One Hundred SMUDGes in S-PLUS: Ultra-diffuse Galaxies Flourish in the Field

Barbosa, C. E.; Zaritsky, Dennis; Donnerstein, Richard L.; Zhang, H.; Dey, Arjun; Oliveira, C. Mendes de; Sampedro, L.; Molino, A.; Costa-Duarte, M. V.; Coelho, P.; Cortesi, A.; Herpich, F. R.; Hernández-Jiménez, J. A.; Santos-Silva, T.; Pereira, Eduardo S.; Werle, Ariel; Overzier, Roderik; Fernandes, R. Cid; Castelli, A. V. Smith; Ribeiro, T.; Schoenell, W.; Kanaan, A.

doi:10.3847/1538-4365/ab7660

Cited by 50 publications

(38 citation statements)

References 105 publications

(194 reference statements)

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“…For convenience, throughout this paper, we use the DF names for these five galaxies, although they all appear in both the Yagi et al (2016) and Zaritsky et al (2019) catalogs as well. The sixth galaxy, known as SMDG1251014+274753 (hereafter we refer to this object as SMDG1251014) is identified by the SMUDGes survey of the Coma cluster (Zaritsky et al 2019;Barbosa et al 2020;Zaritsky et al 2021). The UDG sample is presented in Table 1 and their distribution relative to the Coma cluster is shown in Fig.…”

Section: Udg Samplementioning

confidence: 99%

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

Saifollahi,

Zaritsky,

Trujillo

et al. 2022

Preprint

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We present an analysis of Hubble Space Telescope observations of globular clusters (GCs) in six ultra-diffuse galaxies (UDGs) in the Coma cluster, a sample that represents UDGs with large effective radii (𝑅 e ), and use the results to evaluate competing formation models. We eliminate two significant sources of systematic uncertainty in the determination of the number of GCs, 𝑁 GC by using sufficiently deep observations that (i) reach the turnover of the GC luminosity function and (ii) provide a sufficient number of GCs with which to measure the GC number radial distribution. We find that 𝑁 GC for these galaxies is on average ∼ 20, which implies an average total mass, 𝑀 total , ∼ 10 11 𝑀 when applying the relation between 𝑁 GC and 𝑀 total . This value of 𝑁 GC lies at the upper end of the range observed for dwarf galaxies of the same stellar mass and is roughly a factor of two larger than the mean. The GC luminosity function, radial profile and average colour are more consistent with those observed for dwarf galaxies than with those observed for the more massive (𝐿 * ) galaxies, while both the radial and azimuthal GC distributions closely follow those of the stars in the host galaxy. Finally, we discuss why our observations, specifically the GC number and GC distribution around these six UDGs, pose challenges for several of the currently favoured UDG formation models.

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Section: Udg Samplementioning

confidence: 99%

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

Saifollahi,

Zaritsky,

Trujillo

et al. 2022

Preprint

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“…In Figure 16 we compare the current g−band central surface brightness with what we calculate it would be in 5 Gyr. To calculate the fading, we adopt the stellar population results from Barbosa et al (2020) and allow each galaxy to age passively for an additional 5 Gyr. On average, µ 0,g increases by about 0.9 mag, but the full distribution of sources matches well the range of µ 0,g that we find for our red galaxies.…”

Section: Color Vs Central Surface Brightnessmentioning

confidence: 99%

Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). I. Survey Description and First Results in the Coma Galaxy Cluster and Environs

Zaritsky

Donnerstein

Dey³

et al. 2018

ApJS

Self Cite

110

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We present a homogeneous catalog of 275 large (effective radius 5.3 ) ultra-diffuse galaxy (UDG) candidates lying within an ≈ 290 square degree region surrounding the Coma cluster. The catalog results from our automated postprocessing of data from the Legacy Surveys, a three-band imaging survey covering 14,000 square degrees of the extragalactic sky. We describe a pipeline that identifies UDGs and provides their basic parameters. The survey is as complete in these large UDGs as previously published UDG surveys of the central region of the Coma cluster. We conclude that the majority of our detections are at roughly the distance of the Coma cluster, implying effective radii ≥ 2.5 kpc, and that our sample contains a significant number of analogs of DF 44, where the effective radius exceeds 4 kpc, both within the cluster and in the surrounding field. The g − z color of our UDGs spans a large range, suggesting that even large UDGs may reflect a range of formation histories. A majority of the UDGs are consistent with being lower stellar mass analogs of red sequence galaxies, but we find both red and blue UDG candidates in the vicinity of the Coma cluster and a relative overabundance of blue UDG candidates in the lower density environments and the field. Our eventual processing of the full Legacy Surveys data will produce the largest, most homogeneous sample of large UDGs.

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“…It has the background galaxy LEDA 783199 in its vicinity, but no distance information is available in that case. Assuming a conservative distance of 100 Mpc, this would translate into M r = −14.4 mag and an effective radius of r eff = 4 kpc, which are plausible properties for an ultra-diffuse galaxy in the background (e.g., Barbosa et al 2020).…”

Section: Membership Of the Dwarf Galaxy Candidatementioning

confidence: 99%

Abundance of dwarf galaxies around low-mass spiral galaxies in the Local Volume

Müller

Jerjen

2020

A&A

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The abundance of satellite dwarf galaxies has long been considered a crucial test for the current model of cosmology leading to the well-known missing satellite problem. Recent advances in simulations and observations have allowed the study of dwarf galaxies around host galaxies in more detail. Using the Dark Energy Camera we surveyed a 72 deg 2 area of the nearby Sculptor group, also encompassing the two low-mass Local Volume galaxies NGC 24 and NGC 45 residing behind the group, to search for as yet undetected dwarf galaxies. Apart from the previously known dwarf galaxies we found only two new candidates down to a 3σ surface brightness detection limit of 27.4 r mag arcsec −2. Both systems are in projection close to NGC 24. However, one of these candidates could be an ultra-diffuse galaxy associated with a background galaxy. We compared the number of known dwarf galaxy candidates around NGC 24, NGC 45, and five other well-studied low-mass spiral galaxies (NGC 1156, NGC 2403, NGC 5023, M 33, and the LMC) with predictions from cosmological simulations, and found that for the stellar-to-halo mass models considered, the observed satellite numbers tend to be on the lower end of the expected range. This could mean either that there is an overprediction of luminous subhalos in ΛCDM or that we are missing some of the satellite members due to observational biases.

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One Hundred SMUDGes in S-PLUS: Ultra-diffuse Galaxies Flourish in the Field

Cited by 50 publications

References 105 publications

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). I. Survey Description and First Results in the Coma Galaxy Cluster and Environs

Abundance of dwarf galaxies around low-mass spiral galaxies in the Local Volume

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