Luminosity Functions and Host-to-host Scatter of Dwarf Satellite Systems in the Local Volume

Carlsten, Scott G.; Greene, Jenny E.; Peter, Annika H. G.; Beaton, Rachael L.; Greco, Johnny P.

doi:10.3847/1538-4357/abd039

Cited by 65 publications

(136 citation statements)

References 170 publications

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“…Right: As the left-hand panel, but for high-resolution satellites with μ V ,eff < 28.3 and M V < −9 within a projected radius of 150 kpc of the central galaxy averaged over 1000 lines of sight. This mimics the selection function of the Milky Way mass galaxies in the Local Volume described in table 3 ofCarlsten et al (2021), the luminosity functions of which are shown by the thin lines.…”

supporting

confidence: 60%

Determining the full satellite population of a Milky Way-mass halo in a highly resolved cosmological hydrodynamic simulation

Grand

Marinacci

Pakmor

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We investigate the formation of the satellite galaxy population of a Milky Way-mass halo in a very highly resolved magneto-hydrodynamic cosmological zoom-in simulation (baryonic mass resolution mb = 800 $\rm M_{\odot }$). We show that the properties of the central star-forming galaxy, such as the radial stellar surface density profile and star formation history, are: i) robust to stochastic variations associated with the so-called ‘Butterfly Effect’; and ii) well converged over 3.5 orders of magnitude in mass resolution. We find that there are approximately five times as many satellite galaxies at this high resolution compared to a standard ($m_b\sim 10^{4-5}\, \rm M_{\odot }$) resolution simulation of the same system. This is primarily because 2/3rds of the high resolution satellites do not form at standard resolution. A smaller fraction (1/6th) of the satellites present at high resolution form and disrupt at standard resolution; these objects are preferentially low-mass satellites on intermediate- to low-eccentricity orbits with impact parameters ≲ 30 kpc. As a result, the radial distribution of satellites becomes substantially more centrally concentrated at higher resolution, in better agreement with recent observations of satellites around Milky Way-mass haloes. Finally, we show that our galaxy formation model successfully forms ultra-faint galaxies and reproduces the stellar velocity dispersion, half-light radii, and V-band luminosities of observed Milky Way and Local Group dwarf galaxies across 6 orders of magnitude in luminosity (103-$10^{9}\, \rm L_{\odot }$).

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supporting

confidence: 60%

Determining the full satellite population of a Milky Way-mass halo in a highly resolved cosmological hydrodynamic simulation

Grand

Marinacci

Pakmor

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…arcsec −2 , as established by Whiting et al (2007), for the isolated dwarfs. This is similar to what Carlsten et al (2021) quotes as the 90% completeness limit, 26.0 -26.5 mags. arcsec −2 , around 10 massive galaxies in the Local Volume, observed with CFHT imaging.…”

Section: Dwarfs In the Local Group In The Futuresupporting

confidence: 87%

Solo dwarfs IV: comparing and contrasting satellite and isolated dwarf galaxies in the Local Group

Higgs

McConnachie

2021

Monthly Notices of the Royal Astronomical Society

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We compare and contrast the stellar structures of isolated Local Group dwarf galaxies, as traced by their oldest stellar populations, with the satellite dwarf galaxies of the Milky Way and M 31. All Local Group dwarfs with Mv ≤ −6 and μo < 26.5 mags arcsec−2 are considered, taking advantage of measurements from surveys that use similar observations and analysis techniques. For the isolated dwarfs, we use the results from Solitary Local (Solo) Dwarf Galaxy Survey. We begin by confirming that the structural and dynamical properties of the two satellite populations are not obviously statistically different from each other, but we note that there many more satellites around M 31 than around the Milky Way down to equivalent magnitude and surface brightness limits. We find that dwarfs in close proximity to a massive galaxy generally show more scatter in their Kormendy relations than those in isolation. Specifically, isolated Local Group dwarf galaxies show a tighter trend of half-light radius versus magnitude than the satellite populations, and similar effects are also seen for related parameters. There appears to be a transition in the structural and dynamical properties of the dwarf galaxy population around ∼400 kpc from the Milky Way and M 31, such that the smallest, faintest, most circular dwarf galaxies are found closer than this separation. We discuss the impact of selection effects on our analysis, and we argue that our results point to the significance of tidal interactions on the population of systems within approximately 400 kpc from the MW and M 31.

