adsabs/AstroCLIMB huggingface dataset:
Paper: The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources 
Authors: Ana Acebron, Claudio Grillo, Sherry H. Suyu, Giuseppe Angora, Pietro Bergamini, Gabriel B. Caminha, Sebastian Ertl, Amata Mercurio, Mario Nonino, Piero Rosati, Han Wang, Andrea Bolamperti, Massimo Meneghetti, Stefan Schuldt, Eros Vanzella
Figure caption: Reconstructed surface-brightness distribution of the QSO host galaxy at z = 2.1992 from the position-based GLEE lens model (see Sections 3.2 and 4), where the surface-brightness distribution is not considered as an observable in the lens model. The same panels, field of view, and orientation as in Figure 4 are shown.
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: Light curves of XTE J1829−098 obtained with the RXTE PCA (bottom), Swift BAT (middle), and MAXI (top). The BAT and MAXI light curves were rebinned to 25 and 10 days, respectively, while the PCA light curve was not rebinned from the original light curve. The dashed green lines indicate the times of predicted source outbursts using our updated outburst ephemeris (Section 3.4, Table 3). The three activity epochs (“I,” “II,” and “‘III”) are shown at the top of the plot. During Epochs I and III outbursts are detected, while no strong outbursts are apparent during Epoch II.
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: Light curves of XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI observations folded on the orbital period using only data from Epochs I and III. The BAT and MAXI light curves were folded into 95 bins for one cycle, but only phases near periastron passage (0.75–1.25) are plotted. The green lines mark the triangular profile from Equation (1) fitted to the unfolded light curves from those epochs. Parameters are given in Table 3.
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: Swift BAT light curve of GS 1843−02 (2S 1845−024) folded on its orbital period. The light curve was folded into 500 bins for one cycle, but only phases near periastron passage (0.75–1.25) are plotted. Phase zero corresponds to periastron passage. The green lines show the two triangular profiles used to characterize the outburst in this source that was fitted to the unfolded light curve.
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: Power spectra of light curves of XTE J1829−098 during Epoch I and III obtained with the RXTE PCA (bottom), Swift BAT (middle), and MAXI (top). The solid green line shows the orbital period, and the dashed green lines show the harmonics of this. The dotted–dashed red line marks twice the orbital period. The peak at ∼3.5 days in the power spectrum of the PCA light curve is due to the observing cadence.
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: Top: the PCA light curve of XTE J1829−098 for Epoch I. The red line shows the fit to the outbursts from the PCA alone (Table 2), and the dashed green line shows the results from simultaneously fitting all three light curves (Table 3). Bottom: the residuals from the simultaneous fit.
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: Light curves of XTE J1829−098 from RXTE PCA (bottom), Swift BAT (middle), and MAXI (top) observations folded on the orbital period. The BAT and MAXI light curves use 50 bins to cover one cycle, while the PCA light curve is not binned from the original light curve. Data are selected for the three Epochs marked in Figure 1.
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: Spin period vs. orbital period for high-mass X-ray binaries. The letters indicate the type of mass transfer believed to be taking place in each system. R = Roche-lobe overflow, W = wind accretion from a supergiant, and B = accretion from a Be star decretion disk. The parameters of XTE J1829−098 are marked with the dashed circled red X, those of GS 1843-02 with the solid red circle, A0538–66 with the red box, and AX J0049.4−7323 with the red diamond. For system parameters see, e.g., F. Fortin et al. (2023), M. Neumann et al. (2023), and V. Kim et al. (2023).
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: Power spectra of light curves of XTE J1829−098 during Epoch II obtained with the RXTE PCA (bottom), Swift BAT (middle), and MAXI (top). The solid green line shows the orbital period, and the dashed green lines show the harmonics of this. The strongest peak in the MAXI power spectrum corresponds to the precession period of the ISS.
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: Pulse period history of XTE J1829−098 taken from Table 4. The RXTE PCA measurement from MJD 53,216 is not plotted because of its large uncertainty. The vertical dashed lines indicate the divisions between the three Epochs.
