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Introduction RGS data analysis EPIC Pn data analysis Conclusions

The X-ray spectral signatures from the complex

circumnuclear regions in the Compton Thick Sy2,

Tololo 0109-383

Andrea Marinucci

Universitá degli studi Roma Tre

Stefano Bianchi, Giorgio Matt

Universitá degli studi Roma Tre

Andrew C. Fabian

Institute of Astronomy, Cambridge

Kazushi Iwasawa

Osservatorio Astronomico di Bologna

Giovanni Miniutti

Centro de Astrobiología (CSIC–INTA), Dep. de Astrofísica, LAEFF

Enrico Piconcelli

Osservatorio Astronomico di Roma (INAF)

Andrea Marinucci (Roma Tre) 26 Maggio 2010 1 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Table of contents

1 Introduction

2 RGS: phenomenological spectral analysis

3 RGS: CLOUDY self-consistent model

4 EPIC Pn: 5-10 keV spectral analysis

5 EPIC Pn: 0.6-10 keV spectral analysis

6 Conclusions

Andrea Marinucci (Roma Tre) 26 Maggio 2010 2 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Table of contents

1 Introduction

2 RGS: phenomenological spectral analysis

3 RGS: CLOUDY self-consistent model

4 EPIC Pn: 5-10 keV spectral analysis

5 EPIC Pn: 0.6-10 keV spectral analysis

6 Conclusions

Andrea Marinucci (Roma Tre) 26 Maggio 2010 2 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Table of contents

1 Introduction

2 RGS: phenomenological spectral analysis

3 RGS: CLOUDY self-consistent model

4 EPIC Pn: 5-10 keV spectral analysis

5 EPIC Pn: 0.6-10 keV spectral analysis

6 Conclusions

Andrea Marinucci (Roma Tre) 26 Maggio 2010 2 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Table of contents

1 Introduction

2 RGS: phenomenological spectral analysis

3 RGS: CLOUDY self-consistent model

4 EPIC Pn: 5-10 keV spectral analysis

5 EPIC Pn: 0.6-10 keV spectral analysis

6 Conclusions

Andrea Marinucci (Roma Tre) 26 Maggio 2010 2 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Table of contents

1 Introduction

2 RGS: phenomenological spectral analysis

3 RGS: CLOUDY self-consistent model

4 EPIC Pn: 5-10 keV spectral analysis

5 EPIC Pn: 0.6-10 keV spectral analysis

6 Conclusions

Andrea Marinucci (Roma Tre) 26 Maggio 2010 2 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Table of contents

1 Introduction

2 RGS: phenomenological spectral analysis

3 RGS: CLOUDY self-consistent model

4 EPIC Pn: 5-10 keV spectral analysis

5 EPIC Pn: 0.6-10 keV spectral analysis

6 Conclusions

Andrea Marinucci (Roma Tre) 26 Maggio 2010 2 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

The importance of being a Sy2

Most of our knowledge on the X-ray properties circumnuclear matter in Seyfert galaxies

is based on the brightest Compton-thick Seyfert 2 sources, such as Circinus (Matt et al.

1999, Sambruna et al. 2001, Molendi et al. 2003), NGC 1068 (Kinkhabwala et al. 2002,

Matt et al. 2004) and Mrk 3 (Sako et al. 2000, Bianchi et al. 2005).

Tololo 0109-383 (a.k.a. NGC 424, z=0.0117) is one

of the brightest Compton-thick Seyfert galaxies

(Matt et al. 2000).

It was observed (for less than 10 ks) by Chandra and

XMM-Newton (Matt et al. 2003).

We present here a new, long (∼ 100 ks)

XMM-Newton observation of this Tololo 0109-383, to

investigate the properties of its circumnuclear

regions in higher detail.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 3 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

The importance of being a Sy2

Most of our knowledge on the X-ray properties circumnuclear matter in Seyfert galaxies

is based on the brightest Compton-thick Seyfert 2 sources, such as Circinus (Matt et al.

1999, Sambruna et al. 2001, Molendi et al. 2003), NGC 1068 (Kinkhabwala et al. 2002,

Matt et al. 2004) and Mrk 3 (Sako et al. 2000, Bianchi et al. 2005).

Tololo 0109-383 (a.k.a. NGC 424, z=0.0117) is one

of the brightest Compton-thick Seyfert galaxies

(Matt et al. 2000).

