Tomography of the Ie-Re and L-Sigma Planes

D’Onofrio, M.; Chiosi, C.

doi:10.3390/universe8010008

Cited by 4 publications

(5 citation statements)

References 85 publications

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“…This happens because several objects have large negative β values. As we show below, both positive and negative values of β are possible and, as demonstrated by D'Onofrio & Chiosi (2021), this is a necessary condition for reproducing the L − σ distribution starting from the I e − R e distribution (and vice versa).…”

Section: The Ssrs At High Redshiftmentioning

confidence: 64%

“…The aim of this paper is to show that combining VT with the L = L 0 σ β relation (which is a proxy for evolution, in which β and L 0 vary from galaxy to galaxy and over the course of time) has many positive consequences (see D 'Onofrio et al 2017'Onofrio et al , 2019'Onofrio et al , 2020D'Onofrio & Chiosi 2021, for earlier studies along this line of thought). The variation of β and L 0 with time traces the path followed by each galaxy in the various SSRs.…”

Section: Discussionmentioning

confidence: 99%

“…In previous papers on this subject, we brought attention to some of the advantages offered by the joint use of the VT and the L = L 0 (t)σ β(t) law (D'Onofrio et al 2017(D'Onofrio et al , 2019(D'Onofrio et al , 2020D'Onofrio & Chiosi 2021, 2022. Accepting the idea of a variable β parameter, which can take either positive or negative values, yields a simple explanation for the shifts of galaxies along the SSRs.…”

Section: Introductionmentioning

confidence: 99%

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The scaling relations of galaxies back in time: The road toward virialization

D’Onofrio¹,

Chiosi²

2023

A&A

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Context. The structural scaling relations (SSRs) of galaxies, that is, the observed correlations between effective radius, effective surface intensity, and velocity dispersion, are important tools for understanding how evolution proceeds. Aims. In this paper, we aim to demonstrate that the evolution of the SSRs back in time is governed by a combination of virial theorem (VT) and the relation L = L0′(t)σβ(t), where the parameters β and L0′ vary with time and from galaxy to galaxy. Methods. Using the WINGS database for the galaxies at redshift z = 0 and the Illustris-1 and IllustrisTNG databases of artificial galaxies, for the galaxies up to redshift z = 4, we analyse the SSRs back in time and, by means of simple algebraic expressions for L0′ and β (functions of time and other physical quantities), we derive the expected paths followed by galaxies in the various SSRs toward the distributions observed at z = 0. Results. The distribution of galaxies in the SSRs is ultimately related to the evolution in luminosity and velocity dispersion, which are empirically mirrored by the L = L0′(t)σβ(t) law. Furthermore, the β parameter works as a thermometer of the virialization of a galaxy. This parameter can assume either positive or negative values, and its absolute value attains high values when the galaxy is close to the virial condition, while it tends to zero when the galaxy is far from this condition. Conclusions. As the SSRs change with time, the method proposed in this paper allows us to decipher the temporal evolution of galaxies.

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Section: The Ssrs At High Redshiftmentioning

confidence: 64%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The scaling relations of galaxies back in time: The road toward virialization

D’Onofrio¹,

Chiosi²

2023

A&A

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“…The aim of this paper is to prove that the difficulties encountered in understanding the distribution of galaxies on the FP in the parameter space σ, R e I e , and its projections on the three coordinate planes, can be removed by introducing the L = L 0 σ β relation as a proxy of evolution, in which β and L 0 vary from galaxy to galaxy and for each of them in the course of time (see D 'Onofrio et al 2017a'Onofrio et al , 2019'Onofrio et al , 2020D'Onofrio & Chiosi 2021, for previous efforts along this line of thought). The continuous variation in β and L 0 traces the path followed by each ETG in the L − σ plane.…”

