Prospects for the direct WHIM detection by Athena The soft X-ray - - PowerPoint PPT Presentation

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Prospects for the direct WHIM detection by Athena The soft X-ray - - PowerPoint PPT Presentation

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SLIDE 1

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Prospects for the direct WHIM detection by Athena

The soft X-ray WHIM emission with WFI Andrzej M. Sołtan & Agata Ró˙ za´ nska

Nicolaus Copernicus Astronomical Center Warszawa

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 1 / 27

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SLIDE 2

Outline

1

Dark baryons

2

WHIM as seen by XMM-Newton

3

WHIM by Athena WFI

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 2 / 27

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SLIDE 3

Outline

1

Dark baryons

2

WHIM as seen by XMM-Newton

3

WHIM by Athena WFI

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 3 / 27

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SLIDE 4

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 4 / 27

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SLIDE 5

Local baryon deficit

Ωlum ≃ Ω⋆ + ΩHI + ΩX:clusters ≈ 0.012 h−2

70

Ωb ≈ (0.045 ± 0.057) (Primeval abundances D, 3He, 4He, Li) > 0.037 h−1

70

(Ly-α forest at z ≈ 2)

Ωlum < Ωb < Ωm ≈ 0.3

⇑ ⇑ Baryon deficyt Dark matter h70 = Ho/70 km s−1Mpc−1

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 5 / 27

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SLIDE 6

Four phases of baryonic matter

1 Condensed δ > 1000 T < 105 K stars, interstel- lar matter 2 Hot T > 107 K intracluster gas 3 Diffuse δ < 20 T < 105 K Ly-α forest 4 Warm 105 < T < 107 K WHIM Warm-Hot Intergalactic Medium

Davé et al., ApJ, 552, 473 (2001).

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 6 / 27

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SLIDE 7

Shane & Wirtanen, Lick counts

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 7 / 27

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SLIDE 8

Where are the baryons ?

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 8 / 27

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SLIDE 9

Yoshida et al., ApJ 618, 91 (2005)

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 9 / 27

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SLIDE 10

Baryons and Dark Matter

Suto et al., JKAS 37, 387 (2004)

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 10 / 27

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SLIDE 11

Outline

1

Dark baryons

2

WHIM as seen by XMM-Newton

3

WHIM by Athena WFI

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 11 / 27

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SLIDE 12

X-ray sky

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 12 / 27

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SLIDE 13

XRB vs galaxies

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 13 / 27

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SLIDE 14

XRB vs galaxies

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 14 / 27

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SLIDE 15

X-ray background (XRB)

The XRB at energies above ∼ 1 keV is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below ∼ 1 keV some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments.

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27

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SLIDE 16

X-ray background (XRB)

The XRB at energies above ∼ 1 keV is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below ∼ 1 keV some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments.

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27

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SLIDE 17

X-ray background (XRB)

The XRB at energies above ∼ 1 keV is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below ∼ 1 keV some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments.

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27

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SLIDE 18

X-ray background (XRB)

The XRB at energies above ∼ 1 keV is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below ∼ 1 keV some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments.

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27

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SLIDE 19

X-ray background (XRB)

The XRB at energies above ∼ 1 keV is generated by a population of discrete extragalactic sources (mostly AGNs). At enegries below ∼ 1 keV some (basicly unknown) contribution to the XRB generate also: local (Galactic) hot plasma and the WHIM. Fluctuations of the XRB at arcmin scale are generated by a nonuniform distribution of sources contributing to the XRB: AGNs and WHIM. The WHIM is strongly correlated with galaxies. WHIM in emission: spherical halos rather than filaments.

