The MUSE <i>Hubble</i> Ultra Deep Field Survey

Leclercq, Floriane; Bacon, Roland; Verhamme, Anne; Garel, Thibault; Blaizot, Jérémy; Brinchmann, Jarle; Cantalupo, Sebastiano; Claeyssens, Adélaïde; Conseil, Simon; Contini, T.; Hashimoto, T.; Herenz, Edmund Christian; Kusakabe, Haruka; Marino, R. A.; Maseda, Michael V.; Matthee, Jorryt; Mitchell, Peter D.; Pezzulli, Gabriele; Richard, Johan; Schmidt, Kasper B.; Wisotzki, L.

doi:10.1051/0004-6361/201937339

Cited by 85 publications

(100 citation statements)

References 74 publications

(91 reference statements)

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“…5). This resembles recent results at z ≈ 3 − 4 (Claeyssens et al 2019;Leclercq et al 2020) who report somewhat redder Lyα lines at lower surface brightness compared to the Lyα line profile at peak surface brightness, and which they suggest to be indicative of resonant scattering and to support the idea that most of the Lyα emission originates from the UV peak.…”

Section: A Single Source Illuminating a Complex Structuresupporting

confidence: 90%

The nature of CR7 revealed with MUSE: a young starburst powering extended Ly α emission at z = 6.6

Matthee

Pezzulli

Mackenzie

et al. 2020

Monthly Notices of the Royal Astronomical Society

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CR7 is among the most luminous Lyman-α emitters (LAEs) known at z = 6.6 and consists of at least three UV components that are surrounded by Lyman-α (Lyα) emission. Previous studies have suggested that it may host an extreme ionising source. Here, we present deep integral field spectroscopy of CR7 with VLT/MUSE. We measure extended emission with a similar halo scale length as typical LAEs at z ≈ 5. CR7’s Lyα halo is clearly elongated along the direction connecting the multiple components, likely tracing the underlying gas distribution. The Lyα emission originates almost exclusively from the brightest UV component, but we also identify a faint kinematically distinct Lyα emitting region nearby a fainter component. Combined with new near-infrared data, the MUSE data show that the rest-frame Lyα equivalent width (EW) is ≈100 Å. This is a factor four higher than the EW measured in low-redshift analogues with carefully matched Lyα profiles (and thus arguably HI column density), but this EW can plausibly be explained by star formation. Alternative scenarios requiring AGN powering are also disfavoured by the narrower and steeper Lyα spectrum and much smaller IR to UV ratio compared to obscured AGN in other Lyα blobs. CR7’s Lyα emission, while extremely luminous, resembles the emission in more common LAEs at lower redshifts very well and is likely powered by a young metal poor starburst.

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Section: A Single Source Illuminating a Complex Structuresupporting

confidence: 90%

The nature of CR7 revealed with MUSE: a young starburst powering extended Ly α emission at z = 6.6

Matthee

Pezzulli

Mackenzie

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Tracing the CGM gas in ionized emission from rest-frame UV lines has revealed large extended halos around high-z galaxies. The Lyα emission is seen to be distributed as a more or less uniform sphere around the galaxies (Wisotzki et al 2016;Leclercq et al 2017Leclercq et al , 2020 or show more complex structures (e.g., Cantalupo et al 2014;Vernet et al 2017;Li et al 2019;Martin et al 2019). Observing the CGM in emission such as Lyα is thus a powerful tool to probe the extent and structure of the CGM.…”

Section: Importance Of Multi-phase Observations and The Nature Of The Emission Regionmentioning

confidence: 99%

“…forming galaxies at redshifts 3 ≤ z ≤ 6 in the Hubble Deep Field South and other regions (Wisotzki et al 2016;Leclercq et al 2017Leclercq et al , 2020Bielby et al 2020). Extended Lyα halos have also shown kinematic signs, suggesting large-scale rotation of accreting material (Prescott et al 2015) and a filamentary structure (Cantalupo et al 2014;Vernet et al 2017;Martin et al 2019;Umehata et al 2019).…”

Section: Introductionmentioning

confidence: 99%

ALMA and MUSE observations reveal a quiescent multi-phase circumgalactic medium around the z ≃ 3.6 radio galaxy 4C 19.71

