adsabs/AstroCLIMB huggingface dataset:
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage. II. Results of Four Seasons of Observation
Authors: Hai-Cheng Feng, Sha-Sha Li, J. M. Bai, H. T. Liu, Kai-Xing Lu, Yu-Xuan Pang, Mouyuan Sun, Jian-Guo Wang, Yang-Wei Zhang, Shuying Zhou
Figure caption: Mean spectrum for each observing season. The spectra are vertically shifted by an interval of 0.5 × 10−13 erg s−1 cm−2 Å−1 to facilitate distinction, with red, green, blue, and black representing S1, S2, S3, and S4, respectively.
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage. II. Results of Four Seasons of Observation
Authors: Hai-Cheng Feng, Sha-Sha Li, J. M. Bai, H. T. Liu, Kai-Xing Lu, Yu-Xuan Pang, Mouyuan Sun, Jian-Guo Wang, Yang-Wei Zhang, Shuying Zhou
Figure caption: Light curves and results of ICCF analysis for each observing season. In each ICCF panel, the black line is the ICCF, the green histogram represents the CCCD, and the red dashed line denotes zero lag.
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Similar to Figure 7, but for a GRB 230307A-like event with f  p  = 0.7 and ε  p /ε  e  = 3.
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Similar to Figure 7, but for a GRB 090902B-like event.
Paper: Neutrino Constraints and Detection Prospects from Gamma-Ray Bursts with Different Jet Compositions
Authors: Yang-Dong-Jun Ou, Hou-Jun Lü, Xue-Zhao Chang, Xiao-Xuan Liu, En-Wei Liang
Figure caption: Similar to Figure 9, but for a GRB 080916C-like event.
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage. II. Results of Four Seasons of Observation
Authors: Hai-Cheng Feng, Sha-Sha Li, J. M. Bai, H. T. Liu, Kai-Xing Lu, Yu-Xuan Pang, Mouyuan Sun, Jian-Guo Wang, Yang-Wei Zhang, Shuying Zhou
Figure caption: Correlations of R Hβ  vs. L 5100 (left) and ΔR Hβ  vs. ﹩\dot{{\mathscr{M}}}﹩ (right). To ensure a consistent comparison, all luminosities have been recalculated following P. Du & J.-M. Wang (2019). In the left panel, the dotted and dashed lines represent the linear fit from P. Du et al. (2018b) for AGNs with ﹩\dot{{\mathscr{M}}}\lt 3﹩ and ﹩\dot{{\mathscr{M}}}\geqslant 3﹩, respectively. In the right panel, the horizontal and vertical gray dashed lines indicate ΔR Hβ  = 0 and ﹩\dot{{\mathscr{M}}}=3﹩, respectively.
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage. II. Results of Four Seasons of Observation
Authors: Hai-Cheng Feng, Sha-Sha Li, J. M. Bai, H. T. Liu, Kai-Xing Lu, Yu-Xuan Pang, Mouyuan Sun, Jian-Guo Wang, Yang-Wei Zhang, Shuying Zhou
Figure caption: Velocity-resolved lags for Hα, Hβ, and Hγ in each observing season. In each panel, the lower plot displays the rms spectrum, while the upper plot shows the observed τ cent for each flux bin, separated by the vertical red dashed lines. The horizontal dotted line and the associated blue shaded region represent the overall lag of the emission line and its corresponding uncertainty.
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage. II. Results of Four Seasons of Observation
Authors: Hai-Cheng Feng, Sha-Sha Li, J. M. Bai, H. T. Liu, Kai-Xing Lu, Yu-Xuan Pang, Mouyuan Sun, Jian-Guo Wang, Yang-Wei Zhang, Shuying Zhou
Figure caption: The relationship between σ line and lags for all emission lines in our observations. The black points represent the observed τ cent of the emission lines listed in Table 4, while the red points include a correction of an additional of 4 days to account for the continuum lag between optical and UV. The black and red dashed lines represent fits to the black and red points, respectively, using the relation ﹩{\sigma }_{\mathrm{line}}\propto {\tau }_{\mathrm{cent}}^{\beta }﹩. The blue and green solid lines show the fits with β fixed at 0.5.