It was observed (for less than 10 ks) by Chandra and

XMM-Newton (Matt et al. 2003).

We present here a new, long (∼ 100 ks)

XMM-Newton observation of this Tololo 0109-383, to

investigate the properties of its circumnuclear

regions in higher detail.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 3 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

The importance of X-ray spectroscopy

Using the RGS and the EPIC Pn spectra interesting properties of the circumnuclear

environment of AGNs can be drawn.

RGS Spectrum

EPIC Pn Spectrum

Ionisation state of the soft X-ray

emitting gas.

O vii K α Triplet diagnostics

O vii, O viii, C vi sharp RRC

emission lines.

Properties of the circumnuclear molecular

torus (geometry, abundances).

Compton reflection

Neutral Fe and Ni Kα fluorescent

lines.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 4 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

The importance of X-ray spectroscopy

Using the RGS and the EPIC Pn spectra interesting properties of the circumnuclear

environment of AGNs can be drawn.

RGS Spectrum

EPIC Pn Spectrum

Ionisation state of the soft X-ray

emitting gas.

O vii K α Triplet diagnostics

O vii, O viii, C vi sharp RRC

emission lines.

Properties of the circumnuclear molecular

torus (geometry, abundances).

Compton reflection

Neutral Fe and Ni Kα fluorescent

lines.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 4 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

The importance of X-ray spectroscopy

Using the RGS and the EPIC Pn spectra interesting properties of the circumnuclear

environment of AGNs can be drawn.

RGS Spectrum

EPIC Pn Spectrum

Ionisation state of the soft X-ray

emitting gas.

O vii K α Triplet diagnostics

O vii, O viii, C vi sharp RRC

emission lines.

Properties of the circumnuclear molecular

torus (geometry, abundances).

Compton reflection

Neutral Fe and Ni Kα fluorescent

lines.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 4 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

The importance of X-ray spectroscopy

Using the RGS and the EPIC Pn spectra interesting properties of the circumnuclear

environment of AGNs can be drawn.

RGS Spectrum

EPIC Pn Spectrum

Ionisation state of the soft X-ray

emitting gas.

O vii K α Triplet diagnostics

O vii, O viii, C vi sharp RRC

emission lines.

Properties of the circumnuclear molecular

torus (geometry, abundances).

Compton reflection

Neutral Fe and Ni Kα fluorescent

lines.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 4 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

The importance of X-ray spectroscopy

Using the RGS and the EPIC Pn spectra interesting properties of the circumnuclear

environment of AGNs can be drawn.

RGS Spectrum

EPIC Pn Spectrum

Ionisation state of the soft X-ray

emitting gas.

O vii K α Triplet diagnostics

O vii, O viii, C vi sharp RRC

emission lines.

Properties of the circumnuclear molecular

torus (geometry, abundances).

Compton reflection

Neutral Fe and Ni Kα fluorescent

lines.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 4 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

The importance of X-ray spectroscopy

Using the RGS and the EPIC Pn spectra interesting properties of the circumnuclear

environment of AGNs can be drawn.

RGS Spectrum

EPIC Pn Spectrum

Ionisation state of the soft X-ray

emitting gas.

O vii K α Triplet diagnostics

O vii, O viii, C vi sharp RRC

emission lines.

Properties of the circumnuclear molecular

torus (geometry, abundances).

Compton reflection

Neutral Fe and Ni Kα fluorescent

lines.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 4 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

The importance of X-ray spectroscopy

Using the RGS and the EPIC Pn spectra interesting properties of the circumnuclear

environment of AGNs can be drawn.

RGS Spectrum

EPIC Pn Spectrum

Ionisation state of the soft X-ray

emitting gas.

O vii K α Triplet diagnostics

O vii, O viii, C vi sharp RRC

emission lines.

Properties of the circumnuclear molecular

torus (geometry, abundances).

Compton reflection

Neutral Fe and Ni Kα fluorescent

lines.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 4 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: phenomenological spectral analysis

The soft X-ray RGS spectrum is mostly due to line emission, from H-like and He-like C,

N, O and Ne, as well as Fe L-shell.

The spectrum also presents radiative

recombination continua (RRC) from O vii,

O viii and C vi. These features were fitted

with the REDGE model in XSPEC.

