The galaxy size–halo mass scaling relations and clustering properties of central and satellite galaxies

Rodríguez, Facundo; Montero-Dorta, Antonio D.; Angulo, Raúl E.; Artale, M. Celeste; Merchán, Manuel

doi:10.1093/mnras/stab1571

Cited by 24 publications

(7 citation statements)

References 134 publications

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“…The contribution of other properties such as spin, concentration or age seem to be equally relevant and significant, but it is important to bear in mind that our prediction for galaxy radius is still not optimal. These results seem to be connected with the shape of the (halo/stellar) mass-size relation (see, e.g., Rodriguez et al 2021): at the high-mass end, central galaxy size is proportional to halo mass, but the relation is basically flat at the low-mass end. Reproducing and physically modeling the scatter in the mass-size relation will be the subject of further investigation.…”

Section: Discussionmentioning

confidence: 85%

Mimicking the halo-galaxy connection using machine learning

de Santi,

Rodrigues,

Montero-Dorta

et al. 2022

Preprint

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Elucidating the connection between the properties of galaxies and the properties of their hosting haloes is a key element in theories of galaxy formation. When the spatial distribution of objects is also taken under consideration, investigating the halo-galaxy connection becomes very relevant for cosmological measurements. In this paper, we use machine learning (ML) techniques to analyze these intricate relations in the IllustrisTNG300 magnetohydrodynamical simulation. We employ four different algorithms: extremely randomized trees (ERT), K-nearest neighbors (kNN), light gradient boosting machine (LGBM), and neural networks (NN), along with a stacked model where we combine results from all four approaches. Overall, the different ML algorithms produce consistent results in terms of predicting galaxy properties from a set of input halo properties that include halo mass, concentration, spin, and halo overdensity. For stellar mass, the (predicted v. true) Pearson correlation coefficient is 0.98, dropping down to 0.7-0.8 for specific star formation rate (sSFR), colour, and size. In addition, we test an existing data augmentation technique, designed to alleviate the problem of unbalanced datasets, and show that it improves slightly the shape of the predicted distributions. We also demonstrate that our predictions are good enough to reproduce the power spectra of multiple galaxy populations, defined in terms of stellar mass, sSFR, colour, and size with high accuracy. Our results align with previous reports suggesting that certain galaxy properties cannot be reproduced using halo features alone.

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Section: Discussionmentioning

confidence: 85%

Mimicking the halo-galaxy connection using machine learning

de Santi,

Rodrigues,

Montero-Dorta

et al. 2022

Preprint

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“…Among other advantages, it was found that this galaxy group sample presents excellent agreement between the mass it provides and those obtained by weak gravitational lensing techniques (Gonzalez et al 2021). In addition, it was highly efficient at comparing properties of central and satellite galaxies with the results obtained in simulations (Rodriguez et al 2021). Our final galaxy catalog is a volume-limited sample of galaxies up to z = 0.1, comprising 134405 objects with angular positions, spectroscopic magnitudes, and other astrophysical data, together with their corresponding group and halo host membership and mass.…”

Section: The Group Galaxy Catalogmentioning

confidence: 85%

How galaxies populate halos in extreme density environments: An analysis of the halo occupation distribution in SDSS

Alfaro

Rodríguez

Ruiz

et al. 2022

A&A

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Context. Recent works have shown that the properties of galaxy populations in simulated dark matter halos vary with large-scale environments. These results suggest a variation in the halo occupation distribution (HOD) in extreme density environments since the dynamical and astrophysical conditions prevailing in these regions may significantly affect the formation and evolution of their halos and residing galaxies, influencing the mean number of satellite galaxies. To analyze these effects, we identify cosmic voids and future virialized structures (FVSs) in the Sloan Digital Sky Server Data Release 12 (SDSS-DR12) and estimate the HOD within these super-structures using group catalogs as dark matter halo proxies. Aims. Our goal is to use observational galaxy data to characterize the HOD within cosmic voids and FVSs, explore the different properties of these galaxies' populations, and compare them with the general results outside of these super-structures. Methods. We used a publicly available observational galaxy catalog with information on redshifts, positions, magnitudes, and other astrophysical features to build a volume complete galaxy sample and identify cosmic voids and FVSs. Using a publicly available galaxy group catalog as a proxy to dark matter halos, we computed the HOD within both types of super-structures for different absolute magnitude thresholds. We also studied the dependence of the results on the main void and FVS properties, density, and volume. We also analyzed the main characteristics of the stellar content of galaxies inside these extreme-density regions such as the mean stellar age and the stellar mass. In all cases, we compared the results with those derived from the field sample, defined by objects outside of both types of environments. Results. Inside cosmic voids, we find a strong decrease in the HOD concerning the field results. In the most extreme cases, that is to say groups with masses above ∼ 10 13 h −1 M , the mean number of satellites fall to ∼ 50 percent. Inside FVSs, the HOD shows a significant increase to the field, with a ∼ 40 percent excess in the mean number of satellites for groups with masses around 10 14 h −1 M . These results are present for the different galaxy luminosity ranges explored. In both environments, the differences with respect to the field increases for the extreme values of the density environments. However, we obtain no signs of variations related to intrinsic characteristics of the super-structures, indicating that the effects mainly depend on the density of the large-scale environment. In addition, we find that the cumulative distribution of the mean age of stars of the central galaxy also varies in the different regions; this suggests that the history of the formation of the dark matter halos may be different. Finally, we explore the HOD for the 25% youngest (oldest) galaxies, based on the mean age of their stars. We find that for the low-mass groups the youngest galaxies are only present inside voids, and they are generally central galaxies. On the othe...

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“…From Equation 7, plus the correlation between the mass enclosed in a GCS (M GCS ) and the halo mass (M h ) from Harris et al (2015), and the r eff,gal -to-M h relations from the literature (e.g. Kravtsov 2013;Rodriguez et al 2021), the r eff,gal and the r eff,GCS come to be related by a power-law with exponent ≈ 1.4 (shown with a dotted line in Fig. 10).…”

Section: Scaling Relations Involving Other Parametersmentioning

confidence: 99%

Scaling relations for globular cluster systems in early-type galaxies. II. Is there an environmental dependence?

De Bortoli,

Caso,

Ennis

et al. 2022

Preprint

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The current properties of globular cluster systems (GCSs) are the result of the evolution experienced by their host galaxies, which shape the richness of the GCS as well as its spatial distribution, among other features. We carry out an analysis of the projected radial distribution of globular clusters for a sample of almost 30 early-type galaxies (ETGs) of intermediate and low luminosity, located in cluster environments (Virgo, Fornax and Coma). We also include in the study six ETGs, for which the parameters of their GCS radial profiles are publicly available. The final analysis is performed on an enlarged sample (∼ 100 GCSs), by adding the GCSs of ETGs from our previous paper (Paper I). Scaling relations involving different parameters of the GCSs are obtained for the whole sample and complement those obtained in Paper I. Several of such relations point to a second-order dependence on the environmental density. Finally, the results are analysed in the literature context.

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The galaxy size–halo mass scaling relations and clustering properties of central and satellite galaxies

Cited by 24 publications

References 134 publications

Mimicking the halo-galaxy connection using machine learning

Mimicking the halo-galaxy connection using machine learning

How galaxies populate halos in extreme density environments: An analysis of the halo occupation distribution in SDSS

Scaling relations for globular cluster systems in early-type galaxies. II. Is there an environmental dependence?

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