E. Danezis*, E. Lyratzi*, D. Stathopoulos*, L. ČE. Danezis*, E. Lyratzi*, D. Stathopoulos*, L. Č. . Popović **, Popović **,

A. Antoniou*, M. S. DimitrijevićA. Antoniou*, M. S. Dimitrijević** , ** , D. Tzimeas*. D. Tzimeas*.

* University of Athens, ** Astronomical Observatory of Belgrade* University of Athens, ** Astronomical Observatory of Belgrade

Some new ideas to study the Quasar’s spectraSome new ideas to study the Quasar’s spectraThe example of C IV emission lines in the UV spectra of 21 HiBALQSOsThe example of C IV emission lines in the UV spectra of 21 HiBALQSOs

BAL Quasars is a category of Active Galactic Nuclei (AGN)

• BALQSOs are classified in the following three BALQSOs are classified in the following three subcategories based on the material producing the BAL subcategories based on the material producing the BAL profiles.profiles.

• High-ionization BALQSOs (HiBALs)High-ionization BALQSOs (HiBALs) contain strong, contain strong,

broad absorption troughs short-ward of high-ionization broad absorption troughs short-ward of high-ionization emission lines (such as C IV, Si IV, N V) and are emission lines (such as C IV, Si IV, N V) and are typically identified through the presence of C IV typically identified through the presence of C IV absorption resonance lines.absorption resonance lines.

• Low-ionization BALQSOs (LoBALs)Low-ionization BALQSOs (LoBALs) contain contain

HiBALHiBAL features but also have absorption from low- features but also have absorption from low-ionization lines such as Mg II. ionization lines such as Mg II.

• LoBALs with excited-state Fe II or Fe IIILoBALs with excited-state Fe II or Fe III absorption absorption are called FeLoBALs.are called FeLoBALs.

SpectralSpectral classification of BALQSOs classification of BALQSOs

In this figure we can see some BALQSOsBALQSOs spectra of all the above categories

The HiBALQSOs absorption Spectral LinesThe HiBALQSOs absorption Spectral Lines

In the spectra of HiBAL QSOs In the spectra of HiBAL QSOs we can detect we can detect absorption lines separated in the following subgroups. absorption lines separated in the following subgroups.

Absorption linesAbsorption lines

1.1. Broad Absorption Lines (BALs) with Broad Absorption Lines (BALs) with complex profiles andcomplex profiles and

2.2. Narrow Absorption Lines (NALs) with Narrow Absorption Lines (NALs) with simple profilessimple profiles

The first subgroupThe first subgroup of absorption lines includes of absorption lines includes lines that show lines that show very broad and complex profilesvery broad and complex profiles.. It is known that BLRs include a large number of It is known that BLRs include a large number of plasma clouds. As a result, the very broad lines plasma clouds. As a result, the very broad lines represent a number of lines of the same ion and represent a number of lines of the same ion and the same wavelength shifted at different the same wavelength shifted at different ΔλΔλ. . This effect occurs because these lines are This effect occurs because these lines are created in different clouds that move radially created in different clouds that move radially and spin with different velocities (and spin with different velocities (Danezis et al. Danezis et al. 2007). 2007).

1. The broad absorption lines1. The broad absorption lines

BAL

BALs profiles of C IV resonance lines with broad and complex profiles

2. Narrow Absorption lines (NALs) with 2. Narrow Absorption lines (NALs) with simple profilessimple profiles

The second subgroupThe second subgroup of absorption lines includes of absorption lines includes spectral lines with simple profiles. One can fit these spectral lines with simple profiles. One can fit these lines using classical distributions such aslines using classical distributions such as Gauss, Gauss, Lorentz or VoigtLorentz or Voigt. In these cases we may be able to . In these cases we may be able to understand the phenomena that take place in the understand the phenomena that take place in the regions which produce the simple lines, but we are not regions which produce the simple lines, but we are not able to calculate the values of the physical parameters able to calculate the values of the physical parameters that describe the absorbing clouds. that describe the absorbing clouds.