Line Id. Energy kT Fluxes

C vi RRC 0.490 +0.001

−0.001

O vii RRC 0.736 +0.003

−0.003

10 +6

−4

6 +3

−3

2.3 +0.7

−0.7

0.8 +0.4

−0.3

O viii RRC 0.871 +0.004

−0.003

6 +3

−3 * 0.3+0.2 −0.2

A weak resonance line compared to the

forbidden or the intercombination lines is

typical of plasmas dominated by

photoionization

(Porquet & Dubau 2000).

Energies are in keV units, fluxes in 10 −5 ph cm −2

s −1 , kT in eV.

The soft X-ray emitting gas is in Photoionisation Equilibrium.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 5 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: phenomenological spectral analysis

The soft X-ray RGS spectrum is mostly due to line emission, from H-like and He-like C,

N, O and Ne, as well as Fe L-shell.

The spectrum also presents radiative

recombination continua (RRC) from O vii,

O viii and C vi. These features were fitted

with the REDGE model in XSPEC.

Line Id. Energy kT Fluxes

C vi RRC 0.490 +0.001

−0.001

O vii RRC 0.736 +0.003

−0.003

10 +6

−4

6 +3

−3

2.3 +0.7

−0.7

0.8 +0.4

−0.3

O viii RRC 0.871 +0.004

−0.003

6 +3

−3 * 0.3+0.2 −0.2

A weak resonance line compared to the

forbidden or the intercombination lines is

typical of plasmas dominated by

photoionization

(Porquet & Dubau 2000).

Energies are in keV units, fluxes in 10 −5 ph cm −2

s −1 , kT in eV.

The soft X-ray emitting gas is in Photoionisation Equilibrium.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 5 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: phenomenological spectral analysis

The soft X-ray RGS spectrum is mostly due to line emission, from H-like and He-like C,

N, O and Ne, as well as Fe L-shell.

The spectrum also presents radiative

recombination continua (RRC) from O vii,

O viii and C vi. These features were fitted

with the REDGE model in XSPEC.

Line Id. Energy kT Fluxes

C vi RRC 0.490 +0.001

−0.001

O vii RRC 0.736 +0.003

−0.003

10 +6

−4

6 +3

−3

2.3 +0.7

−0.7

0.8 +0.4

−0.3

O viii RRC 0.871 +0.004

−0.003

6 +3

−3 * 0.3+0.2 −0.2

A weak resonance line compared to the

forbidden or the intercombination lines is

typical of plasmas dominated by

photoionization

(Porquet & Dubau 2000).

Energies are in keV units, fluxes in 10 −5 ph cm −2

s −1 , kT in eV.

The soft X-ray emitting gas is in Photoionisation Equilibrium.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 5 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: phenomenological spectral analysis

The soft X-ray RGS spectrum is mostly due to line emission, from H-like and He-like C,

N, O and Ne, as well as Fe L-shell.

The spectrum also presents radiative

recombination continua (RRC) from O vii,

O viii and C vi. These features were fitted

with the REDGE model in XSPEC.

Line Id. Energy kT Fluxes

C vi RRC 0.490 +0.001

−0.001

O vii RRC 0.736 +0.003

−0.003

10 +6

−4

6 +3

−3

2.3 +0.7

−0.7

0.8 +0.4

−0.3

O viii RRC 0.871 +0.004

−0.003

6 +3

−3 * 0.3+0.2 −0.2

A weak resonance line compared to the

forbidden or the intercombination lines is

typical of plasmas dominated by

photoionization

(Porquet & Dubau 2000).

Energies are in keV units, fluxes in 10 −5 ph cm −2

s −1 , kT in eV.

The soft X-ray emitting gas is in Photoionisation Equilibrium.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 5 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: CLOUDY self-consistent model

The high quality of the RGS spectrum, coupled with the results from the

phenomenological spectral analysis, encouraged us to build a self-consistent model able

to reproduce the whole spectrum, in a wavelength range from 8 ˚A up to 35 ˚A.

We produced a grid model for xspec using cloudy 08.00.

It is an extension of the same model used in Bianchi et al. 2010.

The main ingredients are:

plane parallel geometry,

flux of photons striking the illuminated face of the cloud given in terms of

ionisation parameter U,

incident continuum modelled as in Korista et al. 97; constant electron density

n e = 10 5 cm −3 ,

grid parameters are log U = [−2.00 : 4.00], step 0.25, and log N H = [19.0 : 23.5],

step 0.1,

only the reflected spectrum, arising from the illuminated face of the cloud, is taken

into account in our model.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 6 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: CLOUDY self-consistent model

The high quality of the RGS spectrum, coupled with the results from the

phenomenological spectral analysis, encouraged us to build a self-consistent model able

to reproduce the whole spectrum, in a wavelength range from 8 ˚A up to 35 ˚A.

