adsabs/AstroCLIMB huggingface dataset:
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: The 100 mK focal plane configuration inside the LATR-Tester optics tube (back view). In this testing configuration, the three nominal detector array positions of the optics tube focal plane are occupied by one detector array, a high-G single-pixel box, and a radio holography receiver.
Paper: Kinematics of Young Stellar Objects under Various Stellar Feedback
Authors: Longhui Yang, Dejian Liu, Chaojie Hao, Zehao Lin, YingJie Li, Yiwei Dong, Zu-Jia Lu, En-Wei Liang, Y. Xu
Figure caption: Parallax distributions and criteria applied to the YSOs in the λ Orionis. The other features are the same as in Figure B1.
Paper: Introducing the Condor Array Telescope. V. Deep Broad- and Narrowband Imaging Observations of the M81 Group
Authors: Kenneth M. Lanzetta, Stefan Gromoll, Michael M. Shara, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Schematic depiction of ionized gas in direction of the M81 Group. Known galaxies of the M81 Group are shown as shaded light-green circles or ovals), clouds of gas are shown as shaded light-blue circles, ovals, or irregular shapes, filamentary (or essentially one-dimensional) structures are shown as pink curves or shaded pink shapes, and apparent or possible bubbles or shells are shown as open yellow circles. Known stars and known galaxies not of the M81 Group are not indicated. Letter designations are positioned to the lower right of corresponding features unless otherwise noted by arrow. The figure is not intended to definitively or exhaustively catalog ionized gas in direction of the M81 Group but rather is intended only to introduce shapes, sizes, and locations of some of extended structures of ionized gas in direction of M81 in order that these structures can be referred to subsequently.
Paper: Introducing the Condor Array Telescope. V. Deep Broad- and Narrowband Imaging Observations of the M81 Group
Authors: Kenneth M. Lanzetta, Stefan Gromoll, Michael M. Shara, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Mosaic-difference image of the M81 Group obtained through [O III] filter formed by subtracting the luminance image from the [O III] image and masking known stars. The image is displayed block averaged by 32 × 32 pixels.
Paper: Introducing the Condor Array Telescope. V. Deep Broad- and Narrowband Imaging Observations of the M81 Group
Authors: Kenneth M. Lanzetta, Stefan Gromoll, Michael M. Shara, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Mosaic-difference image of the M81 Group obtained through [S II] filter formed by subtracting the luminance image from the [S II] image and masking known stars. The image is displayed block averaged by 32 × 32 pixels.
Paper: Introducing the Condor Array Telescope. V. Deep Broad- and Narrowband Imaging Observations of the M81 Group
Authors: Kenneth M. Lanzetta, Stefan Gromoll, Michael M. Shara, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Mosaic image of the M81 Group obtained through the Hα filter. The image is displayed block averaged by 32 × 32 pixels.
Paper: Introducing the Condor Array Telescope. V. Deep Broad- and Narrowband Imaging Observations of the M81 Group
Authors: Kenneth M. Lanzetta, Stefan Gromoll, Michael M. Shara, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Comparison of measurements of bolometric energy fluxes of Hα plus [N II] 658.4 nm emission lines of ≈500 H II regions in outskirts of M81 between long-slit spectroscopy obtained by W. Lin et al. (2003) (horizontal axis) and images obtained by Condor (vertical axis). The line segment shows equal energy fluxes.
Paper: Introducing the Condor Array Telescope. V. Deep Broad- and Narrowband Imaging Observations of the M81 Group
Authors: Kenneth M. Lanzetta, Stefan Gromoll, Michael M. Shara, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Mosaic-difference image of the M81 Group obtained through [N II] filter formed by subtracting the luminance image from the [N II] image and masking known stars. The image is displayed block averaged by 32 × 32 pixels.
Paper: Introducing the Condor Array Telescope. V. Deep Broad- and Narrowband Imaging Observations of the M81 Group
Authors: Kenneth M. Lanzetta, Stefan Gromoll, Michael M. Shara, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Mosaic-difference image of the M81 Group obtained through the Hα filter formed by subtracting the luminance image from the Hα image and masking known stars. The image is displayed block averaged by 32 × 32 pixels.
