Lyα Halos around [O iii]-selected Galaxies in HETDEX

Niemeyer, Maja Lujan; Bowman, W. Paul; Ciardullo, Robin; Grönke, Max; Komatsu, Eiichiro; Fabricius, Maximilian; Farrow, Daniel J.; Finkelstein, Steven L.; Gebhardt, Karl; Grönwall, C.; Hill, Gary J.; Liu, Chenxu; Cooper, Erin Mentuch; Schneider, Donald P.; Tuttle, Sarah; Zeimann, Greg

doi:10.3847/2041-8213/ac82e5

Cited by 10 publications

(4 citation statements)

References 47 publications

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“…This could be a hint of the dominance of other processes. A similar conclusion of the dominance of scattered Lyα from central galaxies and possible contribution from the other processes is reached by recent observational studies (Lujan Niemeyer et al 2022a, 2022b. In this way, much information is buried beyond the flattening radius around 20 pkpc, outside of which contributions from central and satellites appear insufficient to explain the observations.…”

Section: Nonnegligible Contribution From In Situ Lyα Productionsupporting

confidence: 74%

“…The circumgalactic medium (CGM) contains vital information on these flow components and thus holds an important key to revealing galaxy evolution (see Tumlinson et al 2017, for a recent review). The CGM of z  2 star-forming galaxies is now routinely detected as diffuse Lyα nebulae, or Lyα halos (LAHs), around star-forming galaxies such as Lyα emitters (LAEs) and Lyman break galaxies (LBGs) at high redshift both individually (Rauch et al 2008;Wisotzki et al 2016;Leclercq et al 2017;Erb et al 2018;Bacon et al 2021;Kusakabe et al 2022) and through a stacking technique (Hayashino et al 2004;Steidel et al 2011;Matsuda et al 2012;Feldmeier et al 2013;Momose et al 2014Momose et al , 2016Xue et al 2017;Lujan Niemeyer et al 2022a, 2022b. Together with a technique based on absorption lines in the spectra of neighboring background sources (Adelberger et al 2005;Steidel et al 2010;Rudie et al 2012;Chen et al 2020;Muzahid et al 2021), LAHs have provided a crucial empirical window into the CGM of distant galaxies.…”

Section: Introductionmentioning

confidence: 99%

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UV and Lyα Halos of Lyα Emitters across Environments at z = 2.84*

Kikuta

Matsuda

Inoue

et al. 2023

ApJ

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We present UV and Lyα radial surface brightness (SB) profiles of Lyα emitters (LAEs) at z = 2.84 detected with the Hyper Suprime-Cam on the Subaru Telescope. The depth of our data, together with the wide-field coverage including a protocluster, enable us to study the dependence of Lyα halos (LAHs) on various galaxy properties, including Mpc scale environments. UV and Lyα images of 3490 LAEs are extracted, and stacking the images yields SB sensitivity of ∼ 1 × 10 − 20 erg s − 1 cm − 2 arcsec − 2 in Lyα, reaching the expected level of optically thick gas illuminated by the UV background at z ∼ 3. Fitting of the two-component exponential function gives the scale-lengths of 1.56 ± 0.01 and 10.4 ± 0.3 pkpc. Dividing the sample according to their photometric properties, we find that, while the dependence of halo scale-length on environment outside of the protocluster core is not clear, LAEs in the central regions of protoclusters appear to have very large LAHs, which could be caused by combined effects of source overlapping and diffuse Lyα emission from cool intergalactic gas permeating the forming protocluster core irradiated by active members. For the first time, we identify UV halos around bright LAEs that are probably due to a few lower-mass satellite galaxies. Through comparison with recent numerical simulations, we conclude that, while scattered Lyα photons from the host galaxies are dominant, star formation in satellites evidently contributes to LAHs, and that fluorescent Lyα emission may be boosted within protocluster cores at cosmic noon and/or near bright QSOs.

