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

Accretion History of Active Black Holes from Type 1 AGN

Astrophysics and Space Science

DOI : 10.1007/s10509-014-1934-7

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)

Eddington ratio

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)

The luminosity limit of Catalogue: The Luminosity Probability Density Function.

The luminosity limit of Catalogue: The Luminosity Probability Density Function.

Largura ideal do Histograma. Regra de Friedmon-Diacones:

Mean Accretion Rate and Mean Luminosity

Mean Accretion Rate and Mean Luminosity

Mean Accretion Rate and Mean Luminosity

Mean Bolometric Luminosity

Mean Eddington Ratio

Mean Mass Accretion Rate

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 ?

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.

Statistic Test● No parametric Bootstrap (Wehrens et al. 2000):

● Confidence Level:

● Standard Error

● Bias:

Testes Estatísticos● Bootstrap NÃO Paramétrico (Wehrens et al. 2000):

https://github.com/duducosmos/pyboostrap

www.cosmicstarformation.com

pycosmicstar

Thanks...