adsabs/AstroCLIMB huggingface dataset:
Paper: High-resolution Observations of a C9.3 White-light Flare and Its Impact on the Solar Photosphere
Authors: Zhe Xu, Xiaoli Yan, Zhentong Li, Liheng Yang, Zhike Xue, Jincheng Wang, Yian Zhou
Figure caption: Panels (a)–(d): NVST TiO images and HMI LOS magnetograms depicting the photospheric evolution leading up to the flare. The red and blue circles mark the spots P and N, which exhibited significant shearing motion. The contour levels in panels (c) and (d) represent the magnetic field strengths of ±200, 500, and 800 G. Panels (e)–(h): NVST Hα images showing the chromospheric evolution toward the flare. The green dotted circle in panels (d) and (f) highlights the magnetic cancellation region. The orange and cyan contours in panel (h) outline the flare kernels observed in the chromosphere and photosphere, respectively. Panel (i)–(l): AIA 304 Å images with a larger field of view, showing the solar jet associated with the flare.
Paper: High-resolution Observations of a C9.3 White-light Flare and Its Impact on the Solar Photosphere
Authors: Zhe Xu, Xiaoli Yan, Zhentong Li, Liheng Yang, Zhike Xue, Jincheng Wang, Yian Zhou
Figure caption: Panels (a) and (b): CHASE continuum image and the Fe I line profiles in the white-light flare region (marked by the black circle). The red, blue, and green cross symbols represent the Fe I line profiles during, before, and after the flare. The corresponding solid curves are the Gaussian fits of the line profiles combined with a linear term. For reference, the black dotted curve shows the Fe I line profile in a nonflaring region. Panels (c) and (d): CHASE Hα image and its line profiles (colored cross symbol) in the white-light flare region. The colored solid curves represent the contrast profiles relative to the reference Hα line profile (black dotted line) from a nonflaring region. The vertical dashed lines in panels (b) and (d) indicate the line centers of the Fe I and Hα lines, respectively.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: Wind observations of the probability density variations of temperature anisotropy vs. parallel plasma beta in different solar wind streams. Panels (a)–(c) show the variations in all solar wind, FSW, and SSW, respectively. Panels (c1)–(c3) present the variations in low-Alfvénicity slow wind (∣σC∣ < 0.25), intermediate-Alfvénicity slow wind (0.35 ≤ ∣σC∣ ≤ 0.65), and high-Alfvénicity slow wind (∣σC∣ > 0.75). The purple, cyan, blue, and red dashed lines in each panel indicate the mirror, ion-cyclotron, parallel firehose, and oblique firehose instabilities, respectively. The black dotted line represents the anticorrelation between temperature anisotropy and parallel plasma beta given by Equation 3. In each panel, the contours indicate 50% and 75% measurement levels. In panels (c2) and (c3), the shaded contours of other types of solar wind are overlapped for comparison, as indicated by the legend.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: Absolute cross-helicity variations at different heliocentric distances. The upper panels show the absolute cross-helicity ∣σC∣ variations with solar wind speed Vp. The blue histogram lines indicate the ratio of high-Alfvénicity (∣σC∣ > 0.75) solar wind at each speed bin. The lower panels show the cross-helicity σC variations with residual energy σR. The color in each grid indicates the occurrence ratio of measurements that is normalized by the maximum number of measurements in all grids.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: Sunspot number and spacecraft data coverage. The monthly mean (blue line) and 13 month smoothed monthly (red line) total sunspot number data are from the SILSO World Data Center (1970–2024). The color bands mark the time coverage for the shown missions, and the vertical dashed lines indicate the time range of selected data in this study.