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage. II. Results of Four Seasons of Observation
Authors: Hai-Cheng Feng, Sha-Sha Li, J. M. Bai, H. T. Liu, Kai-Xing Lu, Yu-Xuan Pang, Mouyuan Sun, Jian-Guo Wang, Yang-Wei Zhang, Shuying Zhou
Figure caption: Velocity-resolved BDs in each observing season. The panels in the left column present the results calculated using the velocity bins of Hα, while those in the right column show the results using the velocity bins of Hβ. In each panel, the plot on the right side illustrates the correlation between the lags and BDs for the corresponding emission line across different velocity bins.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: The composite (unscaled) NIRSpec prism spectrum (2D above, 1D below) of all z ≥ 5 star-forming galaxies from this study, in the rest frame. Several notable features are seen, from a clear Lyα break at λ rest ≃ 1216 Å highlighting the neutral intergalactic medium (IGM) within which most of the objects reside (with some excess UV flux emanating from z < 6 sources where the IGM becomes ionized), to weak UV lines (the blended He II  λ1640 and [O III] λ λ1661, 1666 doublet, as well as C III] λ1909 emission) and both weak and strong optical lines ([O II] λ λ3727, 3730, [Ne III] λ λ3870, 3969, Hδ λ4103, blended Hγ  λ4342 and [O III] λ4364, He I  λ4472, He II  λ4687, Hβ λ4863, [O III] λ λ4960, 5008, He I  λ5877, [O I] λ6302, Hα λ6564, [S II] λ λ6718, 6732, and He I  λ7067), affording a plethora of emission-line indicators for metallicity, dust, radiation field, and star formation diagnostics. Furthermore, despite the low resolution of the prism, strong hints of Fe II absorption can be seen in the rest-frame UV. A clear continuum is also seen at all wavelengths longward of the Lyman and Balmer breaks, indicating the presence of predominantly young, massive stars and longer-lived, lower-mass stars, respectively. The positions of all detected lines are marked by dashed lines (gray for emission lines, black for absorption lines).
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: The UV continuum slopes of z ≥ 5 galaxies from individual sources (points) and composite JWST/NIRSpec prism spectra, the latter binned as a function of redshift only (gray line and gray shaded uncertainties in both panels), z−M UV (navy and orange points for sources with −22.00 < M UV < −19.25 mag and −18.75 < M UV < −16.00 mag, respectively, in the left panel), and z−M * (navy and orange points for sources with log M */M ⊙ > 8.6 and log M */M ⊙ < 8.4, respectively, in the right panel). Individual points (color-coded to their M UV and log M * values, with UV-luminous and/or higher-mass sources in bluer colors and the opposite in redder colors) display a large scatter of values (generally between β ∼ −1.8 to β ∼ −2.8, with a mean 1σ uncertainty of ≃0.22) and an overall declining slope with redshift. Composite points confirm the trend, with clear differences between faint/low-mass systems and their bright/high-mass counterparts and a particularly strong redshift evolution with absolute magnitude but shallower evolution with stellar mass.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: The rest-frame equivalent width of C III] λ λ1907, 1909 line emission as a function of spectroscopic redshift, as measured from our redshift-binned composite spectra. The trend of increasing EW with redshift is well parameterized by a straight-line fit (dashed purple line with pink uncertainties). Measurements from the literature (D. P. Stark et al. 2015, 2017; A. J. Bunker et al. 2023; F. D’Eugenio et al. 2024; R. L. Larson et al. 2023; M. Castellano et al. 2024; S. Carniani et al. 2024) are added as gray points, for comparison.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: The Balmer break as measured directly from our fiducial composite spectra (F  ν4225/F  ν,3565), as a function of redshift (red squares and uncertainties). For comparison, the expected range of values for low-metallicity (0.01–0.2 Z ⊙) and young (5–20 Myr) sources (D. Schaerer 2003) are shown as the gray region. Median values for comparable sources in the SPHINX20 (H. Katz et al. 2023) and FLARES (S. M. Wilkins et al. 2024) simulations are also shown as solid and dashed navy lines, respectively, and the model of A. Ferrara et al. (2023) as a dotted line. All comparisons show agreement with the range of values measured here, as well as the observed trend with redshift.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: The sample of spectroscopically confirmed sources at z ≥ 5 compiled in this work (listed in Tables 3–4 in the Appendix), with continuum measurements available for spectrophotometric scaling in the rest-frame UV. Sources identified in blank fields are shown in blue, while lensed sources (approximately 37% of the parent sample) are plotted in purple. Sources considered to be AGN in this study are indicated with black squares.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: The star-forming main sequence as defined by our sample of confirmed sources, in four redshift bins. Stellar masses are derived from best-fit gsf SED models of the stellar continuum, while SFRs are derived from attenuation-corrected UV luminosities at ∼1600 Å. A best-fit straight line to the 5 < z < 7 data is shown in each panel, along with the J. S. Speagle et al. (2014) relation at z ∼ 6 in the top left panel.