BAL BALNAL NAL

NAL profiles of C IV resonance lines (components)

The HiBAL QSOs emission Spectral LinesThe HiBAL QSOs emission Spectral LinesWe can detect three regions as the origin of emitting radiation

1. Perhaps blobs in the inner accretion1. Perhaps blobs in the inner accretion discdisc

Jian-Min Wang1, Ye-Fei Yuan2, Jian-Min Wang1, Ye-Fei Yuan2, MeiWu1, and Masaaki MeiWu1, and Masaaki Kusunose3Kusunose3The Astrophysical Journal LettersThe Astrophysical Journal Letters

Hideyuki kamaya1Hideyuki kamaya1The Astrophysical Journal, The Astrophysical Journal, 510:862È866, 1999 January 10510:862È866, 1999 January 10

2. Emitting radiation layers in the external . Emitting radiation layers in the external region of the accretion discregion of the accretion disc

S. Veilleux S. Veilleux et al.et al. 2013  2013 ApJApJ 764 15 764 15

In this figure we can see the theoretical emission profiles In this figure we can see the theoretical emission profiles that arise from the disc model as a function of the that arise from the disc model as a function of the inclination angles inclination angles ((ChenChen, , KK. & . & HalpernHalpern, , JJ. . PP. 1989). 1989)

3. Broad and Narrow Line Region Clouds3. Broad and Narrow Line Region Clouds

Arav et al. 1997, Ferland 2004, Laor 2006, Laor et al. 2006Arav et al. 1997, Ferland 2004, Laor 2006, Laor et al. 2006

Emission line profilesEmission line profiles

1.Simple Emission lines2.Multi-component emission lines

In the spectra of HiBAL QSOs we can detect In the spectra of HiBAL QSOs we can detect emission line profiles separated in two subgroupsemission line profiles separated in two subgroups. .

The first subgroupThe first subgroup of emission lines includes lines of emission lines includes lines with simple profileswith simple profiles that we can fit using that we can fit using the the accretion disk model accretion disk model or, a classical distribution as or, a classical distribution as Gauss, Lorentz or VoigtGauss, Lorentz or Voigt..

Simple Emission linesSimple Emission lines

The second subgroupThe second subgroup of of emission lines emission lines includes includes

complex lines that complex lines that cannot cannot be simulated using only be simulated using only

the accretion disk modelthe accretion disk model. This means that the line This means that the line profiles are not due only profiles are not due only to the accretion disk, but to the accretion disk, but there are other regions there are other regions

(clouds, blobs)(clouds, blobs) apart from apart from the disk that play a the disk that play a significant role too.significant role too. The observed HThe observed Hαα line (dots) fitted with multi- line (dots) fitted with multi-

component model (solid line) given by Popović et al. component model (solid line) given by Popović et al. (2002). With dashed lines the disk, broad and narrow (2002). With dashed lines the disk, broad and narrow

spherical components are presented.spherical components are presented.

Multi-component Emission Lines Multi-component Emission Lines

Problems of Problems of HiBAL QSOs spectraHiBAL QSOs spectra

BALR’s spectral line profiles appear to be rather BALR’s spectral line profiles appear to be rather complex in structure. complex in structure. This means that these This means that these spectral lines are not created in a single region spectral lines are not created in a single region but are the spectral synthesis of many discrete but are the spectral synthesis of many discrete lines.lines. These discrete lines are created in separate These discrete lines are created in separate and independent regions (clouds or blobs) that and independent regions (clouds or blobs) that have different spectral characteristics. have different spectral characteristics. (Danezis 1984, 1986, (Danezis 1984, 1986, Danezis et al. 1991, 2003Danezis et al. 1991, 2003 and and Lyratzi & Danezis 2004Lyratzi & Danezis 2004, Boksenberg et al. 2003, Zheng , Boksenberg et al. 2003, Zheng et al. 2001, Dobrzycki et al. 2007et al. 2001, Dobrzycki et al. 2007))..

