florencia jiménez luján

Florencia Jiménez Luján

Measuring Ionisation parameters(ITP-WHT)

BAL QSO meeting 2009Jun 24 – 26

Bologna (Italy)

MEASURING IONISATION PARAMETERS (ITP-WHT)

BAL QSO meeting 2009 – Jun 24 - 26, Bologna (Italy) Florencia Jiménez Luján 2

• Introduction

• Data

• Results

• Future plans

• Summary


Introduction


Urry & Padovani, 1995

Unification of AGN (Active Galactic Nuclei)

QSO (Quasi-Stellar Object, or quasar, QUASi-stellAR) in the center of each AGN: black hole surrounded by an accretion disk

moving clouds: BLR (fast) & NLR (slow)

classification: orientation scenario vs. evolutionary scenario (both???)

know the properties & composition of the medium

(BLR)

(NLR)


Introduction


Elvis, 2000

BAL

NAL

No

abso

rber

sUnification of AGN (Active Galactic Nuclei)






Introduction


Montenegro-Montes et al., 2008

Unification of AGN (Active Galactic Nuclei)





BALQSO have convex radio spectra(typical of CSS/GPS “young” radio sources)CSS: Compact Steep Spectrum; GPS: Gigahertz Peaked Spectrum


Introduction


1210+5256

z = 3.194

r = 18.50

Not inFIRST

q11_020


Introduction


1210+5256

z = 2.560

r = 17.77

FIRST:1.9 mJy

q11_039

MEASURING IONISATION PARAMETERS (ITP-WHT)Data


link



q11_020

Flux

Wavelength (Å)

Central wavelength: 4790 Å (blue arm: b1,b2,b3)



q11_020

Flux

Wavelength (Å)

Central wavelength: 5590 Å (red arm: r1)



q11_020

Flux

Wavelength (Å)

Central wavelength: 6165 Å (red arm: r2,r3)



q11_039

Flux

Wavelength (Å)

Central wavelength: 3970 Å (blue arm: b1)



q11_039

Flux

Wavelength (Å)

Central wavelength: 5144 Å (red arm: r1)


Results


Wavelength (Å)

q11_020

resampling

Wavelength (Å)

Flux

Flux

r1

r2_3

CIVcentral source z = 3.194absorbers z ~ 2.853


Results


q11_020


a b c


Results


q11_020


a: -25500 - -25470 km s-1


Results


q11_020


b: -25410 - -25370 km s-1


Results


q11_020


c: -25320 - -25290 km s-1


Results


q11_020

SiIV

r1

Wavelength (Å)

Flux

central source z = 3.194absorbers z ~ 2.853


Results


q11_020

SiIVcentral source z = 3.194absorbers z ~ 2.853

a b c


Results


q11_020


a: -25500 - -25470 km s-1


Results


q11_020


b: -25410 - -25370 km s-1


Results


q11_020


c: -25320 - -25290 km s-1


Results


q11_020



Results


Wavelength (Å)

q11_039 Flux

b1

OVIcentral source z = 2.560absorbers z ~ 2.527


Results


q11_039


a b c


Results


q11_039


a: -2360 - -2300 km s-1


Results


OVI

b: -2270 - -2220 km s-1 q11_039



Results


OVI

c: -2190 - -2120 km s-1 q11_039



Results


q11_039

SiIV

r1

Wavelength (Å)

Flux



Results


q11_039


a b c


Results


q11_039


a: -2360 - -2300 km s-1


Results


SiIV

b: -2270 - -2220 km s-1 q11_039



Results


SiIV

c: -2190 - -2120 km s-1 q11_039



Results


q11_039



Future plans


• Data analysis of all BAL QSOs (ITP-WHT)

• Comparison with other method (power-law model, Arav’s group). Check compatibility for pure partial covering model with this method (q11_020, q11_039 compatible)

• Variability (q11_030)

• Line-locking

• Estimation of the distances from the absorbers to the central sources (electron densities, VLT data)


Summary


• Data reduction of all BAL QSOs (ITP-WHT)

• Errors in covering factors and optical depths from errors in Ib and Ir (errors in column densities and ionisation parameters from those ones)

• Resampling for different exposures

• Analysis of q11_020 and q11_039 (Ionisation parameters determination)

• Compatibility with other method (Arav’s group) for pure partial covering model

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