Brought to Light. II. Revealing the Origins of Cloaked Spiral Features in Cluster Passive Dwarf Galaxies

Smith, Rory; Michea, Josefina; Pasquali, A.; Calderón-Castillo, Paula; Kraljic, Katarina; Paudel, Sanjaya; Lisker, Thorsten; Shin, Jihye; Ko, Jongwan; Peletier, Reynier F.; Grebel, Eva K.

doi:10.3847/1538-4357/abe1b1

Cited by 18 publications

(14 citation statements)

References 80 publications

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“…Simulations have shown that in this case, the features are expected to be fairly symmetrical for high speed encounters, rather asymmetrical in case of low speed encounters (like M51) (Byrd & Valtonen 1990). In the latter case, the galaxy appearance could be similar to ram pressure stripped cases, but the nearby companion should be still visible, allowing us to distinguish between the two mechanisms (Smith et al 2021).…”

Section: Discussionmentioning

confidence: 90%

The relevance of ram pressure stripping for the evolution of blue cluster galaxies as seen at optical wavelengths

Vulcani,

Poggianti,

Smith

et al. 2022

Preprint

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Ram pressure stripping is one of the most efficient mechanisms able to affect the gas reservoir in cluster galaxies and in the last decades many studies have characterized the properties of stripped galaxies. A definite census of the importance of this process in local clusters is though still missing.Here we characterize the fraction of galaxies showing signs of stripping at optical wavelengths, using the data of 66 clusters from the WINGS and OMEGAWINGS surveys. We focus on the infalling galaxy population and hence only consider blue, bright (B< 18.2) late-type spectroscopically confirmed cluster members within 2 virial radii. In addition to "traditional" stripping candidates (SC) -i.e. galaxies showing unilateral debris and tails -we also consider unwinding galaxies (UG) as potentially stripped galaxies. Recent work has indeed unveiled a connection between unwinding features and ram pressure stripping and even though only integral field studies can inform on how often these features are indeed due to ram pressure, it is important to include them in the global census. We performed a visual inspection of B-band images and here we release a catalog of 143 UG. SC and UG each represent ∼ 15 − 20% of the inspected sample. If we make the assumption that they both are undergoing ram pressure stripping, we can conclude that at any given time in the low-z universe about 35% of the infalling cluster population show signs of stripping in their morphology at optical wavelengths. These fractions depend on color, mass, morphology, and little on clustercentric distance. Making some rough assumptions on the duration of the tail visibility and on the time cluster galaxies can maintain blue colors, we infer that almost all bright blue late-type cluster galaxies undergo a stripping phase during their life, boosting the importance of ram pressure stripping in cluster galaxy evolution.

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Section: Discussionmentioning

confidence: 90%

The relevance of ram pressure stripping for the evolution of blue cluster galaxies as seen at optical wavelengths

Vulcani,

Poggianti,

Smith

et al. 2022

Preprint

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“…In the second paper of this series (Brought to Light II, Smith et al 2021) we simulated dwarf ETGs along different orbits in a Virgo-like cluster potential. We found that tidal triggering can reproduce the disk substructures observed in Virgo dwarf ETGs only when a galaxy contains a cold and thin disk embedded in a more massive and hot disk, and experiences very plunging pericenter passages (r peri < 0.25 r vir ).…”

Section: Implications Of Substructure Morphologymentioning

confidence: 99%

“…In Brought to Light II (Smith et al 2021), we compared the morphology of these substructure features with those arising from high-resolution numerical simulations of tidal harassment by a galaxy cluster potential. We found that the formation of spiral arms and bars can be effectively tidally triggered, during close pericenter passages, in dwarf ETGs that contain a fraction of their stellar disk in a cold, highly rotationally-supported component embedded in a comparatively hotter, little rotationally-supported disk that dominates the total galaxy mass.…”

Section: Introductionmentioning

confidence: 99%

Brought to Light III: Colors of Disk and Clump Substructures in Dwarf Early-Type Galaxies of the Fornax Cluster

