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Metadados

1. Identificação
Tipo de ReferênciaArtigo em Revista Científica (Journal Article)
Sitemtc-m21c.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP3W34R/435EQDP
Repositóriosid.inpe.br/mtc-m21c/2020/08.24.12.26   (acesso restrito)
Última Atualização2020:09.14.17.28.03 (UTC) administrator
Repositório de Metadadossid.inpe.br/mtc-m21c/2020/08.24.12.26.18
Última Atualização dos Metadados2022:08.22.23.20.48 (UTC) administrator
DOI10.1088/1475-7516/2020/08/010
ISSN1475-7516
Chave de CitaçãoFortesMiraStecWuen:2020:WhCoOb
TítuloWhat could be the observational signature of dark matter in globular clusters?
Ano2020
Mês10.1088/1475-7516/2020/08/010
Data de Acesso13 maio 2024
Tipo de Trabalhojournal article
Tipo SecundárioPRE PI
Número de Arquivos1
Tamanho856 KiB
2. Contextualização
Autor1 Fortes, Elaine C. F. S.
2 Miranda, Oswaldo Duarte
3 Stecker, Floyd W.
4 Wuensche, Carlos Alexandre
Identificador de Curriculo1
2 8JMKD3MGP5W/3C9JJ2G
Grupo1
2 DIDAS-CGCEA-INPE-MCTIC-GOV-BR
3
4 DIDAS-CGCEA-INPE-MCTIC-GOV-BR
Afiliação1 Universidade Federal do Pampa (UNIPAMPA)
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 NASA Goddard Space Flight Center
4 Instituto Nacional de Pesquisas Espaciais (INPE)
Endereço de e-Mail do Autor1 elainefortes@unipampa.edu.br
2 oswaldo.miranda@inpe.br
3 floyd.w.stecker@nasa.gov
4 ca.wuensche@inpe.br
RevistaJournal of Cosmology and Astroparticle Physics
Volume8
Páginase010
Nota SecundáriaA1_MATEMÁTICA_/_PROBABILIDADE_E_ESTATÍSTICA A1_ENGENHARIAS_III A1_ASTRONOMIA_/_FÍSICA B1_GEOCIÊNCIAS
Histórico (UTC)2020-08-24 12:26:18 :: simone -> administrator ::
2020-08-24 12:26:20 :: administrator -> simone :: 2020
2020-08-24 12:27:20 :: simone -> administrator :: 2020
2020-08-24 16:47:43 :: administrator -> simone :: 2020
2020-09-14 17:28:03 :: simone -> administrator :: 2020
2022-01-04 01:35:19 :: administrator -> simone :: 2020
2022-03-11 14:28:53 :: simone -> administrator :: 2020
2022-08-22 23:20:48 :: administrator -> simone :: 2020
3. Conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteúdoExternal Contribution
Tipo de Versãopublisher
Palavras-Chaveastrophysical black holes
massive black holes
dark matter theory
particle physics - cosmology connection
ResumoHere we investigate the possibility that some globular clusters (GCs) harbor intermediate mass black holes (BH) in their centers and are also embedded in a low-mass dark matter (DM) halo. Up to date, there is no evidence on whether or not GCs have DM in their constitution. For standard cold DM cosmology, it is expected that GCs form with their own DM halos. Other studies investigate the possibility that GCs were initially embedded in massive DM halos that evolved during the cluster lifetime. An additional intriguing question is related to the existence of intermediate mass black holes (IMBH) in the GCs. The determination of whether GCs hold IMBHs would be able to answer important questions about GCs formation and the circumstances that gave rise to the IMBHs. DM & IMBH in the context of GCs are interesting subjects to be studied and we will perform such studies here, assuming the coexistence of both of them in some GCs. Having such information, we perform the study possible DM signals from GCs. One important subject to be studied is the DM density profile. In the inner regions of GCs, the DM density profile is still an open question of fundamental importance to DM studies, specially for the study of radio and -y-ray emission from DM annihilation in such regions. Here we consider the case of IMBHs in the inner regions of three GCs: 47 Tuc, NGC 6266 and omega Cen. The existence of a black hole (BH) directly affects the matter distribution in its vicinity. These effects are significant for IMBHs as well as supermassive black holes (SMBHs) and can lead to large DM overdensities called spikes. In this paper, we direct our studies to the radio synchrotron emission from DM annihilation with spike profiles around possible IMBHs in GCs. We present our results for synchrotron emission produced by DM annihilation via b (b) over bar channel. We use the best-fit DM mass of 34 GeV and annihilation channel in b (b) over bar used to explain the Galactic center "excess" and perform our analysis for the estimated radio flux. We direct our attention specially to the gamma-ray emission from 47 Tuc. When considering a scenario wich includes a BH and the combined analysis of multi-wavelength studies, we conclude that some parameter choice as the annihilation cross section <sigma v > used to fit the gamma-ray excess differs by many orders of magnitude from the one necessary to fit the radio observations for this globular cluster if we consider the BH scenario.
ÁreaCEA
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4. Condições de acesso e uso
Idiomaen
Arquivo Alvofortes_what.pdf
Grupo de Usuáriossimone
Grupo de Leitoresadministrator
simone
Visibilidadeshown
Política de Arquivamentodenypublisher denyfinaldraft12
Permissão de Leituradeny from all and allow from 150.163
Permissão de Atualizaçãonão transferida
5. Fontes relacionadas
Unidades Imediatamente Superiores8JMKD3MGPCW/3ETR8EH
Lista de Itens Citandosid.inpe.br/bibdigital/2013/10.01.00.07 2
sid.inpe.br/mtc-m21/2012/07.13.14.57.32 1
DivulgaçãoWEBSCI; PORTALCAPES.
Acervo Hospedeirourlib.net/www/2017/11.22.19.04
6. Notas
Campos Vaziosalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel e-mailaddress format isbn label lineage mark mirrorrepository nextedition notes number orcid parameterlist parentrepositories previousedition previouslowerunit progress project rightsholder schedulinginformation secondarydate secondarykey session shorttitle sponsor subject tertiarymark tertiarytype url
7. Controle da descrição
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