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Gas filaments of the cosmic web located around active galaxies in a protocluster

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Science  04 Oct 2019:
Vol. 366, Issue 6461, pp. 97-100
DOI: 10.1126/science.aaw5949

Glowing filaments of the cosmic web

Most gas in the Universe lies in the intergalactic medium, where it forms into sheets and filaments of the cosmic web. Clusters of galaxies form at the intersection of these filaments, fed by gas pulled along them by gravity. Although this picture is well established by cosmological simulations, it has been difficult to demonstrate observationally. Umehata et al. mapped emission from the intergalactic medium in an area around galaxies that are starting to form a cluster (see the Perspective by Hamden). They found that the gas is arranged into filaments, whose position and velocity correlate with star-forming galaxies, supporting the theoretical picture.

Science, this issue p. 97; see also p. 31

Abstract

Cosmological simulations predict that the Universe contains a network of intergalactic gas filaments, within which galaxies form and evolve. However, the faintness of any emission from these filaments has limited tests of this prediction. We report the detection of rest-frame ultraviolet Lyman-α radiation from multiple filaments extending more than one megaparsec between galaxies within the SSA22 protocluster at a redshift of 3.1. Intense star formation and supermassive black-hole activity is occurring within the galaxies embedded in these structures, which are the likely sources of the elevated ionizing radiation powering the observed Lyman-α emission. Our observations map the gas in filamentary structures of the type thought to fuel the growth of galaxies and black holes in massive protoclusters.

Cosmological simulations of structure formation predict that the majority of gas in the intergalactic medium (IGM) is distributed in a cosmic web of sheets and filaments as a consequence of gravitational collapse (1). The intersections of these structures become the locations at which galaxies and their supermassive black holes (SMBHs) form and evolve (2). Streams of cool gas falling along IGM filaments, driven by gravity, are predicted to provide most of the gas required for the growth of galaxies and SMBHs (3, 4). Direct detection of the cosmic web in the early Universe would allow tests of these predictions, both for the large-scale structure and for the formation and evolution of galaxies.

Galaxy formation models predict that at a redshift (z) of ~3, >60% of all gas in the Universe resides in filaments (5). However, their low density makes them difficult to observe in emission. Absorption spectroscopy using background sources, such as quasars, has been the primary method used to trace neutral hydrogen (H i) in the IGM (6, 7), which has provided insights into the nature of the cosmic web (6). Nevertheless, it has not been possible to obtain a detailed picture of these filaments, as information is limited to one dimension along the line of sight to the background source. The low sky density of sufficiently bright background sources prevents study of the cosmic web on scales finer than a few megaparsec (Mpc) (7).

Imaging the cosmic web in emission would provide two-dimensional (2D) information. Filaments are predicted to emit the hydrogen Lyman-alpha (Lyα) line by means of the fluorescence induced by the ultraviolet background (UVB) radiation (8). The intrinsically low intensity of the UVB means the expected surface brightness of a filament is ~2.5 × 10–20 erg s−1 cm−2 arcsec−2 at z ~3 (9), so direct detection of UVB-induced fluorescent emission from IGM filaments has remained elusive (10). To circumvent this limitation, one can examine regions where local ionizing sources, such as star-forming galaxies and/or active galactic nuclei (AGNs), boost the local radiation field and hence elevate the Lyα emission to detectable levels (11). Extended (up to hundreds of kiloparsec) Lyα nebulae have been observed around quasars, with morphologies and kinematics suggestive of cosmic web filaments connecting to the quasar host galaxies (1215). Similarly, using Lyα-emitting galaxies (LAEs) or extended emission arising from the circumgalactic medium (CGM) as tracers, statistical evidence for filaments has been reported (1618). These studies do not directly connect the cosmic web to the population of galaxies and SMBHs on cosmological scales.

We searched for extended filamentary structures using the Multi Unit Spectroscopic Explorer (MUSE) on the European Southern Observatory’s Very Large Telescope (VLT). Our observations targeted the galaxy protocluster SSA22 at z = 3.09 (19), which was already known to host 3D filamentary structures as traced by LAEs on a scale of 30 comoving megaparsec (comoving distances remain constant over time if the two objects are moving with the expansion of the Universe) (20). At the intersection of these large-scale structures lies the protocluster core, where several intensely star-forming galaxies are known to lie within a 2′ by 3′ region around the core, which was previously mapped at 1.1 mm with the Atacama Large Millimeter/submillimeter Array (ALMA) [the ALMA Deep Field in SSA22 (ADF22)] (21). To trace extended Lyα emission in this region, we mapped the ADF22 field with a six-pointing MUSE mosaic covering 116′′ by 169′′, equivalent to 0.9 by 1.3 physical Mpc at z = 3.09 [Fig. 1 (22)].

