adsabs/AstroCLIMB huggingface dataset:
Paper: High Optical-to-X-Ray Polarization Ratio Reveals Compton Scattering in BL Lacertae’s Jet
Authors: Iván Agudo, Ioannis Liodakis, Jorge Otero-Santos, Riccardo Middei, Alan Marscher, Svetlana Jorstad, Haocheng Zhang, Hui Li, Laura Di Gesu, Roger W. Romani, Dawoon E. Kim, Francesco Fenu, Herman L. Marshall, Luigi Pacciani, Juan Escudero Pedrosa, Francisco José Aceituno, Beatriz Agís-González, Giacomo Bonnoli, Víctor Casanova, Daniel Morcuende, Vilppu Piirola, Alfredo Sota, Pouya M. Kouch, Elina Lindfors, Callum McCall, Helen E. Jermak, Iain A. Steele, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Emmanouil Angelakis, Alexander Kraus, Dmitry Blinov, Siddharth Maharana, Rumen Bachev, Jenni Jormanainen, Kari Nilsson, Vandad Fallah Ramazani, Carolina Casadio, Antonio Fuentes, Efthalia Traianou, Clemens Thum, José L. Gómez, Lucio Angelo Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Optical polarization measurements during the IXPE observation. The top panel shows the brightness in magnitudes, the middle panel the polarization degree (%), and the bottom panel the polarization angle (degrees). The gray shaded area marks the duration of the IXPE observation. The different optical bands are marked with different symbols and colors as shown in the legend. The error bars correspond to the 68% (1σ) confidence interval.
Paper: High Optical-to-X-Ray Polarization Ratio Reveals Compton Scattering in BL Lacertae’s Jet
Authors: Iván Agudo, Ioannis Liodakis, Jorge Otero-Santos, Riccardo Middei, Alan Marscher, Svetlana Jorstad, Haocheng Zhang, Hui Li, Laura Di Gesu, Roger W. Romani, Dawoon E. Kim, Francesco Fenu, Herman L. Marshall, Luigi Pacciani, Juan Escudero Pedrosa, Francisco José Aceituno, Beatriz Agís-González, Giacomo Bonnoli, Víctor Casanova, Daniel Morcuende, Vilppu Piirola, Alfredo Sota, Pouya M. Kouch, Elina Lindfors, Callum McCall, Helen E. Jermak, Iain A. Steele, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Emmanouil Angelakis, Alexander Kraus, Dmitry Blinov, Siddharth Maharana, Rumen Bachev, Jenni Jormanainen, Kari Nilsson, Vandad Fallah Ramazani, Carolina Casadio, Antonio Fuentes, Efthalia Traianou, Clemens Thum, José L. Gómez, Lucio Angelo Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Short millimeter wavelength and radio polarization measurements during the IXPE observation. The top panel shows the flux density, the middle panel the polarization degree, and the bottom panel the polarization angle. The gray shaded area marks the duration of the IXPE observation. The different radio frequencies are marked with different symbols and colors as shown in the legend. The error bars correspond to the 68% (1σ) confidence level.
Paper: Properties of “Lite” Intermediate-mass Black Hole Candidates in LIGO-Virgo’s Third Observing Run
Authors: Krystal Ruiz-Rocha, Anjali B. Yelikar, Jacob Lange, William Gabella, Robert A. Weller, Richard O'Shaughnessy, Kelly Holley-Bockelmann, Karan Jani
Figure caption: A comparison of analyses using different waveform models (NRSur7d4q, IMRPhenomXPHM, and SEOBNRv4PHM) is displayed for each event. From left to right, we plot the detector-frame total mass (﹩{M}_{\mathrm{tot}}^{\det }﹩), the mass ratio (q), the effective aligned spin parameter (χeff), the precession spin parameter (χp), and the luminosity distance (DL). The ﹩{M}_{\mathrm{tot}}^{\det }﹩, q, and DL parameters are plotted as the natural logarithm of their respective values for visualization purposes. Note the GW190521 phenomenological model samples are from analysis using IMRPhenomPv3HM.