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: Wind observations of helium abundance features in different solar wind streams. Panels (a)–(c) compare the helium abundance (AHe) variations with solar wind speed in all solar wind, FSW, and SSW, respectively. Panels (d)–(f) present AHe in SSW with low, intermediate, and high Alfvénicities. The overplotted color line in each panel indicates the average AHe for each speed bin. In panels (e)–(f), the average AHe of slow wind with other Alfvénicities are overplotted for comparison, as indicated by the legend. The colors represent the probability density of AHe within each bin. Panels (g)–(i) display the occurrence ratio of AHe in the three types of SSW, and the AHe of FSW is overplotted with a red dashed line for comparison.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: PSP observations of the helium abundance occurrence ratio in different solar wind streams. Panels (a)–(c) compare the AHe variations in all SSW with low, intermediate, and high Alfvénicities, respectively. Panels (d)–(f) and (g)–(i) present the AHe distributions in super-Alfvénic and sub-Alfvénic SSW with low, intermediate, and high Alfvénicities, respectively. In each panel, the red dashed line represents the AHe of FSW.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: PSP observations of the probability density variations of temperature anisotropy vs. parallel plasma beta in different solar wind streams. The format is the same as in Figure 3, except for the dotted–dashed line representing a newly fitted anticorrelation. We further use a slightly stricter criterion to select low-Alfvénicity (i.e., ∣σC∣ < 0.20) and high-Alfvénicity (i.e., ∣σC∣ > 0.80) SSW.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: PSP observations of the probability density variations of temperature anisotropy vs. parallel plasma beta in different solar wind streams. Panels (a)–(c) compare the temperature anisotropy variations in all SSW, super-Alfvénic SSW, and sub-Alfvénic SSW, respectively. Panels (d)–(f) and (g)–(i) present their distributions in super-Alfvénic and sub-Alfvénic SSW with low, intermediate, and high Alfvénicities, respectively. The lines in each panel are indicated by the legend and are the same as those in Figure 5.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: Helios observations of the probability density variations of temperature anisotropy vs. parallel plasma beta in different solar wind streams. The format is the same as in Figure 3.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: Comparison of temperature anisotropy, helium abundance, and Alfvénicity between FSW and HASSW at different heliocentric distances. Panels (a1)–(e1) show the distributions in the FSW at distances below 0.25 au, from 0.3 to 0.5 au, from 0.5 to 0.7 au, from 0.7 to 0.9 au, and at around 1 au, respectively, whereas panels (a2)–(e2) present the same distributions in HASSW. The color in each panel represents the median Alfvénicity in each bin. The blue contours in the top panels indicate the 50% and 75% measurement levels of fast wind, which are correspondingly overplotted with blue shaded contours in the bottom panels for comparison. The red contours in the bottom panels indicate the 50% and 75% measurement levels of HASSW.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: Helios observations of helium abundance features in different solar wind streams. The format is the same as in Figure 6.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: PSP observations of helium abundance features in different solar wind streams. The format is the same as in Figure 6.
Paper: The Temperature Anisotropy and Helium Abundance Features of Alfvénic Slow Solar Wind Observed by Parker Solar Probe, Helios, and Wind Missions
Authors: Jia Huang, Davin E. Larson, Tamar Ervin, Mingzhe Liu, Oscar Ortiz, Mihailo M. Martinović, Zhenguang Huang, Alexandros Chasapis, Xiangning Chu, B. L. Alterman, Zesen Huang, Wenwen Wei, J. L. Verniero, Lan K. Jian, Adam Szabo, Orlando Romeo, Ali Rahmati, Roberto Livi, Phyllis Whittlesey, Samer T. Alnussirat, Justin C. Kasper, Michael Stevens, Stuart D. Bale
Figure caption: PSP observations of absolute cross-helicity variations in different solar wind streams. The format is the same as in Figure 2. From left to right, the panels present the variations in all solar wind, super-Alfvénic solar wind, and sub-Alfvénic solar wind observed by PSP.
