adsabs/AstroCLIMB huggingface dataset:
Paper: Earths Are Not Super-Earths, Saturns Are Not Jupiters: Imprints of Pressure-bump Planet Formation on Planetary Architectures
Authors: Wenrui Xu, 文睿 许, Songhu Wang
Figure caption: Left panel: mass ratio of adjacent planet pairs from the CKSM sample (black dots). The distribution around a given ﹩{({q}_{1}{q}_{2})}^{1/2}﹩ is estimated using a moving window (Appendix B); the line and shaded areas show the median and percentiles corresponding to ±1σ and ±2σ. Middle panel: same as the left panel, but now we fit the distribution of mass ratio to a lognormal distribution. Right panel: updating the width of the lognormal distribution to correct for the increased variance introduced by the uncertainty in planet radii. This is the distribution shown in the bottom panel of Figure 3.
Paper: H I, FRB, What’s Your z: The First FRB Host Galaxy Redshift from Radio Observations
Authors: M. Glowacki, A. Bera, K. Lee-Waddell, A. T. Deller, T. Dial, K. Gourdji, S. Simha, M. Caleb, L. Marnoch, J. Xavier Prochaska, S. D. Ryder, R. M. Shannon, N. Tejos
Figure caption: Intensity, velocity, and dispersion (moments 0, 1, and 2) maps of the MeerKAT H I DDT observations. Top: intensity map radio contours for the two higher-spatial-resolution cubes overlaid on the DECam three-color image. For the lower spatial resolution of these two cubes (robust weighting of 1, radio beam of 19.″3 × 15.″2), contours are at column density multiples of 3 to the power of (1, 1.5, 2, 2.5, ...) of 2.4 × 1019 cm−2, where the lowest contour is at 3σ significance. Negative contours are given as dashed lines at the same levels. The 3σ contour (green) is given for the higher-resolution cube (robust weighting of 0.1, radio beam of 12.″0 × 8.″7), at 1.8 × 1020 cm−2. The FRB localization region is given by the cyan ellipse, enlarged by a factor of 5 for visibility, and is coincident with a peak in H I emission and a faint, apparently red, optical galaxy (noting extinction is a factor). Bottom panels: the highest-spatial-resolution spectral-line velocity and dispersion maps are displayed, produced and masked by SoFiA.
Paper: H I, FRB, What’s Your z: The First FRB Host Galaxy Redshift from Radio Observations
Authors: M. Glowacki, A. Bera, K. Lee-Waddell, A. T. Deller, T. Dial, K. Gourdji, S. Simha, M. Caleb, L. Marnoch, J. Xavier Prochaska, S. D. Ryder, R. M. Shannon, N. Tejos
Figure caption: Top: H I spectra for the FRB host galaxy (red), the neighboring galaxy (blue), and the total combined system including the H I bridge (black). The green shaded region indicates the optical spectroscopic redshift and error obtained in the follow-up optical spectroscopy. Bottom: DEIMOS spectrum of the host galaxy of FRB20230718A. The locations of the detected emission lines in the spectrum (black) are marked with blue dashed lines. The standard deviation per wavelength bin is shown by the dashed red line. The same emission lines (Hα, [N II], and [S II]) from the Milky Way at z = 0.0001 are also visible (thinner pink lines) but the names of the transitions are not marked to avoid clutter.
Paper: H I, FRB, What’s Your z: The First FRB Host Galaxy Redshift from Radio Observations
Authors: M. Glowacki, A. Bera, K. Lee-Waddell, A. T. Deller, T. Dial, K. Gourdji, S. Simha, M. Caleb, L. Marnoch, J. Xavier Prochaska, S. D. Ryder, R. M. Shannon, N. Tejos
Figure caption: Moment maps as in Figure 1, for the two lower-resolution cubes. Contours are at column density multiples of 3 to the power of (1, 1.5, 2, 2.5, ...) of 8.5 × 1018 cm−2 for the “low” (17.5 kλ, radio beam of 33.″2 × 18.″9) resolution cube here (white), where the lowest contour is at 3σ significance, and negative contours are given as dashed lines. The 3σ contour (green) is given for the intensity map for the lowest-resolution cube (radio beam of 38.″6 × 24.″9) at 8.6 × 1018 cm−2. The velocity and dispersion maps are produced from the lowest-resolution cube, again through SoFiA.