Fig. 1 Multiwavelength images of ADF22 illustrating the overdensity of galaxies and AGNs in a narrow redshift range at z = 3.09.

Each panel is centered at (α, δ) = (22h17m34.0s, +00d17m00s), where α is right ascension and δ is declination, and 2′ by 3′ in size, with the inner dashed area showing the MUSE coverage, 116′′ by 169′′ (0.9 by 1.3 Mpc at z ~3.1). North is up and east is left. (A) Pseudocolor map created from the MUSE cube (synthetized V-, R-, and i′-bands are used for the blue, green, and red channels, respectively). (B) The 1.1-mm ALMA continuum map of ADF22 (22). Identified sources at z = 3.09 are marked with white circles (SMGs) and squares (AGNs); positions and redshifts are listed in table S2. (C) Pseudocolor map of the Chandra x-ray data; 2 to 8 keV (hard band), 0.5 to 8 keV (full band), and 0.5 to 2 keV (soft band) are used for the blue, green, and red channels, respectively.

We searched the MUSE data cube for extended Lyα emission in conjunction with a narrow-band image covering the expected wavelength of redshifted Lyα emission taken with Suprime-Cam on the Subaru telescope (22). We identified extended Lyα emission with surface brightness ΣLyα > ~3 × 10–19 erg s−1 cm−2 arcsec−2 across the observed field, visible in the optimally extracted Lyα map [Fig. 2 (22)]. This map shows bright areas associated with the CGM of galaxies, along with several patches of emission at low surface brightness that connect to, but are not immediately associated with, individual galaxies in this region. Most of this low-surface-brightness Lyα emission forms two main filaments running in a north-south direction, each with a total extent of >1 physical megaparsec in projection. The scale of this emission far exceeds the expected size of the dark-matter halo of even the most massive individual galaxies at this epoch (the halo radius is ~100 kiloparsec for a 1012.5 M halo at z~3, where M is the mass of the Sun), so the Lyα signal likely traces a structure connecting several galaxies. This network of filaments likely extends beyond the region that we mapped, because the Lyα emission is detected up to the edge of the MUSE field of view. As shown in Fig. 3, A and B, the majority of the Lyα emission is detected over a line-of-sight velocity range of ~−500 to ~+1000 km s−1 relative to z = 3.09. This velocity range reflects not only the 3D distribution of matter on large scales, but also the gas kinematics within the protocluster core, which, coupled with radiative transfer effects, can produce velocity gradients of several hundreds of kilometers per second.

Fig. 2 Lyα emission map optimally extracted from the MUSE observations and covering the same field as that in Fig. 1.

Lyα emissions largely compose two groups of filamentary structures for >1 physical megaparsec. One high-surface-brightness filament is visible running north to south on the west side of the field, whereas a fainter (and hence more fragmented) structure runs north to south up the east side of the field. Contours with solid, dashed, and dotted lines show Lyα surface brightness levels of ΣLyα = 0.3, 1.0, and 2.0 × 10–18 erg s−1 cm−2 arcsec−2, respectively (these correspond to 2, 7, and 13 σ above the representative noise level). Navy blue contours indicate the extent of the two LABs in this field (23). Positions of SMGs and x-ray–luminous AGNs at z = 3.09 are also shown. The large, filled black circle shows data removed around a foreground, low-redshift galaxy.

Fig. 3 Three-dimensional pictures of Lyα filaments.

(A) Velocity map of the Lyα emission obtained from its flux-weighted centroid in the MUSE data. Image scale and plotting symbols are the same as those in Fig. 2. Coherent velocity trends can be seen along the filament structures. (B) The 3D distribution of Lyα filaments shown with blue [signal-to-noise ratio (SNR) > 2] and magenta (SNR > 5) voxels. The locations of SMGs (without detectable x-ray AGNs, orange circles), AGN-hosting SMGs (red diamonds), and x-ray–luminous AGNs without ALMA 1-mm detections (brown hexagons) are also displayed. The Lyα filaments and SMGs and AGNs are colocated on megaparsec scales.

