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Shape, alignment, and mass distribution of baryonic and dark-matter halos in one EAGLE simulation

hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorPETIT, Q.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorDUCOURANT, C.
hal.structure.identifierJoseph Louis LAGRANGE [LAGRANGE]
dc.contributor.authorSLEZAK, E.
dc.contributor.authorSLUSE, D.
dc.contributor.authorDELCHAMBRE, L.
dc.date.issued2023
dc.identifier.issn0004-6361
dc.description.abstractEnAccurate knowledge of the morphology of halos and its evolution are key constraints on the galaxy formation model as well as a determinant parameter of the strong-lensing phenomenon. Using the cosmological hydrodynamic simulation, the Evolution and Assembly of GaLaxies and their Environments (EAGLE), we aim to provide a comprehensive analysis of the evolution of the morphology of galaxy halos and of their mass distributions with a focus on the snapshot at redshift $z=0.5$. We developed an iterative strategy involving a principal component analysis (PCA) to investigate the properties of the EAGLE halos and the differences in alignment between the various components. The mass distributions of the dark-matter (DM), gas, and star halos are characterised by a half-mass radius, a concentration parameter and (projected) axis ratios. We present statistics of the shape parameters of 336 540 halos from the EAGLE RefL0025N0376 simulation and describe their evolution from redshift $z=15$ to $z=0$. We measured the three-dimensional and two-dimensional projected shape parameters for the DM, the gas, and the star components as well as for all particles. At $z=0.5$, the minor axis of gas aligns with the minor axis of DM for massive halos ($M>10^{12}$ M$_\odot$), but this alignment is poorer for less massive halos. The DM halos axis ratios $b/a$ and $c/a$ have median values of $0.82 \pm 0.11$ and $0.64 \pm 0.12$, respectively. The sphericity of gas in halos w/ and w/o stars appears to be negatively correlated to the total mass, while the sphericity of DM is insensitive to it. The measured projected axis ratios, $b_p/a_p$, of star halos at $z=0.5$ have a median value of $0.80 \pm 0.07$, which is in good agreement with ground-based and space-based measurements within 1 $\sigma$. For DM halos, we measure a value of $0.85 \pm 0.06$.
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.subject.enmethods: numerical
dc.subject.enGalaxy: halo
dc.subject.endark matter
dc.subject.engravitational lensing: strong
dc.title.enShape, alignment, and mass distribution of baryonic and dark-matter halos in one EAGLE simulation
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202244920
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv2212.08880
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA132
bordeaux.volume669
bordeaux.peerReviewedoui
hal.identifierhal-03930907
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-03930907v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2023&rft.volume=669&rft.spage=A132&rft.epage=A132&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=PETIT,%20Q.&DUCOURANT,%20C.&SLEZAK,%20E.&SLUSE,%20D.&DELCHAMBRE,%20L.&rft.genre=article


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