Scaling Properties of Galaxy Groups

Lovisari, Lorenzo; Ettori, S.; Gaspari, M.; Giles, Paul

doi:10.3390/universe7050139

Cited by 73 publications

(52 citation statements)

References 247 publications

(470 reference statements)

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“…X relation observed for groups (Helsdon & Ponman, 2000) relative to clusters (White et al, 1997) indicated a significant deviation from the L X ∝ T 2 X relationship expected for virialized gaseous halos retaining all their baryons in hydrostatic equilibrium (e.g., Balogh et al (1999), see companion review by Lovisari et al (2021)).…”

Section: The Baryonic Content Of Group Halosmentioning

confidence: 82%

“…The IGrM is mainly very hot (T ∼ 10 7 K), but does not primarily radiate via Bremsstrahlung radiation like the intracluster medium (ICM; see Figure 1 of the companion review by Lovisari et al (2021)). Cooling via line emission offers a greater opportunity to form multi-phase, cool (T < 10 5 K) gas, and potentially provide additional fuel to galaxies.…”

Section: Introductionmentioning

confidence: 99%

“…The relationship between the central SMBH and properties of the IGrM/ICM/CGM: The strong correlations between the mass of the central SMBH in a group (M SMBH ) and the temperature and X-ray luminosity (T X and L X ) of the IGrM/ICM (Gaspari et al, 2019;Bogdán et al, 2018), provide fundamental tests of AGN feedback in simulations (see also Section 4 of the companion review by Lovisari et al (2021)). On the one hand, the M SMBH scaling with M halo , assuming T X measures M halo , is a natural expectation of the SMBH growth being controlled by the binding energy of the halo .…”

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confidence: 99%

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Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

et al. 2021

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Galaxy groups are more than an intermediate scale between clusters and halos hosting individual galaxies, they are crucial laboratories capable of testing a range of astrophysics from how galaxies form and evolve to large scale structure (LSS) statistics for cosmology. Cosmological hydrodynamic simulations of groups on various scales offer an unparalleled testing ground for astrophysical theories. Widely used cosmological simulations with ∼(100 Mpc)3 volumes contain statistical samples of groups that provide important tests of galaxy evolution influenced by environmental processes. Larger volumes capable of reproducing LSS while following the redistribution of baryons by cooling and feedback are the essential tools necessary to constrain cosmological parameters. Higher resolution simulations can currently model satellite interactions, the processing of cool (T≈104−5 K) multi-phase gas, and non-thermal physics including turbulence, magnetic fields and cosmic ray transport. We review simulation results regarding the gas and stellar contents of groups, cooling flows and the relation to the central galaxy, the formation and processing of multi-phase gas, satellite interactions with the intragroup medium, and the impact of groups for cosmological parameter estimation. Cosmological simulations provide evolutionarily consistent predictions of these observationally difficult-to-define objects, and have untapped potential to accurately model their gaseous, stellar and dark matter distributions.

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Section: The Baryonic Content Of Group Halosmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

et al. 2021

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“…It can be seen that both types of objects are found in the same, tight, correlation. We won't enter in a detailed discussion of purely X-ray relations and their meaning, we refer the reader to the companion review by Lovisari et al (2021) for a description of X-ray scaling relations in galaxy groups. The result presented in the left panel of Fig.…”

Section: Global Scaling Relationsmentioning

confidence: 99%

Properties of Fossil Groups of Galaxies

Aguerri

Zarattini

2021

Universe

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We review the formation and evolution of fossil groups and clusters from both the theoretical and the observational points of view. In the optical band, these systems are dominated by the light of the central galaxy. They were interpreted as old systems that had enough time to merge all the M* galaxies within the central one. During the last two decades, many observational studies were performed to prove the old and relaxed state of fossil systems. The majority of these studies that spans a wide range of topics including halos global scaling relations, dynamical substructures, stellar populations, and galaxy luminosity functions seem to challenge this scenario. The general picture that can be obtained by reviewing all the observational works is that the fossil state could be transitional. Indeed, the formation of the large magnitude gap observed in fossil systems could be related to internal processes rather than an old formation.

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“…They are an important laboratory to study how different baryonic processes shape the properties of galaxies that reside in these galaxy groups (McCarthy et al 2010;Le Brun et al 2014;Gu et al 2020). Scaling relations between the observable properties of galaxy groups such as their total group luminosity or group velocity dispersion with the halo mass are crucial to develop a phenomenological understanding of galaxy formation within groups (see e.g., Yang et al 2003;Eke et al 2004b;Yang et al 2007;Sheldon et al 2009;Eckmiller et al 2011;Han et al 2015;Viola et al 2015;Lovisari et al 2020Lovisari et al , 2021Gonzalez et al 2021;Yang et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

Rana,

More,

Miyatake

et al. 2021

Preprint

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We utilize the galaxy shape catalogue from the first year data release of the Subaru Hyper Suprime-cam Survey (HSC) to study the dark matter content of galaxy groups in the Universe using weak gravitational lensing. As our lens sample, we use galaxy groups that have been spectroscopically selected from the Galaxy Mass and Assembly (GAMA) galaxy survey in approximately 100 sq. degrees of the sky that overlap with the HSC survey. We restrict our analysis to the 1587 groups with at least five group members. We divide these galaxy groups into six bins each of galaxy group luminosity and group member velocity dispersion and measure the coherent tangential ellipticity pattern on background HSC galaxies imprinted by weak gravitational lensing. We measure the weak lensing signal with a total signal-to-noise ratio of 55 and 51 for these two different selections, respectively. We use a Bayesian halo model framework to infer the halo mass distribution of our galaxy groups binned in the two different observable properties and obtain constraints on the power law scaling relation between mean halo masses and the two group observable properties. We obtain a 5 percent constraint on the amplitude of the scaling relation between halo mass and group luminosity with 𝑀 = (0.81 ± 0.04) × 10 14 ℎ −1 𝑀 for 𝐿 grp = 10 11.5 ℎ −2 𝐿 , and a power law index of 𝛼 = 1.01 ± 0.07. We also obtain a 5 percent constraint on the amplitude of the scaling relation between halo mass and velocity dispersion with 𝑀 = (0.93 ± 0.05) × 10 14 ℎ −1 𝑀 for 𝜎 = 500km s −1 and a power law index 𝛼 = 1.52 ± 0.10, although these scaling relations are sensitive to the exact cuts applied to the number of group members. Comparisons with similar scaling relations from the literature indicate that our results are consistent, but have significantly reduced errors.

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Scaling Properties of Galaxy Groups

Cited by 73 publications

References 247 publications

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

Properties of Fossil Groups of Galaxies

The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

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