We produced a grid model for xspec using cloudy 08.00.

It is an extension of the same model used in Bianchi et al. 2010.

The main ingredients are:

plane parallel geometry,

flux of photons striking the illuminated face of the cloud given in terms of

ionisation parameter U,

incident continuum modelled as in Korista et al. 97; constant electron density

n e = 10 5 cm −3 ,

grid parameters are log U = [−2.00 : 4.00], step 0.25, and log N H = [19.0 : 23.5],

step 0.1,

only the reflected spectrum, arising from the illuminated face of the cloud, is taken

into account in our model.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 6 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: CLOUDY self-consistent model

The high quality of the RGS spectrum, coupled with the results from the

phenomenological spectral analysis, encouraged us to build a self-consistent model able

to reproduce the whole spectrum, in a wavelength range from 8 ˚A up to 35 ˚A.

We produced a grid model for xspec using cloudy 08.00.

It is an extension of the same model used in Bianchi et al. 2010.

The main ingredients are:

plane parallel geometry,

flux of photons striking the illuminated face of the cloud given in terms of

ionisation parameter U,

incident continuum modelled as in Korista et al. 97; constant electron density

n e = 10 5 cm −3 ,

grid parameters are log U = [−2.00 : 4.00], step 0.25, and log N H = [19.0 : 23.5],

step 0.1,

only the reflected spectrum, arising from the illuminated face of the cloud, is taken

into account in our model.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 6 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: CLOUDY self-consistent model

The high quality of the RGS spectrum, coupled with the results from the

phenomenological spectral analysis, encouraged us to build a self-consistent model able

to reproduce the whole spectrum, in a wavelength range from 8 ˚A up to 35 ˚A.

We produced a grid model for xspec using cloudy 08.00.

It is an extension of the same model used in Bianchi et al. 2010.

The main ingredients are:

plane parallel geometry,

flux of photons striking the illuminated face of the cloud given in terms of

ionisation parameter U,

incident continuum modelled as in Korista et al. 97; constant electron density

n e = 10 5 cm −3 ,

grid parameters are log U = [−2.00 : 4.00], step 0.25, and log N H = [19.0 : 23.5],

step 0.1,

only the reflected spectrum, arising from the illuminated face of the cloud, is taken

into account in our model.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 6 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: CLOUDY self-consistent model

The high quality of the RGS spectrum, coupled with the results from the

phenomenological spectral analysis, encouraged us to build a self-consistent model able

to reproduce the whole spectrum, in a wavelength range from 8 ˚A up to 35 ˚A.

We produced a grid model for xspec using cloudy 08.00.

It is an extension of the same model used in Bianchi et al. 2010.

The main ingredients are:

plane parallel geometry,

flux of photons striking the illuminated face of the cloud given in terms of

ionisation parameter U,

incident continuum modelled as in Korista et al. 97; constant electron density

n e = 10 5 cm −3 ,

grid parameters are log U = [−2.00 : 4.00], step 0.25, and log N H = [19.0 : 23.5],

step 0.1,

only the reflected spectrum, arising from the illuminated face of the cloud, is taken

into account in our model.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 6 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: CLOUDY self-consistent model

The high quality of the RGS spectrum, coupled with the results from the

phenomenological spectral analysis, encouraged us to build a self-consistent model able

to reproduce the whole spectrum, in a wavelength range from 8 ˚A up to 35 ˚A.

We produced a grid model for xspec using cloudy 08.00.

It is an extension of the same model used in Bianchi et al. 2010.

The main ingredients are:

plane parallel geometry,

flux of photons striking the illuminated face of the cloud given in terms of

ionisation parameter U,

incident continuum modelled as in Korista et al. 97; constant electron density

n e = 10 5 cm −3 ,

grid parameters are log U = [−2.00 : 4.00], step 0.25, and log N H = [19.0 : 23.5],

step 0.1,

only the reflected spectrum, arising from the illuminated face of the cloud, is taken

into account in our model.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 6 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: CLOUDY self-consistent model

The final Cash/dof= 4567/4429.

The total flux in the 0.35 − 1.55 keV band is (2.2 +0.2

−0.6 ) × 10−13 erg cm −2 s −1 ,

almost equally distributed between the two photoionised phases.

