l. ciesla, f. duras, m. stalevski, w. n. brandt, c. papovich...
TRANSCRIPT
![Page 1: L. Ciesla, F. Duras, M. Stalevski, W. N. Brandt, C. Papovich …people.tamu.edu/~gyang206265/files/xcigale_TAMU_2019sept.pdf · 2020. 1. 26. · X-CIGALE: Fitting AGN/galaxy SED from](https://reader035.vdocuments.us/reader035/viewer/2022071500/611f226736257e0d86602325/html5/thumbnails/1.jpg)
X-CIGALE: Fitting AGN/galaxy SED from X-ray to infrared
Guang YangCollaborators: M. Boquien, V. Buat, D. Burgarella,
L. Ciesla, F. Duras, M. Stalevski, W. N. Brandt, C. Papovich
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Extragalactic surveys are popular today
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CIGALE: a powerful SED fitting code1. Physical: multicomponent models obeying energy conservation
2. Efficient: ~ 100 million models only take <~ 1 day on laptop
3. Modern: Python
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Boquien et al. (2019)
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But the AGN part needs improvement
1. Cannot deal with X-ray data2. AGN torus model is outdated 3. Do not have models of obscured type 1 AGNs
New version: X-CIGALE
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But the AGN part needs improvement
1. Cannot deal with X-ray data2. AGN torus model is outdated 3. Do not have models of obscured type 1 AGNs
New version: X-CIGALE
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X-ray emission is a unique feature of AGNs
Brandt & Alexander (2015)
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AGN X-ray is well correlated with UV
Netzer (2013)Brandt & Alexnader (2015)
SDSStype 1 QSO
𝜶OX slope
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Implementation in X-CIGALE
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An example AGN SED
Fitting with X-ray Fitting without X-ray
AGN overestimated!
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Also good for X-ray undetected galaxies
Most optical/IR sources are X-ray undetected
IR AGN fraction can be constrained even with X-ray upper limit
Deeper X-ray → tighter constraint
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But the AGN part needs improvement
1. Cannot deal with X-ray data2. AGN torus model is outdated 3. Do not have models of obscured type 1 AGNs
New version: X-CIGALE
![Page 13: L. Ciesla, F. Duras, M. Stalevski, W. N. Brandt, C. Papovich …people.tamu.edu/~gyang206265/files/xcigale_TAMU_2019sept.pdf · 2020. 1. 26. · X-CIGALE: Fitting AGN/galaxy SED from](https://reader035.vdocuments.us/reader035/viewer/2022071500/611f226736257e0d86602325/html5/thumbnails/13.jpg)
The AGN unification scheme
Different AGNs are essentially the same type of object
The central engine is obscured by the dusty torus
Type 1 AGN: face on Type 2 AGN: edge on
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AGN torus model in CIGALE
Old: smooth, Fritz et al. (2006)New: clumpy, Stalevski et al. (2012, 2016)
Unphysical: temperature too high (~ million K)
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The old model does not follow energy conservation!
The old model underestimates the dust IR reemission!
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But the AGN part needs improvement
1. Cannot deal with X-ray data2. AGN torus model is outdated 3. Do not have models of obscured type 1 AGNs
New version: X-CIGALE
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Obscured type 1 AGNs are common in X-ray selected sample
AGNs with broad lines
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Can be explained by dust in polar directions
Asmus 2019
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Polar-dust models in X-CIGALE
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Application to real data
Indeed, SDSS AGNs have lower obscuration than COSMOS
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Future work: JWST
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