adsabs/AstroCLIMB huggingface dataset:
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Multiband optical monitoring of POX 52 on 2024 April 11. MuSCAT 4 light curves in the griz bands are shown. No significant intranight variability was detected.
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Left panel: the zoom-in light curve of POX 52 during the LCOGT monitoring. The dotted line indicates the time of intranight monitoring. Right panels: ICCF, JAVELIN, and PyROA results.
Paper: A Direct Measurement of the Electron Density Turbulence Parameter C1 and Implications for the Emission Size of Magnetar XTE J1810-197
Authors: Visweshwar Ram Marthi, Yogesh Maan
Figure caption: Left: the electron density model for gb = −0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩158, the Galactic latitude of J1810−197, out to a distance of 3.6 kpc from Earth. The red marker line is in the direction of the magnetar, with the distances marked in kiloparsecs. Right: the DM–τd of N. D. R. Bhat et al. (2004) is represented by the dashed line; the solid line and the shaded region represent the empirical fit and the error bar ﹩{\sigma }_{{\tau }_{d}}﹩ with α = 4.4 obtained from J. M. Cordes & T. J. W. Lazio (2003), all at 1 GHz. The points represent pulsars within 10∘ of XTE J1810−197 beyond 2.5 kpc; the Galactic center lies just outside the 10∘ circle.
Paper: A Direct Measurement of the Electron Density Turbulence Parameter C1 and Implications for the Emission Size of Magnetar XTE J1810-197
Authors: Visweshwar Ram Marthi, Yogesh Maan
Figure caption: Left: the subband-binned ACF stacked for 20 pulses vs. frequency lag. Right: the measured Δνd values at each subband, along with the error bars and the fits.
Paper: A Direct Measurement of the Electron Density Turbulence Parameter C1 and Implications for the Emission Size of Magnetar XTE J1810-197
Authors: Visweshwar Ram Marthi, Yogesh Maan
Figure caption: The scatter-broadened pulse component, the fit, and the residuals, along with the posterior distribution of the fit parameters.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Comparison of Σ5 for galaxies and LRDs for redshift bin 4.75 < z < 6.5 (top) and 6.5 < z < 8.25 (bottom). The black dashed line represents the 〈Σ5〉 of random points. Note that the LRD histograms are weighted to be normalized compared to the galaxy histograms and have a logarithmic y-axis. LRDs occupy a smaller range of lower densities than galaxies do and are not found in dense environments.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Halo mass from abundance matching (red) over the redshift range 3 < z < 11 with redshift bin size Δz = 1. The SHMR (blue) is calculated from stellar masses extracted by CIGALE for non-AGN models. The SHMR holds relatively constant throughout the bins. The red shaded area is included for visualization and is an estimated fit of our data. Using this estimate fit, we include approximate points (green) for the corresponding SHMR of our halo mass at each redshift available in P. S. Behroozi et al. (2013).
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: The 〈Σ5〉 of each run of a random galaxy sample for redshift bin 4.75 < z < 6.5 (top) and 6.5 < z < 8.25 (bottom). The 〈Σ5〉 for our LRD and galaxy samples are shown in red and blue, respectively, with the 〈Σ5〉 of random points shown with a dashed black line for comparison.
Paper: Chemical Abundances of Seven Stars in the GD-1 Stream
Authors: Jing-Kun Zhao, Guang-Wei Li, Wako Aoki, Gang Zhao, Guo-Chao Yang, Jian-Rong Shi, Hai-Ning Li, Tadafumi Matsuno, Miho Ishigaki, Takuma Suda, Satoshi Honda, Yu-Qin Chen, Qian-Fan Xing, Hong-Liang Yan, Yong Yang, Xian-Hao Ye
Figure caption: Comparison of stellar parameters between this work and reference values. Left: effective temperatures (Teff) derived in this work vs. values from the LAMOST pipeline (black points), MBM (G − GRP) calibrations (blue points), and MBM (G − Ks) calibrations (red points). Right: surface gravity (log g) comparison between our spectroscopic determinations and LAMOST pipeline values. Solid lines in both panels indicate the one-to-one relations.
Paper: Chemical Abundances of Seven Stars in the GD-1 Stream
Authors: Jing-Kun Zhao, Guang-Wei Li, Wako Aoki, Gang Zhao, Guo-Chao Yang, Jian-Rong Shi, Hai-Ning Li, Tadafumi Matsuno, Miho Ishigaki, Takuma Suda, Satoshi Honda, Yu-Qin Chen, Qian-Fan Xing, Hong-Liang Yan, Yong Yang, Xian-Hao Ye
Figure caption: Orbit and CMD of GD-1 stream. Black points are members from R. Ibata et al. (2021), while red points are our seven program stars.
