XEUS: X-ray photoionized plasma diagnostics modelling for XEUS

Th. BollerMPE Garching

He-like triplet simulations

The NGC 6240 case

Observations of obscured Seyfert galaxies

He-like triplet simulations: The Mrk 110 case

90%errosat restframe

XMM-Newton observation of the bright NLS1 Mrk 110

redshifted (z=0.023) and broad (13 eV) emission hump above the 3 limitwith respect to the He-like O VII line ratios for the resonance (r), intercombination (i) and forbidden lines (f).

first detection by Ogle 2004 in NGC 4051, but not redshiftedalso detected by E. Costantini 2005 in Mrk 279, but not redshifted

GR as a function of the distance to the central black hole

Kregion

OVIIprediction!!!

HeI5876H

H

predicts the distance of soft X-raylines to the central BH

soft X-ray lines fill gap between GR in the Optical and HE band

HeII4686

Baseline models pure GR effects or GR + bulk infall motions

GR Doppler factor

rela

tive fl

ux

g = 0.967DPR = 1.4

GR redshift + radial infall

- significant difference between in DPR for pure GR (2.5) and GR+infall (1.4)

- g from theoretical line profile consistent with g calculated from the observed redshift

The DPR is the critical discriminator and can be tested with better statistics

A 30 ks XEUS observation can disentangle between both scenarios

GR Doppler factor

g = 0.972DPR = 2.5

Pure GR redshift

100 ks XEUS NFI OVII simulations based on XMM-Newton data

Energy [keV]

f i

r

Counts

s-1

-1

keV

keV

-1-1ra

tio

O VII

z = 0

f i

r

z= 0.2 z = 0.4

f i

r

z = 0.8

f i

r

Even for the brightest galaxies the temperature und density determinationcan only be predicted for the local universe.

Simulations very uncertain. A factor of about 10 longer XMM-Newton observations are required to constrain the T and element abundances as well as other He-like triptles, e.g. C V, Ne IX, N VI, Mg XI, and SIX III.

The final He-triplet accuracy measurements will be done with XEUS.

Accuracy determination based on XMM-Newton data

rela

tive e

rror

[%]

Relative errors for the r, f, and i lines as a function of z.

Only the R value is constrained in the rest frame.

90%errorsat restframe

only the R value is constrained in the rest frame

the electron density is (3-8).1011 cm-3,

following Porquet and Dubau 2000

The G value (temperature) remains unconstrained

R value determination

The NGC 6240 case

XMM-Newton spectrum of NGC 6240

three plasma temperatures (0.6, 1.2, 5.6 keV) are constrained with a relative error of about 5%

the element abundances remain unconstrained

100 ks XEUS WFI simulations at z=1 and z=2.

the temperatures are constrained by about 3% at z=2.

in the rest frame the element abundances are constrained for He, O, Ne, Mg, and Si at z=1 only O, Ne, Mg, and Si are constrained by about 10%

at z=2 the element abundances remain unconstrained

rest frame z = 1 z = 2

0,00

5,00

10,00

15,00

20,00

25,00

30,00

35,00

40,00

45,00

50,00

He O Ne Mg Si

z=restframe

z=1

z=2

Temperature and abundance determination

the three temperatures are constrained by about 3% at z=2.

at z=2 the element abundances remainunconstrained

The following plots demonstrate that in the case of an obscured Seyfert galaxy the determination of element abundances are very uncertain based on the XMM-Newton statistics.

0,00

10,00

20,00

30,00

40,00

50,00

60,00

70,00

80,00

90,00

100,00

He C N O Ne Mg Al Si S Ar Ca

z=0,38

z=0,5

z=1,0

z=1,2

z=1,5

XMM-Newton

z=0.5 100 ks XEUS NFI z=1.0 100 ks XEUS NFI

rela

tive

err

or

element

Observations of obscured Seyfert galaxies The Mrk 273 case

Summary

To demonstrate the XEUS capabilities for determining the properties of X-ray photoionized plasma parameters in AGN, detailed WFI and NFI simulation have been performed.

One of the most important and challenging goals of XEUS is to precisely measure the plasma temperatures, element abundances as well as Broad-Line Region temperatures and densities from He-like triplets.

It is demonstrated that even for the brightest objects some parameters remain unconstrained in the simulations.

About a factor of 10 longer XMM-Newton observations are required to improve our predictions for X-ray photoionized plasma parameters for XEUS.

This is my suggestion for the XMM-Newton Project Scientist and the next panel members to discuss these results to be able to sharpen the XEUS science before the decision which LM will be dropped is done.