Paper: Changing-look Active Galactic Nuclei Behavior Induced by Disk-captured Tidal Disruption Events
Authors: Yihan Wang, Douglas N. C. Lin, Bing Zhang, Zhaohuan Zhu
Figure caption: Total mass budget for disk/captured TDE and total disrupted mass for relaxation TDE during the lifetime (assumed to be 108 yr) of the AGN for various SMBHs and NSCs. The dashed red line indicates the total mass of the NSC.
Paper: Changing-look Active Galactic Nuclei Behavior Induced by Disk-captured Tidal Disruption Events
Authors: Yihan Wang, Douglas N. C. Lin, Bing Zhang, Zhaohuan Zhu
Figure caption: Surface density Σ and specific scale height h of three different disk models adopted in this Letter.
Paper: Changing-look Active Galactic Nuclei Behavior Induced by Disk-captured Tidal Disruption Events
Authors: Yihan Wang, Douglas N. C. Lin, Bing Zhang, Zhaohuan Zhu
Figure caption: TDE rate from relaxations around dormant SMBHs as a function of time. The radial power-law index of the NSC γ NSC = 2.
Paper: Changing-look Active Galactic Nuclei Behavior Induced by Disk-captured Tidal Disruption Events
Authors: Yihan Wang, Douglas N. C. Lin, Bing Zhang, Zhaohuan Zhu
Figure caption: Schematics of captured tidal disruption events (TDEs) resulting from disk–star interactions (not to scale). For a given semimajor axis, the green region indicates orbits with an orbital inclination greater than the critical inclination I TDE. Stars in these orbits with a capture timescale (given by Equation (21)) shorter than the AGN disk lifetime will be captured by the disk within the tidal disruption radius. Conversely, stars with orbital inclinations smaller than I TDE will be captured by the disk without undergoing direct TDEs.
Paper: Changing-look Active Galactic Nuclei Behavior Induced by Disk-captured Tidal Disruption Events
Authors: Yihan Wang, Douglas N. C. Lin, Bing Zhang, Zhaohuan Zhu
Figure caption: Fraction of CL-AGN among all AGNs as a function of SMBH masses for different TDE mechanisms.
Paper: Changing-look Active Galactic Nuclei Behavior Induced by Disk-captured Tidal Disruption Events
Authors: Yihan Wang, Douglas N. C. Lin, Bing Zhang, Zhaohuan Zhu
Figure caption: TDE rates of different mechanisms (indicated by different line styles) and disk models (indicated by different colors) during the AGN phase for different SMBHs and NSC models.
Paper: Improved Upper Limits on Gravitational-wave Emission from NS 1987A in SNR 1987A
Authors: Benjamin J. Owen, Lee Lindblom, Luciano Soares Pinheiro, Binod Rajbhandari
Figure caption: The left panel displays observational 90% confidence upper limits on h 0 from NS 1987A in 1 Hz bands as a function of frequency. The (red) horizontal solid lines show the range of ﹩{h}_{0}^{\mathrm{age}}﹩ from mass-quadrupole GW emission, Equation (3), and the (green) horizontal dashed lines show the range for r-mode GW emission, Equation (4). (Note that the ﹩{h}_{0}^{\mathrm{age}}﹩ lower limits coincide.) The right panel shows corresponding upper limits on the dimensionless neutron star ellipticity ϵ and r-mode amplitude α.(The data used to create this figure are available.)
Paper: Turbulently Driven Detonation Initiation in Electron-degenerate Matter with Helium
Authors: Gabriel O. Casabona, Robert T. Fisher
Figure caption: A plot showing the effective turbulent burning speed in black in cm s−1, the mean temperature in red in K (both on left axis), and the global abundances of both 4He (dashed blue) and 12C (dashed green) (on right axis) in the HighDen model. The horizontal orange line marks the Chapman–Jouguet detonation velocity calculated from the final ash state. The vertical black line shows the onset of detonation in this model as determined by when v turb > D CJ. The vertical green line indicates the time at which the 12C abundance is maximal.
Paper: Turbulently Driven Detonation Initiation in Electron-degenerate Matter with Helium
Authors: Gabriel O. Casabona, Robert T. Fisher
Figure caption: Analytic curves showing the ratio of the specific nuclear energy rates to the specific turbulent heating rate for the numerical experiments undertaken here: (top) pure helium, (middle) 83.3% 4He with 16.7% 12C seed nuclei at a density of 105 g cm−3, and (bottom) the same composition at 106 g cm−3.
