adsabs/AstroCLIMB huggingface dataset:
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Prospector fitting results of COSMOS-7549, in a similar format as Figure 1. (a) Observed HST and NIRCam photometry shown as blue and green circles, respectively, and the red line shows the best-fit SED. (b) NIRSpec data are shown with a blue line, and the best-fit spectrum is again shown with a red line. The orange line shows the flux uncertainty. (c) Color-composite image of the galaxy in 5″ × 5″ box. (d) Nonparametric SFH derived from fitting using the continuity SFH prior (left) and the bursty SFH prior (right). Each SFH is the same as shown in Figures 4 and 5, respectively. (e) Posterior distribution of the fitted stellar and dust parameters; the green histogram is from the fitting using the continuity prior and the pink histogram is from the bursty prior.
Paper: Predicting Photospheric Ultraviolet Emission from Stellar Evolutionary Models
Authors: Song Wang, Xue Li, Henggeng Han, Jifeng Liu
Figure caption: Left panels: observed NUV magnitudes (points) compared with photospheric NUV magnitudes predicted by different models (e.g., BASTI, PARSEC, MIST, and BT-SETTL). The colors of points in the top panel indicate temperatures. The observed magnitudes are shown with points in the top panel and contours (i.e., orange contours for F to K stars and violet contours for M stars) in the bottom panel. The model magnitudes are calculated as the median magnitudes within a temperature bin of 200 K. The magenta dashed lines are the fitted baselines using the observed sample in Figure 1. Right panels: observed FUV magnitudes (points) compared with photospheric FUV magnitudes predicted by different models (e.g., BASTI, PARSEC, MIST, and BT-SETTL).
Paper: Predicting Photospheric Ultraviolet Emission from Stellar Evolutionary Models
Authors: Song Wang, Xue Li, Henggeng Han, Jifeng Liu
Figure caption: Top panels: fitting results of the relations between NUV/GALEX (left panel), FUV/GALEX (middle panel), and NUV/CSST (right panel) magnitudes and stellar effective temperature T eff. Bottom panels: fitting results of the relations between NUV/GALEX (left panel), FUV/GALEX (middle panel), and NUV/CSST (right panel) magnitudes and stellar color BP−RP.
Paper: Predicting Photospheric Ultraviolet Emission from Stellar Evolutionary Models
Authors: Song Wang, Xue Li, Henggeng Han, Jifeng Liu
Figure caption: Left panels: observed NUV magnitudes (gray points) compared with photospheric NUV magnitudes derived from PARSEC models (blue points; F to K stars) and BT-SETTL models (red points; M stars) using atmospheric parameters (i.e., T eff, logL, [Fe/H]). The observed magnitudes are shown with gray points in the top panel and contours (i.e., orange contours for F to K stars and violet contours for M stars) in the bottom panel. Right panels: observed FUV magnitudes (gray points) compared with photospheric FUV magnitudes derived from PARSEC models (blue points; F to K stars) and BT-SETTL models (red points; M stars).
Paper: Predicting Photospheric Ultraviolet Emission from Stellar Evolutionary Models
Authors: Song Wang, Xue Li, Henggeng Han, Jifeng Liu
Figure caption: Observed NUV and FUV magnitudes for our sample. The black lines are the fitted baselines using the most inactive stars (i.e., with the faintest UV emission).
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Prospector fitting results of 16419. The same format as Figure A7.
Paper: Acoustic Wake in a Singular Isothermal Profile: Dynamical Friction and Gravitational-wave Emission
Authors: Gali Eytan, Vincent Desjacques, Robin Buehler
Figure caption: Shape factor ﹩{ \mathcal F }({ \mathcal M },{r}_{+}/a)﹩ (Equation (67)) as a function of Mach number for three different values of r +/a (see text for details) as quoted in the figure. The thick and thin curves represent the predictions obtained for a truncated isothermal profile and for a uniform sphere, respectively (see text for details). The vertical line indicates the Mach number ﹩{ \mathcal M }=\sqrt{2}﹩ of a circularly moving perturber in an isothermal profile when the latter dominates the mass of the system.