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 15 / 27

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SLIDE 20

Whim emission expected extremely weak ↓ stacking of observations ≡ cross-correlation function Azimuthal symmentry X-ray sky — XMM-Newton archive Galaxy data — APM + MAPS catalogue

(17 − 20 mag, 0.06 z 0.22)

150 pointings × 16000 s × 20 galaxies ∼ 5 × 107 s Order of magnitude ‘deeper’ than 4Ms CDFS

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27

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SLIDE 21

Whim emission expected extremely weak ↓ stacking of observations ≡ cross-correlation function Azimuthal symmentry X-ray sky — XMM-Newton archive Galaxy data — APM + MAPS catalogue

(17 − 20 mag, 0.06 z 0.22)

150 pointings × 16000 s × 20 galaxies ∼ 5 × 107 s Order of magnitude ‘deeper’ than 4Ms CDFS

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27

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SLIDE 22

Whim emission expected extremely weak ↓ stacking of observations ≡ cross-correlation function Azimuthal symmentry X-ray sky — XMM-Newton archive Galaxy data — APM + MAPS catalogue

(17 − 20 mag, 0.06 z 0.22)

150 pointings × 16000 s × 20 galaxies ∼ 5 × 107 s Order of magnitude ‘deeper’ than 4Ms CDFS

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27

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SLIDE 23

Whim emission expected extremely weak ↓ stacking of observations ≡ cross-correlation function Azimuthal symmentry X-ray sky — XMM-Newton archive Galaxy data — APM + MAPS catalogue

(17 − 20 mag, 0.06 z 0.22)

150 pointings × 16000 s × 20 galaxies ∼ 5 × 107 s Order of magnitude ‘deeper’ than 4Ms CDFS

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27

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SLIDE 24

Whim emission expected extremely weak ↓ stacking of observations ≡ cross-correlation function Azimuthal symmentry X-ray sky — XMM-Newton archive Galaxy data — APM + MAPS catalogue

(17 − 20 mag, 0.06 z 0.22)

150 pointings × 16000 s × 20 galaxies ∼ 5 × 107 s Order of magnitude ‘deeper’ than 4Ms CDFS

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27

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SLIDE 25

Whim emission expected extremely weak ↓ stacking of observations ≡ cross-correlation function Azimuthal symmentry X-ray sky — XMM-Newton archive Galaxy data — APM + MAPS catalogue

(17 − 20 mag, 0.06 z 0.22)

150 pointings × 16000 s × 20 galaxies ∼ 5 × 107 s Order of magnitude ‘deeper’ than 4Ms CDFS

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27

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SLIDE 26

Whim emission expected extremely weak ↓ stacking of observations ≡ cross-correlation function Azimuthal symmentry X-ray sky — XMM-Newton archive Galaxy data — APM + MAPS catalogue

(17 − 20 mag, 0.06 z 0.22)

150 pointings × 16000 s × 20 galaxies ∼ 5 × 107 s Order of magnitude ‘deeper’ than 4Ms CDFS

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27

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SLIDE 27

Whim emission expected extremely weak ↓ stacking of observations ≡ cross-correlation function Azimuthal symmentry X-ray sky — XMM-Newton archive Galaxy data — APM + MAPS catalogue

(17 − 20 mag, 0.06 z 0.22)

150 pointings × 16000 s × 20 galaxies ∼ 5 × 107 s Order of magnitude ‘deeper’ than 4Ms CDFS

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27

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SLIDE 28

Whim emission expected extremely weak ↓ stacking of observations ≡ cross-correlation function Azimuthal symmentry X-ray sky — XMM-Newton archive Galaxy data — APM + MAPS catalogue

(17 − 20 mag, 0.06 z 0.22)

150 pointings × 16000 s × 20 galaxies ∼ 5 × 107 s Order of magnitude ‘deeper’ than 4Ms CDFS

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27

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SLIDE 29

Correlation analysis

The WHIM is strongly correlated with the galaxy distribution. At small angular scales, the WHIM structure defines the signal of the cross-correlation function (CCF). At large scales the CCF signal is generated by the large scale fluctuations of the galaxy distribution (the galaxy autocorrelation function).