Paper: Surface Charging of Jupiter’s Moon Europa
Authors: Sachin A. Reddy, Tom A. Nordheim, Camilla D. K. Harris
Figure caption: (a) Secondary emission yields δ  E . (b) The impact on surface potentials at the anti-Jovian hemisphere during eclipse.
Paper: Surface Charging of Jupiter’s Moon Europa
Authors: Sachin A. Reddy, Tom A. Nordheim, Camilla D. K. Harris
Figure caption: Surface potentials as a function of location on Europa’s hemispheres, solar illumination conditions, and magnetospheric plasma properties.
Paper: Surface Charging of Jupiter’s Moon Europa
Authors: Sachin A. Reddy, Tom A. Nordheim, Camilla D. K. Harris
Figure caption: The effects of ionospheric density on surface potential on the trailing hemisphere during eclipse.
Paper: Surface Charging of Jupiter’s Moon Europa
Authors: Sachin A. Reddy, Tom A. Nordheim, Camilla D. K. Harris
Figure caption: Geometry of Europa’s interaction with Jupiter’s magnetosphere. Europa orbits Jupiter at 14 km s−1, while the magnetospheric plasma corotates with Jupiter at 90 km s−1, resulting in a wake forming at Europa’s leading (downstream) hemisphere. Europa also possesses an ionosphere that is expected to be nonuniform and denser at the trailing (upstream) hemisphere. We capture this variability by simulating four discrete surface locations: sub-Jovian 0°, leading 90°, anti-Jovian 180°, and trailing 270°, in both sunlight and eclipse.
Paper: Turbulently Driven Detonation Initiation in Electron-degenerate Matter with Helium
Authors: Gabriel O. Casabona, Robert T. Fisher
Figure caption: Slice plots of specific nuclear energy generation rate and abundance ratio of C from the PureHeHighDen run, through the x-axis in the z–y plane. Each is centered about the hot spot just before leading into a detonation.
Paper: Evidence for a Compact Stellar Merger Origin for GRB 230307A From Fermi-LAT and Multiwavelength Afterglow Observations
Authors: Cui-Yuan Dai, Chen-Lei Guo, Hai-Ming Zhang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: The parameter space diagram derived from the nondetection of GeV afterglow emission. The contour of the number density is calculated using Equation (4), assuming that the radiation efficiency is η  γ  = 0.2. The black solid line represents ν LAT = ν c. The area on the right of the black solid line satisfies ν LAT < ν c, indicating the allowed parameter space. Conversely, the region on the left of the black solid line is the excluded region. Panels (a) through (f) correspond to the following parameter value combinations: (a) z = 0.065, ξ  e  = 0.01; (b) z = 0.065, ξ  e  = 0.1; (c) z = 0.065, ξ  e  = 1; (d) z = 3.87, ξ  e  = 0.01; (e) z = 3.87, ξ  e  = 0.1; (f) z = 3.87, ξ  e  = 1.
Paper: Evidence for a Compact Stellar Merger Origin for GRB 230307A From Fermi-LAT and Multiwavelength Afterglow Observations
Authors: Cui-Yuan Dai, Chen-Lei Guo, Hai-Ming Zhang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Corner plot demonstrating the properties of the eight-dimensional posterior obtained from our MCMC sampling with the Gaussian jet model in the case of z = 0.065. The meaning of the parameters is explained in the text. Dashed lines and labels along the diagonal indicate the median value and symmetric 68% uncertainties (corresponding to the 16 and 84 quantiles) for each parameter’s marginalized distribution. The results of best-fit parameters in other cases can be found in Table 2.
Paper: Evidence for a Compact Stellar Merger Origin for GRB 230307A From Fermi-LAT and Multiwavelength Afterglow Observations
Authors: Cui-Yuan Dai, Chen-Lei Guo, Hai-Ming Zhang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: A comparison between GRB 230307A and GRBs in the Fermi-LAT Second Gamma-Ray Burst Catalog (Ajello et al. 2019) on the fluence in 100 MeV–100 GeV measured by Fermi-LAT vs. the fluence in 10 keV–1 MeV measured by GBM. The black and blue data points represent long and short GRBs, respectively. The red star indicates the upper-limit measurement of GRB 230307A. For comparison, we also show the measurement of GRB 211211A, denoted by the magenta star. The solid, dashed, and dotted gray lines indicate where the ratio of the two fluences is 1, 0.1, and 0.01, respectively.