Paper: Identification of 4876 Bent-tail Radio Galaxies in the FIRST Survey Using Deep Learning Combined with Visual Inspection
Authors: Baoqiang Lao, Heinz Andernach, Xiaolong Yang, Xiang Zhang, Rushuang Zhao, Zhen Zhao, Yun Yu, Xiaohui Sun, Sheng-Li Qin
Figure caption: g–r color vs. absolute r-band magnitude (Mr) for the BTRGs hosts. The blue dashed line represents the relation from S. M. Weinmann et al. (2006) that separates the galaxies into red and blue ones.
Paper: Identification of 4876 Bent-tail Radio Galaxies in the FIRST Survey Using Deep Learning Combined with Visual Inspection
Authors: Baoqiang Lao, Heinz Andernach, Xiaolong Yang, Xiang Zhang, Rushuang Zhao, Zhen Zhao, Yun Yu, Xiaohui Sun, Sheng-Li Qin
Figure caption: Mass vs. redshift distribution of associated clusters. The red and blue lines correspond to the values of M500 = 0.32 × 1014M⊙ and M500 = 1014.5M⊙, respectively. Only the values of M500 provided in Table 2 are shown.
Paper: Identification of 4876 Bent-tail Radio Galaxies in the FIRST Survey Using Deep Learning Combined with Visual Inspection
Authors: Baoqiang Lao, Heinz Andernach, Xiaolong Yang, Xiang Zhang, Rushuang Zhao, Zhen Zhao, Yun Yu, Xiaohui Sun, Sheng-Li Qin
Figure caption: Distributions of the absolute r-band magnitude (Mr) (left panel), and mass of the black hole (MBH) (right panel).
Paper: Identification of 4876 Bent-tail Radio Galaxies in the FIRST Survey Using Deep Learning Combined with Visual Inspection
Authors: Baoqiang Lao, Heinz Andernach, Xiaolong Yang, Xiang Zhang, Rushuang Zhao, Zhen Zhao, Yun Yu, Xiaohui Sun, Sheng-Li Qin
Figure caption: The distribution of OA for all BTRG candidates.
Paper: Multispacecraft Measurements of the Evolving Geometry of the Solar Alfvén Surface over Half a Solar Cycle
Authors: Samuel T. Badman, Michael L. Stevens, Stuart D. Bale, Yeimy J. Rivera, Kristopher G. Klein, Tatiana Niembro, Rohit Chhiber, Ali Rahmati, Phyllis L. Whittlesey, Roberto Livi, Davin E. Larson, Christopher J. Owen, Kristoff W. Paulson, Timothy S. Horbury, Jean Morris, Helen O'Brien, Jean-Baptiste Dakeyo, Jaye L. Verniero, Mihailo Martinovic, Marc Pulupa, Federico Fraschetti
Figure caption: Distribution of heights vs. the solar cycle. The main (bottom) panel shows the distribution of Alfvén surface heights oriented vertically with means indicated by short horizontal bars and colorized as in Figure 3 (black, L1; blue, Solar Orbiter; red, Parker missions) and plotted as a function of time with one distribution per Parker encounter. The top panel shows the monthly smoothed number of sunspots (in red, from the World Data Center SILSO, Royal Observatory of Belgium, Brussels ( F. Clette &  L. Lefèvre 2015)) and CMEs (in blue, from the SOHO/LASCO CME catalog) plotted on the same x-axis. A second y-axis on the right of the main panel computes ﹩{R}_{{\rm{A}}}^{2}{{\rm{\Omega }}}_{\odot }﹩, a figure of merit for angular momentum loss (per unit mass loss; see E. J. Weber & L. Davis 1967).