Paper: Acoustic Wake in a Singular Isothermal Profile: Dynamical Friction and Gravitational-wave Emission
Authors: Gali Eytan, Vincent Desjacques, Robin Buehler
Figure caption: Tangential (left panel) and radial (right panel) friction coefficients ﹩{I}_{\varphi }({ \mathcal M })﹩ and ﹩{I}_{r}({ \mathcal M })﹩ as a function of the Mach number ﹩{ \mathcal M }﹩ in the steady-state regime for a circularly moving perturber in an SIS profile. The dashed curves indicate the contribution from the inner and outer regions (assuming ﹩{{\ell }}_{\max }=12﹩). The (green) dotted–dashed curve is the dipole contribution. For comparison, the infinite, homogeneous result is shown as a (red) dotted curve.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Comparisons of ﹩\mathrm{log}g﹩ derived from the Sonora Elf Owl, ATMO2020++, and ATMO2020 models. The ﹩\mathrm{log}g﹩ values on the x-axis are from the ATMO2020 models, while the y-axis shows the differences in ﹩\mathrm{log}g﹩ between the Sonora Elf Owl and ATMO2020 models (red inverted triangles), as well as between the ATMO2020++ and ATMO2020 models (blue crosses). Notably, the largest red inverted triangle at [2.5, 0.75] represents the overlap of five data points.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Comparisons of the best-fit model spectra derived from Sonora Elf Owl (red) and ATMO2020++ (blue) with the observed spectra (black) of CWISEP J1446−23 (top) and WISEA J2159−48 (bottom). Both models fit the overall spectra better. Specifically, the results of these two models show that the fitting in the wavelength range of 4–4.5 μm differs for different objects.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Comparisons of effective temperature and surface gravity derived from the two models. Parameter values on the x-axis are derived from the Sonora Elf Owl models, while those on the y-axis represent the difference between the ATMO2020++ and Sonora Elf Owl models.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: The spectra of various objects with spectral types spanning from T6 to ≥Y1. The wavelength range is from 0.95 to 12 μm, with main bands of molecular feature listed at the top (same colors indicate the same molecules). The spectral fluxes are normalized at the peak of 10.2 μm.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Best-fitting parameters of Sonora Elf Owl and ATMO2020++ models from Tables 3 and 4 compared with the evolutionary tracks of G. Chabrier et al. (2023).
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: An example showing the calculation of spectral indices using specific wavelength intervals from the spectrum of WISE J2102−44.
Paper: Benchmarking Dielectronic Recombination Rate Coefficients for Carbon-like Ca14+ 
Authors: C. Y. Zhang, B. S. Yan, K. Wang, R. Si, K. Yao, W. L. Ma, Z. K. Huang, W. Q. Wen, X. W. Ma, L. F. Zhu, C. Y. Chen, N. R. Badnell
Figure caption: Comparison of the rate coefficients for Ca14+ from the present FAC single-nl CI, AS single-nl CI, FAC multi-n CI, and AS multi-n CI calculations. The measured recombination spectrum (W. Q. Wen et al. 2020) is also presented. The contributions from 2s 22p 2 nl and 2s2p 3 nl are also shown separately. The strong resonance peaks are labeled based on the new FAC multi-n CI calculation, and the core electrons 1s 2 are omitted.
Paper: Benchmarking Dielectronic Recombination Rate Coefficients for Carbon-like Ca14+ 
Authors: C. Y. Zhang, B. S. Yan, K. Wang, R. Si, K. Yao, W. L. Ma, Z. K. Huang, W. Q. Wen, X. W. Ma, L. F. Zhu, C. Y. Chen, N. R. Badnell
Figure caption: Comparison of the rate coefficients for Ca14+ from the present FAC multi-n CI and AS multi-n CI calculations. The measured recombination spectrum (W. Q. Wen et al. 2020) is also presented. The strong resonance peaks are labeled based on the present FAC calculation, and the core electrons 1s 2 are omitted.