Paper: A Dormant Captured Oort Cloud Comet Awakens: (18916) 2000 OG44
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, Dmitrii E. Vavilov, William A. Burris
Figure caption: 2000 OG44 metrics from UT 1999 January 1 to UT 2032 January 1, with UT 2025 April 1 indicated by a vertical dashed red line. The green line indicates the apparent V-band magnitude (via JPL Horizons). “Observability” is the number of hours 2000 OG44 was above the horizon for the indicated observatory site, in this case 807 (CTIO, Chile) and G37 (Lowell Discovery Telescope near Happy Jack, Arizona), selected as representative examples for the southern and northern hemisphere sites, respectively. Solar oppositions and conjunctions can be identified here as corresponding coincident peaks and troughs in observability and apparent magnitude. The modeled temperatures are bound by the thermophysical extremes: χ = 1 (solid line), the “flat slab” case, and χ = 4 (dashed line), the isothermal approximation. 2000 OG44 has a reported period of ∼22 days, thus temperatures are more likely to be near the χ = 1 line.
Paper: A Dormant Captured Oort Cloud Comet Awakens: (18916) 2000 OG44
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, Dmitrii E. Vavilov, William A. Burris
Figure caption: (18916) 2000 OG44 is centered in these 126″ × 126″ images, with north up and east left. A tail is seen oriented toward the coincident antisolar (yellow arrow) and antimotion (red outlined black arrow) directions as projected on the sky in panels (a) and (b), both comprised of VR-band images acquired with the APO ARCTIC instrument on the 3.5 m ARC telescope in Sunspot, New Mexico. Panels (c)–(h) do not show evidence of activity, likely due to the cessation of activity on 2000 OG44. (a) UT 2023 July 24 σ-clipped coaddition of 18 ARCTIC exposures (3 × 90 s VR band, plus 2 × 60 s + 3 × 45 s + 5 × 30 s r band). (b) UT 2023 July 27 coaddition of 6 × 90 s ARCTIC images. (c) UT 2023 September 16, coadded 2 × 120 s V-band plus 2 × 120 s R-band VATT4K images acquired with the 1.8 m VATT at Mount Graham International Observatory in Arizona. (d) UT 2023 December 12, 7 × 300 s plus 5 × 120 s coadded VR-band ARCTIC exposures. (e) UT 2023 December 15, coadded 18 × 120 s V-band VATT4K exposures. (f) UT 2023 December 19, coadded 2 × 150 s VR-band ARCTIC exposures. (g) UT 2024 January 4, coadded 4 × 60 s VR-band ARCTIC images. (h) UT 2024 April 11, coadded 2 × 300 s r-band exposures with the Large Monolithic Imager on the 4.3 m LDT near Happy Jack, Arizona.
Paper: A Dormant Captured Oort Cloud Comet Awakens: (18916) 2000 OG44
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, Dmitrii E. Vavilov, William A. Burris
Figure caption: 2000 OG44 dynamical modeling results. Panels (c) through (f) comprise 500 orbital clones spanning a Gaussian distribution of orbital element uncertainties. (a) Solar system plot with 2000 OG44. (b) Heliocentric distance of 2000 OG44 and several planets, as seen from Jupiter’s corotating reference frame. (c) Heliocentric distance r. 2000 OG44 crosses the orbit of Jupiter (orange horizontal line at ∼5 au) and Mars (red line at ∼1.5 au). Aphelion and perihelion distances for Jupiter and Mars are shown as shaded regions. (d) Jupiter–2000 OG44 separation. (e) Longitude of perihelion precessing with a period of ∼20 kyr. (f) Number of clones belonging to the named dynamical class; at 4 Myr ago, 99.2% of clones originated in the Oort cloud, with the remaining 0.02% belonging to the JFCs.
Paper: Squeezing Full-shape Dynamical Dark Energy Constraints with Galaxy Alignments
Authors: Junsup Shim, Teppei Okumura, Atsushi Taruya
Figure caption: Improvement in 1D marginalized constraints with IA (left) and FS joint constraints (right), assuming a PFS-like survey with CMB prior included. Joint constraints as fractional errors, σi/θi, are shown. For wa, we show their actual error, σi, since its fiducial value, θi, is zero.
