adsabs/AstroCLIMB huggingface dataset:
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Slices of the 3D radiation–hydrodynamical simulation with i = 30° (R30) at t = 500P0 (P0 ≈ 253 yr, so t ≈ 0.13 Myr), shown in the transformed coordinate system ﹩(r,{\theta }^{{\prime} },{\phi }^{{\prime} })﹩, aligned with the local angular momentum vector at each radius (Figure 2). Left to right: density, temperature, radial velocity, meridional velocity, and the deviation of the azimuthal velocity from Keplerian. All velocity components are projected into the transformed frame. Top to bottom: values at the new midplane (﹩{\theta }^{{\prime} }=\pi /2﹩), at ﹩{z}^{{\prime} }/r=0.2﹩ above the midplane, at the surface of maximum density, and vertical slices in the ﹩{y}^{{\prime} }-{z}^{{\prime} }﹩ and ﹩{x}^{{\prime} }-{z}^{{\prime} }﹩ planes. The disk rotates counterclockwise. The arrows qualitatively indicate the azimuthal locations of velocity maxima, indicating the dominant modes that are present. Some of the grid-like patterns arise from the nearest-neighbor interpolation used in the coordinate transformation. To facilitate comparison with observations, line-of-sight velocities are presented in Figures 15 and 16.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Time evolution of the 3D radiation–hydrodynamical simulation with i = 30° (R30). Top: tilt. Middle: twist angles. Bottom: warp amplitude. Colors from blue to yellow denote increasing time. The first 100P0 (P0 ≈ 253 yr) are omitted to highlight the subsequent evolution. Otherwise, the twist plot would be dominated by oscillatory curves during the first 100P0. The horizontal dashed lines are the shadow’s tilt (30°) and twist angle (90°).
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Time evolution of the tilt (top), twist (middle), and warp (bottom) for three hydrodynamical models, similar to Figure 2. From left to right: 30° shadow (HF30R), 7﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 shadow (HF7R) with an A0 = 20% amplitude, and m = 1, n = 1 shadow models with an A0,11 = 5.4% amplitude (HFm1n1R0p054). The temperature perturbation forms are shown in the insets in the ϕ–z plane.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Mode contributions for selected (m, n) modes shown in Figure 8. Odd-m modes are plotted with solid lines, even-m modes with dashed lines, and the ground mode with a dotted line. The warp mode (m = 1, n = 1) is highlighted in orange. Vertical lines mark inclinations of i = 7﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and 30°, where simulations with prescribed temperature are performed. ηmn = A0,mn/A0.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Warp evolution in a pure hydrodynamical simulation with a prescribed temperature distribution induced by a 30° shadow (H30 with modified outflow boundary conditions). Top panel: surface evolution, analogous to Figure 1. Bottom three panels: evolution of tilt, twist, and warp, analogous to Figure 2.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Contribution of Fourier–Hermite modes in a shadowed disk model transitioning from coplanar to polar configurations in 15° increments. Modes are shown up to n = 3 and m = 15. The warp mode (m = 1, n = 1) is highlighted with red dots. Insets show the corresponding temperature distributions in the ϕ–z plane. ηmn = A0,mn/A0.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Time evolution of the 3D radiation–hydrodynamical simulations for i = 30° (R30, left) and i = 90° (R90, right). Top: surface density. Middle: vertically integrated Reynolds stress normalized by pressure. Bottom: mass accretion rate. Colors from blue to yellow denote increasing time, with t = 5, 105, and 505P0 highlighted by thicker lines (P0 ≈ 253 yr). Solid lines indicate positive values, while dashed lines indicate negative values.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Examples of the decomposition of the temperature perturbations into azimuthal Fourier modes (m) and vertical Hermite modes (n) on a cylindrical surface in the ϕ–z plane.
Paper: HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen
Authors: Nathalie K. Jones, Jason J. Wang, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, William Roberson, Jean-Baptiste Ruffio, Jerry W. Xuan, Bruce A. Macintosh, S. Mark Ammons, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Eugene Chiang, Jeffrey K. Chilcote, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Michael C. Liu, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Jenny Patience, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Aniket Sanghi, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: Reduced flux maps of HD 143811 AB obtained by Gemini/GPI in 2016 and 2019 (left and center) and Keck/NIRC2 in 2022 (right). These images are 2” × 2”. North is up, and east is left. The star is at the center of the image behind the coronagraph. Arrows indicates the location of the planet. Intensity scales are linear and vary for each image in order to highlight the object.