Paper: Multispacecraft Measurements of the Evolving Geometry of the Solar Alfvén Surface over Half a Solar Cycle
Authors: Samuel T. Badman, Michael L. Stevens, Stuart D. Bale, Yeimy J. Rivera, Kristopher G. Klein, Tatiana Niembro, Rohit Chhiber, Ali Rahmati, Phyllis L. Whittlesey, Roberto Livi, Davin E. Larson, Christopher J. Owen, Kristoff W. Paulson, Timothy S. Horbury, Jean Morris, Helen O'Brien, Jean-Baptiste Dakeyo, Jaye L. Verniero, Mihailo Martinovic, Marc Pulupa, Federico Fraschetti
Figure caption: The shape of the solar Alfvén surface 2018–2025. Each panel shows the inferred 2D shape of the Sun’s Alfvén surface near the solar equatorial plane as scaled from L1 data (black), Solar Orbiter data (blue), and Parker data (red) plotted in the Carrington frame. From top left to bottom right, the plots advance chronologically by Parker encounter. The orbit of Parker in the Carrington frame is shown in each case and is colored according to whether it measured super- (magenta) or sub- (lime) Alfvénic wind.
Paper: Multispacecraft Measurements of the Evolving Geometry of the Solar Alfvén Surface over Half a Solar Cycle
Authors: Samuel T. Badman, Michael L. Stevens, Stuart D. Bale, Yeimy J. Rivera, Kristopher G. Klein, Tatiana Niembro, Rohit Chhiber, Ali Rahmati, Phyllis L. Whittlesey, Roberto Livi, Davin E. Larson, Christopher J. Owen, Kristoff W. Paulson, Timothy S. Horbury, Jean Morris, Helen O'Brien, Jean-Baptiste Dakeyo, Jaye L. Verniero, Mihailo Martinovic, Marc Pulupa, Federico Fraschetti
Figure caption: Thickness and asphericity of the Alfvén surface. As in Figure 4, the geometric properties of the Alfvén surface as a function of time are compared to the monthly smoothed number of sunspots (shown in red) and CMEs (in blue). In the middle left panel, the average “thickness” of the surface is plotted vs. time, while the bottom left panel shows the “asphericity,” both in units of solar radii and computed from different spacecraft with the same color scheme as in Figures 3 and 4. The inset on the right illustrates the meaning of these two quantities showing the encounter 1 Alfvén surface computed from L1 data. In this plot, the black noisy line is the average shape as shown in Figure 4, while the gray region is the standard deviation of computed altitudes for each longitude bin. The “thickness” is then the average of this standard deviation over all longitudes. The asphericity is defined via the mean difference between the mean shape of the surface (black noisy line) and the longitude-averaged height (black circle).
Paper: Multispacecraft Measurements of the Evolving Geometry of the Solar Alfvén Surface over Half a Solar Cycle
Authors: Samuel T. Badman, Michael L. Stevens, Stuart D. Bale, Yeimy J. Rivera, Kristopher G. Klein, Tatiana Niembro, Rohit Chhiber, Ali Rahmati, Phyllis L. Whittlesey, Roberto Livi, Davin E. Larson, Christopher J. Owen, Kristoff W. Paulson, Timothy S. Horbury, Jean Morris, Helen O'Brien, Jean-Baptiste Dakeyo, Jaye L. Verniero, Mihailo Martinovic, Marc Pulupa, Federico Fraschetti
Figure caption: Validation of the scaling method. Each panel shows the normalized ground-truth distribution of the heights of measured Alfvén surface crossings (black solid line and dots) and a Gaussian fit to this distribution (black dashed line). Each panel also includes red and cyan distributions that show the results of, respectively, the isopoly intersection method and the simpler construction RA = R/MA as computed (from left to right) from Parker data within its encounters (R < 0.25 au), Solar Orbiter from 0.28 to 1 au, and all observations at L1 over the total time period examined. A shaded blue region indicates the ranges of distances in the corona not probed by Parker, and the light gray shading indicates the narrow range of distances probed in Parker’s most recent encounters. Inset numbers show the distribution median with colors corresponding to respective distributions (black, ground-truth fit; red, Parker wind scaling; cyan, R/MA scaling.
