Kaspi et al 2002

Constraints on the Velocity Distribution in the NGC 3783 Warm AbsorberT. Kallman, Laboratory for X-ray Astrophysics, NASA/GSFC

900 ksec Chandra HETG observation of NGC3783 >100 absorption features blueshifted, v~800 km/s broadened, vturb~300 km/s emission in some components fit to 2 photoionization model components Piecewise continuum Not a full global fit Kaspi et al 2002

>100 absorption features blueshifted, v~800 km/s broadened, vturb~300 km/s emission in some components fit to 2 photoionization model components Fe M shell UTA fitted using Gaussian approximation Full global model Krongold et al 2004

fit to 2 photoionization model components Ionization parameter and temperature are consistent with coexistence in the same physical region Disfavored existence of intermediate ionization gas due to shape of Fe M shell UTA But used simplified atomic model for UTA Krongold et al 2004 Curve of thermal equilibrium for photoionized gas Flux/pressure

Combined model for dynamics and spectrum Assumes ballistic trajectories Favors clumped wind Chelouche and Netzer 2005

Fitted the XMM RGS spectrum using global model Also find evidence for two components Omit Ca Include line-by-line treatment of M shell UTA, but still miss some Claim evidence for higher ionization parameter material require large overabundance of iron Blustin et al. (2004)

Work so far on fitting warm absorber spectra has concentrated on the assumption of a small number of discrete components This places important constraints on the flow dynamics, if it is true There is no obvious a priori reason why outflows should favor a small number or range of physical conditions In this talk I will test models in which the ionization distribution is continuous rather than discrete, and discuss something about what it means Previous tests of this have invoked simplified models for the Fe M shell UTA which may affect the result

Disk winds have smooth density distributions on the scales which can be Calculated… Proga and Kallman 2004

Work so far on fitting warm absorber spectra has concentrated on the assumption of a small number of discrete components This places important constraints on the flow dynamics, if it is true It is not obvious why outflows should favor a small number or range of physical conditions I will examine the robustness of this result and discuss some implications Outline

I will not discuss details about Line Profile Shapes, widths and blueshifts • Lines are not symmetric • blue wing is more extended in lines from ions which occur at smaller ionization parameter (eg. O VIII La vs. S XVI) • Suggests that higher velocity material is less ionized (Ramirez et al. 2005)

As a start, fit to a continuum plus Gaussian absorption lines. Choose a continuum consisting of a double power law plus cold absorption (G1=1.5, G2=3, log(NH)=22.5; This is a cheat because it already takes into account some of the absorbtion, but does not strongly affect the results) 3 4 4 5 5 6 6 7 7 8 8 9 9 10 10 11 11 12 12 13 13 14 14 15 15 16 16 17 17 18 18 19 wavelength (A) c2~64905/8192

Absorption lines are placed randomly and strength and width adjusted to improve the fit. 3 4 4 5 5 6 6 7 7 8 8 9 9 10 10 11 11 12 12 13 13 14 14 15 15 16 16 17 17 18 18 19 wavelength (A) c2~64602/8192

Results of notch model: • requires ~950 lines, Ids for ~100 • c2~9915/8192 • 300 km/s<v/c<2000 • Represents best achievable c2 (by me) • Allows line Ids • Shows distribution of line widths, offsets

Ionization parameter of maximum ion abundance vs. line wavelength for identified lines • requires ~950 lines, Ids for ~100 • c2~9915/8192 • 300 km/s<v/c<2000 • Represents best achievable c2 (by me) • Allows line Ids • Shows distribution of line widths, offsets

Favored region

Photoionization Models • Full global model • Pure absorption (maybe misses something important?) • Single velocity component • Xstar version 2.1l • Inner M shell 2-3 UTAs (FAC; Gu); >400 lines explicitly calculated • Chianti v. 5 data for iron L • Iron K shell data from R matrix (Bautista, Palmeri, Mendoza et al) • Available from xstar website, as are ready-made tables • Not in current release version, 2.1kn4 • Xspec ‘analytic model’ warmabs • Not fully self consistent: assumes uniform ionization absorber, but this is small error for low columns. • Xspec11 only at present, not quite ready for prime time

Comparison of model properties

single Component Fit, logx=2.4 3 4 4 5 5 6 6 7 7 8 8 9 9 10 10 11 11 12 12 13 13 14 14 15 15 16 16 17 17 18 18 19 wavelength (A) Missing lines near 16-17A c2~27811/8192, voff=700 km/s vturb=300 km/s

2 Component Fit, logx=2.4, 0.1 3 4 4 5 5 6 6 7 7 8 8 9 9 10 10 11 11 12 12 13 13 14 14 15 15 16 16 17 17 18 18 19 wavelength (A) Better, Some l discrepancies, Missing lines c2~18516/8192, voff=700 km/s vturb=300 km/s

Fitting absorption only is fraught, due to influence of scattering/reemission

Si VII-XI K lines

Al XII Al XIII

Fe XX-XXII

Fe XXII

Fe XXI

Comparison with previous work

2 component fit: 2 component fit:

What if the distribution is continuous instead?

Continuous distribution, 0.1<logx<2.4 3 4 4 5 5 6 6 7 7 8 8 9 9 10 10 11 11 12 12 13 13 14 14 15 15 16 16 17 17 18 18 19 wavelength (A) Over-predicts the absorption Due to intermediate iron ions c2~20071/8192, voff=700 km/s vturb=300 km/s

Continuous distribution, 0.1<logx<2.4

Kaspi et al 2002

Kaspi et al 2002

Presentation Transcript

Fourier Series Summary (From Salivahanan et al, 2002)

et al.

Cochran, A. et al. 2002

To Know from Dancey et al. (2002)

Yergey et al.(2002)

(Source: Western et al. (2002))

( From Dixon et al., 2002, Nature )

Reading: Barabasi and Oltvai 2004, Milo et al. 2002

HCA 1924/2002 Leung et al v. Hospital Authority

Presenting - Anat Kaspi

Hagting et al (2002) J. Cell Biol. 157 : 1125

Rein et al., 2002 Current Biology

Leeman et al 2004 Moriguti et al 2004 Rosner et al 2003

Article : Parlati et al. 2002 PNAS 99 : 5424-5427

Reading: Barabasi and Oltvai 2004, Milo et al. 2002

Hulot et al., 2002

Shai Kaspi

Shai Kaspi

Credit: Baughman et al. , Science 297 , 787 (2002)