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Section: Nonnegligible Contribution From In Situ Lyα Productionsupporting

confidence: 74%

Section: Introductionmentioning

confidence: 99%

UV and Lyα Halos of Lyα Emitters across Environments at z = 2.84*

Kikuta

Matsuda

Inoue

et al. 2023

ApJ

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“…This could produce the profile seen in Figure 1. However, while extended Lyα emission is present in HETDEX data (Lujan Niemeyer et al 2022a, 2022b, troughs exist when using local sky subtraction and when using full-field sky subtraction. The fullfield sky is measured from all of HETDEX's 34,944 fibers spread over a 21′ field of view.…”

Section: Instrumental and Algorithmic Concernsmentioning

confidence: 99%

Absorption Troughs of Lyα Emitters in HETDEX

Weiss,

Davis,

Gebhardt

et al. 2024

ApJ

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The Hobby–Eberly Telescope Dark Energy Experiment (HETDEX) is designed to detect and measure the redshifts of more than 1 million Lyα emitting galaxies (LAEs) 1.88 < z < 3.52. In addition to its cosmological measurements, these data enable studies of Lyα spectral profiles and the underlying radiative transfer. Using the roughly half a million LAEs in the HETDEX Data Release 3, we stack various subsets to obtain the typical Lyα profile for the z ∼ 2–3 epoch and to understand their physical properties. We find clear absorption wings around Lyα emission, which extend ∼2000 km s−1 both redward and blueward of the central line. Using far-UV spectra of nearby (0.002 < z < 0.182) LAEs in the COS Legacy Archive Spectroscopic Survey treasury and optical/near-IR spectra of 2.8 < z < 6.7 LAEs in the Multi Unit Spectroscopic-Wide survey, we observe absorption profiles in both redshift regimes. Dividing the sample by volume density shows that the troughs increase in higher-density regions. This trend suggests that the depth of the absorption is dependent on the local density of objects near the LAE, a geometry that is similar to damped Lyα systems. Simple simulations of Lyα radiative transfer can produce similar troughs due to absorption of light from background sources by H i gas surrounding the LAEs.

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“…MNRAS 525, 4388-4404 (2023) Farina et al 2019 ;Arrigoni Battaia et al 2019a , b ;O'Sulli v an et al 2020 ;Fossati et al 2021 ) and galaxies (Leclercq et al 2017 ;Wisotzki et al 2018 ), where the integral field spectrographs positioned at the largest observing facilities, such as the Multi-Unit Spectroscopic Explorer (MUSE; Bacon et al 2010 ) at the Very Large Telescope and the Keck Cosmic Web Imager (KCWI; Morrissey et al 2018 ) at the Keck telescope, have been key to significantly improve the detection of this extended Ly α emission (see also e.g. Umehata et al 2019 ;Bacon et al 2021 ;Kusakabe et al 2022 ;Lujan Niemeyer et al 2022 ).…”

mentioning

confidence: 99%

The MUSE Ultra Deep Field (MUDF). IV. A pair of X-ray weak quasars at the heart of two extended Lyα nebulae

Lusso,

Nardini,

Fumagalli

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present the results obtained from follow-up observations of the MUSE Ultra Deep Field (MUDF) at X-ray energies with XMM–Newton. The MUDF is centred on a unique field with two bright, physically associated quasars at z ≃ 3.23, separated by ∼500 kpc in projection. Both quasars are embedded within extended Lyα nebulae ($\gtrsim 100~\rm kpc$ at a surface brightness flux level of ≈6 × 10−19$\rm erg~s^{-1}~cm^{-2}~arcsec^{-2}$), whose elongated morphology is suggestive of an extended filament connecting the quasar haloes. The new X-ray observations presented here allow us to characterise the physical properties (e.g. X-ray slope, luminosities, gas column densities) in the innermost region of the MUDF quasars. We find that both quasars are X-ray underluminous compared to objects at similar ultraviolet luminosities. Based on our X-ray spectral analysis, absorbing columns of NH(z) ≳ 1023 cm−2 appear unlikely, therefore such a weakness is possibly intrinsic. When also including literature data, we do not observe any detectable trend between the area of the nebulae and nuclear luminosities at both the rest-frame 2 keV and 2500 Å. The area is also not correlated with the X-ray photon index nor with the integrated band flux in the hard band (2–10 keV). We also do not find any trend between the extended Lyα emission of the nebulae and the nuclear X-ray luminosity. Finally, the properties of the MUDF quasars’ nebulae are consistent with the observed relation between the Lyα integrated luminosity of the nebulae and their area. Our results suggest that the quasar ionization power is not a strong driver of the morphology and size of the nebulae.

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Lyα Halos around [O iii]-selected Galaxies in HETDEX

Cited by 10 publications

References 47 publications

UV and Lyα Halos of Lyα Emitters across Environments at z = 2.84*

UV and Lyα Halos of Lyα Emitters across Environments at z = 2.84*

Absorption Troughs of Lyα Emitters in HETDEX

The MUSE Ultra Deep Field (MUDF). IV. A pair of X-ray weak quasars at the heart of two extended Lyα nebulae

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