We present an ALMA high-resolution (0.18″ × 0.21″) observation of the 840 μm continuum and [CII] λ157.74 μm line emission in the WISE-SDSS selected hyper-luminous (WISSH) quasi-stellar object (QSO) J1015+0020, at z ∼ 4.4. Our analysis reveals an exceptional overdensity of [CII]-emitting companions with a very small (<150 km s<SUP>-1</SUP>) velocity shift with respect to the QSO redshift. We report the discovery of the closest companion observed so far in submillimetre observations of high-z QSOs. It is only 2.2 kpc distant and merging with J1015+0020, while two other [CII] emitters are found at 8 and 17 kpc. Two strong continuum emitters are also detected at <3.5 arcsec from the QSO. They are likely associated with the same overdense structure of J1015+0020, as they exceed by a factor of 100 the number of expected sources, considering the log(N)-log(S) at 850 μm. The host galaxy of J1015+0020 shows a star formation rate (SFR) of about 100 M<SUB>☉</SUB>yr<SUP>-1</SUP>, while the total SFR of the QSO and its companion galaxies is a factor of ∼10 higher, indicating that substantial stellar mass assembly at early epochs may have taken place in the QSO satellites. For J1015+0020 we computed a black hole mass M<SUB>BH</SUB>∼ 6 × 10<SUP>9</SUP>M<SUB>☉</SUB>. As we resolve the [CII] emission of the QSO, we can compute a dynamical mass of M<SUB>dyn</SUB>∼ 4 × 10<SUP>10</SUP>M<SUB>☉</SUB>. This translates into an extreme ratio M<SUB>dyn</SUB>/M<SUB>BH</SUB>∼ 7, i.e. two orders of magnitude smaller than what is typically observed in local galaxies. The total stellar mass of the QSO host galaxy plus the [CII] emitters in the ALMA field of view already exceeds 10<SUP>11</SUP>M<SUB>☉</SUB>at z ∼ 4.4. These sources will likely merge and develop into a giant galaxy of ∼1.3 × 10<SUP>12</SUP>M<SUB>☉</SUB>. Under the assumption of constant Ṁ<SUB>acc</SUB>or λ<SUB>Edd</SUB>equal to the observed values, we find that the growth timescale of the host galaxy of J1015+0020 is comparable or even shorter than that inferred for the SMBH. Based on data from ALMA cycle 4 program 2016.1.00718.S.
The WISSH quasars project. V. ALMA reveals the assembly of a giant galaxy around a z = 4.4 hyper-luminous QSO
Bischetti, M.;Schneider, R.;VALIANTE, ROSA;
2018-01-01
Abstract
We present an ALMA high-resolution (0.18″ × 0.21″) observation of the 840 μm continuum and [CII] λ157.74 μm line emission in the WISE-SDSS selected hyper-luminous (WISSH) quasi-stellar object (QSO) J1015+0020, at z ∼ 4.4. Our analysis reveals an exceptional overdensity of [CII]-emitting companions with a very small (<150 km s-1) velocity shift with respect to the QSO redshift. We report the discovery of the closest companion observed so far in submillimetre observations of high-z QSOs. It is only 2.2 kpc distant and merging with J1015+0020, while two other [CII] emitters are found at 8 and 17 kpc. Two strong continuum emitters are also detected at <3.5 arcsec from the QSO. They are likely associated with the same overdense structure of J1015+0020, as they exceed by a factor of 100 the number of expected sources, considering the log(N)-log(S) at 850 μm. The host galaxy of J1015+0020 shows a star formation rate (SFR) of about 100 M☉yr-1, while the total SFR of the QSO and its companion galaxies is a factor of ∼10 higher, indicating that substantial stellar mass assembly at early epochs may have taken place in the QSO satellites. For J1015+0020 we computed a black hole mass MBH∼ 6 × 109M☉. As we resolve the [CII] emission of the QSO, we can compute a dynamical mass of Mdyn∼ 4 × 1010M☉. This translates into an extreme ratio Mdyn/MBH∼ 7, i.e. two orders of magnitude smaller than what is typically observed in local galaxies. The total stellar mass of the QSO host galaxy plus the [CII] emitters in the ALMA field of view already exceeds 1011M☉at z ∼ 4.4. These sources will likely merge and develop into a giant galaxy of ∼1.3 × 1012M☉. Under the assumption of constant Ṁaccor λEddequal to the observed values, we find that the growth timescale of the host galaxy of J1015+0020 is comparable or even shorter than that inferred for the SMBH. Based on data from ALMA cycle 4 program 2016.1.00718.S.Pubblicazioni consigliate
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