High-Resolution X-ray Spectroscopy of AGN Warm Absorbers

Rebecca SmithMSSL, UCL

with G. Branduardi-Raymont and M. Page

Aims

Studying a variety of AGN warm absorbers Comparison offers clues to dynamics, chemical

composition, physical structure and origin High-resolution soft X-ray spectra vital

diagnostic tool Three objects presented today, focussing on data

from XMM-Newton RGS

Objects

Markarian 509

Seyfert 1

z=0.034

Very high luminosity Seyfert 1

L2-10keV

= 1.3-2.6x1044erg s-1

Galactic NH=4.4x1020cm-2

Bright X-ray NLS1

L2-10keV

= 2.4x1043erg s-1

Galactic NH=6.4x1020cm-2

Spectral variation between observations

L2-10keV

= 8x1042-3x1043erg s-1

Galactic NH=5.8x1020cm-2

Arakelian 564

NLS1

z=0.025

1H 0707-495

NLS1

z=0.041

Flux

(ph

oton

s m

-2s-1Å

-1)

Markarian 509 Phase 1:

log = 0.89±0.07

outflow vel = 510±200km s-1

NH = 0.79x1021cm-2

Phase 2:

log =2.14±0.08

outflow vel = 260±120km s-1

NH = 0.75x1021cm-2

Phase 3:

log = 3.26±0.03

outflow vel = 60±100km s-1

NH = 5.50x1021cm-2

Wavelength (Å)

XMM-Newton RGS

Smith et al. 2007

T

Thermal Stability Graph

Pressure form ionization parameter:

Phases with the same value of can be in pressure equilibrium and so exist within the same cloud

Smith et al. 2007

Flux

(ph

oton

s m

-2s-1Å

-1)

Arakelian 564 Phase 1:

log = 0.29±0.20

outflow vel = 10±90km s-1

Col Dens = 0.31x1021cm-2

Phase 2:

log = 2.56±0.09

outflow vel = 20±100km s-1

Col Dens = 0.71x1021cm-2

Narrow emission lines from OVIII

and NVII with outflow velocity ~

500km s-1

Wavelength (Å)

Smith et al. in prep

XMM-Newton RGS

1H 0707-495

Energy (keV)

Nor

mal

ized

cou

nts

/s /

keV

Spectral changes between 2000 observation (black) and 2002 observation (red)

Shift in energy of large feature at ~7keV

Gallo et al. 2004

XMM-Newton EPIC PN

2000

2002

2000

20022

Wavelength (Å)

Cou

nts

m-2s-1

Å-1

XMM-Newton RGS 1H 0707-495

Gallo et al. 2004

Two features, with ~8% energy shift

Change in ionization or velocity?

XMM-Newton RGS 1H 0707-495

1H 0707-495XMM-Newton EPIC PN

Wavelength (Å)

Energy (keV)

Cou

nts

m-2s-1Å

-1

norm

aliz

ed c

ount

s s-1

keV

-1

2002

2000

Smith et al. in prep

2002

2000

10 15 20 25 30 35

Cou

nts

m-2s-1

Å-1

XMM-Newton RGS 1H 0707-495

2000

2002

Wavelength (Å)

XMM-Newton RGS

Arakelian 564

Markarian 509

Cou

nts

m-2s-1Å

-1

1H 0707-495 2000

1H 0707-495 2002

10 15 20 25 30 35Wavelength (Å)

Conclusions Have analysed three Seyfert 1s with high-resolution soft X-

ray spectra

Interesting diversity of characteristics in outflows and emission features

Connected UV and X-ray absorbers in Mrk 509 and Ark 564

Mrk 509 shows strong broad emission lines consistent with the optical broad line region

Ark 564 has a highly ionized absorber with a surprisingly low outflow velocity

1H 0707-495 shows dramatic soft X-ray spectral variability in strength of warm absorber and energy of 'shoulder'