Paper: Benchmarking Dielectronic Recombination Rate Coefficients for Carbon-like Ca14+ 
Authors: C. Y. Zhang, B. S. Yan, K. Wang, R. Si, K. Yao, W. L. Ma, Z. K. Huang, W. Q. Wen, X. W. Ma, L. F. Zhu, C. Y. Chen, N. R. Badnell
Figure caption: Comparison of the plasma rate coefficients for Ca14+ from old FAC (W. Q. Wen et al. 2020), old AS (W. Q. Wen et al. 2020), new FAC multi-n CI, and new AS multi-n CI calculations with the experimentally derived values (W. Q. Wen et al. 2020). The FAC results from M. F. Gu (2003) are also presented. The vertical dashed bars denote the boundaries of the PP and CP temperature ranges.
Paper: Spectrophotometric Reverberation Mapping of Intermediate-mass Black Hole NGC 4395
Authors: Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose, Archana Gupta
Figure caption: NGC 4395 is plotted on the black hole mass (M BH) vs. stellar velocity dispersion (σ ⋆) diagram. The dynamically measured black hole masses and σ ⋆ for inactive galaxies are in dark blue open squares, taken from J. Kormendy & L. C. Ho (2013) and J. H. Woo et al. (2015). The RM AGN black hole masses are shown with light blue filled squares, taken from J. H. Woo et al. (2015). The M BH for RM AGNs is based on σ line and the σ ⋆ is also compiled from J. H. Woo et al. (2015). The dark blue and light blue dashed lines are the M BH–σ ⋆ fit for the dynamical M BH of inactive galaxies and RM AGNs, and the solid line illustrates the combined fit for dynamical M BH and RM AGN M BH. The slope and intercept are obtained from J. Kormendy & L. C. Ho (2013) and J. H. Woo et al. (2015), respectively. We plotted the source NGC 4395 with the upper limit of σ ⋆, i.e., 30 km s−1, and measured the [O III]λ5007 and [S II]λ6732 dispersion along with our measured M BH = ﹩{2.2}_{-0.2}^{+0.2}\times {10}^{4}{M}_{\odot }﹩.
Paper: Spectrophotometric Reverberation Mapping of Intermediate-mass Black Hole NGC 4395
Authors: Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose, Archana Gupta
Figure caption: An example of spectral decomposition of the mean spectrum of March 11. The left panel shows the mean spectrum with marked emission-line regions. The right panel presents the decomposition of the Hα component into narrow and broad components with narrow [N II] lines. The broad Hα component is modeled with the double Gaussian shown in green, and the narrow component is modeled with the single Gaussian shown in blue. The narrow [N II] λ6549 and λ6585 emission lines are shown with a single-Gaussian fit in blue. The total line construction is shown in red with the illustrated continuum region. The lower-right panel shows the residual of the fit in black.
Paper: Spectrophotometric Reverberation Mapping of Intermediate-mass Black Hole NGC 4395
Authors: Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose, Archana Gupta
Figure caption: The lag results are plotted; the upper-left panel shows the merged V-band and continuum flux at 5100 Å in units of 10−17 erg cm−2 s−1 Å−1, and the lower-left panel shows the emission-line light curve in units of 10−17 erg cm−2 s−1. The mean-subtracted light curves shown are matched by normalizing the continuum light curve and shifting the emission-line light curve to the final adopted lag values mentioned in Table 4. The upper-right panel depicts the ICCF coefficient (r) resulting from the continuum and emission-line light curve with respect to the lag in minutes. The lower-right panels show the lag histograms obtained using the ICCF and JAVELIN methods. Here, subplots 1, 2, and 6 show the detrended light curves and their respective detrended lag results.
Paper: Spectrophotometric Reverberation Mapping of Intermediate-mass Black Hole NGC 4395
Authors: Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose, Archana Gupta
Figure caption: The plot depicts the Hβ BLR size vs. optical luminosity at 5100 Å. NGC 4395 lies at the low-luminosity end, with an Hβ BLR size of 74.8 light minutes. The other RM sources, such as SEAMBHs (P. Du et al. 2016, 2018; C. Hu et al. 2021; S.-S. Li et al. 2021; orange open circles), SDSS-RM (C. J. Grier et al. 2017; yellow open squares), OzDES (U. Malik et al. 2023; green open diamonds), LAMP (V. U et al. 2022; red open circles), SAMP (J.-H. Woo et al. 2024; blue open hexagons), and others (including, M. C. Bentz et al. 2013; S. Park et al. 2017; S. Rakshit et al. 2019; E. D. Bontà et al. 2020; S. Rakshit 2020; S. Pandey et al. 2022; purple open triangles) are shown. The brown dashed line shows the best-fit R–L relation as obtained by J.-H. Woo et al. (2024).