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: Gas-phase oxygen metallicities as a function of redshift for the stacks derived in this work (blue squares), as estimated from the strong line O32 prescription of R. L. Sanders et al. (2024). Literature points from R. L. Sanders et al. (2024), M. Curti et al. (2024), and K. Nakajima et al. (2023) are plotted as gray symbols. The dashed lines mark levels of constant metallicity in solar units, assuming 12 + log(O/H)⊙ = 8.69 (M. Asplund et al. 2009). A clear trend of decreasing metallicity toward higher redshifts is evident, likely reflecting larger H I gas fractions of high-z sources.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: Composite NIRSpec spectra (solid lines and filled) and their 1σ standard deviations (i.e., dashed line) as a function of spectroscopic redshift. Each composite spectrum is shifted to the rest frame using the median spectroscopic redshift (indicated) of the stack and normalized to its λ ≃ 1750 Å flux. All spectra are vertically offset for clarity, and the positions of several rest-frame optical emission lines are indicated by dashed gray lines.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: The distribution of rest-frame equivalent widths for the rest-frame optical emission lines observed in our redshift-stacked spectra, as measured from the Gaussian fits described in Section 3.7.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: The R23−O32 (left) and Ne3O2−([Ne III] + [O II])/Hδ (right) diagrams tracing the ionization and excitation states of galaxy ISM across cosmic time. In each plot, the values and uncertainties (often smaller than the symbols) for our stacked sources are shown as colored stars (color-coded according to Figure 4), while values from the literature at comparable redshifts (A. J. Cameron et al. 2023; S. Mascia et al. 2023a; K. Nakajima et al. 2023; R. L. Sanders et al. 2023) are shown as gray points with varying marker symbols. GN-z11 is shown as a green diamond in the right panel using values from A. J. Bunker et al. (2023), while GHZ2 is shown as a green square using values from A. Calabro et al. (2024). For reference, the locus of z < 0.3 points from SDSS are shown as a density plot. Tracks from the photoionization models of J. Gutkin et al. (2016) are shown in blue for a variety of metallicities and ionization parameters, where the shade of blue denotes the metallicity (from 0.01 to 0.4 Z ⊙ going from light shaded to dark shaded) and the size of the connecting points describes the ionization parameter (from log U = −3 to −1 in −0.5 intervals, with the largest values represented by the largest circles).
Paper: Disk2Planet: A Robust and Automated Machine Learning Tool for Parameter Inference in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Kwang Moo Yi, Lu Lu, Sifan Wang, Paris Perdikaris
Figure caption: A flow chart illustrating the iterative parameter update procedure in Disk2Planet inverse problem solver. The solver iterates a 5D Gaussian distribution representing the most probable parameters (α, h 0, q, r p, and θ p) that result in the minimal difference between the model and the input data. At each iteration, the Gaussian distribution is refined by testing 128 sets of parameters sampled from the current distribution. These parameters are processed by the ML-based solver PPDONet (Section 2.1) to predict the corresponding disk maps. Differences between these maps and the data are quantified by the score (Section 2.2). The CMA-ES optimizer (Section 2.3) updates the Gaussian distribution to converge toward parameter sets with smaller scores. This process iterates until the distribution converges to the optimal parameters. On the right, we show an example of the inference process: (a) the input surface density map and its true parameters; (b) the evolution of the best score over iterations; (c) the inferred parameters and the corresponding surface density solution.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: Left: the distribution of Lyα rest-frame equivalent widths as a function of spectroscopic redshift for the objects in our fiducial sample. Objects with confirmed Lyα emission from prism observations are highlighted as maroon circles, while undetected sources are represented by 2σ gray upper limits. Dashed lines represent the EW limits used for the construction of the composite spectra. Middle: the same EW measurements from the left panel for Lyα-detected sources only, as a function of absolute magnitude. Similar measurements from P. A. Oesch et al. (2015), M. Tang et al. (2023), and A. Saxena et al. (2024) are plotted for comparison. Right: the same as the middle plot but as a function of O32 parameter. Results for both low- and high-redshift studies using measurements from M. Tang et al. (2021), S. R. Flury et al. (2022), M. Tang et al. (2023), and A. Saxena et al. (2024) are plotted for comparison.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: The percentage slit loss of sources observed with NIRSpec prism compared to NIRCam photometry. The slit loss is defined as the NIRCam photometry minus the NIRSpec pseudophotometry, divided by the NIRCam photometry, and multiplied by 100. Measurements for individual sources are plotted as gray points, while Gaussian fits to the density distribution in each filter are plotted as solid lines with normalized amplitudes. The centroid of each Gaussian is shown as a colored square, shifted by +0.2 μm for clarity. A best-fit exponential function to the squares is shown as a turquoise line. We note that the distributions of single-object points for virtually all bands are Gaussian in shape, except the F115W and F150W bands, which are less well defined and thus appear slightly up- or down-scattered compared to their redder counterparts.