Falkendal

Lehnert

Vernet

et al. 2021

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We present MUSE at VLT imaging spectroscopy of rest-frame ultraviolet emission lines and ALMA observations of the [C I] 3P1−3P0 emission line, probing both the ionized and diffuse molecular medium around the radio galaxy 4C 19.71 at z ≃ 3.6. This radio galaxy has extended Lyα emission over a region ∼100 kpc in size preferentially oriented along the axis of the radio jet. Faint Lyα emission extends beyond the radio hot spots. We also find extended C IV and He II emission over a region of ∼150 kpc in size, where the most distant emission lies ∼40 kpc beyond the north radio lobe and has narrow full width half maximum (FWHM) line widths of ∼180 km s−1 and a small relative velocity offset Δv ∼ 130 km s−1 from the systemic redshift of the radio galaxy. The [C I] is detected in the same region with FWHM ∼ 100 km s−1 and Δv ∼ 5 km s−1, while [C I] is not detected in the regions south of the radio galaxy. We interpret the coincidence in the northern line emission as evidence of relatively quiescent multi-phase gas residing within the halo at a projected distance of ∼75 kpc from the host galaxy. To test this hypothesis, we performed photoionization and photo-dissociated region (PDR) modeling, using the code Cloudy, of the three emission line regions: the radio galaxy proper and the northern and southern regions. We find that the [C I]/C IVλλ1548,1551 and C IVλλ1548,1551/He II ratios of the two halo regions are consistent with a PDR or ionization front in the circumgalactic medium likely energized by photons from the active galactic nuclei. This modeling is consistent with a relatively low metallicity, 0.03 < [Z/Z⊙] < 0.1, and diffuse ionization with an ionization parameter (proportional to the ratio of the photon number density and gas density) of log U ∼ −3 for the two circumgalactic line emission regions. Using rough mass estimates for the molecular and ionized gas, we find that the former may be tracing ≈2−4 orders of magnitude more mass. As our data are limited in signal-to-noise due to the faintness of the line, deeper [C I] observations are required to trace the full extent of this important component in the circumgalactic medium.

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“…In recent years we have used a fraction of our MUSE guaranteed observing time to perform deep field observations in the Hubble Ultra-Deep Field (HUDF, Beckwith et al 2006) at 10 and 30 h depths (Bacon et al 2017). These observations have increased the amount of available spectroscopic information in the HUDF by more than an order of magnitude (Inami et al 2017) and enabled several breakthroughs in our understanding of the high redshift universe, notably the discovery of ubiquitous extended Lyα emission from the CGMs around individual galaxies at z > 3 (Wisotzki et al 2016;Leclercq et al 2017Leclercq et al , 2020.…”

Section: Introductionmentioning

confidence: 99%

The MUSE Extremely Deep Field: The cosmic web in emission at high redshift

Bacon

Mary

Garel

et al. 2021

A&A

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We report the discovery of diffuse extended Lyα emission from redshift 3.1 to 4.5, tracing cosmic web filaments on scales of 2.5−4 cMpc. These structures have been observed in overdensities of Lyα emitters in the MUSE Extremely Deep Field, a 140 h deep MUSE observation located in the Hubble Ultra-Deep Field. Among the 22 overdense regions identified, five are likely to harbor very extended Lyα emission at high significance with an average surface brightness of 5 × 10−20 erg s−1 cm−2 arcsec−2. Remarkably, 70% of the total Lyα luminosity from these filaments comes from beyond the circumgalactic medium of any identified Lyα emitter. Fluorescent Lyα emission powered by the cosmic UV background can only account for less than 34% of this emission at z ≈ 3 and for not more than 10% at higher redshift. We find that the bulk of this diffuse emission can be reproduced by the unresolved Lyα emission of a large population of ultra low-luminosity Lyα emitters (< 1040 erg s−1), provided that the faint end of the Lyα luminosity function is steep (α ⪅ −1.8), it extends down to luminosities lower than 1038 − 1037 erg s−1, and the clustering of these Lyα emitters is significant (filling factor < 1/6). If these Lyα emitters are powered by star formation, then this implies their luminosity function needs to extend down to star formation rates < 10−4 M⊙ yr−1. These observations provide the first detection of the cosmic web in Lyα emission in typical filamentary environments and the first observational clue indicating the existence of a large population of ultra low-luminosity Lyα emitters at high redshift.

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The MUSE Hubble Ultra Deep Field Survey

Cited by 85 publications

References 74 publications

The nature of CR7 revealed with MUSE: a young starburst powering extended Ly α emission at z = 6.6

The nature of CR7 revealed with MUSE: a young starburst powering extended Ly α emission at z = 6.6

ALMA and MUSE observations reveal a quiescent multi-phase circumgalactic medium around the z ≃ 3.6 radio galaxy 4C 19.71

The MUSE Extremely Deep Field: The cosmic web in emission at high redshift

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