Paper: Spectrophotometric Reverberation Mapping of Intermediate-mass Black Hole NGC 4395
Authors: Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose, Archana Gupta
Figure caption: The Hα BLR size vs. monochromatic continuum luminosity at 5100 Å is plotted. Various Hα RM sources (S. Kaspi et al. 2000; M. C. Bentz et al. 2010; C. J. Grier et al. 2017; H. Cho et al. 2020; J.-H. Woo et al. 2024), along with others (such as S. G. Sergeev et al. 2016; H.-C. Feng et al. 2021; S.-S. Li et al. 2022), and the best-fit relation from H. Cho et al. (2023), are plotted. The source NGC 4395 is plotted with our best measurement of 125 light minutes in comparison to the 84 minutes lag obtained by H. Cho et al. (2020).
Paper: Spectrophotometric Reverberation Mapping of Intermediate-mass Black Hole NGC 4395
Authors: Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose, Archana Gupta
Figure caption: The combined V-band image of NGC 4395 obtained on 2022 March 10 using the 1.3 m DFOT. Three comparison stars are marked with white circles, while the target AGN is denoted with a red circle. The slit is oriented to cover both the AGN and a comparison star. The field of view is 66′ (18﹩{}^{{\prime} }﹩ × ﹩{18}^{{\prime} }﹩) for the 1.3 m DFOT.
Paper: Spectrophotometric Reverberation Mapping of Intermediate-mass Black Hole NGC 4395
Authors: Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose, Archana Gupta
Figure caption: The upper panel is the merged light curve of the photometric V band and spectroscopic f 5100 in units of 10−15 erg cm−2 s−1 Å−1, and the lower panel is the Hα emission-line light curve in units of 10−14 erg cm−2 s−1, obtained from spectroscopic data after smoothing by five consecutive data points.
Paper: Spectrophotometric Reverberation Mapping of Intermediate-mass Black Hole NGC 4395
Authors: Shivangi Pandey, Suvendu Rakshit, Krishan Chand, C. S. Stalin, Hojin Cho, Jong-Hak Woo, Priyanka Jalan, Amit Kumar Mandal, Amitesh Omar, Jincen Jose, Archana Gupta
Figure caption: Upper left panel: the continuum and Hα line light curves (arbitrary flux) for the entire two days fitted with a straight line (gray), as mentioned in Section 3.2.2. Lower left panel: the mean-subtracted light curves after detrending are shown. Here, the continuum light curve is normalized, and the emission-line light curve is shifted by a lag of 205 minutes. Right panels: the CCF coefficient (r) along with ICCF and JAVELIN lag histograms before (upper right) and after (lower right) detrending.
Paper: The Oscillation in Evolution of Changing-look Blazar OQ 334
Authors: S. S. Ren, R. X. Zhou, Y. G. Zheng, S. J. Kang
Figure caption: Multiwavelength SED of the CLB across different states during MJD 54628–60387. The dotted blue, green, red, and purple lines represent Syn, SSC, EC, and EBL absorption components, respectively. The solid black line represents the total fitted spectrum of the SED. Red dots denote quasi-simultaneous data, blue dots represent nonquasi-simultaneous data, and gray dots indicate archival data. Each subplot corresponds to epochs T4, F3, T5, B3, T6, F4, T7, B4, T8, F5, T9, B5, T10, F6, T11, B6, T12, and F7 during MJD 54628–60387. The gray background shows the 1σ parameter space of the SED model, starting from the optical observation data points used in the fit. The lower panel of each subplot displays the residuals of the fit. The SED of different states before the T4 epoch (i.e., MJD 54628–58677) have been fitted in S. S. Ren et al. (2024).