Paper: Chandra Rules Out Super-Eddington Accretion Models for Little Red Dots
Authors: Andrea Sacchi, Ákos Bogdán
Figure caption: Comparison between the upper limits on the X-ray emission of LRDs derived in this work and mock spectra corresponding to different scenarios of X-ray weakness. Intrinsic X-ray weakness from super-Eddington accretion from F. Pacucci & R. Narayan (2024) and K. Inayoshi et al. (2024) are reported in blue and green, respectively. For F. Pacucci & R. Narayan (2024), the solid line indicates the mean expected flux, and the dashed lines encompass a region spanning the viewing angles range θ = 30°−80°. For K. Inayoshi et al. (2024), the solid line indicates an Eddington ratio λEdd = 1, and the dashed lines encompass a region that spans the range of Eddington ratios λEdd = 0.3−3. In orange is shown the model for super-Eddington accretion agnslim, assumed by E. Lambrides et al. (2024). In red is shown a standard Compton-thick spectrum (borus02, M. Baloković et al. 2019), the solid lines corresponding to column densities of NH = 1024.5−25 cm−2.
Paper: A JWST View of the Overmassive Black Hole in NGC 4486B
Authors: Behzad Tahmasebzadeh, Matthew A. Taylor, Monica Valluri, Haruka Yoshino, Eugene Vasiliev, Michael J. Drinkwater, Solveig Thompson, Kristen Dage, Patrick Côté, Laura Ferrarese, Tatsuya Akiba, Vivienne Baldassare, Misty C. Bentz, John P. Blakeslee, Holger Baumgardt, Youkyung Ko, Chengze Liu, Ann-Marie Madigan, Eric W. Peng, Joel Roediger, Kaixiang Wang, Tyrone E. Woods
Figure caption: Top row: the left and middle panels show the deconvolved ACS/WFC F850LP and WFPC2 F555W images of NGC 4486B, respectively, with overlaid isophotal contours. The red plus marks the center of the outer isophote. Two distinct nuclei are visible in the WFPC2 F555W image, originally published in T. R. Lauer et al. (1996). The right panel shows the Voronoi-binned S/N map per Å from the JWST/NIRSpec IFU data, revealing a central peak of S/N ≳ 120 that declines to S/N ≳ 48 toward the field edges. The center of the IFU map corresponds to the photometric center (brightest light peak), which we adopt as the dynamical center for our analysis. The HST images are aligned such that the brightest light peak is placed at the center (0, 0) of the coordinate system. All three panels cover the same spatial region. Bottom row: example pPXF spectral fits for the central bin (left) and the outermost Voronoi bin (right), as marked by cyan crosses on the S/N map. In each panel, the observed spectrum is shown in black, the best-fit model in red, and the residuals in green.
Paper: A JWST View of the Overmassive Black Hole in NGC 4486B
Authors: Behzad Tahmasebzadeh, Matthew A. Taylor, Monica Valluri, Haruka Yoshino, Eugene Vasiliev, Michael J. Drinkwater, Solveig Thompson, Kristen Dage, Patrick Côté, Laura Ferrarese, Tatsuya Akiba, Vivienne Baldassare, Misty C. Bentz, John P. Blakeslee, Holger Baumgardt, Youkyung Ko, Chengze Liu, Ann-Marie Madigan, Eric W. Peng, Joel Roediger, Kaixiang Wang, Tyrone E. Woods
Figure caption: Posterior distributions of the model parameters derived from fits to the original data (no masking/shifting). Left: results from the Schwarzschild orbit-superposition method, with parameters including the BH mass (MBH), stellar mass-to-light ratio (M/L), DM peak circular velocity (vhalo), and inclination angle (θ). Right: results of the JAM model, with parameters MBH, M/L, velocity anisotropy (β), and θ. The blue, orange, and green contours indicate the 68%, 95%, and 99.7% confidence levels, respectively. Titles above the one-dimensional histograms show the median values with their uncertainties.
Paper: A Direct Measurement of the Electron Density Turbulence Parameter C1 and Implications for the Emission Size of Magnetar XTE J1810-197
Authors: Visweshwar Ram Marthi, Yogesh Maan
Figure caption: The emission region size at the magnetar constrained by the scattering on a screen at a distance ds from the observer. The crosses mark the coordinates ﹩({d}_{s},{r}_{{\rm{res}}})﹩ for screens at 1 pc, 100 pc, and halfway from the magnetar.
