Baryon effects on the dark matter haloes constrained from strong gravitational lensing

Wang, Lin; Chen, Daming; Li, Ran

doi:10.1093/mnras/stx1617

Cited by 6 publications

(4 citation statements)

References 85 publications

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“…These processes include gas accretion, minor mergers, disc dynamics, halo heating, stellar feedback and AGN feedback. The above are typically dependent on galaxy stellar mass and cosmic epoch (Cano-Díaz et al 2016;Abbott et al 2017;Wang et al 2017;Chiosi et al 2017;García et al 2017;Eales et al 2018;Qin et al 2018;Sánchez et al 2018;Cañas et al 2018;Blanc et al 2019) and possibly affect the shape of the σ sSFR -M ⋆ differently. However, it is difficult to study and especially quantify the effect of the different prescriptions important for galaxy evolution to the scatter solely by using insights from observations.…”

Section: Introductionmentioning

confidence: 99%

An Evolving and Mass-dependent σsSFR–M_⋆ Relation for Galaxies

Katsianis

Zheng

González

et al. 2019

ApJ

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The scatter (σ sSFR ) of the specific star formation rates (sSFRs) of galaxies is a measure of the diversity in their star formation histories (SFHs) at a given mass. In this paper we employ the EAGLE simulations to study the dependence of the σ sSFR of galaxies on stellar mass (M ⋆ ) through the σ sSFR -M ⋆ relation in z ∼ 0 − 4. We find that the relation evolves with time, with the dispersion depending on both stellar mass and redshift. The models point to an evolving U-shape form for the σ sSFR -M ⋆ relation with the scatter being minimal at a characteristic mass M ⋆ of 10 9.5 M ⊙ and increasing both at lower and higher masses. This implication is that the diversity of SFHs increases towards both at the low-and high-mass ends. We find that active galactic nuclei feedback is important for increasing the σ sSFR for high mass objects. On the other hand, we suggest that SNe feedback increases the σ sSFR of galaxies at the low-mass end. We also find that excluding galaxies that have experienced recent mergers does not significantly affect the σ sSFR -M ⋆ relation. Furthermore, we employ the combination of the EAGLE simulations with the radiative transfer code SKIRT to evaluate the effect of SFR/stellar mass diagnostics in the σ sSFR -M ⋆ relation and find that the SFR/M ⋆ methodologies (e.g. SED fitting, UV+IR, UV+IRX-β) widely used in the literature to obtain intrinsic properties of galaxies have a large effect on the derived shape and normalization of the σ sSFR -M ⋆ relation.

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Section: Introductionmentioning

confidence: 99%

An Evolving and Mass-dependent σsSFR–M_⋆ Relation for Galaxies

Katsianis

Zheng

González

et al. 2019

ApJ

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“…However, we do note that this study was based on the simulations of four elliptical galaxies that do not represent the entire population. Moreover, there are known inconsistencies between simulated and observed galaxies (Xu et al 2017;Wang et al 2017;Peirani et al 2019), particularly in the core where time delays are sensitive. As such, if this method is to be competitive going forward in to the era of sub 2% estimates on H0, then we will require not only more accurate simulations, but an understanding of the time delay distributions over a larger population than just four volumes.…”

Section: Discussionmentioning

confidence: 99%

“…We return a consistent lens redshift distribution and the estimated masses are both within the expected true mass, and that the model is not particularly sensitive to this parameter. However, we note that there is debate on the reliability of such simulations at reproducing the properties of galaxies, which may impact these results (Xu et al 2017;Wang et al 2017;Peirani et al 2019).…”

Section: Modelmentioning

confidence: 97%

A 4% measurement of $H_0$ using the cumulative distribution of strong-lensing time delays in doubly-imaged quasars