δρ(θ) = s · P(θ) + s · wgg(θ) · ng

δρ(θ) – average excess of the X-ray flux, s – brightness of the individual WHIM halo around galaxy, P(θ) – normalized surface brightness of the WHIM halo, wgg(θ) – autocorrelation function of galaxies, ng – surface density of galaxies surrounded by the WHIM halos.

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 17 / 27

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SLIDE 30

Correlation analysis

The WHIM is strongly correlated with the galaxy distribution. At small angular scales, the WHIM structure defines the signal of the cross-correlation function (CCF). At large scales the CCF signal is generated by the large scale fluctuations of the galaxy distribution (the galaxy autocorrelation function).

δρ(θ) = s · P(θ) + s · wgg(θ) · ng

δρ(θ) – average excess of the X-ray flux, s – brightness of the individual WHIM halo around galaxy, P(θ) – normalized surface brightness of the WHIM halo, wgg(θ) – autocorrelation function of galaxies, ng – surface density of galaxies surrounded by the WHIM halos.

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 17 / 27

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SLIDE 31

Correlation analysis

The WHIM is strongly correlated with the galaxy distribution. At small angular scales, the WHIM structure defines the signal of the cross-correlation function (CCF). At large scales the CCF signal is generated by the large scale fluctuations of the galaxy distribution (the galaxy autocorrelation function).

δρ(θ) = s · P(θ) + s · wgg(θ) · ng

δρ(θ) – average excess of the X-ray flux, s – brightness of the individual WHIM halo around galaxy, P(θ) – normalized surface brightness of the WHIM halo, wgg(θ) – autocorrelation function of galaxies, ng – surface density of galaxies surrounded by the WHIM halos.

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 17 / 27

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SLIDE 32

Correlation analysis

The WHIM is strongly correlated with the galaxy distribution. At small angular scales, the WHIM structure defines the signal of the cross-correlation function (CCF). At large scales the CCF signal is generated by the large scale fluctuations of the galaxy distribution (the galaxy autocorrelation function).

δρ(θ) = s · P(θ) + s · wgg(θ) · ng

δρ(θ) – average excess of the X-ray flux, s – brightness of the individual WHIM halo around galaxy, P(θ) – normalized surface brightness of the WHIM halo, wgg(θ) – autocorrelation function of galaxies, ng – surface density of galaxies surrounded by the WHIM halos.

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 17 / 27

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SLIDE 33

CCF at high energies

Sołtan, A&A 460, 59 (2006)

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 18 / 27

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SLIDE 34

CCF at soft energies

Sołtan, A&A 460, 59 (2006)

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 19 / 27

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SLIDE 35

WHIM – surface brightness profile

Sołtan, A&A 460, 59 (2006)

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 20 / 27

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SLIDE 36

Outline

1

Dark baryons

2

WHIM as seen by XMM-Newton

3

WHIM by Athena WFI

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 21 / 27

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SLIDE 37

E = 0.3 − 0.5 KeV σ = (2 − 3) × 10−8 cnt s−1 pxl−1 σ = 5.6 × 10−6 cnt s−1 arcmin−1 1 cnt = 0.65 × 10−11 erg cm−2 σ = 5.7 × 10−8 ph cm−2 s

−1 arcmin−1

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 22 / 27

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SLIDE 38

WFI ARF (no filter)

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 23 / 27

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SLIDE 39

WFI background

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 24 / 27

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SLIDE 40

Signal against Noise

∆n = ARF · σ S = ∆n · A · texp N =

  • b · A · texp

S/N = ∆n ·

  • A · texp

b where: ∆n – count excess generated by WHIM per arcmin2 A – solid angle of the WHIM halo texp – exposure time

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 25 / 27

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SLIDE 41

S/N for two mirror modules on-axis

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 26 / 27

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SLIDE 42

Athena ...

... most likely will have the capability to detect the soft X-ray emission from individual WHIM halos accumu- lated around nearby galaxies. A moderate exposure time would be required. Imaging of the detailed structure will need long but still feasible exposures.

Thank you

A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 27 / 27