1.1. The broad and very complex The broad and very complex Absorption Line profilesAbsorption Line profiles

To be more specific, To be more specific, each plasma cloud each plasma cloud produces a classical absorption lineproduces a classical absorption line. If these If these clouds rotate around their centers, with large clouds rotate around their centers, with large velocities and move radially with small velocities and move radially with small velocities, then the produced spectral lines have velocities, then the produced spectral lines have large widths and small shifts. As a result, these large widths and small shifts. As a result, these lines are blended among themselves producing lines are blended among themselves producing a complex profile a complex profile (Danezis 1984, 1986, (Danezis 1984, 1986, Danezis et al. 1991, 2003Danezis et al. 1991, 2003 and Lyratzi & and Lyratzi & Danezis 2004)Danezis 2004)..

Based on this complex structure, many researchers Based on this complex structure, many researchers (Arav et al. 1997, Ferland 2004, Laor 2006, Laor et al. 2006) suggested that BALRs consist of a number of suggested that BALRs consist of a number of independent plasma clouds. Each cloud, supposing it is independent plasma clouds. Each cloud, supposing it is homogenous in its physical properties, should create a homogenous in its physical properties, should create a specific spectral line profile which specific spectral line profile which is described by a is described by a specific mathematical distributionspecific mathematical distribution (known or not). (known or not). However, in the bibliography we cannot find a However, in the bibliography we cannot find a mathematical distribution or a physical model that can mathematical distribution or a physical model that can fit these complex profiles. This lies in the fact fit these complex profiles. This lies in the fact that the that the radiative transfer equations, through a complex radiative transfer equations, through a complex environment of many clouds, were not solved. environment of many clouds, were not solved. As a As a result, until recently, we didn’t have result, until recently, we didn’t have the line function the line function that could theoretically simulate a complex spectral line.that could theoretically simulate a complex spectral line.

The classical mathematical distributions The classical mathematical distributions used for used for fitting spectral lines in QSO’s spectra are fitting spectral lines in QSO’s spectra are Gauss, Gauss, Lorentz and Voigt. Lorentz and Voigt. These distributions describe the These distributions describe the physical conditions of the plasma regions which create physical conditions of the plasma regions which create the studied spectral lines. the studied spectral lines.

In more detail:In more detail:When we fit a spectral line withWhen we fit a spectral line with a Gaussian a Gaussian we accept we accept that in the plasma region, which creates the spectral that in the plasma region, which creates the spectral line, the random, thermal motions of the ions prevail. line, the random, thermal motions of the ions prevail. A Lorentzian A Lorentzian fit implies the existence of pressure in fit implies the existence of pressure in the region which produces the studied spectral line. the region which produces the studied spectral line. A Voigt A Voigt fit fit (Gauss + Lorentz) (Gauss + Lorentz) tells us that in the tells us that in the plasma region we have a combination of thermal plasma region we have a combination of thermal motions of the ions and pressure.motions of the ions and pressure.

2. The classical distributions2. The classical distributions

The problem is that the classical distributions, The problem is that the classical distributions, Gauss, Lorentz and Voigt are not efficient Gauss, Lorentz and Voigt are not efficient enough in describing the BALQSO’s spectra enough in describing the BALQSO’s spectra and as a result and as a result we need some new we need some new distributions,distributions, in order to give a more accurate in order to give a more accurate description to the complex spectra.description to the complex spectra.

However, what was missing, was a distribution However, what was missing, was a distribution able to describe able to describe the rotation of plasma clouds the rotation of plasma clouds (around their centers) or a distribution that (around their centers) or a distribution that could describe the rotation of clouds as well could describe the rotation of clouds as well as the thermal motions of the ions as the thermal motions of the ions simultaneouslysimultaneously. .

3. The radiative transfer equations3. The radiative transfer equationsand the line functionand the line function

In order to fit the BALQSO’s spectra In order to fit the BALQSO’s spectra we need a physical we need a physical model,model, with a mathematical description, which with a mathematical description, which solves solves the radiative transfer equations the radiative transfer equations for a complex plasma for a complex plasma environment and gives the environment and gives the line functionline function that can describe that can describe accurately each complex spectral line. Furthermore, this accurately each complex spectral line. Furthermore, this model must include the mathematical description of the model must include the mathematical description of the previously mentioned distributions.previously mentioned distributions.

