Star formation in low-redshift cluster dwarf galaxies

Rude, Cody; Sultanova, Madina; Gamage, Gihan; Barkhouse, W. A.; Vithanage, Sandanuwan P. Kalawila

doi:10.1093/mnras/staa697

Cited by 6 publications

(5 citation statements)

References 72 publications

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“…We found that in all cases this ratio is lower than 1, meaning that the fraction of dwarfs is lower at short distances from the cluster centre, in agreement with earlier results in the literature (e.g. Popesso et al 2005;Rude et al 2020). A similar finding was noted in Mancera Piña et al (2018) where a lack of UDGs is reported near the cluster centres.…”

Section: Distribution Of Dwarfs Vs Giantssupporting

confidence: 93%

“…Additionally, the cluster cores seem to be a hostile region for dwarfs (Sánchez-Janssen et al 2008;Mancera Piña et al 2018;. A number of studies have used the dwarf-to-giant ratio (DGR) to quantify the fraction across the cluster, for example, Rude et al (2020) combined the luminosity functions (LFs) in the 𝑟 and 𝑢 bands of 15 Abell galaxy clusters and found that the dwarf-to-giant ratio increase at further clustercentric radius. Previously, Barkhouse et al (2009) for a sample of 57 low-redshift Abell clusters found a steady increase of the DGR with increasing clustercentric distance, however, the differences in both works may due to systematical definitions, as mentioned in Rude et al (2020).…”

Section: Introductionmentioning

confidence: 99%

“…A number of studies have used the dwarf-to-giant ratio (DGR) to quantify the fraction across the cluster, for example, Rude et al (2020) combined the luminosity functions (LFs) in the 𝑟 and 𝑢 bands of 15 Abell galaxy clusters and found that the dwarf-to-giant ratio increase at further clustercentric radius. Previously, Barkhouse et al (2009) for a sample of 57 low-redshift Abell clusters found a steady increase of the DGR with increasing clustercentric distance, however, the differences in both works may due to systematical definitions, as mentioned in Rude et al (2020). In any case, the change of the DGR with the clustercentric distance could be due to the variation of giants, dwarfs or both as pointed out in Sánchez-Janssen et al (2008).…”

Section: Introductionmentioning

confidence: 99%

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The dwarf galaxy population in nearby clusters from the KIWICS survey

Choque-Challapa,

Aguerri,

Piña

et al. 2021

Preprint

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We analyse a sample of twelve galaxy clusters, from the Kapteyn IAC WEAVE INT Cluster Survey (KIWICS) looking for dwarf galaxy candidates. By using photometric data in the 𝑟 and 𝑔 bands from the Wide Field Camera (WFC) at the 2.5-m Isaac Newton telescope (INT), we select a sample of bright dwarf galaxies (M 𝑟 ≤ -15.5 mag) in each cluster and analyse their spatial distribution, stellar colour, and as well as their Sérsic index and effective radius. We quantify the dwarf fraction inside the 𝑅 200 radius of each cluster, which ranges from ∼ 0.7 to ∼ 0.9. Additionally, when comparing the fraction in the inner region with the outermost region of the clusters, we find that the fraction of dwarfs tends to increase going to the outer regions. We also study the clustercentric distance distribution of dwarf and giant galaxies (M 𝑟 < -19.0 mag), and in half of the clusters of our sample, the dwarfs are distributed in a statistically different way as the giants, with the giant galaxies being closer to the cluster centre. We analyse the stellar colour of the dwarf candidates and quantify the fraction of blue dwarfs inside the 𝑅 200 radius, which is found to be less than ∼ 0.4, but increases with distance from the cluster centre. Regarding the structural parameters, the Sérsic index for the dwarfs we visually classify as early type dwarfs tends to be higher in the inner region of the cluster. These results indicate the role that the cluster environment plays in shaping the observational properties of low-mass halos.

