adsabs/AstroCLIMB huggingface dataset:
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Deconvolved images of the PSF-subtracted disk in the F300M (left panel) and F360M (center panel) filters, as compared to the pre-convolved model from Section  5.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: The ratio of the F300M and F360M data (left panel) and convolved models (right panel), after dividing each image by the integrated stellar flux across the bandpass. The three white ellipses correspond to the A, B, and C rings from M. Konishi et al. (2016).
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Roll-combined images after PSF subtraction. For each filter, the PSF subtraction was performed using MCRDI. The red dashed line delineates the radius of 50% transmission inside of the coronagraph.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: The fraction of outliers in the L1350 Å–C IV blueshift relation as a function of EW(C IV). We divide the sources based on their EW(C IV) using overlapping bins to account for the limited number of sources at small EWs. The standard deviation of EW(C IV) within each bin is shown as the x-axis error, while the y-axis error represents the binomial uncertainty. The three segments of the dark blue polyline represent the best-fit linear relation in each region, while the vertical blue lines with lighter shaded areas represent the location of the two breakpoints and their uncertainty ranges.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: EW distributions of HILs. In each panel, the black histogram and red lines are the EW distribution and its best-fit log-normal model, respectively. The vertical dash and dashed–dotted lines are the 2σ and 3σ lines of their log-normal distributions, respectively. In addition, the redshift coverage of each HIL, the number of sources, the mean value, and the 3σ range of the best-fit log-normal distribution are depicted in the upper left corner of each panel. As the figure shows, each HIL EW distribution exhibits a prominent tail toward low-EW values, which are consistent with the results in A. M. Diamond-Stanic et al. (2009) and J. Wu et al. (2012).
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: The fraction of outliers in the Baldwin effect as a function of EW(C IV). The method adopted here is consistent with that in Figure 5. The cyan points with error bars represent these fractions. The dark blue polyline segments indicate the best fit for each region, with the vertical blue lines marking the locations of the breakpoints. The light blue shaded areas represent the uncertainties of the two breakpoints, located at ﹩8.{7}_{-0.1}^{+0.1}﹩ Å and ﹩19.{3}_{-0.3}^{+0.3}﹩ Å, respectively.
Paper: Statistical Overview of Long-lived Active Regions Observed across Multiple Carrington Rotations
Authors: Emily I. Mason, Kara L. Kniezewski
Figure caption: Sample image of the layout of the Solar Active Region Spotters project on Zooniverse. The top row shows the SDO AIA composite images for the two candidates (this case is not a match), while the bottom left shows a single HMI magnetogram of the original AR and the bottom right shows a short HMI movie of the subsequent AR’s evolution. The red flags in the top left of each figure denote that the subject pair shown has already garnered enough classifications to be retired.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: Baldwin effect for quasars from the DR16 subsample. The cyan contours, from darker to lighter, represent regions containing 68%, 95%, and 99.7% of the sources, respectively. The solid line indicates the MCMC-fitted linear equation, while the dashed line marks the boundary encompassing approximately 95% of the sources. Objects below this dashed line are considered outliers in the Baldwin effect. The scatter in the Baldwin effect is smaller than that in the L1350Å–C IV blueshift relation.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: The relationship between C IV blueshift and monochromatic luminosity at 1350 Å in the rest frame L1350 Å. The red contours from darker to lighter represent regions containing 68%, 95%, and 99.7% of the sources, respectively. The black solid line represents the linear equation fitted by the MCMC method. The black dashed line marks the boundary of outliers for the L1350 Å–C IV blueshift relation. Region below this dashed line encompasses 95% of the objects, while sources above the line will be considered outliers.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: EW Distributions of LILs. The legend is the same as that in Figure 1.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: EW distributions of narrow emission lines. The legend is the same as that in Figure 1. All narrow lines show a tail toward high EW values but none toward low-EW values, which are exactly opposite to those of HILs.