Paper: Cospatial Multiwavelength Observations of an Eruptive Prominence as the Bright Core of a Coronal Mass Ejection
Authors: Bin Zhuang, Tingyu Gou, Noé Lugaz, Manuela Temmer, Brian E. Wood, Yara De Leo, Shaheda Begum Shaik, Phillip Hess, Carlos R. Braga, Cecilia Mac Cormack, Xiaolei Li
Figure caption: Variation of the emission intensity of the core region with height at different times as the prominence propagates upward. The X-axis also reflects a time variation from approximately 14:00 to 15:06 UT, although the sampling is not uniform because the prominence velocity changes over time and different wavelengths are observed at slightly different times. The left panel shows three subregions selected for the intensity measurement. The three right panels show the emission intensity variations of the three subregions, normalized by their respective maximum values, measured across three wavelength channels of 174 Å, 304 Å, and WL. The two solid curves show the expected emission variation with height, assuming mass conservation and constant temperature. See details in Appendix B.
Paper: Multispacecraft Measurements of the Evolving Geometry of the Solar Alfvén Surface over Half a Solar Cycle
Authors: Samuel T. Badman, Michael L. Stevens, Stuart D. Bale, Yeimy J. Rivera, Kristopher G. Klein, Tatiana Niembro, Rohit Chhiber, Ali Rahmati, Phyllis L. Whittlesey, Roberto Livi, Davin E. Larson, Christopher J. Owen, Kristoff W. Paulson, Timothy S. Horbury, Jean Morris, Helen O'Brien, Jean-Baptiste Dakeyo, Jaye L. Verniero, Mihailo Martinovic, Marc Pulupa, Federico Fraschetti
Figure caption: Illustration of the scaling intersection method. Left panel: 2D column-normalized histogram of VA and VSW observations at L1 with mean (blue), standard deviations (blue bars), and a fit to the mean (black) showing a clear monotonic relationship. Right panel: “isopoly” VSW and VA profiles (see Appendix B) colored by asymptotic wind speed reflecting the systematic relationship at 1 au from the left panel and their intersections and ranges in VR–R space. The propagated standard deviation of the intersection along each speed profile is indicated with black bars. In this work, we estimate the Alfvén surface height and critical speed with these types of intersections with the specific VSW and VA curve selected by the nearest neighbors for a given measurement (R, VSW, VA).
Paper: Multispacecraft Measurements of the Evolving Geometry of the Solar Alfvén Surface over Half a Solar Cycle
Authors: Samuel T. Badman, Michael L. Stevens, Stuart D. Bale, Yeimy J. Rivera, Kristopher G. Klein, Tatiana Niembro, Rohit Chhiber, Ali Rahmati, Phyllis L. Whittlesey, Roberto Livi, Davin E. Larson, Christopher J. Owen, Kristoff W. Paulson, Timothy S. Horbury, Jean Morris, Helen O'Brien, Jean-Baptiste Dakeyo, Jaye L. Verniero, Mihailo Martinovic, Marc Pulupa, Federico Fraschetti
Figure caption: Data set coverage for producing VSW and VA estimates. For each instrument whose data are used in this work, a colored horizontal bar is shown, with gaps where no data are available. The color scheme differentiates Parker, Solar Orbiter, and L1-based measurements as in Figures 3– 5. For each spacecraft/location, a summation bar at the top indicates overall coverage for both VSW and VA. An inset panel indicates the solar cycle comparison, and vertical bars and labels indicate the time stamps of each Parker perihelion.
Paper: Cospatial Multiwavelength Observations of an Eruptive Prominence as the Bright Core of a Coronal Mass Ejection
Authors: Bin Zhuang, Tingyu Gou, Noé Lugaz, Manuela Temmer, Brian E. Wood, Yara De Leo, Shaheda Begum Shaik, Phillip Hess, Carlos R. Braga, Cecilia Mac Cormack, Xiaolei Li
Figure caption: Scaling process for SolO/EUI-FSI images. The left panels show the variation of the brightness (in arbitrary units) along with heliocentric distance in 174 Å (top) and 304 Å (bottom), respectively. The dashed and dotted lines indicate the fitted results. See the detailed scaling process in the text. The right panels show the original (left) and scaled (right) images in 174 Å (top) and 304 Å (bottom), respectively.