Michea,

Pasquali,

Smith

et al. 2022

Preprint

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It has been well established that dwarf early-type galaxies (ETGs) can often exhibit a complex morphology, whereby faint spiral arms, bars, edge-on disks or clumps are embedded in their main, brighter diffuse body. In our first paper (Brought to Light I: Michea et al. 2021), we developed a new method for robustly identifying and extracting substructures in deep imaging data of dwarf ETGs in the Virgo galaxy cluster. Here we apply our method to a sample of 23 dwarf ETGs in the Fornax galaxy cluster, out of which 9 have disk-like and 14 have clump-like substructures. According to Fornax Deep Survey (FDS) data, our sample constitutes 12% of all dwarf ETGs in Fornax brighter than M r = −13 mag, and contains all cases that unequivocally exhibit substructure features. We use g and r-band FDS images to measure the relative contribution of the substructures to the total galaxy light and to estimate their g − r colors. We find that substructures typically contribute 8.7% and 5.3% of the total galaxy light in the g and r bands, respectively, within two effective radii. Disk substructures are usually found in dwarf ETGs with redder global colors, and they can be either as red as or bluer than their galaxy's diffuse component. In contrast, clump substructures are found in comparatively bluer dwarf ETGs, and they are always bluer than their galaxy's diffuse component. These results provide further evidence that dwarf ETGs can hide diverse complex substructures, with stellar populations that can greatly differ from those of the dominant diffuse light in which they are embedded.

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“…In "Brought to Light II" (Smith et al 2021), we compared the morphology of these substructure features with those arising from high-resolution numerical simulations of tidal harassment by a galaxy-cluster potential. We found that the formation of spiral arms and bars can be effectively tidally triggered, during close pericenter passages, in dwarf ETGs that contain a fraction of their stellar disk in a cold, highly rotationally supported component embedded in a comparatively hotter, lesser rotationally supported disk that dominates the total galaxy mass.…”

Section: Introductionmentioning

confidence: 99%

Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster

Michea¹,

Pasquali²,

Smith³

et al. 2022

Self Cite

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It has been well established that dwarf early-type galaxies (ETGs) can often exhibit a complex morphology, whereby faint spiral arms, bars, edge-on disks, or clumps are embedded in their main, brighter diffuse body. In our first paper (“Brought to Light I”), we developed a new method for robustly identifying and extracting substructures in deep imaging data of dwarf ETGs in the Virgo galaxy cluster. Here we apply our method to a sample of 23 dwarf ETGs in the Fornax galaxy cluster, out of which 9 have disk-like and 14 have clump-like substructures. According to Fornax Deep Survey (FDS) data, our sample constitutes 12% of all dwarf ETGs in Fornax brighter than M r = − 13 mag, and contains all cases that unequivocally exhibit substructure features. We use g- and r-band FDS images to measure the relative contribution of the substructures to the total galaxy light and to estimate their g − r colors. We find that the substructures typically contribute 8.7% and 5.3% of the total galaxy light in the g and r bands, respectively, within two effective radii. Disk substructures are usually found in dwarf ETGs with redder global colors, and they can be either as red as or bluer than their galaxy’s diffuse component. In contrast, the clump substructures are found in comparatively bluer dwarf ETGs, and they are always bluer than their galaxy’s diffuse component. These results provide further evidence that dwarf ETGs can hide diverse complex substructures, with stellar populations that can greatly differ from those of the dominant diffuse light in which they are embedded.

show abstract

Brought to Light. II. Revealing the Origins of Cloaked Spiral Features in Cluster Passive Dwarf Galaxies

Cited by 18 publications

References 80 publications

The relevance of ram pressure stripping for the evolution of blue cluster galaxies as seen at optical wavelengths

The relevance of ram pressure stripping for the evolution of blue cluster galaxies as seen at optical wavelengths

Brought to Light III: Colors of Disk and Clump Substructures in Dwarf Early-Type Galaxies of the Fornax Cluster

Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster

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