Paper: A Host Galaxy Morphology Link between Quasiperiodic Eruptions and Tidal Disruption Events
Authors: Olivier Gilbert, John J. Ruan, Michael Eracleous, Daryl Haggard, Jessie C. Runnoe
Figure caption: A comparison of our measured morphological properties of QPEs (blue circles) to both TDEs (red stars) and the control galaxy sample (gray contours enclosing 10%, 30%, and 50% of the sample). This control galaxy sample is matched in both stellar mass and redshift to the QPE host galaxy sample. The columns show the distributions in Sérsic index n (left column), (B/T)g (center column), and stellar mass density ﹩{{\rm{\Sigma }}}_{{M}_{\star }}﹩ (right column) as a function of galaxy stellar mass M⋆ (top row) and black hole mass MBH. The three objects with a red star in a blue circle are the three QPE+TDE host galaxies. Smoothed histograms of these quantities from a kernel density estimator are also shown. Both QPE and TDE host galaxies have similar high n, (B/T)g, ﹩{{\rm{\Sigma }}}_{{M}_{\star }}﹩ relative to the control sample, suggesting a link between QPEs and TDEs based on their host galaxy morphologies. Furthermore, both QPE and TDE hosts have undermassive MBH relative to the control sample, suggesting they lie systematically below the M⋆–MBH galaxy scaling relation.
Paper: H I 21 cm Absorption Associated with Foreground Galaxies on Top of Quasars
Authors: Labanya K. Guha, Raghunathan Srianand, Rajeshwari Dutta
Figure caption: Optical properties of GOTOQs observed with the uGMRT. Each horizontal panel consists of two plots: the left plot displays the nebular emissions detected in the continuum-subtracted SDSS/eBOSS quasar spectrum, where the prominent nebular emission lines from the foreground galaxy are marked by red dashed vertical lines, and the fit to the data is shown in blue. The right plot shows a composite griz band DESI-LIS image of the quasar field, with the quasar marked by a red star and the observing fiber outlined by a blue circle. Flux scales in the left panels are in the units of 10−17 erg s−1 cm−2 Å−1.
Paper: A Host Galaxy Morphology Link between Quasiperiodic Eruptions and Tidal Disruption Events
Authors: Olivier Gilbert, John J. Ruan, Michael Eracleous, Daryl Haggard, Jessie C. Runnoe
Figure caption: Surface brightness profile bulge+disk fits for our sample QPE host galaxies. The left panels show the 121 × 121 pixel g-band coadded image cutouts centered on the host galaxy. The middle-left panels show our best-fit two-component (disk+bulge) Sérsic ellipse models. The middle-right panels show the residuals of our model. The right panels show the one-dimensional surface brightness profile fits, where the observed data are represented by black open circles, the bulge by the orange line, the disk by the green line, and the total model (i.e., bulge+disk) by the blue line. The residuals are shown as the red filled circles under the plot.
Paper: A Host Galaxy Morphology Link between Quasiperiodic Eruptions and Tidal Disruption Events
Authors: Olivier Gilbert, John J. Ruan, Michael Eracleous, Daryl Haggard, Jessie C. Runnoe
Figure caption: Continuation of the surface brightness profile bulge+disk fits of our sample of 13 TDE-only host galaxies.
Paper: A Host Galaxy Morphology Link between Quasiperiodic Eruptions and Tidal Disruption Events
Authors: Olivier Gilbert, John J. Ruan, Michael Eracleous, Daryl Haggard, Jessie C. Runnoe
Figure caption: Continuation of the surface brightness profile bulge+disk fits of our sample of QPE host galaxies.
Paper: A Host Galaxy Morphology Link between Quasiperiodic Eruptions and Tidal Disruption Events
Authors: Olivier Gilbert, John J. Ruan, Michael Eracleous, Daryl Haggard, Jessie C. Runnoe
Figure caption: Surface brightness profile bulge+disk fits of our sample of 13 TDE-only host galaxies.
Paper: H I 21 cm Absorption Associated with Foreground Galaxies on Top of Quasars
Authors: Labanya K. Guha, Raghunathan Srianand, Rajeshwari Dutta
Figure caption: Integrated optical depth for H I 21 cm absorption in GOTOQs compared to the color excess, E(B − V), caused by line-of-sight reddening. The occurrence of negative E(B − V) values indicates possible systematic uncertainty of ∼0.1 mag due to the quasar-to-quasar SED variations. However realistic estimation of error in E(B − V) will be achieved if we can use simultaneous SED measurements covering the rest UV-to-IR range. The solid orange line represents the best-fit relation, while the shaded region indicates the 1σ uncertainty in the fit. The purple line and the corresponding shaded region correspond to the best-fit relation taken from H. Liszt (2019) for the Milky Way H I 21 cm absorbers.
