Spectral variations of Lyman $\alpha$ emission within strongly lensed sources observed with MUSE

Claeyssens, Adélaïde; Richard, Johan; Blaizot, Jérémy; Garel, Thibault; Leclercq, Floriane; Patrício, Vera; Verhamme, Anne; Wisotzki, L.; Bacon, Roland; Carton, David; Clément, Benjamin; Herenz, Edmund Christian; Marino, R. A.; Muzahid, Sowgat; Saust, R.; Schaye, Joop

doi:10.1093/mnras/stz2492

Cited by 58 publications

(76 citation statements)

References 52 publications

(67 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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“…Simple, idealized models of Lyα radiation transfer with a central ionizing point source surrounded by a homogeneous, spherically symmetric shell of gas with a range of neutral hydrogen column density (N(H )), dust opacity, velocity, and temperature (the so-called "shell model", see e.g., Zheng & Miralda-Escudé 2002;Verhamme et al 2006) have been surprisingly successful in explaining a large variety of Lyα line profiles (e.g., Hashimoto et al 2015;Gronke 2017). Using the shell model, Verhamme et al (2018) found a correlation between FWHM and V offset (see also Claeyssens et al 2019). The left panel of Fig.…”

Section: Discussionmentioning

confidence: 99%

MUSEQuBES: calibrating the redshifts of Ly α emitters using stacked circumgalactic medium absorption profiles

Muzahid

Schaye

Marino

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT Ly α emission lines are typically found to be redshifted with respect to the systemic redshifts of galaxies, likely due to resonant scattering of Ly α photons. Here, we measure the average velocity offset for a sample of 96 z ≈ 3.3 Ly α emitters (LAEs) with a median Ly α flux (luminosity) of ${\approx}10^{-17}~\rm erg~cm^{-2}~s^{-1}$ (${\approx}10^{42}~\rm erg~s^{-1}$) and a median star formation rate (SFR) of ≈1.3 $\rm M_{\odot }~yr^{-1}$ (not corrected for possible dust extinction), detected by the Multi-Unit Spectroscopic Explorer as part of our MUSEQuBES circumgalactic medium (CGM) survey. By postulating that the stacked CGM absorption profiles of these LAEs, probed by eight background quasars, must be centred on the systemic redshift, we measure an average velocity offset, Voffset = 171\pm 8 km s−1, between the Ly α emission peak and the systemic redshift. The observed Voffset is lower by factors of ≈1.4 and ≈2.6 compared to the velocity offsets measured for narrow-band-selected LAEs and Lyman break galaxies, respectively, which probe galaxies with higher masses and SFRs. Consistent with earlier studies based on direct measurements for individual objects, we find that the Voffset is correlated with the full width at half-maximum of the red peak of the Ly α line, and anticorrelated with the rest-frame equivalent width. Moreover, we find that Voffset is correlated with SFR with a sub-linear scaling relation, $V_{\rm offset}\propto \rm SFR^{0.16\pm 0.03}$. Adopting the mass scaling for main-sequence galaxies, such a relation suggests that Voffset scales with the circular velocity of the dark matter haloes hosting the LAEs.

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“…The origin of this Lyman-α emission is complex, and only the brightest Lyman-α haloes are sufficiently extended to allow spatially resolved analyses in the absence of any lensing effect (Erb et al 2018;Leclercq et al 2020) and test predictions from simulations. MUSE observations on lensing clusters offer the power to identify extended gas around high redshift galaxies (once magnified), allowing detailed studies of the spectral line properties within multiple regions, in particular through bright Lyman-α extended haloes (Patrício et al 2016;Smit et al 2017;Caminha et al 2016b;Vanzella et al 2017;Claeyssens et al 2019). Figure 12 shows a very clear example taken from our sample of extended emission detected over the z = 4.086 source originally identified by Cohen & Kneib (2002) in RXJ1347.…”

Section: Resolved Properties Of High Redshift Galaxiesmentioning

confidence: 98%

“…Examples of pyplatefit spectral fitting, for two sources in our catalogues. Top row shows the case of the bright z = 4.03 galaxy in MACS0940(Claeyssens et al 2019) with zcon f = 3 and the bottom row a MUSELET-selected galaxy at z = 0.337 and zcon f = 2 in the same cluster field (M364). The left panel gives an overview of the spectrum, while the middle and right panels zoom in on specific spectral line fits.…”

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confidence: 99%

An atlas of MUSE observations towards twelve massive lensing clusters

Richard

Claeyssens

Lagattuta

et al. 2021

A&A

112

131

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Context. Spectroscopic surveys of massive galaxy clusters reveal the properties of faint background galaxies thanks to the magnification provided by strong gravitational lensing. Aims. We present a systematic analysis of integral-field-spectroscopy observations of 12 massive clusters, conducted with the Multi Unit Spectroscopic Explorer (MUSE). All data were taken under very good seeing conditions (∼0″.6) in effective exposure times between two and 15 h per pointing, for a total of 125 h. Our observations cover a total solid angle of ∼23 arcmin2 in the direction of clusters, many of which were previously studied by the MAssive Clusters Survey, Frontier Fields (FFs), Grism Lens-Amplified Survey from Space and Cluster Lensing And Supernova survey with Hubble programmes. The achieved emission line detection limit at 5σ for a point source varies between (0.77–1.5) × 10−18 erg s−1 cm−2 at 7000 Å. Methods. We present our developed strategy to reduce these observational data, detect continuum sources and line emitters in the datacubes, and determine their redshifts. We constructed robust mass models for each cluster to further confirm our redshift measurements using strong-lensing constraints, and identified a total of 312 strongly lensed sources producing 939 multiple images. Results. The final redshift catalogues contain more than 3300 robust redshifts, of which 40% are for cluster members and ∼30% are for lensed Lyman-α emitters. Fourteen percent of all sources are line emitters that are not seen in the available HST images, even at the depth of the FFs (∼29 AB). We find that the magnification distribution of the lensed sources in the high-magnification regime (μ = 2–25) follows the theoretical expectation of N(z) ∝ μ−2. The quality of this dataset, number of lensed sources, and number of strong-lensing constraints enables detailed studies of the physical properties of both the lensing cluster and the background galaxies. The full data products from this work, including the datacubes, catalogues, extracted spectra, ancillary images, and mass models, are made available to the community.

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Spectral variations of Lyman $\alpha$ emission within strongly lensed sources observed with MUSE

Cited by 58 publications

References 52 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

MUSEQuBES: calibrating the redshifts of Ly α emitters using stacked circumgalactic medium absorption profiles

An atlas of MUSE observations towards twelve massive lensing clusters

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