AGN Diagnostic Plot In The WISE And 3XMM Era: The Role Of Variability

2016

Publication Year

2020-04-29T15:23:56Z

Acceptance in OA@INAF

AGN Diagnostic Plot In The WISE And 3XMM Era: The Role Of Variability

Title

Zaino, Alessandra; SEVERGNINI, Paola; Vignali, C.; DELLA CECA, Roberto; Ballo, L. Authors 10.5281/zenodo.163800 DOI http://hdl.handle.net/20.500.12386/24337 Handle

AGN diagnostic plot

in the WISE and 3XMM era:

the role of variability

Alessandra Zaino

(University of Bologna)

In collaboration with:

P.Severgnini (INAF – Brera Observatory)

C.Vignali (Dept. of Physics and Astronomy, University of Bologna)

R.Della Ceca (INAF – Brera Observatory)

Outline

q

2XMM-IRAS vs 3XMM-WISE diagnostic plot

q

Catching the origin of variability

q

Some examples of variable sources

Compton thin AGN

Unobscured AGN

145 sources

F

(4.5-12 keV)>10

_{erg cm}

_s

0.14 Jy < F

< 544 Jy

Diagnostic plot for AGN classification

HR4 =

_{cts (4.5-12 keV) + cts (2-4.5 keV)}

cts (4.5-12 keV) - cts (2-4.5 keV)

2XMM-IRAS vs 3XMM-WISE plot

•  Stability of the

diagnostic plot

•  Only <5% of the sources

change its location

within the plot

3XMM-WISE

29%

27%  

8%

36%

2XMM-IRAS

30%

26%

8%

36%

Sources with multiple detections in the 3XMM catalogue

Does variability play a role?

NGC 214

NGC 4388

NGC 6860

Sources with multiple detections in the 3XMM catalogue

check for

variability

Does variability play a role?

ΔF

>2

and/or

ΔHR4 >2

~55% of the sources

_{~33% of the sources}

with multiple detections

Some examples of variable sources - NGC 6860

z ~ 0.015

t

3/2009

= 175.9 ks

t

= 21.4 ks

3/2006

Winter et al. (2010)

Winter et al. (2007)

Some examples of variable sources - NGC 6860

§  absorbed powerlaw

§  ionized absorber

§  reflection component

§  FeI k

line

z ~ 0.015

Γ = 1.93

lum

=(6.15

)10

_{erg s}

Γ = 1.79

Some examples of variable sources - NGC 4388

z ~ 0.008

t

= 7.3 ks

12/2002

t

= 3.8 ks

7/2002

t

= 37.7 ks

6/2011

Some examples of variable sources - NGC 4388

z ~ 0.008

§  thermal components:

kT

= (0.19 ± 0.01) keV

kT

= (0.67

) keV

§

scattering < 1%

§

absorbed powerlaw: Γ = 1.7 (fixed)

§

reflection component + FeI k

line

+0.04  

lumlum_2-10keV 2-10keV ~ 9 10~ 10 42 _{erg s}-1

42 _{erg s}-1

Some examples of variable sources - NGC 214

7/2003

t

= 7.9 ks

8/2005

t

= 2.6 ks

Some examples of variable sources - NGC 214

§ 

thermal component: kT = 0.35

keV

§

scattering < 1%

§

absorbed powerlaw: Γ = 1.9 (fixed)

§

reflection component

+0.29

z ~ 0.015

lum

lum

~ 10

~ 10

_{erg s}

42

_{erg s}

N

= (1.23

)10

_cm

Conclusions and future perspectives

Future perspectives:

o  Carry out variable sources spectral analysis

o  XMM/NuSTAR proposal to investigate the origin of variability

o  Investigation of starbursts variability

Conclusions:

o  Plot stability

o  Diagnostic plot as hint of the origin of source variability

o  Overall, plot in agreement with spectral analysis

o  Revisiting mid-IR/X-ray selection of local AGN sources with the

latest 3XMM and WISE data

o  Investigation of the role of variability within the AGN selection

and classification through a diagnostic plot

Than

k you