Paper: H I 21 cm Absorption Associated with Foreground Galaxies on Top of Quasars
Authors: Labanya K. Guha, Raghunathan Srianand, Rajeshwari Dutta
Figure caption: Lower panel: integrated H I 21 cm optical depth as a function of the impact parameter of galaxies. Blue points represent the GOTOQs, with newly observed GOTOQs using uGMRT highlighted by square boxes, while the remaining data points are taken from the literature. Green points indicate the quasar–galaxy pairs studied by R. Dutta et al. (2017c), and orange points correspond to quasar–galaxy pairs from the literature and compiled in R. Dutta et al. (2017c). Filled points denote H I 21 cm detections in absorption, whereas hollow points represent the 3σ upper limits on the integrated optical depth. Upper panel: normalized histogram of the impact parameter distribution for H I 21 cm detections and nondetections.
Paper: H I 21 cm Absorption Associated with Foreground Galaxies on Top of Quasars
Authors: Labanya K. Guha, Raghunathan Srianand, Rajeshwari Dutta
Figure caption: Covering fraction of H I 21 cm absorbers (C21) as a function of impact parameter. Blue points show C21 across four impact parameter bins (0–8, 8–16, 16–24, and 24–40 kpc) for integrated optical depth sensitivities of 0.3 km s−1 for the GOTOQs and the QGPs studied and compiled from literature by R. Dutta et al. (2017c). Red points are taken from N. Gupta et al. (2021).
Paper: H I 21 cm Absorption Associated with Foreground Galaxies on Top of Quasars
Authors: Labanya K. Guha, Raghunathan Srianand, Rajeshwari Dutta
Figure caption: H I 21 cm absorption spectra of three GOTOQs: J0758+1136 (left panel), J1159+5820 (middle panel), and J1451+0857 (right panel). The individual Gaussian components are shown as blue dashed lines, while the overall fits to the absorption profiles are shown in solid red lines. The upper x-axis indicates the corresponding velocities relative to the emission redshifts of the foreground galaxies.
Paper: H I 21 cm Absorption Associated with Foreground Galaxies on Top of Quasars
Authors: Labanya K. Guha, Raghunathan Srianand, Rajeshwari Dutta
Figure caption: DESI-LIS r-band continuum images of the GOTOQs observed with the uGMRT. The green contours represent the radio continuum flux density from uGMRT observations with a 6.25 MHz bandwidth, centered on the expected H I 21 cm absorption frequency. The outermost green contour in each panel corresponds to 10σ above the median noise level, with successive inner contours increasing by factors of 2. The blue star marks the optical centroid of the background quasar. The black contours in each panel correspond to 3σ above the median noise level, with successive inner contours increasing by factors of 2. The uGMRT synthesized beam is shown with the red ellipse at the bottom-left corner in each panel.
Paper: H I 21 cm Absorption Associated with Foreground Galaxies on Top of Quasars
Authors: Labanya K. Guha, Raghunathan Srianand, Rajeshwari Dutta
Figure caption: Estimation of the line-of-sight reddening of the background quasar caused by the foreground galaxy for the GOTOQ J0758+1136. The black spectrum is the observed spectrum of the background quasar, while the blue spectrum shows the template quasar spectrum redshifted to the redshift of the quasar. The red curve corresponds to the best-fit spectrum, obtained by applying a color excess of E(B − V) = −0.071 to the template spectrum at the redshift of the foreground galaxy. In this case, the quasar spectrum tends to be bluer than the template spectrum used. Such measurements are useful for quantifying the scatter in E(B − V) propagating from the spread in the QSO SEDs.
Paper: H I 21 cm Absorption Associated with Foreground Galaxies on Top of Quasars
Authors: Labanya K. Guha, Raghunathan Srianand, Rajeshwari Dutta
Figure caption: Same as the above figure, but for the GOTOQ J1451+0857.
