Low surface brightness galaxies in <i>z</i> &gt; 1 galaxy clusters: HST approaching the progenitors of local ultra diffuse galaxies

Bachmann, Aisha; Burg, R. F. J. van der; Fensch, Jérémy; Brammer, Gabriel; Muzzin, Adam

doi:10.1051/0004-6361/202040097

Cited by 8 publications

(7 citation statements)

References 38 publications

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“…88/0.31 to 88/0.59), close to the (van der Burg et al 2017) scaling relation. Whether this is inconsistent with an of evolution in UDG abundance with redshift (as suggested by Bachmann et al 2021) is not clear given the large scatter in UDG abundance at z = 0 and the large uncertainties in our measurement.…”

Section: Abundancecontrasting

confidence: 59%

“…Since then, more UDGs have been identified in Coma (Koda et al 2015), Virgo (Mihos et al 2015), and Fornax (Muñoz et al 2015), as well as groups and the field (Leisman et al 2017;Román & Trujillo 2017a). In addition to many objects identified in the local Universe, UDGs have also been identified in the Hubble Frontier Fields (Janssens et al 2017;Lee et al 2017;Janssens et al 2019;Lee et al 2020) and z ∼ 1 clusters (Bachmann et al 2021). Given their puzzling nature, optically-identified UDGs have been followed up with spectroscopy (Gu et al 2018;Ruiz-Lara et al 2018;Ferré-Mateu et al 2018;van Dokkum et al 2019;Gannon et al 2022), X-ray (Mirakhor & Walker 2021), UV (Boissier et al 2008), IR (Pandya et al 2018;Buzzo et al 2022), and radio (Leisman et al 2017;Papastergis et al 2017;Struble 2018) observations across a wide range of environments (Leisman et al 2017;Prole et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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PEARLS: Low Stellar Density Galaxies in the El Gordo Cluster Observed with JWST

Carleton¹,

Cohen²,

Frye³

et al. 2023

Preprint

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A full understanding of how unusually large "Ultra Diffuse Galaxies" (UDGs) fit into our conventional theory of dwarf galaxy formation remains elusive, despite the large number of objects identified locally. A natural extension of UDG research is the study of similar galaxies at higher redshift to establish how their properties may evolve over time. However, this has been a challenging task given how severely cosmological surface brightness dimming inhibits our ability to detect low-surface brightness galaxies at high-z. Here, we present a sample of low stellar surface density galaxies (LDGs) at moderate redshift, likely the progenitors of local UDGs, identified in deep near-IR JWST observations of the El Gordo cluster at z = 0.87. By stacking 8 NIRCAM filters, reach an apparent surface brightness sensitivity of 24.59 mag arcsec −2 , faint enough to be complete to the bright end of the LDG population. Our analysis identifies significant differences between this population and UDGs observed locally, including differences in their color and size distributions, which suggest that the UDG progenitors at high-z are bluer and more extended than UDGs at z = 0. This suggests that multiple mechanisms are responsible for UDG formation and that prolonged transformation of cluster dwarfs is not a primary UDG formation mechanism at high-z. Furthermore, we find a slight overabundance of LDGs in El Gordo, and, in contrast to findings in local clusters, our analysis does not show a deficit of LDGs in the center of El Gordo, implying that tidal destruction of LDGs is significant between z = 0.87 and z = 0.

show abstract

Section: Abundancecontrasting

confidence: 59%

Section: Introductionmentioning

confidence: 99%

PEARLS: Low Stellar Density Galaxies in the El Gordo Cluster Observed with JWST

Carleton¹,

Cohen²,

Frye³

et al. 2023

Preprint

View full text Add to dashboard Cite

show abstract

“…This suggests an overall UDG abundance ranging from 283 to 382 (i.e., 283/1.00 to 283/0.74), close to the van der Burg et al (2017) scaling relation. Whether this is inconsistent with an of evolution in UDG abundance with redshift (as suggested by Bachmann et al 2021) is not clear given the large scatter in UDG abundance at z = 0 and the large uncertainties in our measurement.…”