Paper: A JWST View of the Overmassive Black Hole in NGC 4486B
Authors: Behzad Tahmasebzadeh, Matthew A. Taylor, Monica Valluri, Haruka Yoshino, Eugene Vasiliev, Michael J. Drinkwater, Solveig Thompson, Kristen Dage, Patrick Côté, Laura Ferrarese, Tatsuya Akiba, Vivienne Baldassare, Misty C. Bentz, John P. Blakeslee, Holger Baumgardt, Youkyung Ko, Chengze Liu, Ann-Marie Madigan, Eric W. Peng, Joel Roediger, Kaixiang Wang, Tyrone E. Woods
Figure caption: Kinematic profiles of vo and σo along the kinematic major axis. Red points show the JWST/NIRSpec IFU data with their associated uncertainties, while the red line indicates the best-fit axisymmetric model. The blue points represent the CFHT/SIS data and uncertainties from J. Kormendy et al. (1997), and the blue line indicates the best-fit model. Vertical dashed lines mark the expected BH sphere of influence (Rinfl) and the galaxy’s effective radius (Re), both are indicated relative to the center of our dynamical model, where the BH is assumed to reside at R = 0.
Paper: A JWST View of the Overmassive Black Hole in NGC 4486B
Authors: Behzad Tahmasebzadeh, Matthew A. Taylor, Monica Valluri, Haruka Yoshino, Eugene Vasiliev, Michael J. Drinkwater, Solveig Thompson, Kristen Dage, Patrick Côté, Laura Ferrarese, Tatsuya Akiba, Vivienne Baldassare, Misty C. Bentz, John P. Blakeslee, Holger Baumgardt, Youkyung Ko, Chengze Liu, Ann-Marie Madigan, Eric W. Peng, Joel Roediger, Kaixiang Wang, Tyrone E. Woods
Figure caption: Kinematic maps represented by the GH coefficients (v0, σ0, h3, and h4) are shown for NGC 4486B. The first row displays the JWST/NIRSpec IFU data, the second row shows the best-fitting Schwarzschild model based on the JWST data set. The third row presents the best-fitting model for the modified data where the σ peak is masked, and the fourth row shows the best-fitting model for data where the σ peak valuesare shifted to the center.
Paper: Chandra Rules Out Super-Eddington Accretion Models for Little Red Dots
Authors: Andrea Sacchi, Ákos Bogdán
Figure caption: Exposure-corrected Chandra image in the 0.3–7 keV X-ray band of the CDF-S, for which ≈7 Ms of total exposure time is available, making it the deepest Chandra data set available to date. The location of each of the 55 LRDs considered in this work is indicated by a white circle with fixed 8″ radius for illustration purposes.
Paper: 3D Fast-mode Wave Propagation from Corona to Chromosphere: Triggering Mechanism for 3D Oscillations of Filaments
Authors: Yunxue Huang, Qin Feng, Yuhu Miao, Zhining Qu, Ke Yu, Hongfei Liang, Yu Liu, Xinping Zhou
Figure caption: The horizontal oscillation of the filaments. Panels (a1)–(a3) show the filaments in AIA 171 Å, CHASE Hα, and SMART Hα images, where the color lines marked the path to get time–distance stack plots to study their oscillation in different directions. In panels (a1) and (a3), the paths start at the center of the circle, while in panel (a2), the paths separated by a 15° angle are located on the arc and are marked with solid dots. Panel (b1) shows the horizontal oscillation of filament F1 along slice 1 in panel (a1). Panel (b2) is an example of the filament oscillation in the direction of slice 3 in panel (a2), while panel (b3) is an example of filament F3’s oscillation in the direction of slice 1 of panel (a3). The gray curves in panels (b1) and (b2) are the oscillation curve that manually marked the positions used for fitting. The black curve is the detrended curve of the oscillation curve obtained by subtracting the smooth velocity using a 10 minute boxcar, where the red curve is its fitting result using the formula ﹩f(t)=A{e}^{(-t/\tau )}{\rm{\cos }}(2\pi /T+\phi )﹩. The fitting results are listed in the corresponding panel.
Paper: 3D Fast-mode Wave Propagation from Corona to Chromosphere: Triggering Mechanism for 3D Oscillations of Filaments
Authors: Yunxue Huang, Qin Feng, Yuhu Miao, Zhining Qu, Ke Yu, Hongfei Liang, Yu Liu, Xinping Zhou
Figure caption: Time–distance stack plots showing the evolution of the EUV wave and Moreton wave, as obtained from the AIA 211, 193, 171, 94, 131, 304, and 335 Å, SUTRI 465 Å, and SMART Hα. The deceleration and initial speed of the wave obtained by fitting the spines in the time–distance stack plots are listed in corresponding panels, where the red dotted curved lines are the fitting results using a second-order polynomial function. Panel (g) marks the oscillations of the filaments.