Paper: Evidence for a Compact Stellar Merger Origin for GRB 230307A From Fermi-LAT and Multiwavelength Afterglow Observations
Authors: Cui-Yuan Dai, Chen-Lei Guo, Hai-Ming Zhang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: The best-fit model for the multiwavelength light curve of GRB 230307A using the Gaussian jet model in the cases of z = 0.065 (left panel) and z = 3.87 (right panel). The cyan vertical dashed lines mark the time when ﹩{\nu }_{{\rm{m}}}={\nu }_{{I}_{{\rm{c}}}}﹩, determined through the analytic method Sari et al. (1998).
Paper: Evidence for a Compact Stellar Merger Origin for GRB 230307A From Fermi-LAT and Multiwavelength Afterglow Observations
Authors: Cui-Yuan Dai, Chen-Lei Guo, Hai-Ming Zhang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Same as Figure 4, but for the case of z = 3.87.
Paper: Evidence for a Compact Stellar Merger Origin for GRB 230307A From Fermi-LAT and Multiwavelength Afterglow Observations
Authors: Cui-Yuan Dai, Chen-Lei Guo, Hai-Ming Zhang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: The distribution of galactocentric projected offsets for GRBs. The samples for short GRBs are extracted from (Fong et al. 2022; O’Connor et al. 2022), whereas the sample for long GRBs is obtained from (Blanchard et al. 2016).
Paper: Delayed and Fast-rising Radio Flares from an Optical and X-Ray-detected Tidal Disruption Event in the Center of a Dwarf Galaxy
Authors: Fabao Zhang, Xinwen Shu, Lei Yang, Luming Sun, Zhumao Zhang, Yibo Wang, Guobin Mou, Xue-Guang Zhang, Tianyao Zhou, Fangkun Peng
Figure caption: Optical light curves of  AT 2018cqh observed with ZTF and Gaia. Note that the quiescent host emission has been subtracted in all light curves. We performed joint fits to the ZTF r-band and Gaia G-band light curves with a TDE model using the MOSFiT code. The best model realizations are shown in gray curves, which are constructed from the posterior parameter distribution at the 68% confidence level.
Paper: A Massive Protocluster Anchored by a Luminous Quasar at z = 6.63
Authors: Feige Wang, Jinyi Yang, Joseph F. Hennawi, Xiaohui Fan, Minghao Yue, Eduardo Bañados, Shane Bechtel, Fuyan Bian, Sarah Bosman, Jaclyn B. Champagne, Frederick B. Davies, Roberto Decarli, Emanuele Paolo Farina, Chiara Mazzucchelli, Bram Venemans, Fabian Walter
Figure caption: (a) Large-scale overdensity of LAEs around quasar J0910–0414. The background image is HSC z-band image. The red dot denotes the position of the quasar. The blue dots represent LAE candidates identified from deep Subaru imaging, the green dots represent spectroscopically confirmed LAEs at z > 6.5, and the orange point represents a spectroscopically confirmed low-z galaxy. The overdensity of LAEs within the yellow box (14 × 30 arcmin2 or ∼35 × 74 cMpc2) is ﹩\delta ={4.3}_{-0.9}^{+1.1}﹩. The colored contours are overdensity isolines of LAEs, which were estimated using a quartic kernel and a grid size of 1′. The blue, light blue, pink, and red lines denote overdensity δ = 3, 4, 5, and 6, respectively. The black dashed and solid lines represent r = 50 cMpc (at z=6.63) and ﹩r=40^{\prime} ﹩ (∼99 cMpc at z = 6.63), respectively. The average LAE surface density was estimated using galaxies located between these two lines. (b) Small-scale overdensity of [C II]-emitting galaxies identified from ALMA observations. (c) The zoomed-in [C II]-flux integrated map of the quasar host galaxy and a satellite galaxy (C) with [C II] emission.