Paper: Properties of “Lite” Intermediate-mass Black Hole Candidates in LIGO-Virgo’s Third Observing Run
Authors: Krystal Ruiz-Rocha, Anjali B. Yelikar, Jacob Lange, William Gabella, Robert A. Weller, Richard O'Shaughnessy, Kelly Holley-Bockelmann, Karan Jani
Figure caption: Jensen–Shannon divergence (JSD) values between the one-dimensional marginalized posteriors of total mass in the detector frame (M﹩{}_{{\rm{tot}}}^{{\rm{\det }}}﹩), mass ratio (q), the effective aligned spin parameter (χeff), and effective precession spin parameter (χp). The dashed lines correspond to a JSD value of 0.02 bits (red) and 0.15 bits (green), respectively, which is a conventional value above which differences between posteriors are assumed to be significant. Note the GW190521 phenomenological model samples are from the analysis using IMRPhenomPv3HM.
Paper: Properties of “Lite” Intermediate-mass Black Hole Candidates in LIGO-Virgo’s Third Observing Run
Authors: Krystal Ruiz-Rocha, Anjali B. Yelikar, Jacob Lange, William Gabella, Robert A. Weller, Richard O'Shaughnessy, Kelly Holley-Bockelmann, Karan Jani
Figure caption: Left: posterior distribution of the chirp mass of the binary in the source frame as a function of the inferred effective inspiral spin parameter. Right: posterior distributions of the mass and the dimensionless spin of the remnant black hole according to the RIFT inference using the NRSur7dq4 model. The two-dimensional plot for both panels shows the 90% credible regions of inference using RIFT with the NRSur7dq4 model. The thick grey and filled black posteriors represent the LVK posterior distributions for GW170502 and GW190521, respectively, with the NRSur7dq4 waveform model.
Paper: Properties of “Lite” Intermediate-mass Black Hole Candidates in LIGO-Virgo’s Third Observing Run
Authors: Krystal Ruiz-Rocha, Anjali B. Yelikar, Jacob Lange, William Gabella, Robert A. Weller, Richard O'Shaughnessy, Kelly Holley-Bockelmann, Karan Jani
Figure caption: Heat map showing the probabilities that the primary and secondary objects lie in the PISN mass-gap region of [60, 120] M⊙ (first and second rows), the probability that the primary is heavier than 120 M⊙ (third row), and the probability that the final remnant is in the IMBH mass region (≥100 M⊙; last row). The numbers in the individual rectangles denote the respective probabilities in percentages. The color bar shows the color scale of probabilities in percentages.
Paper: Properties of “Lite” Intermediate-mass Black Hole Candidates in LIGO-Virgo’s Third Observing Run
Authors: Krystal Ruiz-Rocha, Anjali B. Yelikar, Jacob Lange, William Gabella, Robert A. Weller, Richard O'Shaughnessy, Kelly Holley-Bockelmann, Karan Jani
Figure caption: Marginal probability distribution of the primary (left) and secondary (right) black holes in the source frame, as inferred through RIFT with the NRSur7dq4 model. The gray and filled black posteriors are for GW170502 and GW190521, respectively, with the NRSur7dq4 model. The red shaded area highlights the expected PISN mass gap from [60 to 120] M⊙.
Paper: Properties of “Lite” Intermediate-mass Black Hole Candidates in LIGO-Virgo’s Third Observing Run
Authors: Krystal Ruiz-Rocha, Anjali B. Yelikar, Jacob Lange, William Gabella, Robert A. Weller, Richard O'Shaughnessy, Kelly Holley-Bockelmann, Karan Jani
Figure caption: Marginal probability distribution of the effective precession spin parameter (χp) for the events as inferred through RIFT with the NRSur7dq4 model, compared against the prior (dashed blue) on the parameter.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: Panel (a): volume rendering of the projection of the current density onto the B field, j∥. Panel (b): xy-slice of j∥ at z = 90 c/ωp. Streamlines of the in-plane magnetic field b⊥ are in the foreground. Panel (c): fiducial SOM segmentation, color coded by the cluster identified via aweSOM. From observation and the radar charts in Figure 2, green and orange correspond to regions in between double current sheets, purple to current sheets aligned with B, and blue to current sheets antialigned with B. Blue contours are regions where j∥ > 2 j∥,rms, and red contours are regions where j∥ < −2 j∥,rms.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: Fiducial SOM representation of the plasma turbulence data with unified distance matrix (U-matrix). Each pixel in the map corresponds to a node in the lattice; the nodes are color coded by their final cluster assignment. Cluster centroids are marked with white circles. In this example, seven clusters are identified. The map is overlaid with U-matrix isocontours, visualizing the lattice-space distance between the nodes. The style of the isocontours represents the value of the U-matrix in ascending order: dotted lines, dotted–dashed lines, dashed lines, and solid lines, respectively. The radar charts visualize the relative importance of each feature of the given cluster.