Paper: The Oscillation in Evolution of Changing-look Blazar OQ 334
Authors: S. S. Ren, R. X. Zhou, Y. G. Zheng, S. J. Kang
Figure caption: Fermi-LAT SED for the MJD 54628–60387 epoch. The solid black line represents the best fit from the likelihood analysis over the entire energy range. Blue dots denote γ-ray data points, while green downward arrows indicate the upper energy limits. The purple area represents the 1σ confidence band. The “letters + numbers” in each subgraph correspond to the states listed in Table 1. The corresponding images for the epochs F1, T1, B1, T2, F2, T3, and B2 are from S. S. Ren et al. (2024).
Paper: The Oscillation in Evolution of Changing-look Blazar OQ 334
Authors: S. S. Ren, R. X. Zhou, Y. G. Zheng, S. J. Kang
Figure caption: Comparison of γ-ray photon spectral index from S. S. Ren et al. (2024) with the equivalent width of Mg II from H. D. Mishra et al. (2021). Green triangles, purple prisms, and gray stars represent the BL Lac state, FSRQ state, and transition state, respectively. The dashed red line represents EW = 5 Å, while the two dotted blue lines correspond to =2.0 and =2.2.
Paper: The Oscillation in Evolution of Changing-look Blazar OQ 334
Authors: S. S. Ren, R. X. Zhou, Y. G. Zheng, S. J. Kang
Figure caption:  γ-ray and X-ray light curve in MJD 54628–60387. The upper panel shows γ-ray data ranging from 0.1 to 300 GeV, while the lower panel displays X-ray data spanning 0.3–10 keV. Labels such as F 1 and B 1 indicate the first occurrence of OQ 334 in the FSRQ and BL Lac states, respectively. We discarded data points with TS ≥ 15. The corresponding MJD for the epochs B1, F2, and B2 are from S. S. Ren et al. (2024).
Paper: Bright in the Black: Searching for Electromagnetic Counterparts to Gravitational-wave Candidates in LIGO-Virgo-KAGRA Observation Runs with AstroSat-CZTI
Authors: Gaurav Waratkar, Varun Bhalerao, Dipankar Bhattacharya
Figure caption: AstroSat coverage statistics for the injection set of the O4 run of LVK GW detectors (R. W. Kiendrebeogo et al. 2023) as described in Section 4.3. The histogram (solid) shows the recovery of 7126 binary black holes, where we have 74.33% of events that are recovered with a coverage higher than 10% of the sky map (black), while 7.35% of events have a coverage lower than that (green). The other histogram (dashed) shows the recovery of 1132 injections with at least one neutron star component, where we have 70.49% recovered injections with at least 10% coverage of the sky map (black), while 5.21% had a coverage lower than that (green). The blue and orange markers show the events in the SAA and data gaps, respectively, for BBH and NS component injections (blue and orange, respectively).
Paper: Bright in the Black: Searching for Electromagnetic Counterparts to Gravitational-wave Candidates in LIGO-Virgo-KAGRA Observation Runs with AstroSat-CZTI
Authors: Gaurav Waratkar, Varun Bhalerao, Dipankar Bhattacharya
Figure caption: Top: detection probability curves of 500 realizations (blue) of 118 BBH nondetections from the ongoing O4 run of LVK GW detectors, combined with the nondetection data from previous runs of LVK GW detectors computed in Section 4.2.2. Each of the blue lines shows the joint detection probability of AstroSat detecting at least one out of 118 BBH events predicted in the O4 run, along with the 57 BBH nondetections from previous runs, as described in Section 4.3. Bottom: histogram of the isotropic luminosities we can rule out with 50% (brown dashed line) and 90% (black-dashed line) confidence given these 500 realizations. We show that typically these realizations cluster around an L iso of 1049 erg s−1, apart from cases where nearby BBH events (at distances of 106, 113 Mpc) become a part of the realization, and hence, completely dominate the joint-probability curve. In such cases, we would be able to probe even fainter luminosities of 1049 erg s−1.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: The median over frequency of the ratio of the solar measurement of the primary beam with the one-, two-, and four-template best-fit holographic reconstructions, for each of the four sources overlapping the solar decl. range and in each copolarization. In general, the inclusion of cross-polarization information in the reconstruction dramatically improves agreement between the two data sets in the main lobe, where beamwidth and primary-null level discrepancies due to polarization leakage cause the holography to deviate from the solar measurement by as much as a factor >2 at the decl. of Hya A.