This model must be able to calculate not only the This model must be able to calculate not only the physical parameters that describe the complex studied physical parameters that describe the complex studied spectral line profile, spectral line profile, but also the parameters of each one but also the parameters of each one of the single spectral lines that compose the complex of the single spectral lines that compose the complex profile. profile. As a consequence, by describing each spectral As a consequence, by describing each spectral line separately, we describe the physical conditions of line separately, we describe the physical conditions of each absorbing plasma cloud.each absorbing plasma cloud.

In this figure we can see In this figure we can see the emission and the the emission and the

absorption components absorption components of the C IV resonance of the C IV resonance

spectral lines that spectral lines that construct the C IV construct the C IV

complex line profilecomplex line profile

Finally, the model, in its mathematical Finally, the model, in its mathematical description, description, should include the geometry of the should include the geometry of the regionsregions that produce the studied spectral lines. that produce the studied spectral lines. The model must be self-consistent, and the The model must be self-consistent, and the theory that underlies the model theory that underlies the model must not go must not go against the physical principles against the physical principles that we already that we already know that apply in the broad line region.know that apply in the broad line region.

The reasons for choosing GR ModelThe reasons for choosing GR Model((GGauss-auss-RRotation Model)otation Model)

In our researchIn our research we use the GR Model we use the GR Model for the following reasons:for the following reasons:

((Danezis et alDanezis et al. 2007, . 2007, PASJPASJ, 59, 827, 59, 827 ) )

In the context of GR Model,In the context of GR Model, the radiative transfer the radiative transfer equation for a complex atmosphere has been solvedequation for a complex atmosphere has been solved. By solving the equation (Danezis et al 2007), we By solving the equation (Danezis et al 2007), we calculated the final calculated the final line functionline function that can fit not only that can fit not only each one of the spectral lines (emission or absorption) each one of the spectral lines (emission or absorption) but all the complex spectral regions of an ion line but all the complex spectral regions of an ion line (e.g. (e.g. C IV C IV λλ 1548.187 Å, 1550.772 Åλλ 1548.187 Å, 1550.772 Å) )

1.1. Solving the radiative transfer equationSolving the radiative transfer equation The line functionThe line function

ggg

jejejej

iii LLSLII expexp1exp0

The final The final line functionline function can fit not only each one of the spectral lines can fit not only each one of the spectral lines (emission or absorption) (emission or absorption) but all the complex spectral regions of an ion but all the complex spectral regions of an ion

line line (e.g. C IV λλ 1548.187 Å, 1550.772 Å)

Example based on the problemsExample based on the problems

• ΙΙλ0λ0:: is the initial radiation intensity, is the initial radiation intensity,

• LLii, L, Lejej, L, Lgg: : are the distribution functions of the are the distribution functions of the

absorption coefficients absorption coefficients kkλiλi, k, kλejλej, k, kλgλg,,

• ξ:ξ: is the optical depth in the centre of the the spectral line,spectral line,

• SSλejλej:: is the source function, that is constant is the source function, that is constant

during one observationduring one observation..

ggg

jejejej

iii LLSLII expexp1exp0

In the line functionIn the line function

2. Creating two new distribution functions2. Creating two new distribution functions

GR Model includes the creation of two new GR Model includes the creation of two new distributions,distributions, the Rotation distribution the Rotation distribution (Danezis, E. et al. 2003) that describes the (Danezis, E. et al. 2003) that describes the rotation of the plasma clouds and the rotation of the plasma clouds and the GGauss-auss-RRotation distributionotation distribution (Danezis et al. 2006b, (Danezis et al. 2006b, Danezis et al. 2007a, Lyratzi et al. 2009) which Danezis et al. 2007a, Lyratzi et al. 2009) which describes the combination of the random describes the combination of the random motions of the clouds’ ions and the self-rotation motions of the clouds’ ions and the self-rotation of the clouds. of the clouds.

If If then then

if if thenthen

The The L(L(λλ)) is a function of is a function of ΔλΔλrotationrotation (from where we can (from where we can calculate calculate VVrorott) and ) and λλ0 0 = = λλlablab + + ΔλΔλradialradial (from where we can (from where we can calculate calculate VVradrad).