Paper: The First Radio View of a Type Ibn Supernova in SN 2023fyq: Understanding the Mass-loss History in the Last Decade before the Explosion
Authors: Raphael Baer-Way, Nayana A. J., Wynn Jacobson-Galán, Poonam Chandra, Maryam Modjaz, Samantha C. Wu, Daichi Tsuna, Raffaella Margutti, Ryan Chornock, Craig Pellegrino, Yize Dong, Maria R. Drout, Charles D. Kilpatrick, Dan Milisavljevic, Daniel Patnaude, Candice Stauffer
Figure caption: The mass-loss picture of SN 2023fyq that we derive based on our radio modeling. Left: derived effective mass-loss rate as a function of days after explosion, as well as years before explosion, assuming the observed CSM speed of 1700 km s−1. We denote the period over which optical precursor emission (at signal-to-noise ratio > 3) was detected (S. J. Brennan et al. 2024), to illustrate how the precursor outbursts may have been creating the CSM we observe in the radio. No precursor data could be obtained beyond 7 yr before the explosion, since the Zwicky Transient Facility/ATLAS surveys had not started then. Right: CSM density associated with the mass-loss rate as a function of the CSM radius. We also show r−3 and r−2 density profiles, along with profiles from merger simulations by D. Tsuna et al. (2024). Our data suggest enhanced mass loss, with a sudden drop between 5 and 8 yr before the explosion revealed by our upper limit. We emphasize that some jump in density, potentially due to shock breakout, would be needed to consistently explain our data points and the early data point from Y. Dong et al. (2024) in the r−2 case. Our last 3σ upper limits are consistent with the D. Tsuna et al. (2024) density profile extrapolation, given that this profile assumes that the mass loss starts directly at 4 yr before the explosion (for our assumed CSM speed).
Paper: The First Radio View of a Type Ibn Supernova in SN 2023fyq: Understanding the Mass-loss History in the Last Decade before the Explosion
Authors: Raphael Baer-Way, Nayana A. J., Wynn Jacobson-Galán, Poonam Chandra, Maryam Modjaz, Samantha C. Wu, Daichi Tsuna, Raffaella Margutti, Ryan Chornock, Craig Pellegrino, Yize Dong, Maria R. Drout, Charles D. Kilpatrick, Dan Milisavljevic, Daniel Patnaude, Candice Stauffer
Figure caption: Radio SEDs of SN 2023fyq at Δt ≈ 58–525 days. The downward triangles represent 3σ flux density upper limits. The solid black lines denote the overall SSA+ external FFA model we derive self-consistently (see Section 3.1). The solid green lines denote the intrinsic SSA model using the calculated Fp/νp from Equation (5). The values of the best-fit parameters are displayed in Table 2. We also show the extrapolated models with dashed black and green lines at Δt ≈ 525 days with the flux density upper limits, to emphasize the discrepancy between the models and the nondetections, indicating a decrease in the mass-loss rate at ∼ 5–10 yr before the explosion.
Paper: The First Radio View of a Type Ibn Supernova in SN 2023fyq: Understanding the Mass-loss History in the Last Decade before the Explosion
Authors: Raphael Baer-Way, Nayana A. J., Wynn Jacobson-Galán, Poonam Chandra, Maryam Modjaz, Samantha C. Wu, Daichi Tsuna, Raffaella Margutti, Ryan Chornock, Craig Pellegrino, Yize Dong, Maria R. Drout, Charles D. Kilpatrick, Dan Milisavljevic, Daniel Patnaude, Candice Stauffer
Figure caption: The unabsorbed X-ray light curves of the detected SNe Ibn, along with the nondetections of SN 2023fyq. The Swift data on SN 2006jc, SN 2010al, and SN 2022ablq are from S. Immler et al. (2008), E. O. Ofek et al. (2013), and C. Pellegrino et al. (2024). The downward triangles represent 3σ upper limits from Chandra and Swift for SN 2023fyq. Deeper, earlier observations will be vital to constrain the subclass better at X-ray wavelengths.
