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![Constraints on the total thermal energy within r 200c [see Eq. (40)] of hot gas in halos inferred from the break model analysis. We compare our constraints to the simulation-based predictions of Battaglia et al. [10], finding good agreement at high halo mass but differences at low mass.](profile/Martin-Rodriguez-Monroy/publication/362647901/figure/fig2/AS:11431281078849750@1660304622407/Constraints-on-the-total-thermal-energy-within-r-200c-see-Eq-40-of-hot-gas-in-halos.png)
Constraints on the total thermal energy within r 200c [see Eq. (40)] of hot gas in halos inferred from the break model analysis. We compare our constraints to the simulation-based predictions of Battaglia et al. [10], finding good agreement at high halo mass but differences at low mass.
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Hot, ionized gas leaves an imprint on the cosmic microwave background via the thermal Sunyaev Zel'dovich (tSZ) effect. The cross-correlation of gravitational lensing (which traces the projected mass) with the tSZ effect (which traces the projected gas pressure) is a powerful probe of the thermal state of ionized baryons throughout the Universe, and...
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Context 1
... now use our inferred model constraints to generate constraints on the pressure profiles of halos as a function of mass and redshift. In Fig. 9 we show our constraints on the total thermal energy of hot gas inside r 200c ...
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... from unity in the mass range 10 13 < M 200c ðM ⊙ =hÞ < 2 × 10 14 at 3.0σ, 4.0σ, and 5.4σ for z ¼ 0.1, 0.2, and 0.4, respectively (see the left panel of Fig. 9). Similar conclusions were reached when extrapolating the tSZ analysis around Sloan Digital Sky Survey (SDSS) galaxy samples to smaller radii (see Amodeo et ...
Context 3
... now use our inferred model constraints to generate constraints on the pressure profiles of halos as a function of mass and redshift. In Fig. 9 we show our constraints on the total thermal energy of hot gas inside r 200c ...
Context 4
... from unity in the mass range 10 13 < M 200c ðM ⊙ =hÞ < 2 × 10 14 at 3.0σ, 4.0σ, and 5.4σ for z ¼ 0.1, 0.2, and 0.4, respectively (see the left panel of Fig. 9). Similar conclusions were reached when extrapolating the tSZ analysis around Sloan Digital Sky Survey (SDSS) galaxy samples to smaller radii (see Amodeo et ...
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