Paper: H I 21 cm Absorption Associated with Foreground Galaxies on Top of Quasars
Authors: Labanya K. Guha, Raghunathan Srianand, Rajeshwari Dutta
Figure caption: Same as the above figure, but for the GOTOQ J1159+5820.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: Different possible (time-integrated) CR escape contributions for AT2019dsg (pure 56Fe injection; observer’s frame with adiabatic losses during transport only). Left panel: diffusive (direct) escape including free-streaming neutron escape; middle panel: advective escape for the optimistic case of an outflow with v = 0.5c; right panel: final release at the end of the simulated TDE evolution (after tdyn), assuming that the injection ceases and the magnetic fields decay and all leftover nonthermal CRs are released. The different colors correspond to spectra summed over different mass groups, see the legend in the right panel: H (red; A = 1), He (gray; 1 < A ≤ 4), N (green; 4 < A ≤ 14), Si (yellow; 14 < A ≤ 28), and Fe (blue, 28 < A ≤ 56), and the black curves show the total escape spectrum. Dashed curves illustrate the hypothetical spectrum if the primary 56Fe was escaping free-streamingly for comparison (which can be lower than the other curves because it represents a single isotope only).
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: Relevant interaction and energy loss rates (in the source frame) as a function of E (in the observer’s frame) for AT2019dsg and ZA = 56Fe injection. Solid curves refer to the peak time of the TDE, and dashed curves refer to the time of the neutrino emission. The dynamical rate (﹩{t}_{{\rm{dyn}}}^{-1}﹩) corresponds to the evolution of the whole system, and the free-streaming rate is R/c. The shaded region is beyond the assumed maximal injection energy.
Paper: Ultrahigh-energy Cosmic Rays from Neutrino-emitting Tidal Disruption Events
Authors: Pavlo Plotko, Walter Winter, Cecilia Lunardini, Chengchao Yuan,  成 超 袁
Figure caption: Time evolution of the diffusive UHECR escape (luminosity) for the different mass groups (same colors as in Figure 2) for AT2019dsg (left panel) and AT2019aalc (right panel). The optical-UV (black dotted curves), IR (black dashed–dotted curves), and neutrino (black dashed curves) luminosities are shown as well (νμ and ﹩{\bar{\nu }}_{\mu }﹩ including flavor mixing); the arrows mark the actual times of the neutrino arrivals. Here, pure 56Fe injection is assumed, and the UHECR luminosities are integrated in the energy range above 109 GV (observer’s frame), whereas the neutrino luminosities are integrated over the full energy range.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Hα spectra of the flare event EK3 on 2021 April 21. (a) Light curve of Hα EW (red). Typical error bars are shown in the top right and the period used to create the pre-flare template spectrum is indicated in the top left with a black arrow. The gray dashed line indicates the background level. The black arrow marks the time used to create the preflare template median spectrum. (b) Dynamic spectrum of the Hα line after subtracting the preflare spectrum. The dotted line shows the line center. (c) Time evolution of the preflare-subtracted Hα spectra, shown from top to bottom. Each spectrum is time-averaged to improve S/N. Black error bars with points show uncertainties. Red lines are fitted spectra with the Gaussian function for data with sufficient S/N. Each fitting parameter of Doppler shift and line width is indicated in the upper right of each spectrum. The above explanations are applied to Figures 1–10.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Same as Figure 1, but for the flare event EK5 on 2022 February 23. In panel (a), the black line represents the TESS light curve, which is consistently used in figures for events with available TESS data. The TESS light curve shows three potential WLFs around t ∼ 10, ∼220, and ∼380 minutes, although their significance is low compared to the noise level. The Hα data appear to exhibit corresponding peaks; however, the first and second flares do not return to the quiescent level and are instead connected. The final Hα peak at t ∼ 400 minutes falls below the flare threshold (ΔEW > 0.1). Therefore, although multiple Hα peaks are present, they are treated as a single, complex flare in this study.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Same as Figure 1, but for the flare event EK9 on 2023 March 8.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Same as Figure 1, but for the flare event EK10 on 2024 March 20.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Same as Figure 1, but for the flare event EK4 on 2021 April 30.