Silicate emission in a type-2 quasar: JWST/MIRI constraints on torus geometry and radiative feedback

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Table 1.

Properties of the QSO2 J1010 (SDSS J101043.36+061201.4).

SDSS z	0.0977
D_L (Mpc)	449
Scale (kpc/arcsec)	1.807
A_V (mag)	1.1
log L_bol (erg s⁻¹)	45.55
log L_1.4 GHz (W Hz⁻¹)	24.37
log M_BH (M_⊙)	8.4 ± 0.8
log $\frac{L_{bol}}{L_{Edd}}$ $\frac{L_{\rm bol}}{L_{\rm Edd}}$	−0.8 ± 0.8
log M_* (M_⊙)	11.0 ± 0.2
SFR (M_⊙ yr⁻¹)	32, 34, 7
log N $_{H}^{CO}$ $_{\mathrm{H}}^{\mathrm{CO}}$ (cm⁻²)	22.3

Notes. A_V derived from H_α/H_β reported by Kong & Ho (2018) and the extinction law from Cardelli et al. (1989). Bolometric luminosity calculated by applying the correction factor of 474 from Lamastra et al. (2009) to the extinction-corrected [O III] 5007 Å luminosity from Kong & Ho (2018), and 1.4 GHz luminosity and stellar mass from Ramos Almeida et al. (2022). BH mass and Eddington ratio are from Kong & Ho (2018). The SFRs were derived from the total IR luminosity from Ramos Almeida et al. (2022), from spectral synthesis modeling of the SDSS spectra performed by Bessiere et al. (2024), and from the nuclear 11.3 μm PAH detected in the JWST/MIRI spectrum from Ramos Almeida et al. (2025). The gas column density comes from Ramos Almeida et al. (2025) and it was measured from the ALMA CO(2-1) observations studied in Ramos Almeida et al. (2022).

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