Paper: Squeezing Full-shape Dynamical Dark Energy Constraints with Galaxy Alignments
Authors: Junsup Shim, Teppei Okumura, Atsushi Taruya
Figure caption: 2D confidence ellipse contours for the DE EOS and As parameters for w0waCDM and its one-parameter extension, including CMB prior. 1σ confidence contours are shown. Correlation coefficient ρXY for a pair of cosmological parameters, X and Y, is calculated as ﹩{\rho }_{XY}={C}_{XY}/\sqrt{{C}_{XX}{C}_{YY}}﹩ using the error covariance matrix, ﹩{{\boldsymbol{C}}}_{XY}={({\tilde{{\boldsymbol{F}}}}_{XY})}^{-1}﹩.
Paper: Squeezing Full-shape Dynamical Dark Energy Constraints with Galaxy Alignments
Authors: Junsup Shim, Teppei Okumura, Atsushi Taruya
Figure caption: 2D confidence ellipses for DE EOS parameters of the most extended dynamical DE model, w0waCDM+(Ωk, mν, γ) assuming a PFS-like survey. Contours represent 1σ confidence regions, and the CMB prior is included. The contour for “IA” is obtained from PEE and PgE.
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: Flux density F  ν  (black markers; in units of erg cm−2 s−1 Hz−1) at frequency ν (Hz) and SED (open markers; in units of erg cm−2 s−1) of BL Lac from radio to γ-ray frequencies during the time span of the IXPE observations. The different colored lines correspond to the power-law fits used for the estimation of the spectral indices (α, where F  ν  ∝ ν  α ) of each band, as specified in the legend and the Appendix, Table 4.
Paper: Retention of Surface Water on Tidally Locked Rocky Planets in the Venus Zone around M Dwarfs
Authors: Yueyun Ouyang, Feng Ding, 峰 丁, Jun Yang, 军 杨
Figure caption: (A) Relation between the global mean outgoing longwave radiation (OLR) and the surface temperature of the nightside (lower x-axis) when pdry = 1 bar and ﹩{f}_{{\rm{C}}{{\rm{O}}}_{2}}=376﹩ ppmv. The upper x-axis shows the corresponding surface temperature of the dayside, and the scale is not linear. States P1 and P3 correspond to equilibrium states with the same OLR of 587.2 W m−2, and point P2 marks the maximum OLR value emitted by the planet. Red and blue curves further show the dayside and nightside OLR as a function of the nightside surface temperature. (B), (D) Vertical temperature profiles in the dayside (red) and nightside (blue) columns of states P1 (B) and P3 (D). (C), (E) Vertical profiles of relative humidity in the dayside (red) and nightside (blue) columns that measure the degree of water vapor saturation in the air column of states P1 (C) and P3 (E). The title of each panel gives the value of uniform specific humidity in the atmosphere.
Paper: Gravitational-wave Parameter Estimation in Non-Gaussian Noise Using Score-based Likelihood Characterization
Authors: Ronan Legin, Maximiliano Isi, Kaze W. K. Wong, Yashar Hezaveh, Laurence Perreault-Levasseur
Figure caption: Example of a sampled posterior distribution using SLIC (blue) vs. using a Gaussian likelihood (orange). The ground truth model parameter is located at the intersection of the black lines. In the top right corner, the true signal is shown in orange superposed on top of the mock observation in blue. The contours represent the 68% and 99% credible intervals. The ground truth parameters of the waveform are ﹩{ \mathcal M }=22.8{M}_{\odot }﹩, η = 0.187, χ1 = −0.807, χ2 = −0.889, dL = 678 Mpc, and ϕc = 0.830. The true trigger time, tc, in relative and absolute GPS time is 1.501 s and 1,128,689,443.501 s, respectively. The LIGO noise segment used in this mock observation starts at an absolute GPS time of 1,128,689,442 s and lasts for 4 s. The signal-to-noise ratio of the ground truth waveform is 11.7. While a loud glitch like this one could be handled by existing cleaning procedures, SLIC has the advantage of implicitly factoring in the distribution of expected glitch morphologies, as well as folding in uncertainty about the glitch directly into the posterior (rather than removing a point estimate), all without the need to be manually triggered and while remaining computationally scalable to thousands of signals; SLIC also applies to more subtle noise artifacts that would not be targeted for bespoke cleaning.