Paper: 3D Fast-mode Wave Propagation from Corona to Chromosphere: Triggering Mechanism for 3D Oscillations of Filaments
Authors: Yunxue Huang, Qin Feng, Yuhu Miao, Zhining Qu, Ke Yu, Hongfei Liang, Yu Liu, Xinping Zhou
Figure caption: Time sequence of SMART Hα images showing the oscillation of the filaments in the LOS direction at three different times. The five columns, from left to right, represent images from bands shifting −1.25 Å, −0.5 Å, 0.0 Å, +0.5 Å, and +1.25 Å from the Hα line center (6562.8 Å), respectively. Images in the same row are taken at a near simultaneous time with reference to the Hα center image. The four white crosses on F1, F2, and F3 in panel (a3) are the positions where Doppler velocities are measured, while the two green crosses are used to get the background intensity.
Paper: Flash Ionization of the Early Universe by Population III.1 Supermassive Stars
Authors: Jonathan C. Tan
Figure caption: Thomson optical depth to electron scattering, τ, integrated out to redshift, z. The blue solid line is the estimated contribution from “standard” galaxies (B. E. Robertson et al. 2015) and AGN (although note AGN are expected to make only a minor contribution). The red dotted line shows the contribution from Population III.1 supermassive stars with epoch of peak flash ionization at zflash = 20. The red dashed line shows the corresponding model for zflash = 25 (see the main text). The lower gray shaded area shows τ = 0.06 ± 0.005, which is representative of values derived from most recent analyses of Planck CMB data (e.g., Planck Collaboration et al. 2020; R. de Belsunce et al. 2021). The upper gray shaded area shows τ = 0.09 ± 0.01 that is needed to alleviate negative neutrino masses and dynamical dark energy (T. Jhaveri et al. 2025; N. Sailer et al. 2025).
Paper: Chemical Abundances of Seven Stars in the GD-1 Stream
Authors: Jing-Kun Zhao, Guang-Wei Li, Wako Aoki, Gang Zhao, Guo-Chao Yang, Jian-Rong Shi, Hai-Ning Li, Tadafumi Matsuno, Miho Ishigaki, Takuma Suda, Satoshi Honda, Yu-Qin Chen, Qian-Fan Xing, Hong-Liang Yan, Yong Yang, Xian-Hao Ye
Figure caption: Abundance pattern of seven member stars (black points for six stars and square for carbon star) and comparison with dwarf galaxies and the halo stars of Milky Way. Gray points are metal-poor stars from H. Li et al. (2022). Colored symbols are from dwarf galaxies.
Paper: Chemical Abundances of Seven Stars in the GD-1 Stream
Authors: Jing-Kun Zhao, Guang-Wei Li, Wako Aoki, Gang Zhao, Guo-Chao Yang, Jian-Rong Shi, Hai-Ning Li, Tadafumi Matsuno, Miho Ishigaki, Takuma Suda, Satoshi Honda, Yu-Qin Chen, Qian-Fan Xing, Hong-Liang Yan, Yong Yang, Xian-Hao Ye
Figure caption: Panel (a): [Na/Fe] vs. [O/Fe]. Panel (b): [Na/Fe] vs. [Mg/Fe]. Panels (c), (d), (e), (f), and (g): relation between Teff and [Na/Fe], [Mg/Fe], [Cr/Fe], [Ba/Fe], and [Eu/Fe]. Panel (h): the relation between [Ba/Fe] and [Eu/Fe]. Red line is the line fit.
Paper: Metal-polluted Population III Galaxies and How to Find Them
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Daniel Schaerer, Alessandro Marconi, Ioanna Koutsouridou, Stefano Carniani
Figure caption: Left: schematic representation of the evolutionary stages of a PopIII galaxy, based on the ratio between PopIII and total M⋆. Right: density distributions of NEFERTITI PopIII galaxies on the EW(He IIλ4686) vs. [O III]λ5007/Hβ diagram for logU = −1. The colors represent different evolutionary stages, as shown in the left-side scheme. The dotted (solid) lines include 95% (68%) of the population. The horizontal dashed line is the lower limit of the PopIII diagnostic from K. Nakajima & R. Maiolino (2022), with the shaded area below highlighting the AGN and black hole (BH) contamination zone.
