement with current N-body simulations of cold dark matter.

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“…If our subhalos are to represent globular star clusters instead of dark matter subhalos, then their core radii should be smaller, of order a few tens of parsecs (Faisst et al 2022). To span the approximate range of possible core radii, we do three sets of calculations, with 22, 44, and 88 pc, but show only the 22 and 88 pc results in most of the plots.…”

Section: Subhalos In the Lens Planementioning

confidence: 99%

Flashlights: Properties of Highly Magnified Images Near Cluster Critical Curves in the Presence of Dark Matter Subhalos

Williams,

Kelly,

Treu

et al. 2024

ApJ

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Dark matter subhalos with extended profiles and density cores, and globular star clusters of mass 106–108 M ⊙ that live near the critical curves in galaxy cluster lenses can potentially be detected through their lensing magnification of stars in background galaxies. In this work, we study the effect such subhalos have on lensed images, and compare to the case of more well-studied microlensing by stars and black holes near critical curves. We find that the cluster density gradient and the extended mass distribution of subhalos are important in determining image properties. Both lead to an asymmetry between the image properties on the positive- and negative-parity sides of the cluster that is more pronounced than in the case of microlensing. For example, on the negative-parity side, subhalos with cores larger than about 50 pc do not generate any images with magnification above ∼100 outside of the immediate vicinity of the cluster critical curve. We discuss these factors using analytical and numerical analysis, and exploit them to identify observable signatures of subhalos: Subhalos create pixel-to-pixel flux variations of ≳0.1 mag on the positive-parity side of clusters. These pixels tend to cluster around (otherwise invisible) subhalos. Unlike in the case of microlensing, signatures of subhalo lensing can be found up to 1″ away from the critical curves of massive clusters.

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What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST

Cited by 12 publications

References 93 publications

An Atlas of Color-selected Quiescent Galaxies at z > 3 in Public JWST Fields

An Atlas of Color-selected Quiescent Galaxies at z > 3 in Public JWST Fields

Exploring the correlation between dark matter, intracluster light, and globular cluster distribution in SMACS0723

Flashlights: Properties of Highly Magnified Images Near Cluster Critical Curves in the Presence of Dark Matter Subhalos

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