Paper: HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen
Authors: Nathalie K. Jones, Jason J. Wang, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, William Roberson, Jean-Baptiste Ruffio, Jerry W. Xuan, Bruce A. Macintosh, S. Mark Ammons, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Eugene Chiang, Jeffrey K. Chilcote, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Michael C. Liu, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Jenny Patience, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Aniket Sanghi, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: (Left) Astrometric measurements for HD 143811 AB b as a function of observational epoch. Points in blue are from GPI, and red denotes Keck NIRC2. The gray lines show the path of a stationary background object, while the blue regions show the paths of possible orbits for a planetary-mass bound companion. With these three epochs, HD 143811 AB b is confirmed to be a bound substellar companion at high confidence. (Top right) Orbit fits to the full relative astrometry data set, with each orbit representing a random draw from the posterior and color-coded by the epoch. (Bottom right) The same orbit tracks but zoomed in to the available data. Orbit fits are consistent with an e ≲ 0.5 orbit with moderate inclination and an orbital period of ∼300 yr.
Paper: HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen
Authors: Nathalie K. Jones, Jason J. Wang, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, William Roberson, Jean-Baptiste Ruffio, Jerry W. Xuan, Bruce A. Macintosh, S. Mark Ammons, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Eugene Chiang, Jeffrey K. Chilcote, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Michael C. Liu, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Jenny Patience, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Aniket Sanghi, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: Resulting ﹩{\chi }_{\nu }^{2}﹩ as a function of Teff from spectral comparison of HD 143811 AB b with comparison library. Fit values using the PHOENIX stellar models are shown in red, while the Exo-REM comparisons are shown in blue. Note the different y-axes. Both fits prefer the Exo-REM models over PHOENIX, though the addition from Keck focuses the fit to ∼1100 K.
Paper: HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen
Authors: Nathalie K. Jones, Jason J. Wang, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, William Roberson, Jean-Baptiste Ruffio, Jerry W. Xuan, Bruce A. Macintosh, S. Mark Ammons, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Eugene Chiang, Jeffrey K. Chilcote, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Michael C. Liu, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Jenny Patience, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Aniket Sanghi, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: Spectrum of HD 143811 AB b from GPI data (blue, H band) and Keck (red, L′ band). We also plot the best-fit Exo-REM model (solid gray; χ2 = 3.31) as well as a second Exo-REM model with a Teff 150 K higher (dashed gray; χ2 = 5.27).
Paper: HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen
Authors: Nathalie K. Jones, Jason J. Wang, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, William Roberson, Jean-Baptiste Ruffio, Jerry W. Xuan, Bruce A. Macintosh, S. Mark Ammons, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Eugene Chiang, Jeffrey K. Chilcote, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Michael C. Liu, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Jenny Patience, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Aniket Sanghi, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: Color–magnitude diagram showing HD 143811 AB b (red square) with directly imaged companions, field objects (colored circles), and young/low-gravity objects (squares), which is accessed using species (T. Stolker et al. 2020). The color of the field objects varies according to spectral type (color bar is above the plot).
Paper: HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen
Authors: Nathalie K. Jones, Jason J. Wang, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, William Roberson, Jean-Baptiste Ruffio, Jerry W. Xuan, Bruce A. Macintosh, S. Mark Ammons, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Eugene Chiang, Jeffrey K. Chilcote, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Michael C. Liu, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Jenny Patience, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Aniket Sanghi, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: Orbital motion from the OFTI fit to the relative astrometry of HD 143811 AB b. Over the next decade, separation is expected to decrease slightly, while the position angle increases (counterclockwise motion).
