Intrinsic alignments of the extended radio continuum emission of galaxies in the EAGLE simulations

Hill, Alexander D.; Crain, Robert A.; McCarthy, Ian G.; Brown, S F

doi:10.1093/mnras/stac304

Cited by 3 publications

(16 citation statements)

References 122 publications

(156 reference statements)

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“…The DM and stellar distributions show the closest alignment with a median difference of ∼ 8-9 degrees at the two radial distances considered (also see fig. 13 in Hill et al 2021). GCs are more aligned with the stellar than with the DM distribution of their host halo, although the median misalignment angles among all components only differ by ∼ 2-3 degrees.…”

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confidence: 90%

“…We do so by modelling the projected spatial distributions (as described by the particles) with ellipses. We follow the methods outlined by Thob et al (2019) and Hill et al (2021Hill et al ( , 2022 5 , which we summarize below.…”

Section: Projected Morphology Of Dm Stars and Gcsmentioning

confidence: 99%

“…Previous studies have already found that galaxies in the EAGLE simulations are well aligned with the local mass distribution, but are often misaligned with respect to the global halo. This indicates that the stellar component traces the local DM distribution, which is the dominant matter component, and that the structure of the DM halo changes from the inner to the outer halo (Velliscig et al 2015a;Hill et al 2021).…”

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confidence: 93%

“…from the Euclid and Rubin observatories). Using the EAGLE simulations, the stellar component of galaxies is found to be well aligned with the local mass distribution, but is often misaligned significantly with respect to the global halo (Velliscig et al 2015a;Hill et al 2021). This indicates that stars follow the local DM distribution, and that the orientation of the DM distribution changes from the inner to the outer halo.…”

Section: Introductionmentioning

confidence: 99%

“…see fig. 7 of Hill et al 2021). We have also examined the ellipticities and the misalignment for different galaxy stellar mass bins, but no trends could be identified.…”

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confidence: 99%

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Constraining the shape of dark matter haloes with globular clusters

Reina-Campos¹,

Trujillo-Gomez²,

Pfeffer³

et al. 2022

Preprint

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We explore how diffuse stellar light and globular clusters (GCs) can be used to trace the matter distribution of their host halo using an observational methodology. For this, we use 117 simulated dark matter (DM) haloes from the (34.4 cMpc) 3 periodic volume of the E-MOSAICS project. For each halo, we compare the stellar surface brightness and GC projected number density maps to the surface densities of DM and total mass. We find that the dominant structures identified in the stellar light and in the GCs correspond closely with those from the DM and total mass. Our method is unaffected by the presence of satellites and its precision improves with fainter GC samples. We recover tight relations between the profiles of stellar surface brightness and GC number density to those of the DM, suggesting that the profile of DM can be accurately recovered from the stars and GCs (𝜎 ≤ 0.5 dex). We quantify the projected morphology of DM, stars and GCs, and find that the stars and GCs are more flattened than the DM. Additionally, the semi-major axes of the distribution of stars and GCs are typically misaligned by ∼ 10 degrees from that of DM. We demonstrate that deep imaging of diffuse stellar light and GCs can place constraints on the shape, profile and orientation of their host halo. These results extend down to haloes with central galaxies 𝑀 ★ ≥ 10 10 M , and the analysis will be applicable to future data from the Euclid, Roman and the Rubin observatories

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confidence: 90%

Section: Projected Morphology Of Dm Stars and Gcsmentioning

confidence: 99%

mentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

“…see fig. 7 of Hill et al 2021). We have also examined the ellipticities and the misalignment for different galaxy stellar mass bins, but no trends could be identified.…”

mentioning

confidence: 99%

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Constraining the shape of dark matter haloes with globular clusters

Reina-Campos¹,

Trujillo-Gomez²,

Pfeffer³

et al. 2022

Preprint

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Intrinsic alignments of bulges and discs

Jagvaral

Singh

Mandelbaum

2022

Monthly Notices of the Royal Astronomical Society

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Galaxies exhibit coherent alignments with local structure in the Universe. This effect, called Intrinsic Alignments (IA), is an important contributor to the systematic uncertainties for wide-field weak lensing surveys. On cosmological distance scales, intrinsic shape alignments have been observed in red galaxies, which are usually bulge-dominated; while blue galaxies, which are mostly disc-dominated, exhibit shape alignments consistent with a null detection. However, disc-dominated galaxies typically consist of two prominent structures: disc and bulge. Since the bulge component has similar properties as elliptical galaxies and is thought to have formed in a similar fashion, naturally one could ask whether the bulge components exhibit similar alignments as ellipticals? In this paper, we investigate how different components of galaxies exhibit IA in the TNG100-1 cosmological hydrodynamical simulation, as well as the dependence of IA on the fraction of stars in rotation-dominated structures at z = 0. The measurements were controlled for mass differences between the samples. We find that the bulges exhibit significantly higher IA signals, with a nonlinear alignment model amplitude of $A_I = 2.98^{+0.36}_{-0.37}$ compared to the amplitude for the galaxies as a whole (both components), $A_I = 1.13^{+0.37}_{-0.35}$. The results for bulges are statistically consistent with those for elliptical galaxies, which have $A_I = 3.47^{+0.57}_{-0.57}$. These results highlight the importance of studying galaxy dynamics in order to understand galaxy alignments and their cosmological implications.

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Constraining the shape of dark matter haloes with globular clusters and diffuse stellar light in the E-MOSAICS simulations

Reina-Campos

Trujillo-Gomez

Pfeffer

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We explore how diffuse stellar light and globular clusters (GCs) can be used to trace the matter distribution of their host halo using an observational methodology. For this, we use 117 simulated dark matter (DM) haloes from the $(34.4~\rm cMpc)^3$ periodic volume of the e-mosaics project. For each halo, we compare the stellar surface brightness and GC projected number density maps to the surface density of DM. We find that the dominant structures identified in the stellar light and in the GCs correspond closely with those from the DM. Our method is unaffected by the presence of satellites and its precision improves with fainter GC samples. We recover tight relations between the dimensionless profiles of stellar-to-DM surface density and GC-to-DM surface density, suggesting that the profile of DM can be accurately recovered from the stars and GCs (σ ≤ 0.5 dex). We quantify the projected morphology of DM, stars and GCs, and find that the stars and GCs are more flattened than the DM. Additionally, the semi-major axes of the distribution of stars and GCs are typically misaligned by ∼10 degrees from that of DM. We demonstrate that deep imaging of diffuse stellar light and GCs can place constraints on the shape, profile and orientation of their host halo. These results extend down to haloes with central galaxies M⋆ ≥ 1010 M⊙, and the analysis will be applicable to future data from the Euclid, Roman and the Rubin observatories

show abstract

Intrinsic alignments of the extended radio continuum emission of galaxies in the EAGLE simulations

Cited by 3 publications

References 122 publications

Constraining the shape of dark matter haloes with globular clusters

Constraining the shape of dark matter haloes with globular clusters

Intrinsic alignments of bulges and discs

Constraining the shape of dark matter haloes with globular clusters and diffuse stellar light in the E-MOSAICS simulations

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