12

4cos

0

2200

0

zrotation

rotation

02cos1 L

12

4cos

0

2200

0

zrotation

rotation

0L

Rotation DistributionRotation Distribution

We want to point out that the Rotation distribution We want to point out that the Rotation distribution represents the rotation of plasma clouds around their centers represents the rotation of plasma clouds around their centers

and not around the galactic center.and not around the galactic center.

The Gauss-Rotation distributionThe Gauss-Rotation distribution

2

2

0000

0

coscos22

cos222

d

zerf

zerf

zL final

radlab 0

c

Vz rot

Vradial

Vrotation

DanezisDanezis et al. et al. 2007 PASJ, Danezis et al. SPIG 20062007 PASJ, Danezis et al. SPIG 2006

Gaussian typical Gaussian typical deviationdeviation

x

u duexerf0

22

0

2ln2

c

Vrandom Vrandom

GR Model includes the GR Model includes the physical physical expressionexpression of the mathematical of the mathematical

distributions Gauss, Lorentz and Voigtdistributions Gauss, Lorentz and Voigt

ggg

jejejej

iii LLSLII expexp1exp0

In the case of the following line functionIn the case of the following line function::

TheThe andand are the distribution are the distribution functions of the absorption and the emission functions of the absorption and the emission component, respectivelycomponent, respectively..

The factorThe factor LL must include the geometry and all must include the geometry and all the principle physical conditions of the region the principle physical conditions of the region that produces the spectral line. that produces the spectral line. These physical These physical conditions indicate the exact distribution that conditions indicate the exact distribution that we must use. we must use.

iiLe ejejLej eS

1

This means that This means that

if we choose the right physical conditions in the if we choose the right physical conditions in the calculations of the factor calculations of the factor LL, the functions , the functions andand can have the form of a can have the form of a Gauss, Gauss, Lorentz, Voigt, Rotation or GRLorentz, Voigt, Rotation or GR distribution distribution function.function.In this case In this case we do not use the pure mathematical we do not use the pure mathematical distributionsdistributions that do not include any physical that do not include any physical parameter, but parameter, but the physical expression of these the physical expression of these distributions.distributions.

iiLe

ejejLej eS

1

ggg

jejejej

iii LLSLII expexp1exp0

In the case of In the case of GR model GR model for the classical distributions we for the classical distributions we use the physical expressions belowuse the physical expressions below: :

For the For the GaussGauss distribution, distribution, LL takes the takes the form:form:

2

20

2

eLG

For the For the LorentzLorentz distribution, distribution, LL takes the takes the form: form:

2

01

1

LL

For the For the VoigtVoigt distribution, distribution, LL takes takes the form: the form:

de

LV

2

2

2

1

2

20

We can calculate some important parameters of the We can calculate some important parameters of the plasma clouds that construct theplasma clouds that construct the components of the components of the observed spectral feature, such as:observed spectral feature, such as:

Using the GR modelUsing the GR model

Direct calculationsDirect calculations The apparent rotational velocities The apparent rotational velocities of absorbing or emitting of absorbing or emitting density layers density layers (V(Vrotrot)) The apparent radial velocities The apparent radial velocities of absorbing or emitting density of absorbing or emitting density layers layers (V(Vradrad)) The Gaussian typical deviation The Gaussian typical deviation of the ions’ random motions of the ions’ random motions (σ) (σ) The optical depth The optical depth in the center of the absorption or emission in the center of the absorption or emission components components (ξ(ξii))

Indirect calculationsIndirect calculations The random velocities The random velocities of the ionsof the ions (V(Vrandomrandom)) The FWHM The FWHM The absorbed or emitted energy The absorbed or emitted energy (Ε(Εa, Ee)a, Ee) The column density The column density (CD)(CD)