Paper: True Pair-instability Supernova Descendant: Implications for the First Stars’ Mass Distribution
Authors: Ioanna Koutsouridou, Stefania Salvadori, Ása Skúladóttir
Figure caption: Top: predicted fraction of mono-enriched PISN descendants in the inner halo as a function of [Fe/H], when varying the characteristic mass of the Pop III IMF, for x = 2.35 (left); and when varying x, for m ch = 70 M ⊙ (right; Equation (3)). A Gaussian error of 0.2 dex has been applied to model predictions to account for observational uncertainties. Data points show the observed fractions (Section 2.2), also listed on top. Bottom: predicted fraction of all [Fe/H] ≤ − 2 inner halo stars that have inherited at least 10%, 50%, 70%, 80%, or 90% of their metals from a 250 to 260 M ⊙ PISN, for different m ch (left) and slope x (right) of the Pop III IMF. The X mark denotes that at least one star, J1010+2358, out of 15,000 VMP stars in the LAMOST sample has been imprinted by a 250–260 M ⊙ PISN (Section 2.1). Histograms and shaded areas represent the mean and standard deviation of 200 runs of each model.
Paper: True Pair-instability Supernova Descendant: Implications for the First Stars’ Mass Distribution
Authors: Ioanna Koutsouridou, Stefania Salvadori, Ása Skúladóttir
Figure caption: Left: measured chemical abundances of J1010+2358 (black points with errorbars) compared to (i) a 260 M ⊙ PISN (red); (ii) 10% of metals by a 260 M ⊙ PISN and 90% by a primordial faint SN (yellow) or a primordial core-collapse SN (blue; yields by Heger & Woosley 2010); (iii) 30% of metals by a massive PISN and 70% by a Population II SN (gray; Limongi & Chieffi 2018); (iv) 85% of metals by a massive PISN and 15% by a Type Ia SN (cyan; model W70 by Iwamoto 1999). Right: minimum ﹩{\chi }_{\nu }^{2}﹩ of the fit to J1010+2358's chemical abundances with different fractions of PISN enrichment, ﹩{f}_{\mathrm{PISN}}﹩, from a mass ﹩{m}_{\mathrm{PISN}}﹩ progenitor, and the rest from Pop III SNe.
Paper: True Pair-instability Supernova Descendant: Implications for the First Stars’ Mass Distribution
Authors: Ioanna Koutsouridou, Stefania Salvadori, Ása Skúladóttir
Figure caption: Confidence levels at which we can exclude a Pop III IMF with characteristic mass m ch and slope x, based on (i) the nondetection of mono-enriched PISNe descendants in the SAGA catalog at [Fe/H] < − 2.5 (top-left; red contours), and (ii) the discovery of J1010+2358 among 15000 VMP LAMOST stars (bottom-right), assuming that J1010+2358 has inherited >70% (green contours) or >90% (blue contours) of its metals from a 250 to 260 M ⊙ PISN. Dashed lines show linear fits to the 75% confidence levels. The central, light-yellow area represents Pop III IMFs that remain possible.
Paper: Did a Kilonova Set Off in Our Galactic Backyard 3.5 Myr ago?
Authors: Leonardo Chiesa, Albino Perego, Federico Maria Guercilena
Figure caption: Radioactivity distances as a function of t wind for the BLh models with q = 1.0 (left) and q = 0.7 (right). The BNS merger is assumed to occur t = 3.5 Mya. The bands account for different polar angles, i.e., θ 1 ∈ [40°, 60°] for q = 1, θ 2 ∈ [20°, 40°] for q = 0.7. The horizontal lines mark R LB and R fade.
Paper: Did a Kilonova Set Off in Our Galactic Backyard 3.5 Myr ago?
Authors: Leonardo Chiesa, Albino Perego, Federico Maria Guercilena
Figure caption: Isotopic ratio between 60Fe and 244Pu as a function of time for the BLh, q = 1.0 model with t wind = 200 ms (blue), and for the BLh, q = 0.7 model with t wind = 100 ms (orange). The bands represent the variability in the polar angle considering the same intervals as in Figure 2. The horizontal and vertical bands show instead the measured ratio (Wallner et al. 2021) and a ±1 Myr uncertainty about the fiducial value t = 3.5 Mya, respectively.
Paper: Did a Kilonova Set Off in Our Galactic Backyard 3.5 Myr ago?
Authors: Leonardo Chiesa, Albino Perego, Federico Maria Guercilena
Figure caption: Isotopic ratio between 60Fe and 244Pu for all the models listed in Table 1 as a function of the polar angle θ. The bands represent the variability in the wind duration, t wind ∈ [50, 200] ms, with larger (smaller) ratios related to a longer (shorter) duration. The horizontal band corresponds to the measured ratio (Wallner et al. 2021).