A systemic blueshift of −230 +90

−120 km s−1 is required by the fit.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 7 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

RGS: CLOUDY self-consistent model

Detected emission lines in the XMM-Newton RGS spectra of Tololo 0109-383.

Line Id. E T Energy kT Fluxes

(a) (b) (c) (d)

C vi Kα 0.367 0.3675 +0.0002

−0.0002

- 1.4 +0.9

−0.8

1.24 0.57 0.67

N vii Kα 0.500 0.500 +0.005

−0.007

- 0.5 +0.3

−0.2

0.32 0.23 0.09

0.561 (f) 0.5616 +0.0001

−0.0001

- 5.0 +0.7

−0.7

3.82 0.53 3.28

O vii Kα 0.569 (i) 0.569 - < 0.7 0.94 0.13 0.81

0.574 (r) 0.5736 +0.0007

−0.0005

- 1.0 +0.5

−0.4

0.98 0.21 0.76

O viii Kα 0.654 0.6537 +0.0006

−0.0006

- 1.1 +0.3

−0.3

1.12 0.99 0.13

O vii RRC 0.739 0.736 +0.003

−0.003

6 +3

−3

0.8 +0.4

−0.3

0.72 0.19 0.53

O viii RRC 0.871 0.871 +0.004

−0.003

6 +3

−3 * 0.3+0.2 −0.2

0.60 0.54 0.06

0.905 (f) 0.904 +0.001

−0.003

- 0.4 +0.3

−0.2

Ne ix Kα 0.915 (i) 0.916 - 0.3 +0.3

−0.2

0.922 (r) 0.921 +0.001

−0.001

- 0.5 +0.3

−0.2

0.40 0.25 0.15

0.13 0.08 0.05

0.20 0.12 0.08

(a) Calculated fluxes with the phenomenological analysis; (b) Line fluxes extrapolated from the

RGS1+RGS2 best fit with CLOUDY; (c) Line fluxes arising from the component with higher

photoionisation parameter (log U = 1.3 +0.3

−0.2 , log N H = 21.9 +0.8

−0.6

); (d) Line fluxes arising from the

second photoionised phase (log U = 0.1 +0.2

−0.8 , log N H = 21.7 +0.4

−0.5 ).

Andrea Marinucci (Roma Tre) 26 Maggio 2010 8 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

EPIC Pn: 5-10 keV spectral analysis

In the hard part of the spectrum (5-10 keV), prominent emission lines can be clearly

observed. Following Iwasawa et al. 2001 and Matt et al. 2003, it has been fitted with a

model composed of a strongly absorbed (2 × 10 24 cm −2 ) power-law with Γ = 2, a pure

cold reflection component (model pexrav in xspec) and as many emission lines as

required, all of them described by Gaussian profiles with a resulting χ 2 /dof = 49/58.

Id. Energy EW

Fe Kα 6.40 +0.02

−0.01

810 +130

−80

Fe Kβ 7.058 ∗ < 90

Fe XXVI Kα 6.966 ∗ 120 +70

−80

Ni Kα 7.472 ∗ 170 ± 70

Fe XXV Kα (f) 6.637 ∗ < 140

Fe XXV Kα (r) 6.700 ∗ < 150

Fe Kα Compton S. 6.300 ∗ 210 ± 80

∗ fixed at the theoretical value.

Energies are in keV and EWs in eV.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 9 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

EPIC Pn: 5-10 keV spectral analysis

In the hard part of the spectrum (5-10 keV), prominent emission lines can be clearly

observed. Following Iwasawa et al. 2001 and Matt et al. 2003, it has been fitted with a

model composed of a strongly absorbed (2 × 10 24 cm −2 ) power-law with Γ = 2, a pure

cold reflection component (model pexrav in xspec) and as many emission lines as

required, all of them described by Gaussian profiles with a resulting χ 2 /dof = 49/58.

Id. Energy EW

Fe Kα 6.40 +0.02

−0.01

810 +130

−80

Fe Kβ 7.058 ∗ < 90

Fe XXVI Kα 6.966 ∗ 120 +70

−80

Ni Kα 7.472 ∗ 170 ± 70

Fe XXV Kα (f) 6.637 ∗ < 140

Fe XXV Kα (r) 6.700 ∗ < 150

Fe Kα Compton S. 6.300 ∗ 210 ± 80

∗ fixed at the theoretical value.