In our study, we solved the radiative transfer equations In our study, we solved the radiative transfer equations (Danezis et al. 2003, Ap&SS, 284, 1119) and thus we (Danezis et al. 2003, Ap&SS, 284, 1119) and thus we have the final line function. Having the line function we have the final line function. Having the line function we proved that in the case proved that in the case of a group of absorption lines,of a group of absorption lines, the the derived complex spectral line profile is described by a derived complex spectral line profile is described by a new function which is not the superposition of absorption new function which is not the superposition of absorption components but the mathematical product of themcomponents but the mathematical product of them ( ). ( ). This means that the final complex profile is not the sum This means that the final complex profile is not the sum of different functions ( ) but the mathematical product of different functions ( ) but the mathematical product of them. Each individual function describes the of them. Each individual function describes the absorption component of each cloud. The product of a absorption component of each cloud. The product of a series of functions ( ) series of functions ( ) is a new function is a new function and has nothing to do with the sum of functionsto do with the sum of functions ( ).( ).

We point out that…We point out that…

In contrary, in the case of a group of emission in the case of a group of emission spectral linesspectral lines the derived complex spectral line

profile is described by the sumby the sum of different different functionsfunctions and not the product of them

ggg

jejejej

iii LLSLII expexp1exp0

Data and Spectral AnalysisData and Spectral Analysis

In this work we study the emission resonance lines of In this work we study the emission resonance lines of C IV C IV λλλλ 1548.187, 1550.772 Å in the spectra of 21 1548.187, 1550.772 Å in the spectra of 21 HiBAL QSOs.HiBAL QSOs. The spectra were obtained from the The spectra were obtained from the SDSS DR7 database and they cover the spectral SDSS DR7 database and they cover the spectral range 3800 – 9200 Å.range 3800 – 9200 Å.

For the UV continuum we used the 0.5 power law For the UV continuum we used the 0.5 power law index.index.

During the fitting process we use the minimum During the fitting process we use the minimum required components which are necessary in order to required components which are necessary in order to get the best fit. The number of required components get the best fit. The number of required components is tested using F-test while the best fit is checked is tested using F-test while the best fit is checked using T-test.using T-test.

In Table 1 we present the In Table 1 we present the studied QSOsstudied QSOs..

In Column 1 the name of each QSO is given In Column 2 we present the Modified Julian Date, the Plate and the Fiber.

In column 3 we can see the redshift of each active galaxy and

In Column 4 we give the date that each spectrum was obtained.

Table IObject Name (SDSS) MJD-Plate-Fiber Redshift Date

J004323.43-001552.4 51794 0393 181‐ ‐ 2,81671 7/9/2000, 8:10

J104109.86+001051.76 51913 0274 482‐ ‐ 2,25924 4/1/2001, 11:00

J001502.26+001212.4 51795 0389 465‐ ‐ 2,85152 7/9/2000, 6:08

J104841.03+000042.81 51909 0276 310‐ ‐ 2,03044 31/12/2000, 11:08

J015048.83+004126.29 51793 0402 505‐ ‐ 3,70225 6/9/2000, 10:06

J102517.58+003422.17 51941 0272 501‐ ‐ 1,88842 1/2/2001, 9:30

J031828.91-001523.17 51929 0413 170‐ ‐ 1,98447 20/1/2001, 4:23

J010336.40-005508.7 51816 0396 297‐ ‐ 2,44295 29/9/2000, 8:28

J005419.99+002727.9 51876 0394 514‐ ‐ 2,51946 21/11/2000, 2:17

J004732.73+002111.3 51794 0393 588‐ ‐ 2,87768 7/9/2000, 8:10

J023908.99-002121.42 51821 0408 179‐ ‐ 3,74 4/10/2000, 9:38

J004041.39-005537.3 51794 0393 298‐ ‐ 2,09094 7/9/2000, 8:10

J001438.28-010750.1 51795 0389 211‐ ‐ 1,81564 7/9/2000, 6:08

J023252.80-001351.17 51820 0407 158‐ ‐ 2,03289 3/10/2000, 9:41

J001025.90+005447.6 51795 0389 332‐ ‐ 2,84727 7/9/2000, 6:08

J110041.20+003631.98 51908 0277 437‐ ‐ 2,01143 30/12/2000, 11:19

J000056.89-010409.7 51791 0387 098‐ ‐ 2,12325 4/9/2000, 7:08

J003551.98+005726.4 51793 0392 449‐ ‐ 1,90110 6/9/2000, 8:20

J015024.44+004432.99 51793 0402 485‐ ‐ 2,00596 6/9/2000, 10:06

J000103.85-104630.2 52143-650-133 2.081 28/2/2000 5:52

J000913.77-095754.5 52141-651-519 2.076 28/2/2000 5:52

In the figures below we present the fitted spectra of the In the figures below we present the fitted spectra of the 2121 QSOs. QSOs. The black line represents the observed spectrum and the blue line The black line represents the observed spectrum and the blue line

represents the GR Model fit.represents the GR Model fit.

