apresentação no graco 2014
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Minha apresentação no GRACO 2014TRANSCRIPT
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The co-evolution of cosmic star formation rate and the
active supermassive black holes
Dr. Eduardo dos Santos Pereira.Dr. Oswaldo Duarte Miranda
Divisão de AstrofíscaDAS/INPE
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Accretion History of Active Black Holes from Type 1 AGN
Astrophysics and Space Science
DOI : 10.1007/s10509-014-1934-7
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Data Analysis
● Sloan Digital Sky Survey Data Release 7.● The quasar complementary catalogue of
Sloan Digital Sky Survey Data Release 7 by Shen et al. (2011)
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Eddington ratio
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The luminosity limit of Catalogue: The Luminosity Probability Density Function.
Data From CatalogueSave Data into
DataBaseBinning in mass
Redishift.
Friedmon-Diacones rule:
If the number of data is greater than N
Obtain the mean Luminosity
If w is greater than Δlog(L)
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The luminosity limit of Catalogue: The Luminosity Probability Density Function.
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The luminosity limit of Catalogue: The Luminosity Probability Density Function.
Largura ideal do Histograma. Regra de Friedmon-Diacones:
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Mean Accretion Rate and Mean Luminosity
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Mean Accretion Rate and Mean Luminosity
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Mean Accretion Rate and Mean Luminosity
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Mean Bolometric Luminosity
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Mean Eddington Ratio
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Mean Mass Accretion Rate
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TO DO
● Obtain the Duty Cycle of AGN's tipe 1.
● Driver et al. 2013 suggested an model to Cosmic Star Formation rate (CSFR) for bojo and disk.
● The CSFR of the bojo and disk trace the growth of SMBH ?
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ρBH=∫mi
mfnmdm
ρBH=∫mi
mf ∂n∂ t
mdm
∂n∂ t
−∂<m>n
∂m=0
Pereira & Miranda (2011):
ρBH=ρstar
(1+z)P( z)
dtdz
Star Formation rate and BH accretion History.
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Statistic Test● No parametric Bootstrap (Wehrens et al. 2000):
● Confidence Level:
● Standard Error
● Bias:
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Testes Estatísticos● Bootstrap NÃO Paramétrico (Wehrens et al. 2000):
https://github.com/duducosmos/pyboostrap
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www.cosmicstarformation.com
pycosmicstar
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Thanks...