Mapping the dynamics of a giant Ly α halo at z = 4.1 with MUSE: the energetics of a large-scale AGN-driven outflow around a massive, high-redshift galaxy

Swinbank, A. M.; Vernet, J.; Smail, Ian; Breuck, C. De; Bacon, Roland; Contini, T.; Richard, Johan; Röttgering, H. J. A.; Urrutia, T.; Venemans, Bram

doi:10.1093/mnras/stv366

Cited by 65 publications

(61 citation statements)

References 90 publications

(132 reference statements)

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“…Such extended Lyα haloes have been detected in several other HzRGs (e.g. van Ojik et al 1996;Reuland et al 2003;Swinbank et al 2015). The Lyα halo in MRC0943-242 shows a linear filament, Bifrost, connecting Yggdrasil with the two brightest dust continuum components (Thor and Odin), strongly suggesting that they are physically connected (see Fig.…”

Section: Ionised Gasmentioning

confidence: 59%

The mysterious morphology of MRC0943-242 as revealed by ALMA and MUSE

Gullberg

Breuck

Lehnert

et al. 2016

A&A

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We present a pilot study of the z = 2.923 radio galaxy MRC0943-242, where we combine information from ALMA and MUSE data cubes for the first time. Even with modest integration times, we disentangle the AGN and starburst dominated components. These data reveal a highly complex morphology as the AGN, starburst, and molecular gas components show up as widely separated sources in dust continuum, optical continuum, and CO line emission observations. CO(1−0) and CO(8−7) line emission suggest that there is a molecular gas reservoir offset from both the dust and the optical continuum that is located ∼90 kpc from the AGN. The UV line emission has a complex structure in emission and absorption. The line emission is mostly due to a large scale ionisation cone energised by the AGN, and a Lyα emitting bridge of gas between the radio galaxy and a heavily star-forming set of components. Strangely, the ionisation cone has no Lyα emission. We find this is due to an optically thick layer of neutral gas with unity covering fraction spread out over a region of at least ∼100 kpc from the AGN. Other less thick absorption components are associated with Lyα emitting gas within a few tens of kpc from the radio galaxy and are connected by a bridge of emission. We speculate that this linear structure of dust, Lyα and CO emission, and the redshifted absorption seen in the circum nuclear region may represent an accretion flow feeding gas into this massive AGN host galaxy.

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Section: Ionised Gasmentioning

confidence: 59%

The mysterious morphology of MRC0943-242 as revealed by ALMA and MUSE

Gullberg

Breuck

Lehnert

et al. 2016

A&A

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“…Decarli et al (2016) and Aravena et al (2016) observed a comparable shift in the compact starforming galaxy ASPECSC.1 (z=2.54). In a similar fashion, the Lyα extended emission not associated with the radio jet, the rest-frame UV continuum, and the dust emission (albeit the coarse spatial resolution) appear to be offset in the z=4.11 radio galaxy TNJ1338−1942(e.g., De Breuck et al 2004Zirm et al 2005;Venemans et al 2007;Swinbank et al 2015).…”

Section: The Host Galaxy Of J0305−3150mentioning

confidence: 99%

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

Farina

Venemans

Decarli

et al. 2017

ApJ

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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arcsec 2 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 Lya ( )=(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 6 H~c m −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 . 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.

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“…The intrinsic brightness of these objects makes it possible to probe deeply into the physics of the gas, even to resolve the spatial variation of the Ly α line at kpc scales (e.g. Weijmans et al 2010;Swinbank et al 2015;Prescott et al 2015), but ideally, one would like to pursue similar studies on typical high redshift galaxies, which requires a very high signal-to-noise only achievable with the next generation of ground-based optical and near-infrared telescopes.…”

Section: Introductionmentioning

confidence: 99%

A young star-forming galaxy atz= 3.5 with an extended Lyman α halo seen with MUSE

Patrício

Richard

Verhamme

et al. 2016

Mon. Not. R. Astron. Soc.

101

102

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A young star-forming galaxy at z = 3.5 with an extended Lyman α halo seen with MUSE ABSTRACTSpatially resolved studies of high redshift galaxies, an essential insight into galaxy formation processes, have been mostly limited to stacking or unusually bright objects. We present here the study of a typical (L * , M = 6 ×10 9 M ) young lensed galaxy at z = 3.5, observed with MUSE, for which we obtain 2D resolved spatial information of Ly α and, for the first time, of C iii] emission. The exceptional signal-to-noise of the data reveals UV emission and absorption lines rarely seen at these redshifts, allowing us to derive important physical properties (T e ∼15600 K, n e ∼300 cm −3 , covering fraction f c ∼ 0.4) using multiple diagnostics. Inferred stellar and gas-phase metallicities point towards a low metallicity object (Z stellar = ∼ 0.07 Z and Z ISM < 0.16 Z ). The Ly α emission extends over ∼10 kpc across the galaxy and presents a very uniform spectral profile, showing only a small velocity shift which is unrelated to the intrinsic kinematics of the nebular emission. The Ly α extension is ∼4 times larger than the continuum emission, and makes this object comparable to low-mass LAEs at low redshift, and more compact than the Lyman-break galaxies and Lyα emitters usually studied at high redshift. We model the Ly α line and surface brightness profile using a radiative transfer code in an expanding gas shell, finding that this model provides a good description of both observables.

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Mapping the dynamics of a giant Ly α halo at z = 4.1 with MUSE: the energetics of a large-scale AGN-driven outflow around a massive, high-redshift galaxy

Cited by 65 publications

References 90 publications

The mysterious morphology of MRC0943-242 as revealed by ALMA and MUSE

The mysterious morphology of MRC0943-242 as revealed by ALMA and MUSE

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

A young star-forming galaxy atz= 3.5 with an extended Lyman α halo seen with MUSE

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