Paper: High-resolution Imaging of the Magnetic Reconfiguration of the Corona from inside the Corona by WISPR on Parker Solar Probe
Authors: Angelos Vourlidas, Evangelos Paouris, Mark G. Linton, Guillermo Stenborg, Paulett C. Liewer, Pete Riley, Phillip Hess, Russell A. Howard, Nour E. Raouafi
Figure caption: Top: zoomed-in HELIOS snapshot showing the candidate source regions of the HCS folds (left). For viewing purposes, the red arrows roughly outline the “edge” of the HCS in the extrapolations (blue line) and the edges in the visible light emission in a WISPR-I image (right). Bottom left: HELIOS snapshot showing the intersection between the computed HCS and the WISPR-I FOV from over the west limb. Bottom right: triangulation analysis of several coronal rays. The same WISPR-I image, as above, with superimposed locations of the tracked rays. The numbers refer to the angular distance of the ray from WISPR. Rays from a wide angular distance range 52°–144° are visible in WISPR at any given time. Their orientation matches the HCS location.
Paper: High-resolution Imaging of the Magnetic Reconfiguration of the Corona from inside the Corona by WISPR on Parker Solar Probe
Authors: Angelos Vourlidas, Evangelos Paouris, Mark G. Linton, Guillermo Stenborg, Paulett C. Liewer, Pete Riley, Phillip Hess, Russell A. Howard, Nour E. Raouafi
Figure caption: EUV 193/195 Å image of the solar corona overlaid with the heliospheric current sheet (HCS) from a PFSS model. PSP’s position at 12:00 UT on 23rd (yellow), 24th (green), and 25th (blue) shows its rapid traversal of Carrington longitudes near perihelion. WISPR’s approximate field of view is indicated by arcs representing the Thomson sphere (thick dashed) and plateau (thin dashed). The locations of features discussed in the text are also marked by the orange arrows and box.
Paper: High-resolution Imaging of the Magnetic Reconfiguration of the Corona from inside the Corona by WISPR on Parker Solar Probe
Authors: Angelos Vourlidas, Evangelos Paouris, Mark G. Linton, Guillermo Stenborg, Paulett C. Liewer, Pete Riley, Phillip Hess, Russell A. Howard, Nour E. Raouafi
Figure caption: WISPR-I sequence of the HCS reconfiguration taken from the LW movie (Figure 1). The time of each image is also shown. (a) Full WISPR-I frame marking a thinning outward-stretching feature (arrows) and the cropped region (dashed line box) shown in panels (b)–(j). (b)–(d) The feature, likely associated with compressed plasma around the HCS, expands radially, forming an S-shaped structure in its middle and eventually splitting in two. (e)–(g) The sunward portion develops into a train of collapsing loops, which turns into a series of “tadpoles.” (h)–(j) Three tadpoles form and descend toward the Sun.
Paper: High-resolution Imaging of the Magnetic Reconfiguration of the Corona from inside the Corona by WISPR on Parker Solar Probe
Authors: Angelos Vourlidas, Evangelos Paouris, Mark G. Linton, Guillermo Stenborg, Paulett C. Liewer, Pete Riley, Phillip Hess, Russell A. Howard, Nour E. Raouafi
Figure caption: Snapshots of the in/out formation event taken from the LW movie (Figure 1). Left: full-size WISPR-I LW frame at 19:20 UT showing the in/out location, the three components (“in,” “out,” and “L”), and the zoomed-in region (dashed line box) shown in the top-right panel. The other two panels show the evolution of the pair in time. They have been scaled down along the horizontal axis for easier display. The three rightmost panels trace the “out” component further out to demonstrate its evolution toward a circular morphology. The sequence can be appreciated better in the accompanying LW movie (Figure 1).
Paper: A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b
Authors: Johanna K. Teske, Nicole L. Wallack, Anjali A. A. Piette, Lisa Dang, Tim Lichtenberg, Mykhaylo Plotnykov, Raymond Pierrehumbert, Emma Postolec, Samuel Boucher, Alex McGinty, Bo Peng, Diana Valencia, Mark Hammond
Figure caption: The same as Figure 2 but now including the Eureka! reduction+fitting, showing the estimated increase due to correlated noise, as described in Appendix B (red diamonds and error bars).