Energies are in keV and EWs in eV.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 9 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

EPIC Pn: 5-10 keV spectral analysis

From the FWHM of the neutral Fe Kα line (FWHM=5287 +1760

−2200 km s−1 ) a

possible estimate to the inner radius of the molecular torus can be inferred:

r = 0.04 +0.06

−0.02 sin2 i pc

A choice of 30 ∘ or 60 ∘ leads to central values of 0.01 and 0.03 pc, respectively, for

the inner radius.

the iron abundance is measured by the depth of the iron edge in the Compton

reflection continuum, i.e. A F e = 1.00 +0.25

−0.17 in solar units.

from the observed Ni Kα to Fe Kα line fluxes, we can instead estimate the relative

abundances of the two elements.

The expected ratio ranges from 0.03 to 0.045 (Basko et al. 1978).

In our case, we measure 0.12 ± 0.05 (considering only the flux of the iron Kα core

line, excluding the CS), significantly larger than the expected one, indicating a

nickel-to-iron overabundance by a factor ≃ 2.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 10 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

EPIC Pn: 5-10 keV spectral analysis

From the FWHM of the neutral Fe Kα line (FWHM=5287 +1760

−2200 km s−1 ) a

possible estimate to the inner radius of the molecular torus can be inferred:

r = 0.04 +0.06

−0.02 sin2 i pc

A choice of 30 ∘ or 60 ∘ leads to central values of 0.01 and 0.03 pc, respectively, for

the inner radius.

the iron abundance is measured by the depth of the iron edge in the Compton

reflection continuum, i.e. A F e = 1.00 +0.25

−0.17 in solar units.

from the observed Ni Kα to Fe Kα line fluxes, we can instead estimate the relative

abundances of the two elements.

The expected ratio ranges from 0.03 to 0.045 (Basko et al. 1978).

In our case, we measure 0.12 ± 0.05 (considering only the flux of the iron Kα core

line, excluding the CS), significantly larger than the expected one, indicating a

nickel-to-iron overabundance by a factor ≃ 2.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 10 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

EPIC Pn: 5-10 keV spectral analysis

From the FWHM of the neutral Fe Kα line (FWHM=5287 +1760

−2200 km s−1 ) a

possible estimate to the inner radius of the molecular torus can be inferred:

r = 0.04 +0.06

−0.02 sin2 i pc

A choice of 30 ∘ or 60 ∘ leads to central values of 0.01 and 0.03 pc, respectively, for

the inner radius.

the iron abundance is measured by the depth of the iron edge in the Compton

reflection continuum, i.e. A F e = 1.00 +0.25

−0.17 in solar units.

from the observed Ni Kα to Fe Kα line fluxes, we can instead estimate the relative

abundances of the two elements.

The expected ratio ranges from 0.03 to 0.045 (Basko et al. 1978).

In our case, we measure 0.12 ± 0.05 (considering only the flux of the iron Kα core

line, excluding the CS), significantly larger than the expected one, indicating a

nickel-to-iron overabundance by a factor ≃ 2.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 10 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

EPIC Pn: 0.6-10 keV spectral analysis

Taking into account the results from the soft X-ray RGS spectrum, we finally performed

a self-consistent fit in the whole EPIC pn band (0.6-10 keV).

The final fit is good (χ 2 = 189/161 dof).

The best fit values for the three photoionisation components are:

log U 1 < −1.8, log N H1 = 21.49 +0.38

−0.14 ;

log U 2 = 1.47 +0.06

−0.07 , log N H2 = 21.6 ± 0.2;

log U 3 = 2.32 +0.10

−0.14 , log N H3 < 20.9.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 11 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

EPIC Pn: 0.6-10 keV spectral analysis

Taking into account the results from the soft X-ray RGS spectrum, we finally performed

a self-consistent fit in the whole EPIC pn band (0.6-10 keV).

The final fit is good (χ 2 = 189/161 dof).

The best fit values for the three photoionisation components are:

log U 1 < −1.8, log N H1 = 21.49 +0.38

−0.14 ;

log U 2 = 1.47 +0.06

−0.07 , log N H2 = 21.6 ± 0.2;

log U 3 = 2.32 +0.10

−0.14 , log N H3 < 20.9.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 11 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

EPIC Pn: 0.6-10 keV spectral analysis

Taking into account the results from the soft X-ray RGS spectrum, we finally performed

a self-consistent fit in the whole EPIC pn band (0.6-10 keV).

