ABSTRACT The fraction of ‘dark pixels’ in the Ly$$\alpha$$ and other Lyman-series forests at $$z\sim 5$$–6 provides a powerful constraint on the end of the reionization process. Any spectral region showing transmission must be highly ionized, while dark regions could be ionized or neutral, thus the dark pixel fraction provides a (nearly) model independent upper limit to the volume-filling fraction of the neutral intergalactic medium, modulo choices in binning scale and dark pixel definition. Here, we provide updated measurements of the 3.3 comoving Mpc dark pixel fraction at $z=4.85$–6.25 in the Ly$$\alpha$$, Ly$$\beta$$, and Ly$$\gamma$$ forests of 34 deep $$5.8 \lesssim z\lesssim 6.6$$ quasar spectra from the (enlarged) XQR−30 sample. Using the negative pixel method to measure the dark pixel fraction, we derive fiducial $$1\sigma$$ upper limits on the volume-average neutral hydrogen fraction of $$\langle x_{\rm HI} \rangle \le \lbrace 0.030+0.048,0.095+0.037,0.191+0.056,0.199+0.087\rbrace$$ at $$\bar{z}=\lbrace 5.481,5.654,5.831,6.043\rbrace$$ from the optimally sensitive combination of the Ly$$\beta$$ and Ly$$\gamma$$ forests. We further demonstrate an alternative method that treats the forest flux as a mixture of dark and transparent regions, where the latter are modelled using a physically motivated parametric form for the intrinsic opacity distribution. The resulting model-dependent upper limits on $$\langle x_{\rm HI} \rangle$$ are similar to those derived from our fiducial model-independent analysis. We confirm that the bulk of reionization must be finished at $z>6$, while leaving room for an extended ‘soft landing’ to the reionization history down to $$z\sim 5.4$$ suggested by Ly$$\alpha$$ forest opacity fluctuations.
more »
« less
The hydrodynamic response of small-scale structure to reionization drives large IGM temperature fluctuations that persist to z = 4
ABSTRACT The thermal history and structure of the intergalactic medium (IGM) at $$z \ge 4$$ is an important boundary condition for reionization, and a key input for studies using the Ly $$\alpha$$ forest to constrain the masses of alternative dark matter candidates. Most such inferences rely on simulations that lack the spatial resolution to fully resolve the hydrodynamic response of IGM filaments and minihaloes to H i reionization heating. In this letter, we use high-resolution hydrodynamic + radiative transfer simulations to study how these affect the IGM thermal structure. We find that the adiabatic heating and cooling driven by the expansion of initially cold gas filaments and minihaloes sources significant small-scale temperature fluctuations. These likely persist in much of the IGM until $$z \le 4$$. Capturing this effect requires resolving the clumping scale of cold, pre-ionized gas, demanding spatial resolutions of $${\le} 2$$ $$h^{-1}$$kpc. Pre-heating of the IGM by X-rays can slightly reduce the effect. Our preliminary estimate of the effect on the Ly $$\alpha$$ forest finds that, at $$\log (k /[{\rm km^{-1} s}]) = -1.0$$, the Ly $$\alpha$$ forest flux power (at fixed mean flux) can increase $${\approx} 10~{{\ \rm per\ cent}}$$ going from 8 and 2 $$h^{-1}$$kpc resolution at $$z = 4{\!-\!}5$$ for gas ionized at $$z \ \lt\ 7$$. These findings motivate more careful analyses of how the effects studied here affect the Ly $$\alpha$$ forest.
more »
« less
- Award ID(s):
- 2045600
- PAR ID:
- 10616018
- Publisher / Repository:
- Monthly Notices of the Royal Astronomical Society
- Date Published:
- Journal Name:
- Monthly Notices of the Royal Astronomical Society: Letters
- Volume:
- 533
- Issue:
- 1
- ISSN:
- 1745-3925
- Page Range / eLocation ID:
- L100 to L106
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
More Like this
-
-
null (Ed.)ABSTRACT We study the projected spatial offset between the ultraviolet continuum and Ly α emission for 65 lensed and unlensed galaxies in the Epoch of Reionization (5 ≤ z ≤ 7), the first such study at these redshifts, in order to understand the potential for these offsets to confuse estimates of the Ly α properties of galaxies observed in slit spectroscopy. While we find that ∼40 per cent of galaxies in our sample show significant projected spatial offsets ($$|\Delta _{\rm {Ly}\alpha -\rm {UV}}|$$), we find a relatively modest average projected offset of $$|\widetilde{\Delta }_{\rm {Ly}\alpha -\rm {UV}}|$$ = 0.61 ± 0.08 proper kpc for the entire sample. A small fraction of our sample, ∼10 per cent, exhibit offsets in excess of 2 proper kpc, with offsets seen up to ∼4 proper kpc, sizes that are considerably larger than the effective radii of typical galaxies at these redshifts. An internal comparison and a comparison to studies at lower redshift yielded no significant evidence of evolution of $$|\Delta _{\rm {Ly}\alpha -\rm {UV}}|$$ with redshift. In our sample, ultraviolet (UV)-bright galaxies ($$\widetilde{L_{\mathrm{ UV}}}/L^{\ast }_{\mathrm{ UV}}=0.67$$) showed offsets a factor of three greater than their fainter counterparts ($$\widetilde{L_{\mathrm{ UV}}}/L^{\ast }_{\mathrm{ UV}}=0.10$$), 0.89 ± 0.18 versus 0.27 ± 0.05 proper kpc, respectively. The presence of companion galaxies and early stage merging activity appeared to be unlikely causes of these offsets. Rather, these offsets appear consistent with a scenario in which internal anisotropic processes resulting from stellar feedback, which is stronger in UV-brighter galaxies, facilitate Ly α fluorescence and/or backscattering from nearby or outflowing gas. The reduction in the Ly α flux due to offsets was quantified. It was found that the differential loss of Ly α photons for galaxies with average offsets is not, if corrected for, a limiting factor for all but the narrowest slit widths (<0.4 arcsec). However, for the largest offsets, if they are mostly perpendicular to the slit major axis, slit losses were found to be extremely severe in cases where slit widths of ≤1 arcsec were employed, such as those planned for James Webb Space Telescope/NIRSpec observations.more » « less