Harvey

2020

Preprint

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In the advent of large scale surveys, individually modelling strong-gravitational lenses and their counterpart time-delays in order to precisely measure H 0 will become computationally expensive, and highly complex. A complimentary approach is to study the cumulative distribution function (CDF) of time-delays where the global population of lenses is modelled along with H 0 . In this paper we use a suite of hydro-dynamical simulations to estimate the CDF of time-delays from doubly-imaged quasars for a realistic distribution of lenses. We find that the CDFs exhibit large amounts of halohalo variance, regulated by the density profile inner slope and the total mass within 5kpc. With the objective of fitting to data, we compress the CDFs using Principal Component Analysis and fit a Gaussian Processes Regressor consisting of three physical features: the redshift of the lens, z L ; the power law index of the halo, α, and the mass within 5kpc, plus four cosmological features. Assuming a flat Universe, we fit our model to 27 doubly-imaged quasars finding Hand Ω Λ = 0.7 +0.04 −0.04 . We compare our estimates of z L and log(M (< 5kpc)/M ) to the data and find that within the sensitivity of the data, they are not systematically biased. We generate mock CDFs and find with that the Vera Rubin Observatory (VRO) could measure σ/H 0 to < 3%, limited by the precision of the model. If we are to exploit fully VRO, we require simulations that sample a larger proportion of the lens population, with a variety of feedback models, exploring all possible systematics.

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“…First of all, in spite of its larger flexibility compared to more simple lens models, it still allows for most of the interesting properties for lensing studies to be calculated fully analytically, as demonstrated by Du et al (2020). Secondly, contrary to most of the other popular analytical mass models used in lensing, the BPL model has the same global characteristics as the Zhao models, often used to model dark matter haloes (Navarro et al 1997;Hague & Wilkinson 2013Di Cintio et al 2014;Mollitor et al 2015;Tollet et al 2016;Allaert et al 2017;Dekel et al 2017;Wang et al 2017;Katz et al 2017;Cautun et al 2020;Freundlich et al 2020b;Hayashi et al 2020). The fact that the BPL models cannot be supported by an isotropic (or radially anisotropic) distribution function limits the attractiveness of this family of models to some degree.…”

Section: Data Availabilitymentioning

confidence: 99%

The dynamical structure of broken power-law and double power-law models for dark matter haloes

Baes,

Camps

2021

Preprint

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Galaxy kinematics and gravitational lensing are two complementary ways to constrain the distribution of dark matter on galaxy scales. The typical dark matter density profiles adopted in dynamical studies cannot easily be adopted in lensing studies. Ideally, a mass model should be used that has the global characteristics of realistic dark matter distributions, and that allows for an analytical calculation of the magnifications and deflection angles. A simple model with these properties, the broken-power-law (BPL) model, has very recently been introduced. We examine the dynamical structure of the family of BPL models. We derive simple closed expressions for basic dynamical properties, and study the distribution function under the assumption of velocity isotropy. We find that none of the BPL models with realistic parameters has an isotropic distribution function that is positive over the entire phase space, implying that the BPL models cannot be supported by an isotropic velocity distribution, or models with a more radially anisotropic orbital structure. This result limits the attractiveness of the BPL family as a tool for lensing studies to some degree. More generally, we find that not all members of the general family of double power-law or Zhao models, often used to model dark matter haloes, can be supported by an isotropic or radially anisotropic distribution function. In other words, the distribution function may become negative even for spherically symmetric models with a well-behaved density profile.

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Baryon effects on the dark matter haloes constrained from strong gravitational lensing

Cited by 6 publications

References 85 publications

An Evolving and Mass-dependent σsSFR–M_⋆ Relation for Galaxies

An Evolving and Mass-dependent σsSFR–M_⋆ Relation for Galaxies

A 4% measurement of $H_0$ using the cumulative distribution of strong-lensing time delays in doubly-imaged quasars

The dynamical structure of broken power-law and double power-law models for dark matter haloes

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Baryon effects on the dark matter haloes constrained from strong gravitational lensing

Cited by 6 publications

References 85 publications

An Evolving and Mass-dependent σsSFR–M⋆ Relation for Galaxies

An Evolving and Mass-dependent σsSFR–M⋆ Relation for Galaxies

A 4% measurement of $H_0$ using the cumulative distribution of strong-lensing time delays in doubly-imaged quasars

The dynamical structure of broken power-law and double power-law models for dark matter haloes

Contact Info

Product

Resources

About

An Evolving and Mass-dependent σsSFR–M_⋆ Relation for Galaxies

An Evolving and Mass-dependent σsSFR–M_⋆ Relation for Galaxies