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1. Identity statement
Reference TypeJournal Article
Sitemtc-m21b.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP3W34P/3QL7HSP
Repositorysid.inpe.br/mtc-m21b/2018/03.02.16.20
Last Update2018:05.03.13.04.23 (UTC) simone
Metadata Repositorysid.inpe.br/mtc-m21b/2018/03.02.16.20.14
Metadata Last Update2019:01.14.17.05.24 (UTC) administrator
DOI10.1093/mnras/stx3241
ISSN0035-8711
1365-2966
Labelself-archiving-INPE-MCTIC-GOV-BR
Citation KeyOldWPGMSTBYCMSSCBPLS:2018:ImDySu
TitleGalaxy cluster mass reconstruction project - III: the impact of dynamical substructure on cluster mass estimates
Year2018
Access Date2024, May 16
Type of Workjournal article
Secondary TypePRE PI
Number of Files1
Size1027 KiB
2. Context
Author 1 Old, L.
 2 Wojtak, R.
 3 Pearce, F. R.
 4 Gray, M. E.
 5 Mamon, G. A.
 6 Sifón, C.
 7 Tempel, E.
 8 Biviano, A.
 9 Yee, H. K. C.
10 Carvalho, Reinaldo Ramos de
11 Müller, V.
12 Sepp, T.
13 Skibba, R. A.
14 Croton, D.
15 Bamford, S. P.
16 Power, C.
17 von der Linden, A.
18 Saro, A.
Resume Identifier 1
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10 8JMKD3MGP5W/3C9JJ5B
Group 1
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10 DIDAS-CGCEA-INPE-MCTIC-GOV-BR
Affiliation 1 University of Toronto
 2 Stanford University
 3 University of Nottingham
 4 University of Nottingham
 5 Sorbonne Universités
 6 Princeton University
 7 Leibniz-Institut für Astrophysik Potsdam (AIP)
 8 INAF-Osservatorio Astronomico di Trieste
 9 University of Toronto
10 Instituto Nacional de Pesquisas Espaciais (INPE)
11 Leibniz-Institut für Astrophysik Potsdam (AIP)
12 Tartu Observatory
13 University of California
14 Swinburne University of Technology
15 University of Nottingham
16 University of Western Australia
17 Stony Brook University
18 INAF-Osservatorio Astronomico di Trieste
Author e-Mail Address 1
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10 reinaldo.decarvalho@inpe.br
JournalMonthly Notices of the Royal Astronomical Society
Volume475
Number1
Pages853-866
Secondary MarkA1_QUÍMICA A1_INTERDISCIPLINAR A1_GEOCIÊNCIAS A1_ENGENHARIAS_III A2_MATEMÁTICA_/_PROBABILIDADE_E_ESTATÍSTICA A2_ASTRONOMIA_/_FÍSICA B2_ENSINO B5_ENGENHARIAS_IV
History (UTC)2018-03-02 16:25:08 :: simone -> administrator :: 2018
2018-03-03 04:09:36 :: administrator -> simone :: 2018
2018-05-03 13:04:23 :: simone -> administrator :: 2018
2019-01-04 16:56:03 :: administrator -> simone :: 2018
2019-01-07 11:32:26 :: simone -> administrator :: 2018
2019-01-14 17:05:24 :: administrator -> simone :: 2018
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
KeywordsCosmological parameters
Galaxies: Clusters: General
Galaxies: Groups: General
Galaxies: Haloes
Galaxies: Kinematics and dynamics
Large-scale structure of Universe
AbstractWith the advent of wide-field cosmological surveys, we are approaching samples of hundreds of thousands of galaxy clusters. While such large numbers will help reduce statistical uncertainties, the control of systematics in cluster masses is crucial. Here we examine the effects of an important source of systematic uncertainty in galaxy-based cluster mass estimation techniques: the presence of significant dynamical substructure. Dynamical substructure manifests as dynamically distinct subgroups in phase-space, indicating an 'unrelaxed' state. This issue affects around a quarter of clusters in a generally selected sample. We employ a set of mock clusters whose masses have been measured homogeneously with commonly used galaxy-based mass estimation techniques (kinematic, richness, caustic, radial methods). We use these to study how the relation between observationally estimated and true cluster mass depends on the presence of substructure, as identified by various popular diagnostics.We find that the scatter for an ensemble of clusters does not increase dramatically for clusters with dynamical substructure. However, we find a systematic bias for all methods, such that clusters with significant substructure have higher measured masses than their relaxed counterparts. This bias depends on cluster mass: the most massive clusters are largely unaffected by the presence of significant substructure, but masses are significantly overestimated for lower mass clusters, by ~10 per cent at 1014 and ≳20 per cent for ≲1013.5. The use of cluster samples with different levels of substructure can therefore bias certain cosmological parameters up to a level comparable to the typical uncertainties in current cosmological studies.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDAS > Galaxy cluster mass...
doc Directory Contentaccess
source Directory Contentthere are no files
agreement Directory Content
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4. Conditions of access and use
data URLhttp://mtc-m21b.sid.inpe.br/ibi/8JMKD3MGP3W34P/3QL7HSP
zipped data URLhttp://mtc-m21b.sid.inpe.br/zip/8JMKD3MGP3W34P/3QL7HSP
Languageen
User Groupsimone
Reader Groupadministrator
simone
Visibilityshown
Archiving Policyallowpublisher allowfinaldraft
Read Permissionallow from all
Update Permissionnot transferred
5. Allied materials
Next Higher Units8JMKD3MGPCW/3ETR8EH
Citing Item Listsid.inpe.br/mtc-m21/2012/07.13.14.58.48 1
DisseminationWEBSCI; PORTALCAPES; MGA; COMPENDEX.
Host Collectionsid.inpe.br/mtc-m21b/2013/09.26.14.25.20
6. Notes
Empty Fieldsalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel e-mailaddress format isbn lineage mark mirrorrepository month nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress project rightsholder schedulinginformation secondarydate secondarykey session shorttitle sponsor subject targetfile tertiarymark tertiarytype url
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