Paper: Between the Extremes: A JWST Spectroscopic Benchmark for High-redshift Galaxies Using ∼500 Confirmed Sources at z ≥ 5
Authors: Guido Roberts-Borsani, Tommaso Treu, Alice Shapley, Adriano Fontana, Laura Pentericci, Marco Castellano, Takahiro Morishita, Pietro Bergamini, Piero Rosati
Figure caption: A comparison between the median spectrum of sources with EW0,Lyα  > 30 Å (LAEs; blue) and those with EW0,Lyα  < 10 Å (non-LAEs; black). The two spectra are well matched in median redshift and absolute magnitude, allowing for a close comparison of intrinsic properties: the two spectra reveal modest differences in UV slope, but significant differences in line intensity and ratios (e.g., the presence or otherwise of C IV, C III], and He II + [O III] in the rest-frame UV), as well as in the rest-frame optical continuum. Overall, the LAE stack appears to represent sources with more extreme ionizing fields, lower metallicities and stellar masses, and young stellar populations, suggesting intrinsic properties—in addition to environmental effects—play some role in regulating the visibility of strong Lyα.
Paper: Disk2Planet: A Robust and Automated Machine Learning Tool for Parameter Inference in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Kwang Moo Yi, Lu Lu, Sifan Wang, Paris Perdikaris
Figure caption: The framework of conventional inverse problem solvers. Each iteration begins with an estimation of the system configuration, which includes parameters in a disk–planet system. This configuration is sent to a numerical solver to generate the resulting disk maps. Expert analysis then evaluates the visual discrepancies between the simulation outcomes and the observational data, leading to iterative refinements of the system parameters.
Paper: Disk2Planet: A Robust and Automated Machine Learning Tool for Parameter Inference in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Kwang Moo Yi, Lu Lu, Sifan Wang, Paris Perdikaris
Figure caption: Score calculation for three cases of input data. Block (A): for noisy input data, the score is calculated the same way as for noise-free data. Block (B): for input data with missing areas, only the available pixels are used. Block (C): for input data containing multiple quantities, the error for each quantity is calculated, and then the average of all errors is taken as the score.
Paper: Disk2Planet: A Robust and Automated Machine Learning Tool for Parameter Inference in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Kwang Moo Yi, Lu Lu, Sifan Wang, Paris Perdikaris
Figure caption: Ground truth and inferred planet masses in 256 tests using full noise-free maps of surface density as input. The tests achieve an r2-score (Equation (3)) of 0.9994 and an inference uncertainty σ of 0.0073, indicating near-perfect agreement (red solid line). See Section 3.1 for details.
Paper: Revealing the Elusive Companion of the Red Giant Binary 2MASS J05215658+4359220 from UV HST and Astrosat/UVIT Data
Authors: Luciana Bianchi, John Hutchings, Ralph Bohlin, David Thilker, Emanuele Berti
Figure caption: STIS UV+optical spectra (G230L+G430L+G750L combined, flux in erg cm−2 s−1 Å−1) plotted in black, with the best-fit two-component stellar models: T eff = 4250 K, log g = 2.0 for the RG (purple), and T eff = 6000 K, log g = 3.0 for the companion (cyan). A metallicity of 10 times less than solar provides the best match to all major spectral features for the derived log g, and an extinction of E  B−V  = 0.5 (assuming a Milky Way–type extinction, with R  V  = 3.1) yields the overall best match to the SED across the whole range. The summed flux of the two models is shown in orange (middle and bottom panels). With the Gaia DR3 distance, scaling the best-fit-model fluxes to the STIS fluxes accounting for the derived extinction, yields radii of R RG = 27.8 and R comp = 2.7 R ⊙. In the top and bottom panels the systematic error (dashed line) and statistical error (dotted lines) of the STIS spectra are also shown. Shortwards of ∼2400 Å the data yield only an upper limit to the flux (see Figure 5).
Paper: Revealing the Elusive Companion of the Red Giant Binary 2MASS J05215658+4359220 from UV HST and Astrosat/UVIT Data
Authors: Luciana Bianchi, John Hutchings, Ralph Bohlin, David Thilker, Emanuele Berti
Figure caption: As in the previous figure: STIS UV+optical spectra (G230L+G430L+G750L combined, flux in erg cm−2 s−1 Å−1) plotted in black, with the best-fit two-component stellar models, using models with metallicity Z = 0.006: The RG results do not differ from the previous case except for a slightly lower radius: T eff = 4250 K, log g = 2.0, and R RG = 27.7R ⊙ (purple model), but a worse fit of broad line features is seen between 3000 and 4000 Å, largely compensated by adjusting the companion’s parameters: T eff = 5750 K, log g = 3.0, and R comp = 4.2R ⊙ (cyan model). Extinction of E  B–V  = 0.5 still yields the best solution. The summed flux of the two models is shown in orange (middle and bottom panels). In the top and bottom panels the systematic error (dashed line) and statistical error (dotted lines) of the STIS spectra are also shown.