Paper: Did a Kilonova Set Off in Our Galactic Backyard 3.5 Myr ago?
Authors: Leonardo Chiesa, Albino Perego, Federico Maria Guercilena
Figure caption:  60Fe and 244Pu masses ejected in BLh models with q = 1.0 (left) and q = 0.7 (right) as a function of the polar angle θ. The contribution from the dynamical and spiral-wave wind ejecta are shown separately. The band represents the variability in the wind duration, t wind ∈ [50, 200] ms, with larger (smaller) isotopic masses related to a longer (shorter) duration.
Paper: A Massive Protocluster Anchored by a Luminous Quasar at z = 6.63
Authors: Feige Wang, Jinyi Yang, Joseph F. Hennawi, Xiaohui Fan, Minghao Yue, Eduardo Bañados, Shane Bechtel, Fuyan Bian, Sarah Bosman, Jaclyn B. Champagne, Frederick B. Davies, Roberto Decarli, Emanuele Paolo Farina, Chiara Mazzucchelli, Bram Venemans, Fabian Walter
Figure caption: Left: surface density of LAE candidates as a function of narrow-band magnitude. The density of LAE in the central ∼14  ×  30 arcmin2 region (solid red points) is ﹩{4.3}_{-0.9}^{+1.1}﹩ times higher than that measured in the outskirts (r > 50 cMpc) of our HSC field and that measured in other LAE surveys (Ouchi et al. 2010; Shibuya et al. 2018; Ono et al. 2021). Right: cumulative overdensity profile of galaxies in quasar fields. The orange squares and red dots denote the overdensity profiles measured in J0910–0414 field for [C II] emitters and LAEs, respectively. The black open squares and open circles denote the overdensity profiles of [C II] emitters and LAEs measured from three quasar fields with [C II] companion galaxies. The black dotted line represents the expected overdensity profile of LAEs in quasar fields (Shen et al. 2007; Ouchi et al. 2018; García-Vergara et al. 2019). The magenta dashed line denotes the expected overdensity profile of CO emitters in quasar fields (García-Vergara et al. 2022). The blue dotted–dashed line shows the expected overdensity profile of LAEs in average protocluster fields (Hennawi et al. 2015).
Paper: A Massive Protocluster Anchored by a Luminous Quasar at z = 6.63
Authors: Feige Wang, Jinyi Yang, Joseph F. Hennawi, Xiaohui Fan, Minghao Yue, Eduardo Bañados, Shane Bechtel, Fuyan Bian, Sarah Bosman, Jaclyn B. Champagne, Frederick B. Davies, Roberto Decarli, Emanuele Paolo Farina, Chiara Mazzucchelli, Bram Venemans, Fabian Walter
Figure caption: Left: the [C II] spectra (after continuum subtraction in the uv plane) of [C II] emitters. Their redshifts are z = 6.6266 ± 0.0001, 6.6272 ± 0.0001, and 6.6379 ± 0.0001 for SMG-A, SMG-B, and SMG-C, respectively. Middle and right: the optical spectra of spectroscopically confirmed LAEs. The identifications of these LAEs are labeled as Arabic numerals in Figure 1. These galaxies have redshifts of z = 6.54–6.64. Detailed information of the galaxies are listed in Table 1. The spectra for LAE-05 and LAE-08 are from IMACS observations, and the remaining spectra are from DEIMOS observations.
Paper: A Massive Protocluster Anchored by a Luminous Quasar at z = 6.63
Authors: Feige Wang, Jinyi Yang, Joseph F. Hennawi, Xiaohui Fan, Minghao Yue, Eduardo Bañados, Shane Bechtel, Fuyan Bian, Sarah Bosman, Jaclyn B. Champagne, Frederick B. Davies, Roberto Decarli, Emanuele Paolo Farina, Chiara Mazzucchelli, Bram Venemans, Fabian Walter
Figure caption: A double-peaked LAE identified in the highly ionized quasar vicinity. The red asterisk indicates the position of the quasar while the black circle highlight the relative position of the LAE-11 to the quasar. The black line shows the spectrum of the LAE and the gray line denotes the error vector. LAE-11 shows a widely separated double-peaked Lyα line. The detection of the blue peak of the double-peaked Lyα line in this galaxy indicates that the strong quasar radiation has ionized its vicinity.