JWST ERS Program Q3D: The pitfalls of virial black hole mass constraints shown for a z ∼ 3 quasar with an ultramassive host

作者：C. Bertemes, Dominika Wylezalek, D.S.N. Rupke, Nadia L. Zakamska, S. Veilleux, Benedikt M. Beckmann, Andrey Vayner, S. Sankar, Yuzo Ishikawa, Nadiia Diachenko, Weiwei Liu, Yu‐Ching Chen, Jerome Seebeck, D. Lutz, Guilin Liu · 发表于：Astronomy and Astrophysics · 年份：2024 · DOI：10.1051/0004-6361/202450451 · 被引用次数：16 · 研究领域：Astrophysical Phenomena and Observations、Pulsars and Gravitational Waves Research、Relativity and Gravitational Theory

We present observations with the Mid-InfraRed Instrument (MIRI) and Near-InfraRed Spectrograph (NIRSpec) on board the James Webb Space Telescope (JWST), targeting the extremely red quasar J165202.64+172852.3 at z = 2.948 (dubbed J1652). As one of the most luminous quasars known to date, it drives powerful outflows and hosts a clumpy starburst, in the midst of several interacting companions. We estimated the black hole (BH) mass of the system based on the broad H α and H β lines, as well as the broad Pa β emission in the infrared and Mg II in the ultraviolet. We recovered a very broad range of mass estimates, with individual constraints ranging between log M BH ∼ 9 and 10.2, which is extended further if we impose a uniform broad line region geometry at all wavelengths. The large spread may be caused by several factors: uncertainties on measurements (insufficient sensitivity to detect the broadest component of the faint Paschen β line, spectral blending, ambiguities in the broad or narrow component distinction, etc.), lack of virial equilibrium, and uncertainties on the luminosity-inferred size of the broad line region (BLR). The exotic nature of our target (luminous, starburst, powerful outflows, high accretion rate, and dusty centre) is another likely contribution to the large uncertainties. We broadly constrained the stellar mass of J1652 by fitting the spectral energy distribution, which suggests that the host is extremely massive, at ∼10 12.1 M ⊙ , with a 1.1 dex uncertain...