The presence of relativistic jets is usually associated with a highly spinning accreting black hole (e.g., Blandford & Znajek 1977 Tchekhovskoy et al. They are characterized by the presence of two collimated relativistic jets of plasma emitted from the central SMBH and extended up to a few Mpcs (e.g., see Blandford et al. 2016).Įven more challenging is the discovery of high- z massive SMBHs hosted in radio-loud 1 (RL or jetted) AGN. 2020), or intense gas accretion in a super-Eddington phase (e.g., Alexander & Natarajan 2014 Madau et al. 2018), the runaway merger of stellar-mass black holes (e.g., Lupi et al. 2016), co-action among dynamical processes, gas collapse, and star formation (e.g., Devecchi & Volonteri 2009 Boekholt et al. 2006 Latif & Schleicher 2015), the collapse of Population III stars (e.g., Bond 1984 Alvarez et al. The most popular scenarios to explain the mass assembly of several million solar mass black holes in the early Universe include the direct collapse of massive gas clouds (e.g., Haehnelt & Rees 1993 Begelman et al. These discoveries indicate a fast and efficient growth for black holes that challenges the currently accepted theoretical model of SMBH formation (e.g., Volonteri 2010 Latif & Ferrara 2016). These studies have shown that the high-redshift AGN discovered to date are typically powered by SMBHs more massive than 10 8–10 9 M ⊙, comparable to the most massive black holes at any redshift. 2008, 2011, 2019 Trakhtenbrot & Netzer 2012), it has been possible to estimate the mass of the SMBHs hosted by high- z AGN (e.g., Jiang et al. With the so-called single-epoch (SE) method (e.g., Vestergaard & Peterson 2006 Vestergaard & Osmer 2009 Shen et al.

An accurate determination of SMBH masses of z > 6 AGN is a prerequisite to fully understanding the physics, demographics (e.g., black holes mass function), and relations with their host galaxies. These earliest AGN are fundamental to studying the early growth of supermassive black holes (SMBHs, e.g., see Inayoshi et al.

High-redshift ( z > 6) active galactic nuclei (AGN) are direct probes of the Universe at an age less than 1 Gyr after the Big Bang. Key words: galaxies: active / galaxies: high-redshift / galaxies: jets / quasars: emission lines / quasars: supermassive black holes / quasars: individual: PSO J030947.49+271757.31 This requirement suggests either earlier periods of rapid black hole growth with super-Eddington accretion or a scenario in which only part of the released gravitational energy goes toward heating the accretion disk and feeding the black hole. In a Eddington-limited accretion scenario and assuming a radiative efficiency of 0.3, typical of a fast rotating SMBH, a seed black hole of more than 10 6 M ⊙ at z = 30 is indeed required to reproduce the mass of PSO J0309+27 at a redshift of 6. The existence of such a massive SMBH just ∼900 million years after the Big Bang challenges models of the earliest SMBH growth, especially if jetted active galactic nuclei are indeed associated with a highly spinning black hole, as is currently assumed. Thanks to these observations, we were able to model the accretion disk and to derive an independent estimate of the black hole mass of PSO J0309+27, confirming the value inferred from the virial technique. We also obtained new photometric observations with the Telescopio Nazionale Galileo in J and K bands to better constrain the NIR spectral energy distribution of the source. From the CIV λ1549 broad emission line, we found that PSO J0309+27 is powered by a 1.45 −0.85 +1.89 × 10 9 M ⊙ supermassive black hole (SMBH) with a bolometric luminosity of ∼8 × 10 46 erg s −1 and an Eddington ratio equal to 0.44 −0.35 +0.78. We present the results of a new LUCI/Large Binocular Telescope near-infrared (NIR) spectroscopic observation of PSO J030947.49+271757.31 (hereafter PSO J0309+27), the highest redshift blazar known to date ( z ∼ 6.1). INAF – Osservatorio di Astrofisica e Scienza dello Spazio, Via Piero Gobetti 93/3, 40129 Bologna, Italy INAF – Istituto di Radioastronomia, Via Gobetti 101, 40129 Bologna, Italy INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF), Via A. INAF – Fundación Galileo Galilei, Rambla José Ana Fernandez Pérez 7, 38712 Breña Baja, TF, Spain

Occhialini – Università degli Studi di Milano Bicocca, Piazza della Scienza 3, 20126 Milano, Italy INAF – Osservatorio Astronomico di Brera, Via Brera, 28, 20121 Milano, ItalyĮ-mail: – Università degli Studi dell’Insubria, Via Valleggio 11, 22100 Como, Italyĭipartimento di Fisica G.

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Blueshift e redshift