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“…One important test for cosmological simulations is that they need to produce the right amount of luminous low-mass galaxies. The LF obtained from FDS data can be used for making such a 2020), respectively, and the data for other groups are from Carlsten et al (2021). The last column lists the number of galaxies in the samples.…”

Section: Comparison Of the Luminosity Function With Illustristngmentioning

confidence: 99%

“…Results of the K-S tests (p values) when comparing the likelihood that the V-band LFs of different samples are drawn from the same distribution. Fornax and Fornax A data are from this work, Centaurus A data are from Müller et al (2019), LG and Virgo data are from Ferrarese et al (2016) and Ferrarese et al (2020), respectively, and the data for other groups are fromCarlsten et al (2021). The last column lists the number of galaxies in the samples.…”

mentioning

confidence: 99%

The Fornax Deep Survey (FDS) with VST XII: Low surface brightness dwarf galaxies in the Fornax cluster

Venhola¹,

Peletier²,

Salo³

et al. 2021

Preprint

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Context. Low surface brightness (LSB) dwarf galaxies in galaxy clusters are an interesting group of objects as their contribution to the galaxy luminosity function and their evolutionary paths are not yet clear. Increasing the completeness of our galaxy catalogs is crucial for understanding these galaxies, which have effective surface brightnesses below 23 mag arcsec −2 (in optical). Progress is continuously being made via the performance of deep observations, but detection depth and the quantification of the completeness can also be improved via the application of novel approaches in object detection. For example, the Fornax Deep Survey (FDS) has revealed many faint galaxies that can be visually detected from the images down to a surface brightness level of 27 mag arcsec −2 , whereas traditional detection methods, such as using Source Extractor (SE), fail to find them. Aims. In this work we use a max-tree based object detection algorithm (Max-Tree Objects, MTO) on the FDS data in order to detect previously undetected LSB galaxies. After extending the existing Fornax dwarf galaxy catalogs with this sample, our goal is to understand the evolution of LSB dwarfs in the cluster. We also study the contribution of the newly detected galaxies to the faint end of the luminosity function. Methods. We test the detection completeness and parameter extraction accuracy of MTO using simulated and real images. We then apply MTO to the FDS images to identify LSB candidates. The identified objects are fitted with 2D Sérsic models using GALFIT and classified as imaging artifacts, likely cluster members, or background galaxies based on their morphological appearance, colors, and structure.Results. With MTO, we are able to increase the completeness of our earlier FDS dwarf catalog (FDSDC) 0.5-1 mag deeper in terms of total magnitude and surface brightness. Due to the increased accuracy in measuring sizes of the detected objects, we also add many small galaxies to the catalog that were previously excluded as their outer parts had been missed in detection. We detect 265 new LSB dwarf galaxies in the Fornax cluster, which increases the total number of known dwarfs in Fornax to 821. Using the whole cluster dwarf galaxy population, we show that the luminosity function has a faint-end slope of α=-1.38±0.02. We compare the obtained luminosity function with different environments studied earlier using deep data but do not find any significant differences. On the other hand, the Fornax-like simulated clusters in the IllustrisTNG cosmological simulation have shallower slopes than found in the observational data. We also find several trends in the galaxy colors, structure, and morphology that support the idea that the number of LSB galaxies is higher in the cluster center due to tidal forces and the age dimming of the stellar populations. The same result also holds for the subgroup of large LSB galaxies, so-called ultra-diffuse galaxies.

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Luminosity Functions and Host-to-host Scatter of Dwarf Satellite Systems in the Local Volume

Cited by 65 publications

References 170 publications

Determining the full satellite population of a Milky Way-mass halo in a highly resolved cosmological hydrodynamic simulation

Determining the full satellite population of a Milky Way-mass halo in a highly resolved cosmological hydrodynamic simulation

Solo dwarfs IV: comparing and contrasting satellite and isolated dwarf galaxies in the Local Group

The Fornax Deep Survey (FDS) with VST XII: Low surface brightness dwarf galaxies in the Fornax cluster

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