The evolution of substructure in galaxy, group and cluster haloes — III. Comparison with simulations
Identifieur interne : 000276 ( Main/Exploration ); précédent : 000275; suivant : 000277The evolution of substructure in galaxy, group and cluster haloes — III. Comparison with simulations
Auteurs : James E. Taylor [États-Unis, Royaume-Uni] ; Arif Babul [Canada]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2005-12-01.
English descriptors
- KwdEn :
Abstract
In a previous paper, we described a new method for including detailed information about substructure in semi-analytic models of halo formation based on merger trees. In this paper, we compare the predictions of our model with results from self-consistent numerical simulations. We find that in general the two methods agree extremely well, particularly once numerical effects and selection effects in the choice of haloes are taken into account. As expected from the original analyses of the simulations, we see some evidence for artificial overmerging in the innermost regions of the simulated haloes, either because substructure is being disrupted artificially or because the group-finding algorithms used to identify substructure are not detecting all the bound clumps in the highest-density regions. Our analytic results suggest that greater mass and force resolution may be required before numerical overmerging becomes negligible in all current applications. We discuss the implications of this result for observational and experimental tests of halo substructure, such as the analysis of discrepant magnification ratios in strongly lensed systems, terrestrial experiments to detect dark matter particles directly or indirect detection experiments searching for positrons, gamma-rays, neutrinos or other dark matter decay or annihilation products.
Url:
DOI: 10.1111/j.1365-2966.2005.09581.x
Affiliations:
Links toward previous steps (curation, corpus...)
Le document en format XML
<record><TEI wicri:istexFullTextTei="biblStruct"><teiHeader><fileDesc><titleStmt><title>The evolution of substructure in galaxy, group and cluster haloes — III. Comparison with simulations</title><author><name sortKey="Taylor, James E" sort="Taylor, James E" uniqKey="Taylor J" first="James E." last="Taylor">James E. Taylor</name></author><author><name sortKey="Babul, Arif" sort="Babul, Arif" uniqKey="Babul A" first="Arif" last="Babul">Arif Babul</name></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:EE3CCC5CCD9534BF9F8A3C100625237086DC154D</idno><date when="2005" year="2005">2005</date><idno type="doi">10.1111/j.1365-2966.2005.09581.x</idno><idno type="url">https://api.istex.fr/document/EE3CCC5CCD9534BF9F8A3C100625237086DC154D/fulltext/pdf</idno><idno type="wicri:Area/Main/Corpus">000594</idno><idno type="wicri:Area/Main/Curation">000594</idno><idno type="wicri:Area/Main/Exploration">000276</idno><idno type="wicri:explorRef" wicri:stream="Main" wicri:step="Exploration">000276</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a">The evolution of substructure in galaxy, group and cluster haloes — III. Comparison with simulations</title><author><name sortKey="Taylor, James E" sort="Taylor, James E" uniqKey="Taylor J" first="James E." last="Taylor">James E. Taylor</name><affiliation></affiliation><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Caltech MC 105–24, 1200 East California Blvd., Pasadena, CA 91125</wicri:regionArea><wicri:noRegion>CA 91125</wicri:noRegion></affiliation><affiliation wicri:level="1"><country wicri:rule="url">Royaume-Uni</country></affiliation></author><author><name sortKey="Babul, Arif" sort="Babul, Arif" uniqKey="Babul A" first="Arif" last="Babul">Arif Babul</name><affiliation wicri:level="1"><country xml:lang="fr">Canada</country><wicri:regionArea>Elliott Building, 3800 Finnerty Road, Victoria, BC V8P 1A1</wicri:regionArea><wicri:noRegion>BC V8P 1A1</wicri:noRegion></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbrev">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><publisher>Blackwell Science Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2005-12-01">2005-12-01</date><biblScope unit="volume">364</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="535">535</biblScope><biblScope unit="page" to="551">551</biblScope></imprint><idno type="ISSN">0035-8711</idno></series><idno type="istex">EE3CCC5CCD9534BF9F8A3C100625237086DC154D</idno><idno type="DOI">10.1111/j.1365-2966.2005.09581.x</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>dark matter</term><term>galaxies: clusters: general</term><term>galaxies: formation</term><term>galaxies: haloes</term><term>gravitational lensing</term><term>methods: numerical</term></keywords></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract">In a previous paper, we described a new method for including detailed information about substructure in semi-analytic models of halo formation based on merger trees. In this paper, we compare the predictions of our model with results from self-consistent numerical simulations. We find that in general the two methods agree extremely well, particularly once numerical effects and selection effects in the choice of haloes are taken into account. As expected from the original analyses of the simulations, we see some evidence for artificial overmerging in the innermost regions of the simulated haloes, either because substructure is being disrupted artificially or because the group-finding algorithms used to identify substructure are not detecting all the bound clumps in the highest-density regions. Our analytic results suggest that greater mass and force resolution may be required before numerical overmerging becomes negligible in all current applications. We discuss the implications of this result for observational and experimental tests of halo substructure, such as the analysis of discrepant magnification ratios in strongly lensed systems, terrestrial experiments to detect dark matter particles directly or indirect detection experiments searching for positrons, gamma-rays, neutrinos or other dark matter decay or annihilation products.</div></front></TEI><affiliations><list><country><li>Canada</li><li>Royaume-Uni</li><li>États-Unis</li></country></list><tree><country name="États-Unis"><noRegion><name sortKey="Taylor, James E" sort="Taylor, James E" uniqKey="Taylor J" first="James E." last="Taylor">James E. Taylor</name></noRegion></country><country name="Royaume-Uni"><noRegion><name sortKey="Taylor, James E" sort="Taylor, James E" uniqKey="Taylor J" first="James E." last="Taylor">James E. Taylor</name></noRegion></country><country name="Canada"><noRegion><name sortKey="Babul, Arif" sort="Babul, Arif" uniqKey="Babul A" first="Arif" last="Babul">Arif Babul</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
EXPLOR_STEP=$WICRI_ROOT/Wicri/Amerique/explor/CaltechV1/Data/Main/Exploration
HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 000276 | SxmlIndent | more
Ou
HfdSelect -h $EXPLOR_AREA/Data/Main/Exploration/biblio.hfd -nk 000276 | SxmlIndent | more
Pour mettre un lien sur cette page dans le réseau Wicri
{{Explor lien
|wiki= Wicri/Amerique
|area= CaltechV1
|flux= Main
|étape= Exploration
|type= RBID
|clé= ISTEX:EE3CCC5CCD9534BF9F8A3C100625237086DC154D
|texte= The evolution of substructure in galaxy, group and cluster haloes — III. Comparison with simulations
}}
| This area was generated with Dilib version V0.6.32. |  |