Paper: Quasar Radiative Feedback May Suppress Galaxy Growth on Intergalactic Scales at z = 6.3
Authors: Yongda Zhu, Eiichi Egami, Xiaohui Fan, Fengwu Sun, George D. Becker, Christopher Cain, Huanqing Chen, Anna-Christina Eilers, Yoshinobu Fudamoto, Jakob M. Helton, Xiangyu Jin, Maria Pudoka, Andrew J. Bunker, Zheng Cai, Jaclyn B. Champagne, Zhiyuan Ji, Xiaojing Lin, Weizhe Liu, 刘伟哲, Hai-Xia Ma, Zheng Ma, Roberto Maiolino, George H. Rieke, Marcia J. Rieke, Pierluigi Rinaldi, Yang Sun, Wei Leong Tee, Feige Wang, Jinyi Yang, Minghao Yue, Junyu Zhang
Figure caption: Left: field-averaged detection completeness for galaxies with L5008 > 1042 erg s−1 as a function of projected transverse distance Δr (cMpc) from J0100+2802, for the SAPPHIRES (blue squares) and EIGER (gray circles) mosaics. The horizontal dashed lines mark 50% and 60% completeness. The vertical dotted line at Δr = 7 cMpc indicates where both fields reach ≳50% completeness (from injection-recovery tests). Right: [O III]-to-UV luminosity ratio (﹩{\mathrm{log}}_{10}({L}_{5008}/{L}_{1500})﹩) versus Δr for galaxies that pass the Δr-dependent completeness cut (>50%; red points). The solid black line is the best-fit linear trend derived from the unbinned data points, and the shaded band shows the 16th to 84th percentile bootstrap interval from mock downsampling to uniform 60% completeness. Binned averages (five galaxies per bin) are shown as red squares with error bars, which represent 1σ uncertainties in the mean within each bin. The dotted–dashed purple curve shows the expected quasar photoionization rate, and the right-hand axis gives ﹩{\mathrm{log}}_{10}({{\rm{\Gamma }}}_{{\rm{QSO}}}/{{\rm{\Gamma }}}_{{\rm{bg}}})﹩.
Paper: Quasar Radiative Feedback May Suppress Galaxy Growth on Intergalactic Scales at z = 6.3
Authors: Yongda Zhu, Eiichi Egami, Xiaohui Fan, Fengwu Sun, George D. Becker, Christopher Cain, Huanqing Chen, Anna-Christina Eilers, Yoshinobu Fudamoto, Jakob M. Helton, Xiangyu Jin, Maria Pudoka, Andrew J. Bunker, Zheng Cai, Jaclyn B. Champagne, Zhiyuan Ji, Xiaojing Lin, Weizhe Liu, 刘伟哲, Hai-Xia Ma, Zheng Ma, Roberto Maiolino, George H. Rieke, Marcia J. Rieke, Pierluigi Rinaldi, Yang Sun, Wei Leong Tee, Feige Wang, Jinyi Yang, Minghao Yue, Junyu Zhang
Figure caption: Left: [O III]-to-UV luminosity ratio (﹩{\mathrm{log}}_{10}({L}_{5008}/{L}_{1500})﹩) versus local overdensity, estimated with a k = 5 nearest-neighbor metric in three dimensions over the full sample of 130 emitters (5.3 < z < 6.9) and normalized to the field average. The combined control sample (foreground z ≈ 6.2 plus background z ≈ 6.8; blue hexagons) shows a weak positive trend (ρ = 0.18, p = 0.255), while the z ≈ 6.3 near-QSO sample (red circles) shows a negative trend (ρ = −0.63, p = 0.002). The full sample shows no significant correlation (ρ = −0.05, p = 0.600). These patterns indicate that the quasar-distance dependence is unlikely to be driven by local overdensity alone. Right: rest-frame UV luminosity (﹩{\mathrm{log}}_{10}{L}_{1500}﹩) as a function of transverse distance Δr from J0100+2802. Both the near-zQSO and control samples show no significant trend with distance, with a typical scatter of about 0.2 dex. The y-axis span (in dex) matches Figure 2 (right) for visual comparison.