As we study the emission lines of the 21 HiHiBALQSOsBALQSOs with GR model we can calculate the

values of: the typical standard deviation ((σ),σ), the Lorentz distributiondistribution factor ((γγ)), , the source function at the observation time (S(See),), the FWHMFWHM, the column

density (CD)(CD),, the optical depth of the line center ((ξ) ξ) and the emission energy (E(Eemem).).

In the following table we can see the values of the In the following table we can see the values of the above important parameters.above important parameters.

The 21 HiBALQSOs were sorted in descending order of the clouds radial velocities beginning with the QSO that had the cloud with the highest radial velocity

# SDSS Name <Vrad> <σe> <ξ> <FWHM> <Ee> <CD> <γ>

1 J001502.26+001212.4 1934,5 8 0,5225 20,6325 5,019255 3,26E+102 J005419.99+002727.9 1354 11 0,5035 19,97 6,0717835 3,95E+10 0,383 J004041.39-005537.3 1161 10 0,76 20,2765 10,781985 7,01E+10 0,824 J104841.03+000042.81 1161 9,5 0,8075 18,5785 10,4530745 6,80E+10 0,415 J001025.90+005447.6 1112 6,5 1,425 19,2205 21,32396 1,39E+116 J023252.80-001351.17 1083,5 7 0,855 19,0495 9,721844 6,32E+107 J015048.83+004126.29 1064 8 0,5985 16,301 6,705215 4,36E+10 1,008 J104109.86+001051.76 967,5 10 0,7125 19,6875 9,8472525 6,40E+10 0,719 J004732.73+002111.3 774 11 0,8075 22,1155 17,0788 1,11E+11 0,71

10 J015024.44+004432.99 774 5 1,9 13,678 20,719395 1,35E+11 1,4111 J102517.58+003422.17 774 10,5 0,4465 20,744 6,1385985 3,99E+10 1,0012 J000913.77-095754.5 774 5 0,7 9,818 7,30375 4,75E+10 0,7113 J031828.91-001523.17 725,5 13,5 0,6175 28,322 9,884429 6,43E+10 1,1214 J023908.99-002121.42 678 10 0,76 19,3155 10,421867 6,78E+10 0,3815 J001438.28-010750.1 580,5 7,5 1,425 17,192 20,025975 1,30E+11 0,7116 J010336.40-005508.7 580,5 3 2,185 8,141 21,84706 1,42E+11 1,0017 J000103.85-104630.2 580,5 9 0,95 19,4225 15,809955 1,03E+11 0,9418 J004323.43-001552.4 387 11 0,57 20,737 6,241643 4,06E+10 0,6319 J000056.89-010409.7 97 5,2 0,95 10,973 16,622395 1,08E+11 0,8220 J110041.20+003631.98 0 9,5 0,76 18,4035 11,31933 7,38E+10 0,4521 J003551.98+005726.4 0 7 0,855 14,221 11,186945 7,27E+10 0,71

MeanMean    788,69788,69 8,448,44 0,910,91 17,9417,94 12,1212,12 7,88E+107,88E+10 0,770,77

STDVSTDV    460,43460,43 2,572,57 0,460,46 4,554,55 5,525,52 3,59E+103,59E+10 0,270,27

MaxMax 1249,121249,12 11,0111,01 1,371,37 22,4922,49 17,6417,64 1,15E+111,15E+11 1,041,04

MinMin 328,26328,26 5,875,87 0,450,45 13,3913,39 6,606,60 4,29E+104,29E+10 0,50,5