The final fit is good (χ 2 = 189/161 dof).

The best fit values for the three photoionisation components are:

log U 1 < −1.8, log N H1 = 21.49 +0.38

−0.14 ;

log U 2 = 1.47 +0.06

−0.07 , log N H2 = 21.6 ± 0.2;

log U 3 = 2.32 +0.10

−0.14 , log N H3 < 20.9.

Andrea Marinucci (Roma Tre) 26 Maggio 2010 11 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Conclusions

The soft X-ray RGS spectrum of Tololo 0109-383 is mostly due to line emission,

from H-like and He-like C, N, O and Ne, as well as Fe L-shell, as commonly found

in obscured AGN (Guainazzi & Bianchi 2007),

the soft X-ray emitting region is in Photoionisation Equilibrium,

a self-consistent photoionisation model well reproduces the RGS spectrum,

adopting two gas phases with different ionisation parameters and column densities,

the high-energy part of the spectrum confirmed its nature as a Compton-thick

source,

when the self-consistent model is applied to the 0.6-10 keV band of the EPIC Pn

spectrum, a third photoionised phase is needed to account for emission lines with

higher ionisation potential. Even if the χ 2 /dof is good, the underprediction of

some emission lines suggests a more complex interaction between the different

photoionised phases.

Details in: Marinucci A., Bianchi S., Matt G., Fabian A. C., Iwasawa K., Miniutti G.,

Piconcelli E. ’The X-ray spectral signatures from the complex circumnuclear

regions in the Compton Thick Sy2, Tololo 0109-383’ (in prep.)

Andrea Marinucci (Roma Tre) 26 Maggio 2010 12 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Conclusions

The soft X-ray RGS spectrum of Tololo 0109-383 is mostly due to line emission,

from H-like and He-like C, N, O and Ne, as well as Fe L-shell, as commonly found

in obscured AGN (Guainazzi & Bianchi 2007),

the soft X-ray emitting region is in Photoionisation Equilibrium,

a self-consistent photoionisation model well reproduces the RGS spectrum,

adopting two gas phases with different ionisation parameters and column densities,

the high-energy part of the spectrum confirmed its nature as a Compton-thick

source,

when the self-consistent model is applied to the 0.6-10 keV band of the EPIC Pn

spectrum, a third photoionised phase is needed to account for emission lines with

higher ionisation potential. Even if the χ 2 /dof is good, the underprediction of

some emission lines suggests a more complex interaction between the different

photoionised phases.

Details in: Marinucci A., Bianchi S., Matt G., Fabian A. C., Iwasawa K., Miniutti G.,

Piconcelli E. ’The X-ray spectral signatures from the complex circumnuclear

regions in the Compton Thick Sy2, Tololo 0109-383’ (in prep.)

Andrea Marinucci (Roma Tre) 26 Maggio 2010 12 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Conclusions

The soft X-ray RGS spectrum of Tololo 0109-383 is mostly due to line emission,

from H-like and He-like C, N, O and Ne, as well as Fe L-shell, as commonly found

in obscured AGN (Guainazzi & Bianchi 2007),

the soft X-ray emitting region is in Photoionisation Equilibrium,

a self-consistent photoionisation model well reproduces the RGS spectrum,

adopting two gas phases with different ionisation parameters and column densities,

the high-energy part of the spectrum confirmed its nature as a Compton-thick

source,

when the self-consistent model is applied to the 0.6-10 keV band of the EPIC Pn

spectrum, a third photoionised phase is needed to account for emission lines with

higher ionisation potential. Even if the χ 2 /dof is good, the underprediction of

some emission lines suggests a more complex interaction between the different

photoionised phases.

Details in: Marinucci A., Bianchi S., Matt G., Fabian A. C., Iwasawa K., Miniutti G.,

Piconcelli E. ’The X-ray spectral signatures from the complex circumnuclear

regions in the Compton Thick Sy2, Tololo 0109-383’ (in prep.)

Andrea Marinucci (Roma Tre) 26 Maggio 2010 12 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Conclusions

The soft X-ray RGS spectrum of Tololo 0109-383 is mostly due to line emission,

from H-like and He-like C, N, O and Ne, as well as Fe L-shell, as commonly found

in obscured AGN (Guainazzi & Bianchi 2007),

the soft X-ray emitting region is in Photoionisation Equilibrium,

a self-consistent photoionisation model well reproduces the RGS spectrum,

adopting two gas phases with different ionisation parameters and column densities,

the high-energy part of the spectrum confirmed its nature as a Compton-thick

source,

when the self-consistent model is applied to the 0.6-10 keV band of the EPIC Pn

spectrum, a third photoionised phase is needed to account for emission lines with

higher ionisation potential. Even if the χ 2 /dof is good, the underprediction of

some emission lines suggests a more complex interaction between the different

photoionised phases.