Paper: Sharp Periodic Flares and Long-term Variability in the High-mass X-Ray Binary XTE J1829−098 from RXTE PCA, Swift BAT, and MAXI Observations
Authors: Robin H. D. Corbet, Ralf Ballhausen, Peter A. Becker, Joel B. Coley, Felix Fuerst, Keith C. Gendreau, Sebastien Guillot, Nazma Islam, Gaurava Kumar Jaisawal, Peter Jenke, Peter Kretschmar, Alexander Lange, Christian Malacaria, Mason Ng, Katja Pottschmidt, Pragati Pradhan, Paul S. Ray, Richard E. Rothschild, Philipp Thalhammer, Lee J. Townsend, Joern Wilms, Colleen A. Wilson-Hodge, Michael T. Wolff
Figure caption: PCA (bottom), BAT (middle), and MAXI (top) light curves of XTE J1829−098 folded on twice the assumed orbital period for Epochs I and III only.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: From left to right: the moment-0, moment-1, and moment-2 maps derived from the C III] emission of GN-z11. The black contours indicate 2σ, 4σ, 6σ, and 8σ for C III] intensity. The moment-1 and moment-2 maps are derived by fitting the profiles of C III] doublets, as shown in Figure 3. The color bar is plotted in an arbitrary unit for the moment-0 map, while it is plotted in units of kilometers per second for the moment-1 and moment-2 maps. There exists a velocity gradient from north to south—see the text for details.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption:  v rot/σ  v  of GN-z11 compared to those obtained by previous studies at different redshifts. Our results of GN-z11 are shown with the red star and square, which show v rot/σ  v  obtained with GalPak3D modeling and the observed kinematic ratio Δv obs/σ med, respectively. The blue circles are galaxies whose [C II] kinematics are measured with ALMA, taken from M. Neeleman et al. (2020) and E. Parlanti et al. (2023). The blue squares are recent JWST results using the NIRSpec MSA, taken from A. de Graaff et al. (2023), F. Rizzo et al. (2020), F. Fraternali et al. (2021), F. Rizzo et al. (2021), and T. Tsukui & S. Iguchi (2021), while the blue triangles and diamonds are taken from E. J. Nelson et al. (2023) and Z. Li et al. (2023a), respectively, who use the NIRCam WFSS.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: Spectra of C III] in the central 49 = 7 × 7 pixels of Figure 1. In each pixel with sufficient S/N, we overplot the best-fit profile (blue solid curve) composed of two Gaussian components (dashed curves). The red shades highlight the [C III] λ1907 component that is used to derive the line-of-sight velocity and velocity dispersion, with the red vertical line indicating the central velocity.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: Circular velocities of GN-z11 at R e (red star) and virial radius of the DM halo (red circle). The red diamond represents the offset He II clump identified by R. Maiolino et al. (2023), assuming its velocity shift originates from rotation around the center of GN-z11. The black lines are the simulation predictions of T. Kimm et al. (2015), normalized to match the DM mass and halo radius of GN-z11. The notations CO, MFB, and MFBmp are taken from T. Kimm et al. (2015), representing no mechanical/kinetic feedback, mechanical feedback, and the most efficient case (mechanical feedback with a porous interstellar medium), respectively.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: Integrated C III] spectra of S/N > 2 pixels on the northern (top), southern (middle), and entire (bottom) areas of GN-z11. In the same manner as Figure 3, we show the best-fit profile, but with the flux ratio [C III] λ1907/C III] λ1909 as a free parameter. The solid vertical lines indicate the centroids of [C III] λ1907 and C III] λ1909 obtained from the best-fit profile. The left and right boundaries of the shaded areas are obtained from the best-fit profiles with the flux ratio fixed to 0.588 (n e = 105 cm−3) and 1.48 (n e = 100 cm−3), respectively. The velocity offset between the northern and southern pixels cannot be explained by the variation of the flux ratio, unless n e changes by 3 orders of magnitude.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: Radial profile of surface brightness of C III] and the continuum compared to the shape of the PSF. The C III] profile is more extended than the continuum and PSF, enabling the analysis of kinematics.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: Rotation velocity and velocity dispersion as a function of stellar mass. The symbols are the same as those in Figure 8. The gray crosses are z ∼ 2 galaxies taken from N. M. Förster Schreiber et al. (2018). The gray line in the left panel indicates the Tully–Fisher relation calculated by E. M. DiTeodoro et al. (2021).
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: Moment maps compared with the best-fit rotation disk model. From left to right: observed data, GalPak3D model, and the residuals.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: The same as Figure 1, but for N IV]  λ1486.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: Corner plot for the posterior distribution of parameters of the rotating disk model.
