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

✷♠♠ ❚❤❡ ✜rst s❝✐❡♥t✐✜❝ ❊①♣❧♦r✐♥❣ t❤❡ ❍♦t ❛♥❞ ❝♦♥❢❡r❡♥❝❡ ❞❡❞✐❝❛t❡❞ ❊♥❡r❣❡t✐❝ ❯♥✐✈❡rs❡✿ t♦ t❤❡ ❆t❤❡♥❛ ❳✲r❛② ♦❜s❡r✈❛t♦r② 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

Outline Dark baryons 1 WHIM as seen by XMM-Newton 2 WHIM by Athena WFI 3 A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 2 / 27

Outline Dark baryons 1 WHIM as seen by XMM-Newton 2 WHIM by Athena WFI 3 A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 3 / 27

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

Local baryon deficit Ω lum ≃ Ω ⋆ + Ω HI + Ω X : clusters ≈ 0 . 012 h − 2 70 (Primeval abundances D, 3 He, 4 He, Li) Ω b ≈ ( 0 . 045 ± 0 . 057 ) > 0 . 037 h − 1 (Ly- α forest at z ≈ 2) 70 Ω lum < Ω b < Ω m ≈ 0 . 3 ⇑ ⇑ Baryon deficyt Dark matter h 70 = H o / 70 km s − 1 Mpc − 1 A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 5 / 27

Four phases of baryonic matter T < 10 5 K 1 Condensed δ > 1000 stars, interstel- lar matter T > 10 7 K 2 Hot intracluster gas T < 10 5 K 3 Diffuse δ < 20 Ly- α forest 10 5 < T < 10 7 K 4 Warm 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

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

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

Yoshida et al., ApJ 618, 91 (2005) A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 9 / 27

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

Outline Dark baryons 1 WHIM as seen by XMM-Newton 2 WHIM by Athena WFI 3 A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 11 / 27

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

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

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

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

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

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

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

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

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 × 10 7 s Order of magnitude ‘deeper’ than 4Ms CDFS A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 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 × 10 7 s Order of magnitude ‘deeper’ than 4Ms CDFS A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 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 × 10 7 s Order of magnitude ‘deeper’ than 4Ms CDFS A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 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 × 10 7 s Order of magnitude ‘deeper’ than 4Ms CDFS A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 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 × 10 7 s Order of magnitude ‘deeper’ than 4Ms CDFS A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 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 × 10 7 s Order of magnitude ‘deeper’ than 4Ms CDFS A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 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 × 10 7 s Order of magnitude ‘deeper’ than 4Ms CDFS A.M. Sołtan & Agata Ró˙ za´ nska (NCAC) WHIM with Athena Athena Scientific Conference 16 / 27