Paper: Quasar Radiative Feedback May Suppress Galaxy Growth on Intergalactic Scales at z = 6.3
Authors: Yongda Zhu, Eiichi Egami, Xiaohui Fan, Fengwu Sun, George D. Becker, Christopher Cain, Huanqing Chen, Anna-Christina Eilers, Yoshinobu Fudamoto, Jakob M. Helton, Xiangyu Jin, Maria Pudoka, Andrew J. Bunker, Zheng Cai, Jaclyn B. Champagne, Zhiyuan Ji, Xiaojing Lin, Weizhe Liu, 刘伟哲, Hai-Xia Ma, Zheng Ma, Roberto Maiolino, George H. Rieke, Marcia J. Rieke, Pierluigi Rinaldi, Yang Sun, Wei Leong Tee, Feige Wang, Jinyi Yang, Minghao Yue, Junyu Zhang
Figure caption: Left: predicted quasar photoionization rate ΓQSO relative to the metagalactic UV background Γbg as a function of comoving distance r for four luminous quasars in the EIGER fields at z ≈ 6.3. J0100+2802 (solid purple) exhibits the strongest radiative impact. The horizontal dashed and dotted lines indicate ΓQSO/Γbg = 1 and 103. Right: [O III]-to-UV luminosity ratio ﹩{\mathrm{log}}_{10}({L}_{5008}/{L}_{1500})﹩ versus ﹩{\mathrm{log}}_{10}{{\rm{\Gamma }}}_{{\rm{QSO}}}(r)﹩ for galaxies near J0100+2802 (red circles) and J1148+5251 (blue pentagons). Distances for J1148 sources are rescaled to match the J0100 photoionization profile; the top axis shows the corresponding scaled transverse separation ﹩{\rm{\Delta }}{r}^{{\prime} }﹩ (cMpc). The black curve and shaded band show the best-fit relation and 68% interval from the J0100 field in Figure 2 (right), replotted as a function of ΓQSO(r). The J1148 data show a qualitatively similar but weaker trend, with larger scatter likely due to a smaller sample size and lower quasar luminosity. Despite this, the J1148 binned trend (cyan hexagons) is broadly consistent with the J0100 binned points (orange squares). The other EIGER quasars (J1030+0524, J159−02) lack sufficient [O III] emitters at small radii to assess this effect.
Paper: Quasar Radiative Feedback May Suppress Galaxy Growth on Intergalactic Scales at z = 6.3
Authors: Yongda Zhu, Eiichi Egami, Xiaohui Fan, Fengwu Sun, George D. Becker, Christopher Cain, Huanqing Chen, Anna-Christina Eilers, Yoshinobu Fudamoto, Jakob M. Helton, Xiangyu Jin, Maria Pudoka, Andrew J. Bunker, Zheng Cai, Jaclyn B. Champagne, Zhiyuan Ji, Xiaojing Lin, Weizhe Liu, 刘伟哲, Hai-Xia Ma, Zheng Ma, Roberto Maiolino, George H. Rieke, Marcia J. Rieke, Pierluigi Rinaldi, Yang Sun, Wei Leong Tee, Feige Wang, Jinyi Yang, Minghao Yue, Junyu Zhang
Figure caption: Robustness tests of the suppression of L5008 around J0100+2802. (a) ﹩{\mathrm{log}}_{10}({L}_{5008}/{L}_{1500})﹩ as a function of projected transverse distance Δr (cMpc). Red circles are galaxies near the quasar redshift; blue squares include all galaxies within Δz < 0.5 of the quasar. The horizontal dashed line marks the median of the full sample. (b) Cumulative distributions of ﹩{\mathrm{log}}_{10}({L}_{5008}/{L}_{1500})﹩ for galaxies within Δr < 7 cMpc (red: near zQSO; blue: all galaxies). A two-sample K–S test gives p = 0.006. (c) [O III] luminosity versus Δr for the near-zQSO sample. The black line and gray band show the best-fit linear relation with 16%–84% bootstrap intervals. Purple boxes show the forward-modeled expectation from the J. Matthee et al. (2023) luminosity function convolved with survey completeness, plotted as per-bin medians with 16%–84% ranges (independent across bins). (d) Distribution of p-values from linear fits to 1000 mock realizations (purple CDF). The vertical dashed line marks the observed correlation (p = 0.0205), which lies in the ∼2% tail of the null distribution, indicating that completeness variations alone are unlikely to reproduce the observed trend.