• DOI:10.3847/1538-4357/ac4bcb
• Corpus ID: 245877684

Spectroastrometry and Reverberation Mapping: The Mass and Geometric Distance of the Supermassive Black Hole in the Quasar 3C 273

@article{Li2022SpectroastrometryAR,
  title={Spectroastrometry and Reverberation Mapping: The Mass and Geometric Distance of the Supermassive Black Hole in the Quasar 3C 273},
  author={Yan-Rong Li and Jian-Min Wang and Yu-Yang Songsheng and Zhi-Xiang Zhang and Pu Du and Chen Hu and Ming Xiao},
  journal={The Astrophysical Journal},
  year={2022},
  volume={927}
}

• Yan-Rong Li, Jian-Min Wang, +4 authors M. Xiao
• Published 12 January 2022
• Physics
• The Astrophysical Journal

The quasar 3C 273 has been observed with infrared spectroastrometry (SA) of the broad Paα line and optical reverberation mapping (RM) of the broad Hβ line. SA delivers information about the angular size and structure of the Paα broad-line region (BLR), while RM delivers information about the physical size and structure of the Hβ BLR. Based on the fact that the two BLRs share the mass of the supermassive black hole (SMBH) and viewing inclination, a combination of SA and velocity-resolved RM (SARM) thereby allows us to simultaneously determine the SMBH mass and geometric distance through dynamically modeling the two BLRs. We construct a suite of dynamical models with different geometric configurations and apply a Bayesian approach to obtain the parameter inferences. Overall the obtained masses and distances are insensitive to specific BLR configurations but more or less depend on parameterizations of the vertical distributions. The most probable model, chosen in light of the Bayes factor, yields an angular-size distance log(DA/Mpc)=2.83−0.28+0.32 and an SMBH mass log(M•/M⊙)=9.06−0.27+0.21 , which agree with the relationships between SMBH masses and bulge properties. The BLRs have an inclination of 5−1+1 degrees, consistent with that of the large-scale jet in 3C 273. Our approach reinforces the capability of SARM analysis to measure SMBH masses and distances of active galactic nuclei and quasars even though SA and RM observations are undertaken with different emission lines and/or in different periods.