Paper: The First Radio View of a Type Ibn Supernova in SN 2023fyq: Understanding the Mass-loss History in the Last Decade before the Explosion
Authors: Raphael Baer-Way, Nayana A. J., Wynn Jacobson-Galán, Poonam Chandra, Maryam Modjaz, Samantha C. Wu, Daichi Tsuna, Raffaella Margutti, Ryan Chornock, Craig Pellegrino, Yize Dong, Maria R. Drout, Charles D. Kilpatrick, Dan Milisavljevic, Daniel Patnaude, Candice Stauffer
Figure caption: The peak spectral luminosity versus peak time for SN 2023fyq (taken at 10 GHz) in context with a variety of other radio-detected SNe (A. J. Nayana et al. 2025, and references therein). The speeds noted on the diagonal lines are the shock velocities for pure SSA. 2023fyq is distinct from most other stripped-envelope SNe, likely due to a denser CSM, but it does not reach the peak spectral luminosity of many SNe IIn.
Paper: The First Radio View of a Type Ibn Supernova in SN 2023fyq: Understanding the Mass-loss History in the Last Decade before the Explosion
Authors: Raphael Baer-Way, Nayana A. J., Wynn Jacobson-Galán, Poonam Chandra, Maryam Modjaz, Samantha C. Wu, Daichi Tsuna, Raffaella Margutti, Ryan Chornock, Craig Pellegrino, Yize Dong, Maria R. Drout, Charles D. Kilpatrick, Dan Milisavljevic, Daniel Patnaude, Candice Stauffer
Figure caption: Radio SEDs of SN 2023fyq at VLA frequencies (3–35 GHz) spanning 58–525 days post-explosion. We show the best-fit extrapolated single-epoch FFA models for each epoch, as described in Section 3. The downward-facing triangles denote 3σ flux density upper limits. The parameters for these fits are in Table 2.
Paper: Pan-STARRS Follow-up of the Gravitational-wave Event S250818k and the Light Curve of SN2025ulz
Authors: J. H. Gillanders, M. E. Huber, M. Nicholl, S. J. Smartt, K. W. Smith, K. C. Chambers, D. R. Young, J. W. Tweddle, S. Srivastav, M. D. Fulton, F. Stoppa, G. S. H. Paek, A. Aamer, M. R. Alarcon, A. Andersson, A. Aryan, K. Auchettl, T.-W. Chen, T. de Boer, A. K. H. Kong, J. Licandro, T. Lowe, D. Magill, E. A. Magnier, P. Minguez, T. Moore, G. Pignata, A. Rest, M. Serra-Ricart, B. J. Shappee, I. A. Smith, M. A. Tucker, R. Wainscoat
Figure caption: Results of our Prospector fit to the broadband SED of the host galaxy of SN2025ulz. The main panel presents the posterior distributions for key stellar population parameters, including the surviving stellar mass (M* [M⊙]), mass-weighted age (tMWA [Gyr]), star formation timescale (τ [Gyr]), metallicity (Z [Z⊙]), dust attenuation (AV [AB mag]), and both average star formation rate (SFR100 [M⊙ yr−1]) and specific star formation rate (sSFR100 [yr−1]) over the past 100 Myr. The contours correspond to 1σ, 2σ, and 3σ confidence intervals, and the quoted values represent the median values and 1σ uncertainties. The inset panel shows the observed photometry (blue points), the maximum a posteriori (MAP) model photometry (orange squares), and the best-fitting model SED (red curve) with 1σ confidence interval (shaded). Residuals relative to the MAP model are also shown.