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: SCE result obtained by combining the output of 36 SOM realizations. The left panel shows an xy-slice plot of ΣGsum (signal strength) at z = 90 c/ωp. The right panels show SCE clusters, obtained via making thresholds in the signal strength at 0.25, 0.5, and 0.8, respectively. Red and blue contours are the same as in Figure 1(c), and denote the regions where ∣j∥∣ > 2 j∥,rms. Nominally, cluster 0 (pink) are double current sheets, cluster 1 (gray) are single current sheets aligned with B, cluster 2 (olive) are single current sheets antialigned with B, and cluster 3 (teal) are background plasma.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: Panel (a) and (c): line profiles of j∥, Bn/B0, Bp1/B0, and E · J along the line segment ﹩\overline{AB}﹩. Each inset plot is an xy-slice of j∥ centered on the sheet of interest. Panel (b) and (d): volume rendering of B field lines, interlaced with xy-slices of jz. On the left is an example of a single current sheet; on the right is an example of a double current sheet.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: Similar to panel (c) of Figure 1, but with adjacent clusters 0, 1, 2, and 4 merged into cluster 1. Cluster 1 denotes double current sheets, clusters 4 and 0 denote single current sheets that align with B and antialign with B, respectively.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: Scatterplots of SOM clusters (in the background; similar to Figure 6) and projections of the SOM lattice (in the foreground), where each square is a node, and the stars are locations of the centroids of each cluster. The gray lines represent connected nodes along the X-axis in Figure 2. The two black curves show the horizontal boundaries of the map with Y = 0 and Y = 36.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: Feature-to-feature scatterplots of SOM clusters from Figure 2. For clarity, cluster 6 has been excluded, and a random sample of 105 points (∼5% L3) is drawn for each plot. Each data point is color coded by its assigned cluster label.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: xy-slice of j∥ (top) vs. aweSOM clustering result (bottom) at z = 120 c/ωp. Streamlines in the top panel show the in-plane magnetic field, Bxy. Red and blue contours in the bottom panel show locations where j∥ < −3 j∥,rms, and where j∥ < −3 j∥,rms, respectively. The colors of the clusters have the same physical meaning as in Figure 3.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: xy-slice of current density along z-axis (Jz, top) vs. aweSOM clustering result (bottom) at z = −40 c/ωp for the Harris current sheet simulation. Streamlines in the top panel show in-plane magnetic field lines. Contours in both panels show regions where Jz > 2Jrms, representing the boundary of the Harris current sheet.
Paper: Machine Learning Characterization of Intermittency in Relativistic Pair Plasma Turbulence: Single and Double Sheet Structures
Authors: Trung Ha, Joonas Nättilä, Jordy Davelaar, Lorenzo Sironi
Figure caption: Histograms of each feature used in training, separated by clusters from Figure 2. For clarity, cluster 6 has been omitted.
Paper: Escaping Helium and a Highly Muted Spectrum Suggest a Metal-enriched Atmosphere on Sub-Neptune GJ 3090 b from JWST Transit Spectroscopy
Authors: Eva-Maria Ahrer, Michael Radica, Caroline Piaulet-Ghorayeb, Eshan Raul, Lindsey Wiser, Luis Welbanks, Lorena Acuña, Romain Allart, Louis-Philippe Coulombe, Amy Louca, Ryan MacDonald, Morgan Saidel, Thomas M. Evans-Soma, Björn Benneke, Duncan Christie, Thomas G. Beatty, Charles Cadieux, Ryan Cloutier, René Doyon, Jonathan J. Fortney, Anna Gagnebin, Cyril Gapp, Hamish Innes, Heather A. Knutson, Thaddeus Komacek, Joshua Krissansen-Totton, Yamila Miguel, Raymond Pierrehumbert, Pierre-Alexis Roy, Hilke E. Schlichting
Figure caption: Results of the joint white light-curve fitting. In each of the six panels, the first row shows the raw white light curve in blue, with the best-fitting model overplotted in black. The second row shows the systematics-corrected white light curve, with the best-fitting astrophysics model in black. The third row shows the fit residuals, and the bottom row shows the histogram of the residuals. In the outer grid, the first column of panels corresponds to the first visit with each instrument and the second column to the second visit. The first row of panels shows the order 1 white light curves from NIRISS/SOSS. Note that NIRISS/SOSS order 2 is left out in this figure as it is much noisier compared to order 1 but shows similar systematics. The second and third rows are the NIRSpec/G395H white light curves for the NRS1 and NRS2 detectors, respectively. Note that integrations around the flare have been masked in both detectors of the second NIRSpec visit, and the first 1000 integrations of NIRSpec visit 1 are cut to remove large amounts of correlated noise. The raw, uncut NIRSpec light curves are shown in Figure E1.