In the following diagrams we present the In the following diagrams we present the different values of all the above different values of all the above

parameters as a function of radial parameters as a function of radial velocities, velocities, that is an expression of the that is an expression of the distance from the galactic centerdistance from the galactic center

0

2

4

6

8

0 200 400 600 800 1000 1200 1400 1600 1800 2000

<ξ>

<Vrad> (km/s)

<Vrad> - <ξ>

048

1216202428

0 200 400 600 800 1000 1200 1400 1600 1800 2000<

σe>

<Vrad> (km/s)

<Vrad> - <σe>

01020304050

0 200 400 600 800 1000 1200 1400 1600 1800 2000

<E

e> (e

V)

<Vrad> (km/s)

<Vrad> - <Ee>

0,00E+00

1,00E+11

2,00E+11

3,00E+11

4,00E+11

0 200 400 600 800 1000 1200 1400 1600 1800 2000

<C

.D.>

<Vrad> (km/s)

<Vrad> - <C.D.>

0

20

40

60

0 200 400 600 800 1000 1200 1400 1600 1800 2000<F

WH

M>

(Å)

<Vrad> (km/s)

<Vrad> - <FWHM>

ConclusionsConclusions

1. The main point of our study is that now, The main point of our study is that now, as we can see in the tables above, with as we can see in the tables above, with GR model, we can calculate the values GR model, we can calculate the values of a group of important parameters of of a group of important parameters of the regions that produce the emission or the regions that produce the emission or absorption lines (clouds, blobs, disc). absorption lines (clouds, blobs, disc).

2.After a detailed analysis of the absorption spectra lines of the same group of 21 HiBALQSOs HiBALQSOs (as will be presented by Mr Stathopoulos in a next presentation) we we conclude that conclude that perhapsperhaps the resonance C IV emission spectral lines, present p Cyg present p Cyg profiles. profiles. This means that in a future work This means that in a future work we should try to calculate the mass loss we should try to calculate the mass loss from the regions that create these emission from the regions that create these emission lines.lines.

3.3. We fitted (simulated) all the resonance C IV We fitted (simulated) all the resonance C IV emission lines emission lines with a Voigt distributionwith a Voigt distribution. This This means that in the disc (or cloud) region that means that in the disc (or cloud) region that produces the C IV resonance lines, produces the C IV resonance lines, pressure existspressure exists, perhaps able to perhaps able to create a shock create a shock ((FromerthFromerth & & MeliaMelia 2001) 2001) due to great decrease of the kinematic due to great decrease of the kinematic energy and energy and perhaps this is the reason of the radiant perhaps this is the reason of the radiant energyenergy..

4. As we can see As we can see we simulated the C IV emission we simulated the C IV emission lines with a Voigt distributionlines with a Voigt distribution,, this means with this means with a distribution with one picka distribution with one pick. In the case that the emission lines arise from an In the case that the emission lines arise from an emission disc emission disc ((Holt et alHolt et al. 1992. 1992, Collin, Collin--SouffrinSouffrin 1987, 1987, CollinCollin & & HureHure 2001) 2001), we know that the disc , we know that the disc model indicates such a shape only when the model indicates such a shape only when the observation line and the rotational axis of the disc observation line and the rotational axis of the disc form a small angle between 0-5 degrees form a small angle between 0-5 degrees ((see see AntonucciAntonucci, , RR. 1993).. 1993).

In this figure we can see In this figure we can see the theoretical emission profiles the theoretical emission profiles that arise from the disc model as a function of the that arise from the disc model as a function of the inclination anglesinclination angles ((ChenChen, , KK. & . & HalpernHalpern, , JJ. . PP. 1989). 1989)

In a next presentationIn a next presentation ((Thursday Thursday afternoon) Dr Lyratzi will present an afternoon) Dr Lyratzi will present an importantimportant study of Si IV resonance study of Si IV resonance

lineslines of the same group of 21 of the same group of 21 HiBALQSOs.HiBALQSOs.

Thank you very much for your attentionThank you very much for your attention

Blobs in the inner regions of the accretionBlobs in the inner regions of the accretion discdisc

Artistic depiction