Ratio of black hole to galaxy mass of an extremely red dust-obscured galaxy at z = 2.52

Abstract

We present a near-infrared (NIR) spectrum of WISE J104222.11+164115.3, an extremely red dust-obscured galaxy (DOG), which has been observed with the Long-slit Intermediate Resolution Infrared Spectrograph (LIRIS) on the 4.2m William Hershel Telescope. This object was selected as a hyper-luminous DOG candidate at z ∼ 2 by combining the optical and IR photometric data based on the Sloan Digital Sky Survey (SDSS) and Wide-field Infrared Survey Explorer (WISE), although its redshift had not yet been confirmed. Based on the LIRIS observation, we confirmed its redshift of 2.521 and total IR luminosity of log(L IR /L ⊙ ) = 14.57, which satisfies the criterion for an extremely luminous IR galaxy (ELIRG). Moreover, we indicate that this object seems to have an extremely massive black hole with M BH = 10 10.92 M ⊙ based on the broad Hα line: the host stellar mass is derived as M ⋆ = 10 13.55 M ⊙ by a fit of the spectral energy distribution. Very recently, it has been reported that this object is an anomalous gravitationally lensed quasar based on near-IR high-resolution imaging data obtained with the Hubble Space Telescope. Its magnification factor has also been estimated with some uncertainty (i.e., µ = 53-122). We investigate the ratio of the black hole to galaxy mass, which is less strongly affected by a lensing magnification factor, instead of the absolute values of the luminosities and masses. We find that the M BH /M ⋆ ratio (i.e., 0.0140-0.0204) is significantly higher than the local relation, following a sequence of unobscured quasars instead of obscured objects (e.g., submillimeter galaxies) at the same redshift. Moreover, the LIRIS spectrum shows strongly blueshifted oxygen lines with an outflowing velocity of ∼ 1100 km/s, and our Swift X-ray observation also supports that this source is an absorbed AGN with an intrinsic column density of N int H = 4.9 × 10 23 cm −2 . These results imply that WISE J104222.11+164115.3 is in a blow-out phase at the end of the buried rapid black hole growth.

Supermassive black hole demographics: evading M − σ

“…This evolution fits that of the system WISE J104222.11+164115.3 (Matsuoka et al 2018) discussed above. This appears to be in the blowout phase, which would normally require its SMBH mass M 10 11 M to be close to Mσ.…”

“…The SMBH in NGC 1600 is significantly below it for any spin rate, and this is probably true of NGC 4889 (cf King 2016). A contender for the most extreme system is currently the very dust-obscured WISE J104222.11+164115.3, at redshift z = 2.52 (Matsuoka et al 2018). This galaxy has strongly blueshifted oxygen lines corresponding to an outflow velocity ∼ 1100 km s −1 , close to the prediction in Equation 2.…”

ALMA Reveals a Gas-rich, Maximum Starburst in the Hyperluminous, Dust-obscured Quasar W0533–3401 at z ∼ 2.9

“…A low Eddington ratio in W0533−3401, for instance λ Edd < 0.3, seems not likely, otherwise M BH /M ⋆ of W0533−3401 will be higher than 0.2. Even if taking λ Edd = 1.0, the inferred M BH /M ⋆ of W0533−3401 is not only over one order of magnitude higher than the typical values ∼ 0.0002 − 0.0005 in the local Universe (Kormendy & Ho 2013), but also ∼ 5 times higher than the expected value by the evolutionary trend of M BH /M ⋆ (McLure et al 2006;Peng et al 2006;Merloni et al 2010;Targett et al 2012;Bongiorno et al 2014;Matsuoka et al 2018). We derive the black hole mass growth rateṀ BH of W0533−3401 from the bolometric luminosity by using the relation L AGN = (ηṀ BH c 2 )/(1 − η) and adopting η 1−η = 0.1.…”

A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). II. Physical Properties Derived from the SED Fitting with Optical, Infrared, and Radio Data

“…We have confirmed that the choice of cutoff wavelength does not significantly affect the following results. Table 1 lists the detailed parameter ranges adopted in the SED fitting (see also Matsuoka et al 2018;Chen et al 2019;Toba et al 2019). In addition to the energy balance between UV/optical and IR part, CIGALE takes into account the balance between IR and radio luminosity that is parameterized by q IR , which are eventually an essential framework in CIGALE.…”

“…The mean values of E(B −V ) * of the SDSS-and HSC-level objects are ∼0.19 and ∼0.45, respectively. Indeed, 5 HSC-level objects with mean E(B − V ) * of 0.45 satisfies a criterion of IR-bright dustobscured galaxies with S/N > 3 at 22 µm (see e.g.,Toba et al 2015; Toba & Nagao 2016; Toba et al 2017aToba et al , 2018Noboriguchi et al 2019).…”