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Published October 20, 2017 | Submitted + Published
Journal Article Open

Mapping the Lyα Emission around a z ∼ 6.6 QSO with MUSE: Extended Emission and a Companion at a Close Separation

Abstract

We utilize the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope to search for extended Lyα emission around the z ~ 6.6 QSO J0305−3150. After carefully subtracting the point spread function, we reach a nominal 5σ surface-brightness limit of SB_(5σ) = 1.9 × 10^(−18) erg s^(−1)cm^(−2) arcsec^(−2) over a 1 arcsec2 aperture, collapsing five wavelength slices centered at the expected location of the redshifted Lyα emission (i.e., at 9256 Å). Current data suggest the presence (5σ accounting for systematics) of a Lyα nebula that extends for 9 kpc around the QSO. This emission is displaced and redshifted by 155 km s^(−1) with respect to the location of the QSO host galaxy traced by the [C II] 158 μm emission line. The total luminosity is L(Lyα) = (3.0 ± 0.4) × 10^(42) erg s^(−1). Our analysis suggests that this emission is unlikely to rise from optically thick clouds illuminated by the ionizing radiation of the QSO. It is more plausible that the Lyα emission is due to the fluorescence of the highly ionized optically thin gas. This scenario implies a high hydrogen volume density of n_H ~ 6 cm^(−3). In addition, we detect a Lyα emitter (LAE) in the immediate vicinity of the QSO, i.e., with a projected separation of ~12.5 kpc and a line-of-sight velocity difference of 560 km s^(−1). The luminosity of the LAE is L(Lyα = (2.1 ± 0.2) × 10^(42) erg s^(−1) and its inferred star-formation rate is SFR ~ 1.3 M⊙ yr^(−1). The probability of finding such a close LAE is one order of magnitude above the expectations based on the QSO–galaxy cross-correlation function. This discovery is in agreement with a scenario where dissipative interactions favor the rapid build-up of supermassive black holes at early cosmic times.

Additional Information

© 2017 The American Astronomical Society. Received 2016 November 17; revised 2017 August 30; accepted 2017 September 13; published 2017 October 13. E.P.F., B.P.V., and F.W. acknowledge funding through the ERC grant "Cosmic Dawn." Support for R.D. was provided by the DFG priority program 1573 "The physics of the interstellar medium." S.C. gratefully acknowledges support from Swiss National Science Foundation grant PP00P2_163824. E.P.F. is grateful to M. Fouesneau for providing support in the use of Python for the analysis of the MUSE datacubes, to M. Fumagalli for sharing data on the QSO Q0956+122, and to M. Rauch for providing feedback on the manuscript. We thank the members of the ENIGMA group14 at the Max Planck Institute for Astronomy (MPIA) for helpful discussions. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013); APLpy,15 an open-source plotting package for Python based on Matplotlib (Hunter 2007); and IRAF.16 Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 094.B-0893(A).

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Published - Farina_2017_ApJ_848_78.pdf

Submitted - 1709.06096.pdf

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August 19, 2023
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