The Soft X-ray View of Ultra Fast Outflows

2017

Publication Year

2020-07-27T09:48:44Z

Acceptance in OA@INAF

The Soft X-ray View of Ultra Fast Outflows

Title

Reeves, J.; BRAITO, Valentina; NARDINI, EMANUELE; Matzeu, G.; Lobban, A.; et al.

Authors

http://hdl.handle.net/20.500.12386/26645

The soft X-ray view of Ultra Fast Outflows in AGN

James Reeves (UMBC/Keele)

Main Collaborators:- Valentina Braito, Gabi Matzeu (Brera), Michele

Costa, Andrew Lobban (Keele), Emanuele Nardini, Guido Risaliti

(Arcetri), Ken Pounds (Leicester), Jane Turner (UMBC), Francesco

A persistent, wide-angle wind in PDS 456

(Nardini et al. 2015, Sci)

Is there evidence for a soft X-ray component

of the fast (0.3c) wind in PDS 456?

5x100ks XMM-Newton/NuSTAR observations. Response of iron K profile to continuum variations Nardini+15 Fe K Pcygni A B C D E

Signatures of fast (0.2c) “BAL” like profiles in soft X-rays with XMM-Newton/RGS (OBS E). Velocity widths σ≈10000 km/s.

Broad Soft X-ray Absorption Profiles in PDS 456

(Reeves et al. 2016, ApJ)

OBS B

OBS E

Soft X-ray absorbing gas the likely signature of an inhomogeneous wind, partially obscuring the AGN. Velocities of up to 0.2c, N_H~1022 _cm-2_{, log xi =3.5-4} Absorption primarily due to highly ionized Fe (Fe XX-XXIV) as well as NeIX/X

Broad Soft X-ray Absorption Lines

− 4 − 20 2 4 OBS CD ABS2 ABS1 − 4 − 20 2 4 OBS E EMIS1 ABS1 ABS2 0.8 1 1.2 1.4 − 50

Rest Energy (keV)

2001 ABS1 − 4 − 20 2 4 OBS B RGS$ 0.9 1 1.1 ratio XMM, OBS B. ABS1 ABS2 0.9 1 1.1 ratio XMM, OBS CD. ABS1 ABS2 0.9 1 1.1 ratio XMM, OBS E. ABS1 ABS2 EMIS1 0.8 1 1.2 1.4 1.6 1.8 0.8 0.9 1 1.1 1.2 ratio

Rest Energy (keV)

XMM, 2001

ABS1 ABS2

2017 NuSTAR observation of the wind in PDS 456

10 − 6 10 − 5 10 − 4 Counts s − 1 keV − 1 cm − 2 10 5 20 − 4 − 20 2 σ

Rest Energy (keV)

March 2017, NuSTAR, 200ks G=2.3 powerlaw continuum

Deep+Fast 0.3c Fe K P Cygni profile NO COMPTON HUMP – NOT A DISK REFLECTION SPECTRUM

The Large XMM-Newton Programme on PG1211+143

(Lobban et al. 2015, 2016; Pounds et al. 2016a, b)

PG 1211+143, luminous (L_bol~1046 _{erg/s), nearby, narrow-lined type I quasar (z=0.0809), the}

initial proto-type example of an ultra fast outflow (Pounds et al. 2003). 7 Sequences with XMM-Newton in June/July 2014. Total exposure ~630ks. Note lowest flux during rev 2659 with XMM-Newton.

10 15 20 25 0.8 1 1.2 1.4 ratio Rest Wavelength (Å) Ne IX−X Fe XIX−XXI

Fe UTA O VIII O VII N VII

| |

| |

|

|

|

Is there evidence for the fast outflow in the soft X-ray spectrum of PG

1211? Mean RGS spectrum (June 2014, 600ks exposure)

Blue-shifted absorption profiles revealed in deep RGS exposure of PG 1211+143, e.g. from N, O, Ne, Fe. Systematic velocity shift of 0.06-0.07c. Note position of low ionization UTA component and strong emission (OVII/OVIII).

Mean RGS spectrum of PG 1211 – Best fit XSTAR model

Two main zones. Low ionization:- log xi=1.8+/-0.2, N_H = 4x1020 _cm2_{, v/c = 0.064+/-0.002} High ionization:- log xi=3.4+/-0.2, N_H = 1x1022 _cm2_{, v/c=0.063+/-0.002} 2 × 10 − 12 4 × 10 − 12 6 × 10 − 12 ν F ν (ergs cm − 2 s − 1 ) 10 15 20 25 − 20 2 Residuals ( σ) Rest Wavelength (Å) Ne IX /X , F e L Fe U TA OV III Ly a OV III Ly a OV III He a NV II Ly a OV II RR C OV II He a (r, f) Ne IX He a

Mean RGS spectrum of PG 1211 – OVII/OVIII band

5 × 10 − 12 ν F ν (ergs cm − 2 s − 1 ) 3x10 − 12 18 20 22 − 20 2 Residuals ( σ) Rest Wavelength (Å) Broad (FWHM 10000 km/s) OVII/OVIII emission lines and blueshifted absorption profiles OV III Ly a OV II RR C OV III Ly a OV III He a OV II (f ) OV II (r )

Rapid Variability of Ultra Fast Outflow in PG 1211+143

1 0.5 2 5 10 − 3 2 × 10 − 3 νF ν Flux (keV cm − 2 s − 1 ) Energy (keV) rev 2659 rev 2661 rev 2663 rev 2664 Low flux spectrum in rev 2659. Source then progressively brightens. Soft X-ray absorption is rapidly variable (within 2 orbits), decreasing with increasing flux. PG 1211 undergoes absorption event during rev 2659, increasing in lower ionization absorption. Soft X-ray absorber not a conventional warm absorber. Fast (0.07c) and rapidly variable on timescales of < 1 week. Implies absorber is compact, on scales of 10s Rs, likely part of clumpy disk wind.

Variability of PG 1211 wind seen in RGS spectrum

10

15

20

25

0.5 1 1.5 ratio

Rest Wavelength (Å)

REV 2659

Variability of PG 1211 wind seen in RGS spectrum

10

15

20

25

0.5 1 1.5 ratio

Rest Wavelength (Å)

REV 2661

Variability of PG 1211 wind seen in RGS spectrum

10

15

20

25

0.5 1 1.5 ratio

Rest Wavelength (Å)

REV 2663

Variability of PG 1211 wind seen in RGS spectrum

10

15

20

25

0.5 1 1.5 ratio

Rest Wavelength (Å)

REV 2664

The Wind Structure

10

16

10

17

10

18

₁₀

2

₁₀

3

₁₀

4

R (cm)

R (R

_g

)

Innermost highly ionized wind launched from within 100 Rg (10

16

_{cm) of}

black hole – ultra fast iron K absorption (0.1-0.3c).

Inhomogeneous soft X-ray absorber R≈10

17

_-10

18

_{cm, n}

e

≈10

7

-10

8

cm

-3

, with

thickness ΔR≈10

14-15

_{cm. Filling factor f≈10}

-3

_.