Observations of the SSA22 protocluster have detected 35 Lyα blobs (LABs), defined as extended Lyα nebulae with sizes between several tens and several hundreds of kiloparsec (2325). Two of these LABs lie within our field of view, each with sizes of ~40 kiloparsec when measured at a Lyα surface brightness threshold of ΣLyα = 2.2 × 10–18 erg s−1 cm−2 arcsec−2 (24). Figure 2 shows that these two LABs are parts of a larger network of megaparsec-scale filaments. Embedded in these filaments are also other patches of enhanced Lyα emission, some of which are associated with galaxies. We interpret the previously known LABs as bright knots within a wider network of gas filaments, and surmise that the fainter and more extended Lyα-emitting gas in these filaments has previously eluded detection because of its low surface brightness (18, 26).

To explore the link between these filaments and the associated galaxy population, we measured redshifts of galaxies in this field using a multiwavelength spectroscopic dataset. The deep, 1.1-mm ADF22 map enables us to identify submillimeter galaxies (SMGs), which are massive, intense starburst galaxies with large amounts of gas and dust in their interstellar mediums. The x-ray–luminous AGNs, which host growing SMBHs, were identified from observations using the Chandra space telescope (22, 27). Spectroscopic redshifts for these populations were determined using a combination of emission lines [CO J = 3 → 2, Hβ, and (O iii) 4959 and 5008 Å lines] from ALMA data and observations with the Multi-Object Spectrometer for Infra-Red Exploration (MOSFIRE) on the Keck I telescope (22). We confirmed that 16 SMGs and 8 x-ray–luminous AGNs are protocluster members, with redshifts 3.085 ≤ z ≤ 3.098 (table S2). All of the SMGs and x-ray–luminous AGNs were distributed within the same structure (see Figs. 2 and 3), closely tracking the Lyα filaments both spatially (in projection) and in velocity (fig. S10). A similar pattern was also evident for normal star-forming galaxies and LAEs (fig. S7). We interpret this close alignment as evidence that the Lyα filaments are directly linked to the population of active galaxies and SMBHs. Gas filaments are thought to supply (under the effect of gravity) the fuel for active SMGs and x-ray–luminous AGNs.

The filaments have Lyα brightness above the level expected from fluorescent emission induced by the UVB (8, 11). Radiative transfer calculations predict a maximum surface brightness from optically thick gas of ~2.5 × 10–20 erg s−1 cm−2 arcsec−2 assuming a z~3 UVB (9). Our observations contain emission at levels of ΣLyα ≥ 3 × 10–19 erg s−1 cm−2 arcsec−2, which, in the optically thick limit, requires an intensity of the ionizing radiation field that is >12 times brighter than that predicted by UVB models (22). This corresponds to an ionizing photon flux ϕ > 4 × 106 cm−2 s−1. If we assume that the gas is fully ionized, then the observed surface brightness would imply even higher photon fluxes, densities of ~6 × 10–3 cm−3 (12) for gas at T ~ 104 K (where T is temperature), and a typical filament width of 100 kpc (Fig. 2). Fluctuations in the observed surface brightness suggest a variable density across the structure, as commonly found for bright Lyα nebulae (12). Figure 2 also shows regions at much higher surface brightness, particularly overlapping with galaxies (see also fig. S7). The fainter emission regions display lower velocity dispersions [full width at half maximum (FWHM) ~150 km s−1] than the brighter knots (FWHM ~730 km s−1), where the surface brightness of the latter is similar to the typical brightness of the LABs (figs. S4 and S9). This higher surface brightness may indicate the presence of localized sources of ionization, such as star formation or AGN activity, as commonly seen in LABs (28).