Section: Abundancecontrasting

confidence: 59%

“…Since then, more UDGs have been identified in Coma (Koda et al 2015), Virgo (Mihos et al 2015), and Fornax (Muñoz et al 2015), as well in as groups and the field (Leisman et al 2017;Román & Trujillo 2017a). In addition to many objects identified in the local Universe, UDGs have also been identified in the Hubble Frontier Fields (Janssens et al 2017(Janssens et al , 2019Lee et al 2017Lee et al , 2020 and z ∼ 1 clusters (Bachmann et al 2021). Given their puzzling nature, optically identified UDGs have been followed up with spectroscopy (Ferré-Mateu et al 2018;Gu et al 2018;Ruiz-Lara et al 2018;van Dokkum et al 2019b;Gannon et al 2022), X-ray (Mirakhor & Walker 2021), UV (Boissier et al 2008), IR (Pandya et al 2018;Buzzo et al 2022), and radio (Leisman et al 2017;Papastergis et al 2017;Struble 2018) observations in a wide range of environments (Leisman et al 2017;Prole et al 2019).…”

Section: Introductionmentioning

confidence: 99%

PEARLS: Low Stellar Density Galaxies in the El Gordo Cluster Observed with JWST

Carleton

Cohen

Frye

et al. 2023

ApJ

View full text Add to dashboard Cite

A full understanding of how unusually large ultradiffuse galaxies (UDGs) fit into our conventional theory of galaxy formation remains elusive, despite the large number of objects identified locally. A natural extension of UDG research is the study of similar galaxies at higher redshift to establish how their properties may evolve over time. However, this has been a challenging task given how severely systematic effects and cosmological surface brightness dimming inhibit our ability to analyze low surface brightness galaxies at high z. Here, we present a sample of low stellar surface density galaxies (LDGs) at moderate redshift, likely the progenitors of local UDGs, identified using deep near-IR observations of the El Gordo cluster at z = 0.87 with JWST. By stacking eight NIRCAM filters, we reach an apparent surface brightness sensitivity of 24.59 mag arcsec−2, which is faint enough to be complete to the bright end of the LDG population. Our analysis identifies significant differences between this population and UDGs observed locally, such as their color and size distributions, which suggest that the UDG progenitors at high z are bluer and more extended than UDGs at z = 0. This suggests that multiple mechanisms are responsible for the UDG formation and that prolonged transformation of cluster dwarfs is not a primary UDG formation mechanism at high z. Furthermore, we find a slight overabundance of LDGs in El Gordo, and, in contrast to findings in local clusters, our analysis does not show a deficit of LDGs in the center of El Gordo, implying that tidal destruction of LDGs is significant between z = 0.87 and z = 0.

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“…However, a sample of UDGs in the distant Universe are needed to study their evolution. The farthest UDGs studied are by Bachmann et al (2021), who searched for large low-surfacebrightness galaxies in two clusters at z = 1.13 and z = 1.23. Their work showed an underabundance of UDGs in highredshift clusters, by a factor of ∼3, compared to local clusters.…”

Section: Introductionmentioning

confidence: 99%

Structure and Color Gradients of Ultradiffuse Galaxies in Distant Massive Galaxy Clusters

Zhao,

Liu,

Cui

et al. 2023

ApJ

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We have measured structural parameters and radial color profiles of 108 ultradiffuse galaxies (UDGs), carefully selected from six distant massive galaxy clusters in the Hubble Frontier Fields (HFF) in a redshift range from 0.308 to 0.545. Our best-fitting GALFIT models show that the HFF UDGs have a median Sérsic index of 1.09, which is close to 0.86 for local UDGs in the Coma cluster. The median axis-ratio value is 0.68 for HFF UDGs and 0.74 for Coma UDGs, respectively. The structural similarity between HFF and Coma UDGs suggests that they are the same kind of galaxies seen at different times, and that the structures of UDGs do not change at least for several billion years. By checking the distribution of HFF UDGs in the rest-frame UVJ and UVI diagrams, we find a large fraction of them are star forming. Furthermore, a majority of HFF UDGs show small U − V color gradients within the 1 ∗ R e,SMA region, and the fluctuation of the median radial color profile of HFF UDGs is smaller than 0.1 mag, which is compatible to Coma UDGs. Our results indicate that cluster UDGs may fade or quench in a self-similar way, irrespective of the radial distance, in less than ∼4 Gyr.

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Low surface brightness galaxies in z > 1 galaxy clusters: HST approaching the progenitors of local ultra diffuse galaxies

Cited by 8 publications

References 38 publications

PEARLS: Low Stellar Density Galaxies in the El Gordo Cluster Observed with JWST

PEARLS: Low Stellar Density Galaxies in the El Gordo Cluster Observed with JWST

PEARLS: Low Stellar Density Galaxies in the El Gordo Cluster Observed with JWST

Structure and Color Gradients of Ultradiffuse Galaxies in Distant Massive Galaxy Clusters

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