Section: Discussionmentioning

confidence: 99%

“…In our previous works we tried to highlight some of the advantages offered by coupling the VT with the L = L 0 σ β law. The first efforts were dedicated to understanding the origin of the fundamental plane (FP) of ETGs and the distributions observed in its 2D projections (D 'Onofrio et al 2017a'Onofrio et al , 2019'Onofrio et al , 2020D'Onofrio & Chiosi 2021). While discussing these problems, D 'Onofrio et al (2017b) and D 'Onofrio & Chiosi (2022) advanced the idea that the explanation invoked for the origin of the FP tilt (and its small scatter) should also account for the observed distributions of galaxies in all the 2D projections of the FP.…”

Section: Introductionmentioning

confidence: 99%

A new framework for understanding the evolution of early-type galaxies

D'Onofrio¹,

Chiosi²

2023

A&A

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Context. We have recently suggested that the combination of the scalar virial theorem (M s ∝ R e σ 2 ) and the L = L 0 σ β law, with L 0 and β changing from galaxy to galaxy (and with time), can provide a new set of equations valid for investigating the evolution of early-type galaxies. These equations are able to account for the tilt of the fundamental plane and to explain the observed distributions of early-type galaxies in all its projections. Aims. In this paper we analyze the advantages offered by these equations, derive the β and L 0 parameters for real and simulated galaxies, and demonstrate that depending on the value of β galaxies can move only along some permitted directions in the fundamental plane projections. Then we show that simple galaxy models that grow in mass by infall of gas and form stars with a star formation rate depending on the stellar velocity dispersion nicely reproduce the observed distributions of early-type galaxies in the fundamental plane projections and yield βs that agree with the measured values. Methods. We derive the mutual relationships among the stellar mass, effective radius, velocity dispersion, and luminosity of earlytype galaxies as a function of β and calculate the coefficients of the fundamental plane. Then, using the simple infall models, we show that the star formation history of early-type galaxies is compatible with the σ-dependent star formation rate, and that both positive and negative values of β are possible in a standard theory of galaxy evolution. Results. The parameter β(t) offers a new view of the evolution of early-type galaxies. In brief, it gives a coherent interpretation of the fundamental plane and of the motions of galaxies in its projections; it is the fingerprint of their evolution; it measures the degree of virialization of early-type galaxies; and finally it allows us to infer their evolution in the near past.Conclusions.

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Galaxies’ properties in the Fundamental Plane across time

D’Onofrio,

Chiosi

2024

A&A

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Using the Illustris-1 and IllustrisTNG-100 simulations, we investigate the properties of the Fundamental Plane (FP), which is the correlation between the effective radius the effective surface intensity and the central stellar velocity dispersion sigma of galaxies, at different cosmic epochs. Our aim is to study the properties of galaxies in the FP and its projections across time, adopting samples covering different intervals of mass. We would like to demonstrate that the position of a galaxy in the FP space strongly depends on its degree of evolution, which might be represented by the beta and $ L'_0$ parameters entering the law. Starting from the comparison of the basic relations among the structural parameters of artificial and real galaxies at low redshift, we obtain the fit of the FP and its coefficients at different cosmic epochs for samples of different mass limits. Then, we analyze the dependence of the galaxy position in the FP space as a function of the beta parameter and the star formation rate (SFR). We find that: 1) the coefficients of the FP change with the mass range of the galaxy sample; 2) the low luminous and less massive galaxies do not share the same FP of the bright massive galaxies; 3) the scatter around the fitted FP is quite small at any epoch and increases when the mass interval increases; 4) the distribution of galaxies in the FP space strongly depends on the beta values ( on the degree of virialization and the star formation rate). The FP is a complex surface that is well approximated by a plane only when galaxies share similar masses and condition of virialization.

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Tomography of the Ie-Re and L-Sigma Planes

Cited by 4 publications

References 85 publications

The scaling relations of galaxies back in time: The road toward virialization

The scaling relations of galaxies back in time: The road toward virialization

A new framework for understanding the evolution of early-type galaxies

Galaxies’ properties in the Fundamental Plane across time

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