Paper: Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
Authors: Yi Xu, Masami Ouchi, Hidenobu Yajima, Hajime Fukushima, Yuichi Harikane, Yuki Isobe, Kimihiko Nakajima, Minami Nakane, Yoshiaki Ono, Hiroya Umeda, Hiroto Yanagisawa, Yechi Zhang
Figure caption: The data points are the same as those in Figure 10. The solid lines are the rotation curves given by different mass components, while the red line shows the summed-up values. The DM mass is given by the stellar-to-halo mass relation. For the stellar mass profile, we consider both the point source and extended component identified by S. Tacchella et al. (2023). The gas mass is the subtraction of the stellar and DM mass from the dynamical mass at 2R e. The dashed gray line assumes the same DM mass, but a concentrated distribution with c = 10. The dashed red line including both the stellar mass and c = 10 DM can also explain the observational data.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: Left—The integrated path length for τ eff, [O III] measurements as a function of the transverse distance (r ⊥), adopting an influence radius of 25 h −1 cMpc. Each point is color-coded by the redshift of the [O III] emitter z [O III]. Except for those [O III] emitters at the boundary of the Lyα forest, for most [O III] emitters, the integrated length for τ eff, [O III] measurements is ∼50 h −1 cMpc. Right—The τ eff around the [O III] emitters (τ eff, [O III]) adopting an influence radius of 25 h −1 cMpc, as the function of the [O III] emitter redshift z [O III]. The integrated path length for each τ eff, [O III] measurement is color-coded. The best-fit τ eff redshift evolution from J. Yang et al. (2020b) and S. E. I. Bosman et al. (2022) is denoted by the orange and purple lines, respectively.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: Top—The IGM Lyα effective optical depth τ eff of 14 ASPIRE quasar sightlines used in this work and the τ eff of the stacked Lyα forest spectrum in a bin size of 50 h −1 cMpc. All the lower limits in the τ eff are shown by upward arrows. As a comparison, we show the best-fit τ eff redshift evolution from J. Yang et al. (2020b, orange) and S. E. I. Bosman et al. (2022, purple), derived from larger samples of 32 quasars and 67 quasars. Bottom—The fraction of 2σ lower limits in the τ eff measurements within a redshift bin of d z = 0.1. Beyond z ∼ 6.1, more than 75% of measurements are 2σ lower limits.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: Top—The stacked Lyα forest spectrum (black) of 14 ASPIRE quasar sightlines used in our analysis, adopting a redshift grid of d z = 0.001 from z = 5.435 to z = 6.568. The spectral uncertainty of the stacked spectrum is shown in gray. Bottom—The number of quasar lines of sight (LOSs) available in each pixel of the redshift grid. Nearly all quasars used in this work cover the z ∼ 5.70−6.27 Lyα forest (the green-shaded region). Some pixels are strongly influenced by sky OH emission lines, therefore, they have been removed in the analysis, resulting in troughs shown in the number of quasar LOSs.
Paper: A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O III] Emitters
Authors: Xiangyu Jin, Jinyi Yang, Xiaohui Fan, Feige Wang, Koki Kakiichi, Romain A. Meyer, George D. Becker, Siwei Zou, Eduardo Bañados, Jaclyn B. Champagne, Valentina D'Odorico, Minghao Yue, Sarah E. I. Bosman, Zheng Cai, Anna-Christina Eilers, Joseph F. Hennawi, Hyunsung D. Jun, Mingyu Li, Zihao Li, Weizhe Liu, 伟哲 刘, Maria Pudoka, Sindhu Satyavolu, Fengwu Sun, Wei Leong Tee, Yunjing Wu
Figure caption: Top—The transmitted spectrum of an ASPIRE quasar J0226+0302. The redshift range of the Lyα used in the analysis is displayed in the red-shaded region. The location of the Lyβ emission line is marked by the blue downward arrow. The spatial locations of the [O III] emitters identified in each quasar field are denoted by the yellow-green-filled circles in terms of the [O III] emitter redshift z [O III] and the transverse distance r ⊥ between the [O III] emitter and the central quasar. Bottom—An illustrative figure for measuring the IGM transmission around the [O III] emitters within the Lyα forest of J0226+0302. For each [O III] emitter identified in the quasar field, we put a sphere of a certain radius (“influence radius”) centered at the [O III] emitter. For better visualization, we only show the spheres of three [O III] emitters and the size of the sphere is only for illustrative purposes, not to scale. For an [O III] emitter of which the sphere intersects the Lyα forest, we assume that the [O III] emitter is able to “influence” the Lyα forest.