Deep X-ray surveys

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2016

Publication Year

2020-05-18T13:41:21Z

Acceptance in OA@INAF

Deep X-ray surveys

Title

COMASTRI, Andrea

Authors

http://hdl.handle.net/20.500.12386/24913

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Deep Surveys

Andrea Comastri

INAF-Osservatorio Astronomico di Bologna

P.Ranalli, C.Vignali, N.Cappelluti, R.Gilli, K.Iwasawa, G.

Lanzuisi, F.J. Carrera, M. Brusa, F. Vito, I. Georgantopoulos, E.Rovilos, F.Fiore, F.Civano,W.N. Brandt, P.Tozzi,

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XMM-CDFS deep survey science goals

AGN “fine” spectroscopy beyond the local Universe

evolution, feedback, ...

Census of highly obscured and Compton thick AGN Iron line properties

Variability ...

About 60% of the hard 5-10 keV XRB was resolved

Ranalli+13

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The X-ray sample(s)

] -2 ) [cm intr H log(N 20 21 22 23 24 25 number 0 10 20 30 40 sample (147) Tozzi’s distribution

“2-10 keV selected” flux limited, widely different spectral quality

180 sources > 1.8 x 10-15 _cgs

_{Castello-Mor+13}

75%

Iwasawa+12

46 sources @ z >1.7

The obscured fraction increases toward high-z for luminous

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Distant Compton thick in the CDFS

z=1.53

z=3.70

1 2 5 0 10 4 2×10 4 3×10 4 4×10 4 normalized counts s 1 keV 1 keV ! " # !$%# " &$%# " '$%# " ()*+,-./0123)4(5626 % 2708 % 708

z=1.18

AC+11 AC+11 Georgantopoulos+13 0 1 2 5 10 10 − 5 2 × 10 − 5 3 × 10 − 5 4 × 10 − 5 5 × 10 − 5 normalized counts s − 1 keV − 1 Energy (keV)

z=0.68

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Chandra Results

Gilli+11

z=4.76

Brightman&Ueda12

1 2 5 10 − 8 10 − 7 10 − 6 keV 2 (Photons cm − 2 s − 1 keV − 1) Energy (keV) BzK4892 z=2.578 Feruglio+11

z=2.6

Chandra is/will reach higher redshifts especially with the 7 Ms

Spectral Quality is not good enough for accurate NH measurements in the

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Comparisons

Reflection Dominated 109 Reflection Dominated Reflection Dominated < 5 x 10-15 < 5 x 10-15 < 5 x 10-15 NuSTAR Heavily FLAT < 5 x 10-15 < 5 x 10-15 Moderate FLAT < 5 x 10-15

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Compton thick Fraction

Brightman&Ueda12 Hasinger07 Tozzi+06 Brunner+08 XMMCDFS Ueda+14, GCH07, Buchner+15 NuSTAR Alexander+13

At the limiting fluxes of the XMM and Chandra spectral surveys the number of Compton Thick (CT) AGN is in fairly good agreement with the XRB model expectations.

Looking forward for NuSTAR deep surveys spectral analysis

(Zappacosta+;Del Moro+ in

preparation) to understand the

evolution of the CT obscuring gas and implications for models

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XMM deep X-ray spectrum

voutflow ~0.14c

FX ~ 3 x10-14 LX ~ 2 x 1044 NH~2-3×1023cm-2

X-ray redshift from emission line + edge z~1.6

Resonant FeXXV-XXVI absorption outflow

Vignali+15 1 2 5 10 − 7 10 − 6 10 − 5 keV (Photons cm − 2 s − 1 keV − 1 )

Observed−frame Energy (keV)

em. line abs. line soft comp. nuclear comp. iron edge photo−el. cutoff ~700 ksec

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Redshift from the X-ray spectrum

1 2 5 02 × 10 − 4 4 × 10 − 4 6 × 10 − 4 normalized counts s − 1 keV − 1 keV FX ~ 1.5 x10-14 LX ~ 4 x 1044 NH~5-6×1023cm-2

X-ray redshift from the Kalpha Iron Edge (7.11 keV)

z = 2.03+-0.04 Georgantopoulos+13 10 − 8 10 − 7 10 − 6 10 − 5 keV (Photons cm − 2 s − 1 keV − 1) Detected by NuSTAR in the 8-24 keV band (but not < 8 keV)

The most distant AGN detected above 10 keV

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Brightest sources iron line variability

Iwasawa+15

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Iron line profile

Falocco+15

Low Luminosity

High Luminosity

“Tentative” evidence

of a broad component

cfr. Brusa+05 Chaudary+12

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Iron line profile

Falocco+15

Low Luminosity

High Luminosity

“Tentative” evidence

of a broad component

cfr. Brusa+05 Chaudary+12

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Pushing even deeper is not rewarding especially with 7 Ms Chandra Good quality spectra are absolutely needed for many science goals

NH distribution above 1024 _cm-2_{: relative fraction of reflection}

dominated vs XRB contributors and their volume emissivity/space

density (cfr. Akylas+12;Fabian+16;Esposito&Walter16, XRB is mostly due to

disk reflection rather than CT)

UFO/Outflows at high-z: feedback at work

Iron line, absorption and continuum variability ...

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If I have 10 - 20 Ms

Identify a well defined sample of molecular outflows and UFO only two examples (Tombesi+15;Feruglio+15)

and/or high-redshift interesting objects (cfr. Massimo Cappi review)

Large sample of “representative” heavily obscured AGN,

Iron line intensity and profile distribution beyond the local Universe

COSMOS, (Lanzuisi) XSERVS (Brandt), XXL(Pierre), Stripe82 (La

Massa) are excellent starting points.