-
ABSTRACT Recent quasar absorption line observations suggest that reionization may end as late as $$z \approx 5.3$$. As a means to search for large neutral hydrogen islands at $$z\ \lt\ 6$$, we revisit long dark gaps in the Ly $$\beta$$ forest in Very Large Telescope/X-Shooter and Keck/Echellette Spectrograph and Imager quasar spectra. We stack the Ly $$\alpha$$ forest corresponding to both edges of these Ly $$\beta$$ dark gaps and identify a damping wing-like extended absorption profile. The average redshift of the stacked forest is $z=5.8$. By comparing these observations with reionization simulations, we infer that such a damping wing-like feature can be naturally explained if these gaps are at least partially created by neutral islands. Conversely, simulated dark gaps lacking neutral hydrogen struggle to replicate the observed damping wing features. Furthermore, this damping wing-like profile implies that the volume-averaged neutral hydrogen fraction must be $$\langle x_{\rm H\,{\small {I}}} \rangle \ge 6.1 \pm 3.9~{{\ \rm per\ cent}}$$ at $z = 5.8$. Our results offer robust evidence that reionization extends below $z=6$.more » « less
-
ABSTRACT Our understanding of reionization has advanced considerably over the past decade, with several results now demonstrating that the intergalactic medium transitioned from substantially neutral at z = 7 to largely reionized at z = 6. However, little remains known about the sizes of ionized bubbles at z ≳ 7 as well as the galaxy overdensities which drive their growth. Fortunately, rest-ultraviolet (UV) spectroscopic observations offer a pathway towards characterizing these ionized bubbles thanks to the resonant nature of Lyman-alpha photons. In a previous work, we presented Ly α detections from three closely separated Lyman-break galaxies at z ≃ 6.8, suggesting the presence of a large (R > 1 physical Mpc) ionized bubble in the 1.5 deg2 COSMOS field. Here, we present new deep Ly α spectra of 10 UV-bright ($$\mathrm{\mathit{ M}}_{\mathrm{UV}}^{} \le -20.4$$) z ≃ 6.6–6.9 galaxies in the surrounding area, enabling us to better characterize this potential ionized bubble. We confidently detect (S/N > 7) Ly α emission at z = 6.701–6.882 in nine of ten observed galaxies, revealing that the large-scale volume spanned by these sources (characteristic radius R = 3.2 physical Mpc) traces a strong galaxy overdensity (N/〈N〉 ≳ 3). Our data additionally confirm that the Ly α emission of UV-bright galaxies in this volume is significantly enhanced, with 40 per cent (4/10) showing strong Ly α emission (equivalent width >25 Å) compared to the 8–9 per cent found on average at z ∼ 7. The median Ly α equivalent width of our observed galaxies is also ≈2 times that typical at z ∼ 7, consistent with expectations if a very large (R ∼ 3 physical Mpc) ionized bubble is allowing the Ly α photons to cosmologically redshift far into the damping wing before encountering H i.more » « less
-
ABSTRACT We present the first statistical analysis of kinematically resolved, spatially extended $$\rm Ly\alpha$$ emission around z = 2–3 galaxies in the Keck Baryonic Structure Survey (KBSS) using the Keck Cosmic Web Imager (KCWI). Our sample of 59 star-forming galaxies (zmed = 2.29) comprises the subset with typical KCWI integration times of ∼5 h and with existing imaging data from the Hubble Space Telescope and/or adaptive optics-assisted integral field spectroscopy. The high-resolution images were used to evaluate the azimuthal dependence of the diffuse $$\rm Ly\alpha$$ emission with respect to the stellar continuum within projected galactocentric distances of ≲30 proper kpc. We introduce cylindrically projected 2D spectra (CP2D) that map the averaged $$\rm Ly\alpha$$ spectral profile over a specified range of azimuthal angle, as a function of impact parameter around galaxies. The averaged CP2D spectrum of all galaxies shows clear signatures of $$\rm Ly\alpha$$ resonant scattering by outflowing gas. We stacked the CP2D spectra of individual galaxies over ranges of azimuthal angle with respect to their major axes. The extended $$\rm Ly\alpha$$ emission along the galaxy principal axes is statistically indistinguishable, with residual asymmetry of ≤2 per cent (∼2σ) of the integrated $$\rm Ly\alpha$$ emission. The symmetry implies that the $$\rm Ly\alpha$$ scattering medium is dominated by outflows in all directions within 30 kpc. Meanwhile, we find that the blueshifted component of $$\rm Ly\alpha$$ emission is marginally stronger along galaxy minor axes for galaxies with relatively weak $$\rm Ly\alpha$$ emission. We speculate that this weak directional dependence of $$\rm Ly\alpha$$ emission becomes discernible only when the $$\rm Ly\alpha$$ escape fraction is low. These discoveries highlight the need for similar analyses in simulations with $$\rm Ly\alpha$$ radiative transfer modelling.more » « less
An official website of the United States government