Given the large number of active galaxies in this region, the elevated photon flux required to power the filaments could be provided by the galaxy population identified within our field. To test this hypothesis, we determined the number of ionizing photons provided by x-ray–selected AGNs and SMGs (22). Under the simple assumption that the ionizing sources typically lie 250 kpc from filaments, the required photon flux corresponds to a photon number emission rate of Qion ~1055 s−1 to power the whole filament. The eight x-ray AGNs in the structure have Lx ~1044 erg s−1, corresponding to a total rate of Qion ~1057 s−1, whereas the 16 SMGs that are protocluster members form stars at a rate of 160 to 1700 Myear−1 and hence produce a total of Qion ~1057 s−1. This is sufficient ionizing photon flux to power the filament emission, even under the assumption that only 1% of the photons escape their host galaxies. This simple estimate, although an approximation of the more complex radiative transfer in this region, supports our interpretation that the gas residing in these filamentary structures is ionized by the photons produced by star-forming galaxies and AGNs in the massive protocluster core.

The volume densities of SMGs and x-ray AGNs in this field are about three orders of magnitude higher than the volume average at this epoch (21). Such an overdensity of active populations is very rare (29), and there is little observational evidence regarding how this intense activity is fueled and sustained. Cosmological simulations suggest that rapid infall of gas from the cosmic web in protoclusters may lead to the formation of SMGs (30). Although gas inflows are not directly observable in our data, the location of SMGs and AGNs within the filaments supports the idea that large reservoirs of gas are funneled toward forming galaxies under the effect of gravity, triggering and sustaining their star formation and driving the growth and activity of their central SMBHs. Assuming a typical density of 6 × 10–3 cm−3 for filaments with (projected) thicknesses of ~100 kiloparsec, the region imaged by our observations contains ~1012 M of gas (depending on the filling factor of the gas), which is potentially available to accrete onto galaxies in this region and so fuel their continuing star formation (22).

Our observations have uncovered a large-scale filamentary structure in the emission from the core of the SSA22 protocluster. Evidence of similar structures in other protoclusters from imaging observations (15, 25) suggests that this may be a general feature of protoclusters in the early Universe. The network of filaments in SSA22 is found to connect individual galaxies across a large volume, allowing it to power star formation and black-hole growth in active galaxy populations at z ~3.

Supplementary Materials

science.sciencemag.org/content/366/6461/97/suppl/DC1

Materials and Methods

Figs. S1 to S10

Tables S1 and S2

References (3176)

Data Files S1 and S2

References and Notes

  1. See supplementary materials.
Acknowledgments: We thank the reviewers for their constructive comments, which were very helpful in improving this paper. Our data are based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere. We thank all ESO staff who supported us in observation preparation and execution. We thank the JAO and EA-ARC staffs for preparation, observation, and initial data reduction. ALMA is a partnership of ESO (representing its member states), NSF (United States), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. Some of the data were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. We thank S. Yeh for assistance on the MOSFIRE observations. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very important cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have had the opportunity to conduct observations from this mountain. Funding: H.U., Y.M., B.H., Y.T., and K.K. are supported by JSPS KAKENHI (grant nos. 17K14252, 25287043/17H04831/17KK0098, 19K03925, 17H06130, and 17H06130, respectively). Y.T. acknowledges support from NAOJ (ALMA Scientific Research grant no. 2018-09B). M.F., I.S., and A.M.S. acknowledge support from the Science and Technology Facilities Council (grant no. ST/P000541/1). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant no. 757535). C.S. acknowledges an STFC studentship (grant no. ST/R504725/1). S.C. gratefully acknowledges support from the Swiss National Science Foundation (grant no. PP00P2_163824). Author contributions: H.U. led the project and analyzed the data (MUSE, Subaru, ALMA, Keck). M.F., I.S., S.C., and A.M.S. worked on the MUSE data reduction. C.C.S. worked on the Keck data reduction. Y.M. worked on the Subaru data reduction. M.F. and C.S. performed radiative transfer calculations. R.J.I., A.E.S., J.V., T.Y., Y.T., M.Ku., K.N., M.Ka., B.H., and K.K. contributed to interpreting the results. All authors reviewed, discussed, and commented on the results and the manuscript, and met the journal’s authorship criteria. Competing interests: The authors declare no competing interests. Data and materials availability: The MUSE data are available in the ESO archive at http://archive.eso.org/cms.html under programs 099.A-0638 and 0101.A-0679; the ALMA data are archived at http://almascience.nrao.edu/aq/ under project codes 2013.1.00162.S, 2015.1.00212.S, and 2016.1.00543.S; and MOSFIRE observations are in the Keck Observatory Archive https://www2.keck.hawaii.edu/koa under semester 2017B, program ID S412. Input parameter files for our cloudy simulations are provided in data files S1 and S2.
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