Structure and morphology of the MATLAS dwarf galaxies and their central nuclei

Poulain, Mélina; Marleau, F.; Habas, Rebecca; Duc, Pierre–Alain; Sánchéz-Janssen, R.; Durrell, Patrick R.; Paudel, Sanjaya; Ahad, Syeda Lammim; Chougule, Abhishek; Müller, Oliver; Lim, Sungsoon; Bílek, Michal; Fensch, Jérémy

doi:10.1093/mnras/stab2092

Cited by 33 publications

(68 citation statements)

References 118 publications

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“…The final MATLAS dwarf catalog contains 2210 dwarf galaxies which have been classified as dwarf ellipticals (dEs, 73.4%) and dwarf irregulars (dIrrs, 26.6%). The derivation of additional properties, such as the half light radius R e , the Sersic index n and the axis ratio b/a of the dwarfs, was done using the software galfit (Peng et al 2002(Peng et al , 2010, a two-dimensional surface brightness fitting algorithm developed for the structure modeling of galaxies in astronomical images with an emphasis on the detailed inspection of light profiles (Poulain et al 2021).…”

Section: Dwarf Catalogmentioning

confidence: 99%

“…MATLAS is strictly an imaging survey, but we were able to obtain distance estimates for a number of the dwarf candidates from overlapping, complementary surveys. In total, distances for 325 dwarfs (∼15% of the final catalog) could be estimated in this way and 99% of this subsample was confirmed to be a dwarf based on an absolute magnitude cut of M g = −18 (Habas et al 2020;Poulain et al 2021). Details about the methods leading to the final dwarf catalog and its properties can be found in Habas et al (2020).…”

Section: Dwarf Catalogmentioning

confidence: 99%

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Flattened structures of dwarf satellites around massive host galaxies in the MATLAS low-to-moderate density fields

Heesters

Habas

Marleau

et al. 2021

A&A

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It was first observed in the 1970s that the dwarf galaxies surrounding our Milky Way, so-called satellites, appear to be arranged in a thin, vast plane. Similar discoveries have been made around additional galaxies in the local Universe such as Andromeda, Centaurus A, and potentially M83. In the specific cases with available kinematic data, the dwarf satellites also appear to preferentially co-orbit their massive host galaxy. Planes of satellites are rare in the lambda cold dark matter paradigm, although they may be a natural consequence of projection effects. Such a phase-space correlation, however, remains difficult to explain. In this work we analyzed the 2D spatial distribution of 2210 dwarf galaxies around early-type galaxies (ETGs) in the low-to-medium density fields of the “Mass Assembly of early-Type GaLAxies with their fine Structures” (MATLAS) survey. Under the assumption that the dwarfs are satellite members of the central massive ETG, we identified flattened structures using both a variation in the Hough transform and total least square fitting. In 119 satellite systems, we find 31 statistically significant flattened dwarf structures using a combination of both methods with subsequent Monte Carlo simulations with random data. The vast majority of these dwarf structures lie within the estimated virial radii of the massive host. The major axes of these systems are aligned better than 30° with the estimated orientation of the large-scale structure in nine (50%) cases. Additional distance measurements and future kinematic studies will be required to confirm the planar nature of these structures and to determine if they are corotating systems.

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Section: Dwarf Catalogmentioning

confidence: 99%

Section: Dwarf Catalogmentioning

confidence: 99%

Flattened structures of dwarf satellites around massive host galaxies in the MATLAS low-to-moderate density fields

Heesters

Habas

Marleau

et al. 2021

A&A

Self Cite

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“…The binned galaxy nucleation fraction, NSC masses and stellar masses for galaxies in the Coma, Virgo, Fornax clusters, as well as the MW, M31 and M81, are taken from the compilation of RSJ19 and references therein. During the proofs stage of this manuscript, several other compilations of Local Volume nucleation fraction data were published in the studies of Carlsten et al (2021);Hoyer et al (2021); Zanatta et al (2021); Poulain et al (2021), to which we refer interested readers.…”

Section: Datamentioning

confidence: 99%

On the link between nuclear star cluster and globular cluster system mass, nucleation fraction and environment

Leaman,

van de Ven

2021

Preprint

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We present a simple model for the host mass dependence of the galaxy nucleation fraction ( 𝑓 𝑛𝑢𝑐 ), the galaxy's nuclear star cluster (NSC) mass and the mass in its surviving globular clusters (𝑀 𝐺𝐶,𝑜𝑏𝑠 ). Considering the mass and orbital evolution of a GC in a galaxy potential, we define a critical mass limit (𝑀 𝐺𝐶,𝑙𝑖𝑚 ) above which a GC can simultaneously in-spiral to the galaxy centre due to dynamical friction and survive tidal dissolution, to build up the NSC. The analytic expression for this threshold mass allows us to model the nucleation fraction for populations of galaxies. We find that the slope and curvature of the initial galaxy size-mass relation is the most important factor (with the shape of the GC mass function a secondary effect) setting the fraction of galaxies that are nucleated at a given mass. The well defined skewnormal 𝑓 𝑛𝑢𝑐 −𝑀 𝑔𝑎𝑙 observations in galaxy cluster populations are naturally reproduced in these models, provided there is an inflection in the initial size-mass relation at 𝑀 𝑔𝑎𝑙 ∼ 10 9.5 M . Our analytic model also predicts limits to the 𝑀 𝑔𝑎𝑙 − 𝑀 𝐺𝐶,𝑡𝑜𝑡 and 𝑀 𝑔𝑎𝑙 − 𝑀 𝑁 𝑆𝐶 relations which bound the scatter of the observational data. Moreoever, we illustrate how these scaling relations and 𝑓 𝑛𝑢𝑐 vary if the star cluster formation efficiency, GC mass function, galaxy environment or galaxy size-mass relation are altered. Two key predictions of our model are: 1) galaxies with NSC masses greater than their GC system masses are more compact at fixed stellar mass, and 2) the fraction of nucleated galaxies at fixed galaxy mass is higher in denser environments. That a single model framework can reproduce both the NSC and GC scaling relations provides strong evidence that GC in-spiral is an important mechanism for NSC formation.

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“…These blue-cored dwarf ETGs are usually found in the outskirts of galaxy clusters where the galaxy density is lowest. The more massive dwarf ETGs exhibit nuclei that tend to be somewhat bluer than their host galaxies (Lotz et al 2004;Côté et al 2006;Paudel et al 2010Paudel et al , 2011Neumayer et al 2020;Poulain et al 2021). In addition, spiral arms and bars have been detected in several dwarf ETGs in the Virgo cluster (Jerjen et al 2001;Barazza et al 2002;Ferrarese et al 2006;Lisker et al 2006b), as well as in the Fornax (De Rijcke et al 2003;Venhola et al 2019), Coma , and Perseus clusters (Penny et al 2014).…”

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

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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.

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Structure and morphology of the MATLAS dwarf galaxies and their central nuclei

Cited by 33 publications

References 118 publications

Flattened structures of dwarf satellites around massive host galaxies in the MATLAS low-to-moderate density fields

Flattened structures of dwarf satellites around massive host galaxies in the MATLAS low-to-moderate density fields

On the link between nuclear star cluster and globular cluster system mass, nucleation fraction and environment

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

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