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1. Identity statement
Reference TypeJournal Article
Sitemtc-m21c.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP3W34R/3U2MGUS
Repositorysid.inpe.br/mtc-m21c/2019/09.10.10.43
Last Update2019:09.10.10.43.52 (UTC) simone
Metadata Repositorysid.inpe.br/mtc-m21c/2019/09.10.10.43.52
Metadata Last Update2020:01.06.11.42.19 (UTC) administrator
DOI10.1093/mnrasl/slz084
ISSN0035-8711
1365-2966
Citation KeyCarvalhoCostMourRibe:2019:MaDePr
TitleThe mass density profile and star formation history of Gaussian and non-Gaussian clusters
Year2019
MonthJuly
Access Date2024, May 16
Type of Workjournal article
Secondary TypePRE PI
Number of Files1
Size714 KiB
2. Context
Author1 Carvalho, Reinaldo Ramos de
2 Costa, A. P.
3 Moura, T. C.
4 Ribeiro, A. L. B.
Resume Identifier1 8JMKD3MGP5W/3C9JJ5B
Group1 DIDAS-CGCEA-INPE-MCTIC-GOV-BR
Affiliation1 Instituto Nacional de Pesquisas Espaciais (INPE)
2 Universidade Estadual de Santa Cruz
3 Universidade de São Paulo (USP)
4 Universidade Estadual de Santa Cruz
Author e-Mail Address1 rrdecarvalho2008@gmail.com
JournalMonthly Notices of the Royal Astronomical Society
Volume487
Number1
PagesL86-L90
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)2019-09-10 10:43:52 :: simone -> administrator ::
2019-09-10 10:43:53 :: administrator -> simone :: 2019
2019-09-10 10:44:32 :: simone -> administrator :: 2019
2020-01-06 11:42:19 :: administrator -> simone :: 2019
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
Keywordsgalaxies: clusters: general – galaxies:evolution – galaxies:formation – galaxies:star formation – galaxies:stellar content – galaxies: interactions
AbstractThis paper is the third of a series in which we investigate the discrimination between Gaussian (G) and Non-Gaussian (NG) clusters, based on the velocity distribution of the member galaxies. We study a sample of 177 groups from the Yang catalog in the redshift interval of 0.03 <= z <= 0.1 and masses >= 10(14) M-circle dot. Examining the projected stellar mass density distributions of G and NG groups, we find strong evidence of a higher infall rate in the outskirts of NG groups over the G ones. There is a 61 per cent excess of faint galaxies in NGs when contrasted with G groups, when integrating from 0.8 to 2.OR/R-200. The study of the star formation history (SFH) of ellipticals and spirals in the three main regions of the projected phase space reveals also that the star formation in faint spirals of NG groups is significantly different from their counterpart in the G groups. The assembled mass for faint spirals varies from 59 per cent at 12.7 Gyr to 75 per cent at 8.0 Gyr, while in G systems this variation is from 82 per cent to 91 per cent. This finding may also be interpreted as a higher in fall rate of gas-rich systems in NG groups. This accretion process through the filaments, disturbing the velocity distribution and modifying not only the stellar population of the incoming galaxies but also their SFH, should be seriously considered in modelling galaxy evolution.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDAS > The mass density...
doc Directory Contentaccess
source Directory Contentthere are no files
agreement Directory Content
agreement.html 10/09/2019 07:43 1.0 KiB 
4. Conditions of access and use
data URLhttp://urlib.net/ibi/8JMKD3MGP3W34R/3U2MGUS
zipped data URLhttp://urlib.net/zip/8JMKD3MGP3W34R/3U2MGUS
Languageen
Target Filecarvalho_mass.pdf
User Groupsimone
Reader Groupadministrator
simone
Visibilityshown
Archiving Policyallowpublisher allowfinaldraft
Update Permissionnot transferred
5. Allied materials
Next Higher Units8JMKD3MGPCW/3ETR8EH
Citing Item Listsid.inpe.br/bibdigital/2013/10.01.00.07 3
sid.inpe.br/mtc-m21/2012/07.13.14.58.48 1
DisseminationWEBSCI; PORTALCAPES; MGA; COMPENDEX.
Host Collectionurlib.net/www/2017/11.22.19.04
6. Notes
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