Paper: Escaping Helium and a Highly Muted Spectrum Suggest a Metal-enriched Atmosphere on Sub-Neptune GJ 3090 b from JWST Transit Spectroscopy
Authors: Eva-Maria Ahrer, Michael Radica, Caroline Piaulet-Ghorayeb, Eshan Raul, Lindsey Wiser, Luis Welbanks, Lorena Acuña, Romain Allart, Louis-Philippe Coulombe, Amy Louca, Ryan MacDonald, Morgan Saidel, Thomas M. Evans-Soma, Björn Benneke, Duncan Christie, Thomas G. Beatty, Charles Cadieux, Ryan Cloutier, René Doyon, Jonathan J. Fortney, Anna Gagnebin, Cyril Gapp, Hamish Innes, Heather A. Knutson, Thaddeus Komacek, Joshua Krissansen-Totton, Yamila Miguel, Raymond Pierrehumbert, Pierre-Alexis Roy, Hilke E. Schlichting
Figure caption: GJ 3090 b in context with the population of sub-Neptune planets in equilibrium temperature vs. planet radius space. Markers are colored by the effective temperature of the stellar host, and marker sizes reflect the planet mass. The background shading represents the distribution of sub-Neptune planets from B. J. Fulton et al. (2017), highlighting the radius valley near 1.7 R⊕. Planets with published JWST near-infrared atmosphere spectra are outlined in black and labeled. Planets that will have JWST atmosphere observations by the end of Cycle 3 are outlined in gray.
Paper: Escaping Helium and a Highly Muted Spectrum Suggest a Metal-enriched Atmosphere on Sub-Neptune GJ 3090 b from JWST Transit Spectroscopy
Authors: Eva-Maria Ahrer, Michael Radica, Caroline Piaulet-Ghorayeb, Eshan Raul, Lindsey Wiser, Luis Welbanks, Lorena Acuña, Romain Allart, Louis-Philippe Coulombe, Amy Louca, Ryan MacDonald, Morgan Saidel, Thomas M. Evans-Soma, Björn Benneke, Duncan Christie, Thomas G. Beatty, Charles Cadieux, Ryan Cloutier, René Doyon, Jonathan J. Fortney, Anna Gagnebin, Cyril Gapp, Hamish Innes, Heather A. Knutson, Thaddeus Komacek, Joshua Krissansen-Totton, Yamila Miguel, Raymond Pierrehumbert, Pierre-Alexis Roy, Hilke E. Schlichting
Figure caption: Results from the stctm stellar contamination retrievals and SCARLET joint retrieval of the atmosphere and stellar contamination components for retrievals performed on individual or both NIRISS/SOSS spectra of GJ 3090 b. Left panels: measured transmission spectrum (black data points) for the first (top panel) and the second (bottom panel) NIRISS/SOSS transits, along with the best-fitting model (black line) and sample spectra from the posterior distribution (semitransparent colored lines) from the individual atmosphere + TLS retrievals. We performed the retrievals on the R = 100 exoTEDRF spectra (gray points), also shown binned by a factor of 4 (black points) on the figure for visualization purposes. For the visit 1 (2) spectrum, the best-fit order 2 offset of −14.4 (+94.4) ppm was applied on the data points displayed. Right panels: marginalized posterior distributions on the stellar heterogeneity properties for the first (top) and second NIRISS/SOSS (bottom) visits. We show the results from SCARLET retrievals performed on individual visits (visit 1 in blue, visit 2 in pink) and on both visits assuming a shared atmosphere component but different stellar heterogeneity components (in purple). We also display the posterior distributions from the stctm retrievals to individual visits (green), which only accounts for the impact of the TLS effect on the observations (see Appendix C.2) The inferred heterogeneity properties are different for each visit, as evidenced by the difference in the blueward slope observed in the transmission spectrum. For visit 1, where stellar contamination is not confidently detected (see text), the joint fit to both visits only provides an upper limit on the spot covering fraction and a lower limit on the spot temperature.