The stellar mass Fundamental Plane: the virial relation and a very thin plane for slow rotators

Bernardi, Mariangela; Sánchez, H. Domínguez; Margalef-Bentabol, Berta; Nikakhtar, Farnik; Sheth, Ravi K.

doi:10.1093/mnras/staa1064

Cited by 25 publications

(23 citation statements)

References 40 publications

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“…The deflectors in the quasar lenses with measured time delays of the TDCOSMO sample are massive elliptical galaxies. These galaxies, observationally, follow a tight relation in a luminosity, size and velocity dispersion parameter space (e.g., Faber & Jackson 1976;Auger et al 2010;Bernardi et al 2020), exhibiting a high degree of self-similarity among the population.…”

Section: Deflector Lens Modelmentioning

confidence: 99%

Tdcosmo

Birrer

Shajib

Galan

et al. 2020

A&A

304

184

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The H0LiCOW collaboration inferred via strong gravitational lensing time delays a Hubble constant value of H0 = 73.3−1.8+1.7 km s−1 Mpc−1, describing deflector mass density profiles by either a power-law or stars (constant mass-to-light ratio) plus standard dark matter halos. The mass-sheet transform (MST) that leaves the lensing observables unchanged is considered the dominant source of residual uncertainty in H0. We quantify any potential effect of the MST with a flexible family of mass models, which directly encodes it, and they are hence maximally degenerate with H0. Our calculation is based on a new hierarchical Bayesian approach in which the MST is only constrained by stellar kinematics. The approach is validated on mock lenses, which are generated from hydrodynamic simulations. We first applied the inference to the TDCOSMO sample of seven lenses, six of which are from H0LiCOW, and measured H0 = 74.5−6.1+5.6 km s−1 Mpc−1. Secondly, in order to further constrain the deflector mass density profiles, we added imaging and spectroscopy for a set of 33 strong gravitational lenses from the Sloan Lens ACS (SLACS) sample. For nine of the 33 SLAC lenses, we used resolved kinematics to constrain the stellar anisotropy. From the joint hierarchical analysis of the TDCOSMO+SLACS sample, we measured H0 = 67.4−3.2+4.1 km s−1 Mpc−1. This measurement assumes that the TDCOSMO and SLACS galaxies are drawn from the same parent population. The blind H0LiCOW, TDCOSMO-only and TDCOSMO+SLACS analyses are in mutual statistical agreement. The TDCOSMO+SLACS analysis prefers marginally shallower mass profiles than H0LiCOW or TDCOSMO-only. Without relying on the form of the mass density profile used by H0LiCOW, we achieve a ∼5% measurement of H0. While our new hierarchical analysis does not statistically invalidate the mass profile assumptions by H0LiCOW – and thus the H0 measurement relying on them – it demonstrates the importance of understanding the mass density profile of elliptical galaxies. The uncertainties on H0 derived in this paper can be reduced by physical or observational priors on the form of the mass profile, or by additional data.

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Section: Deflector Lens Modelmentioning

confidence: 99%

Tdcosmo

Birrer

Shajib

Galan

et al. 2020

A&A

304

184

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“…Choosing 'slow' or 'fast rotators' should in principle yield samples with systematically low or high R e /R crit . This may explain the systematic differences in the FP of slow versus fast rotators reported by Bernardi et al (2020). We plan to address this issue more directly, and with an enhanced observational sample, in future work.…”

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confidence: 95%

A unified scenario for the origin of spiral and elliptical galaxy structural scaling laws

Ferrero

Navarro

Abadi

et al. 2021

A&A

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Elliptical (E) and spiral (S) galaxies follow tight, but different, scaling laws that link their stellar masses, radii, and characteristic velocities. Mass and velocity, for example, scale tightly in spirals with little dependence on galaxy radius (the ‘Tully-Fisher relation’; TFR). On the other hand, ellipticals appear to trace a 2D surface in size-mass-velocity space (the ‘Fundamental Plane’; FP). Over the years, a number of studies have attempted to understand these empirical relations, usually in terms of variations of the virial theorem for E galaxies and in terms of the scaling relations of dark matter halos for spirals. We use Lambda cold dark matter (ΛCDM) cosmological hydrodynamical simulations to show that the scaling relations of both ellipticals and spirals arise as the result of (i) a tight galaxy mass–dark halo mass relation and (ii) the self-similar mass profile of cold dark matter halos. In this interpretation, E and S galaxies of a given stellar mass inhabit halos of similar masses, and their different scaling laws result from the varying amounts of dark matter enclosed within their luminous radii. This scenario suggests a new galaxy distance indicator applicable to galaxies of all morphologies and provides simple and intuitive explanations for long-standing puzzles, such as why the TFR is independent of surface brightness, or what causes the ‘tilt’ in the FP. Our results provide strong support for the predictions of ΛCDM in the strongly non-linear regime, as well as guidance for further improvements to cosmological simulations of galaxy formation.

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“…Section 4 compares our low-z analysis with estimates at higher z, and a final section summarizes. Although we concentrate on the size-mass correlation, an understanding of how Re, * /Re evolves also impacts studies of the evolution of the stellar mass Fundamental Plane (Bernardi et al 2020;de Graaff et al 2021). We leave this to future work.…”

Section: Introductionmentioning

confidence: 99%

The half mass radius of MaNGA galaxies: Effect of IMF gradients

Bernardi¹,

Sheth²,

Sánchez³

et al. 2022

Preprint

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Gradients in the stellar populations of galaxies -e.g., in age, metallicity, IMF -can result in gradients in the stellar mass to light ratio, M * /L. Such gradients imply that the distribution of the stellar mass and light are different. For old stellar populations, such as those typical of early-type galaxies at z ∼ 0, the M * /L gradients are weak if driven by variations in age and metallicity. However, if they are driven by variations in the stellar Initial Mass Function (IMF), then they can be significantly larger. An IMF-driven gradient which has M * /L decreasing outwards from the center increases the estimated total stellar mass (M * ) and reduces the scale which contains half this mass (R e, * ), compared to the values of mass and size when the gradient is ignored. We estimate IMF-gradients from spatially resolved spectra of early-type galaxies in the final release of the MaNGA survey, showing that the fractional decrease in R e, * can be significantly larger than the fractional M * increase, especially when the light is more centrally concentrated. The R e, * −M * correlation which results from the IMF-driven M * /L gradients at z ∼ 0 is offset by almost 0.3 dex to smaller sizes compared to when these gradients are ignored. Comparison with higher redshift samples is not straightforward. If it is fair to compare z ∼ 0 'early-type' galaxies with 'quiescent' galaxies at higher-z, then one must be able to consistently account for evolution in stellar population gradients (especially age and IMF) as well as changes in the steepness of the light profile before drawing conclusions about the evolution of the R e, * − M * relation.

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The stellar mass Fundamental Plane: the virial relation and a very thin plane for slow rotators

Cited by 25 publications

References 40 publications

Tdcosmo

Tdcosmo

A unified scenario for the origin of spiral and elliptical galaxy structural scaling laws

The half mass radius of MaNGA galaxies: Effect of IMF gradients

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