Details in: Marinucci A., Bianchi S., Matt G., Fabian A. C., Iwasawa K., Miniutti G.,

Piconcelli E. ’The X-ray spectral signatures from the complex circumnuclear

regions in the Compton Thick Sy2, Tololo 0109-383’ (in prep.)

Andrea Marinucci (Roma Tre) 26 Maggio 2010 12 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Conclusions

The soft X-ray RGS spectrum of Tololo 0109-383 is mostly due to line emission,

from H-like and He-like C, N, O and Ne, as well as Fe L-shell, as commonly found

in obscured AGN (Guainazzi & Bianchi 2007),

the soft X-ray emitting region is in Photoionisation Equilibrium,

a self-consistent photoionisation model well reproduces the RGS spectrum,

adopting two gas phases with different ionisation parameters and column densities,

the high-energy part of the spectrum confirmed its nature as a Compton-thick

source,

when the self-consistent model is applied to the 0.6-10 keV band of the EPIC Pn

spectrum, a third photoionised phase is needed to account for emission lines with

higher ionisation potential. Even if the χ 2 /dof is good, the underprediction of

some emission lines suggests a more complex interaction between the different

photoionised phases.

Details in: Marinucci A., Bianchi S., Matt G., Fabian A. C., Iwasawa K., Miniutti G.,

Piconcelli E. ’The X-ray spectral signatures from the complex circumnuclear

regions in the Compton Thick Sy2, Tololo 0109-383’ (in prep.)

Andrea Marinucci (Roma Tre) 26 Maggio 2010 12 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Conclusions

The soft X-ray RGS spectrum of Tololo 0109-383 is mostly due to line emission,

from H-like and He-like C, N, O and Ne, as well as Fe L-shell, as commonly found

in obscured AGN (Guainazzi & Bianchi 2007),

the soft X-ray emitting region is in Photoionisation Equilibrium,

a self-consistent photoionisation model well reproduces the RGS spectrum,

adopting two gas phases with different ionisation parameters and column densities,

the high-energy part of the spectrum confirmed its nature as a Compton-thick

source,

when the self-consistent model is applied to the 0.6-10 keV band of the EPIC Pn

spectrum, a third photoionised phase is needed to account for emission lines with

higher ionisation potential. Even if the χ 2 /dof is good, the underprediction of

some emission lines suggests a more complex interaction between the different

photoionised phases.

Details in: Marinucci A., Bianchi S., Matt G., Fabian A. C., Iwasawa K., Miniutti G.,

Piconcelli E. ’The X-ray spectral signatures from the complex circumnuclear

regions in the Compton Thick Sy2, Tololo 0109-383’ (in prep.)

Andrea Marinucci (Roma Tre) 26 Maggio 2010 12 / 12


Introduction RGS data analysis EPIC Pn data analysis Conclusions

Conclusions

The soft X-ray RGS spectrum of Tololo 0109-383 is mostly due to line emission,

from H-like and He-like C, N, O and Ne, as well as Fe L-shell, as commonly found

in obscured AGN (Guainazzi & Bianchi 2007),

the soft X-ray emitting region is in Photoionisation Equilibrium,

a self-consistent photoionisation model well reproduces the RGS spectrum,

adopting two gas phases with different ionisation parameters and column densities,

the high-energy part of the spectrum confirmed its nature as a Compton-thick

source,

when the self-consistent model is applied to the 0.6-10 keV band of the EPIC Pn

spectrum, a third photoionised phase is needed to account for emission lines with

higher ionisation potential. Even if the χ 2 /dof is good, the underprediction of

some emission lines suggests a more complex interaction between the different

photoionised phases.

Details in: Marinucci A., Bianchi S., Matt G., Fabian A. C., Iwasawa K., Miniutti G.,

Piconcelli E. ’The X-ray spectral signatures from the complex circumnuclear

regions in the Compton Thick Sy2, Tololo 0109-383’ (in prep.)

Andrea Marinucci (Roma Tre) 26 Maggio 2010 12 / 12

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