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Section: Distribution Of Dwarfs Vs Giantssupporting

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The dwarf galaxy population in nearby clusters from the KIWICS survey

Choque-Challapa,

Aguerri,

Piña

et al. 2021

Preprint

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“…Similar dwarfs are long known to inhabit nearby clusters such as Virgo or Coma (Sandage & Binggeli 1984;Thompson & Gregory 1993). In these dense environments, and due to their relatively weak gravitational potential, dwarf galaxies suffer from quenching of star formation via ram pressure stripping and galaxy-galaxy interactions, reducing even further their brightness (Rude et al 2020).…”

Section: A Perturber To Explain Trmentioning

confidence: 99%

Godzilla, a monster lurks in the Sunburst galaxy

Diego

Pascale

Kavanagh

et al. 2022

A&A

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We model the strong lensing effect in the galaxy cluster PSZ1 G311. 65-18.48 (z=0.443) with an improved version of the hybrid method WSLAP+. We extend the number of constraints by including the position of critical points, which are combined with the classic positional constraints of the lensed galaxies. We pay special attention to a transient candidate source (Tr) previously discovered in the giant Sunburst arc (z=2.37). Our lens model predicts Tr to be within a fraction of an arcsecond from the critical curve, which has a larger magnification factor than previously found, but still not large enough to explain the observed flux and lack of counterimages. Possible candidate counterimages are discussed that would lower the magnification required to explain Tr, but extreme magnification factors (µ > 600) are still required, even in that case. The presence of a small mass perturber with a mass comparable to a dwarf galaxy (M ∼ 10 8 M ) near the position of Tr is needed in order to explain the required magnification and morphology of the lensed galaxy. We discuss how the existence of this perturber could potentially be used to constrain models of dark matter. The large apparent brightness and unresolved nature of the magnified object implies a combination of extreme magnification and a very luminous and compact source (r < 0.4 pc). Possible candidates are discussed, including an hyperluminous star, a small group of stars, or an accretion disk around a relatively small supermassive black hole (SMBH). Based on spectral information and flux requirements, we argue that a luminous blue variable (LBV) star caught during an outburst is the most likely candidate. Owing to the extreme magnification and luminosity of this source, we dub it Godzilla.

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“…Similar dwarfs are long known to inhabit nearby clusters like Virgo or Coma (Sandage & Binggeli 1984;Thompson & Gregory 1993). In these dense environments, and due to their relatively weak gravitational potential, dwarf galaxies suffer from quenching of star formation via ram pressure stripping and galaxy-galaxy interactions, reducing even further their brightness (Rude et al 2020).…”

Section: A Perturber To Explain Trmentioning

confidence: 99%

Godzilla, a monster lurks in the Sunburst galaxy

Diego,

Pascale,

Kavanagh

et al. 2022

Preprint

View full text Add to dashboard Cite

We model the strong lensing effect in the galaxy cluster PSZ1 G311. 65-18.48 (z=0.443) with an improved version of the hybrid method WSLAP+. We extend the number of constraints by including the position of critical points, which are combined with the classic positional constraints of the lensed galaxies. We pay special attention to a transient candidate source (Tr) previously discovered in the giant Sunburst arc (z=2.37). Our lens model predicts Tr to be within a fraction of an arcsecond from the critical curve, having a larger magnification factor than previously found, but still not large enough to explain the observed flux and lack of counterimages. Possible candidate counterimages are discussed that would lower the magnification required to explain Tr, but extreme magnification factors (µ > 1000) are still required, even in that case. The presence of a small mass perturber with a mass comparable to a dwarf galaxy (M ∼ 10 8 M ) near the position of Tr is needed in order to explain the required magnification and morphology of the lensed galaxy. We discuss how the existence of this perturber could potentially be used to constrain models of dark matter. The large apparent brightness and unresolved nature of the magnified object implies a combination of extreme magnification and a very luminous and compact source (r < 0.3 pc). Possible candidates are discussed, including an hyperluminous star or an accretion disc around an intermediate-mass black hole (IMBH). Based on spectral information, we argue that a luminous blue variable (LBV) star caught during an outburst is the most likely candidate. Owing to the extreme magnification and luminosity of this source we dub it Godzilla.

show abstract

Star formation in low-redshift cluster dwarf galaxies

Cited by 6 publications

References 72 publications

The dwarf galaxy population in nearby clusters from the KIWICS survey

The dwarf galaxy population in nearby clusters from the KIWICS survey

Godzilla, a monster lurks in the Sunburst galaxy

Godzilla, a monster lurks in the Sunburst galaxy

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