Paper: Metal-polluted Population III Galaxies and How to Find Them
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Daniel Schaerer, Alessandro Marconi, Ioanna Koutsouridou, Stefano Carniani
Figure caption: Same as Figure 1 but for different emission line ratios and logU = [−3,−2,−1,−0.5, 0]. The thickness of the contours increases with the U value. The empty contours represent AGN models from A. Feltre et al. (2016; gray) and star-forming galaxy models from J. Gutkin et al. (2016; purple). The red dashed lines are our diagnostics for galaxies with >25%M⋆ in PopIII stars (Section 3.2). The gray points are JADES data with tentative He II and C IV detections (S/N > 2), with the darker shade highlighting the sources that we selected as possible PopIII candidates.
Paper: Metal-polluted Population III Galaxies and How to Find Them
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Daniel Schaerer, Alessandro Marconi, Ioanna Koutsouridou, Stefano Carniani
Figure caption: Same as Figure 1 but for He IIλ1640/Hβ vs. [O III]λ5007/Hβ. The gray shaded area represents the region containing 68% of the AGN models from A. Feltre et al. (2016). Points with error bars are observations of LAP1-B (K. Nakajima et al. 2025) and RX J2129-z8He II (X. Wang et al. 2024). The gray arrows are 5σ upper limits from JADES data (F. D’Eugenio et al. 2025).
Paper: A JWST View of the Overmassive Black Hole in NGC 4486B
Authors: Behzad Tahmasebzadeh, Matthew A. Taylor, Monica Valluri, Haruka Yoshino, Eugene Vasiliev, Michael J. Drinkwater, Solveig Thompson, Kristen Dage, Patrick Côté, Laura Ferrarese, Tatsuya Akiba, Vivienne Baldassare, Misty C. Bentz, John P. Blakeslee, Holger Baumgardt, Youkyung Ko, Chengze Liu, Ann-Marie Madigan, Eric W. Peng, Joel Roediger, Kaixiang Wang, Tyrone E. Woods
Figure caption: The BH mass measurements and their 1σ uncertainties for NGC 4486B derived from various dynamical modeling approaches. From top to bottom, the measurements correspond to: (1) the spherical isotropic Jeans modeling from J. Kormendy et al. (1997), (2) axisymmetric JAM modeling, (3) axisymmetric JAM modeling with the σ peak masked, (4) axisymmetric Schwarzschild modeling, (5) axisymmetric Schwarzschild modeling without DM, (6) axisymmetric Schwarzschild modeling with the σ peak masked, and (7) axisymmetric Schwarzschild modeling with the σ peak shifted to the photometric center.
Paper: Metal-polluted Population III Galaxies and How to Find Them
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Daniel Schaerer, Alessandro Marconi, Ioanna Koutsouridou, Stefano Carniani
Figure caption: Same as Figure 3 but for the EWs of UV metal lines vs. their ratio with He II. The black dotted lines identify regions populated only by models with >25% PopIII M⋆.
Paper: Metal-polluted Population III Galaxies and How to Find Them
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Daniel Schaerer, Alessandro Marconi, Ioanna Koutsouridou, Stefano Carniani
Figure caption: Percentages of NEFERTITI PopIII galaxies in different evolutionary stages (see the left side of Figure 1) as a function of the He II/Hβ emission.
Paper: Metal-polluted Population III Galaxies and How to Find Them
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Daniel Schaerer, Alessandro Marconi, Ioanna Koutsouridou, Stefano Carniani
Figure caption: Same as Figure 1 (top row) and Figure 2 (bottom row) but for different U values.
Paper: Discovery of a Pair of Galaxies with Both Hosting X-Ray Binary Candidates at z = 2.544
Authors: Sijia Cai, Zheng Cai, Jianwei Lyu, Yunjing Wu, Xiaojing Lin, Mingyu Li, Junjie Mao, Jiayi Chen, Pengjun Lu
Figure caption: The top three panels show the NIRSpec spectra of UDF3 from the DJA data set, with the upper panel showing the prism spectrum and the middle two panels displaying the grating spectra from G235M/F170LP and G395M/F290LP. We only show the emission-line regions for clearer visualization of the emission-line flux measurements described in Section 3.1. The yellow curve represents the power-law fit to the continuum, and the green curve shows the Gaussian fit to the emission lines. The bottom panel presents the VLT/VIMOS spectrum of UDF3-2 from the VANDELS survey. We bin the spectrum over 3 pixels to enhance the S/N. The solid lines show the flux density, the shaded regions show the corresponding 1σ uncertainties, and the emission and absorption lines are labeled.