adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, 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, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: IXPE DU1 light curve of 3C 84 (in gray). The flare, shaded yellow, is observed simultaneously in all IXPE DUs (orange, green, and magenta light curves in the inset), as well as the simultaneous NuSTAR observation (blue light curve in the inset). This part of the light curve coincides with the period of enhanced activity from 3C 84.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, 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, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Q–U plot (green) for the 2′–3′ region of the Perseus Cluster in 2–8 keV, along with the corresponding values for Stokes rotation along the radial (orange) and azimuthal (blue) directions. This annular region is dominated by thermal emission from the ICM. The error bars are at the 1σ level. For all three cases, there is no evidence of significant polarization of the ICM photons.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, 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, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Polarization contours for 3C 84 using a spectropolarimetric model fit. The red star denotes the best-fit value, while the blue, orange, and green contours correspond to 1σ, 2σ, and 3σ confidence intervals. The dashed line corresponds to the position angle of the radio jet.
Paper: 1000–10,000 M⊙ Primordial Stars Created the Nitrogen Excess in GS 3073 at z = 5.55
Authors: Devesh Nandal, Daniel J. Whalen, Muhammad A. Latif, Alexander Heger
Figure caption: H-R (top) and Kippenhahn diagrams (bottom) for the 7000 M⊙ star. The entire evolution of the star is shown in (a) and (b), its pre-MS evolution is shown in (c) and (d), its core H burning phase is in (e) and (f), and core He burning to the end of Si burning is in (g) and (h). The black and white lines in the Kippenhahn diagrams are isomass and isothermal lines, respectively, and the red and green dots along the track on the lower left in (a) are the zero-age main sequence (ZAMS) positions of 2–120 M⊙ and 1000–10,000 M⊙ Pop III stars for comparison.
Paper: 1000–10,000 M⊙ Primordial Stars Created the Nitrogen Excess in GS 3073 at z = 5.55
Authors: Devesh Nandal, Daniel J. Whalen, Muhammad A. Latif, Alexander Heger
Figure caption: Abundance profiles of the 7000 M⊙ star at three evolutionary stages. Top: beginning of core He burning. Middle: middle of core He burning. Bottom: end of Si burning. Purple and yellow regions mark convective and radiative zones, respectively.
Paper: The Near-ultraviolet Spectra of FU Orionis Accretion Disks
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Gregory J. Herczeg, Kevin France
Figure caption: Top: the C II] (black circles), Fe II] (red triangles), and Mg II (blue squares) line luminosities for the FUOr sample and the CTTS BP Tau. Error bars are drawn, but are smaller than the symbols for most measurements. The empty circle (triangle) for HBC 722 (BP Tau) represents the 3σ upper limit on the C II] (Fe II]) luminosity. The FUOrs are sorted left-to-right in order of increasing Lacc. Middle: the same line C II] and Fe II] luminosities divided by the Mg II luminosities. Bottom: the LC II] measurements plotted against the Lacc for the FUOrs. The black line shows the best-fit relation described in Section 4.2.
Paper: The Near-ultraviolet Spectra of FU Orionis Accretion Disks
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Gregory J. Herczeg, Kevin France
Figure caption: The 2D rectified x2d HST/STIS images for each of our sources. The white hashes mark the locations of the C II] 2326, Fe II] 2500, and Mg II 2800 features, and the surface brightness units are 10−14 erg s−1 cm−2 Å−1 arcsec−2. Notice that the traces of FU Ori, V1515 Cyg, and V960 Mon are all detected down to 1800 Å. BBW 76 is only marginally detected at 2100 Å. V1057 Cyg is only detected redward of the C II feature, with barely any continuum until 2400 Å, and HBC 722 is only detected redward of 2450 Å.
Paper: The Near-ultraviolet Spectra of FU Orionis Accretion Disks
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Gregory J. Herczeg, Kevin France
Figure caption: The posterior distributions for the blackbody fit described in Section 3.2. The red vertical and horizontal lines mark the median values for the histogram, while the blue lines mark the modal values. The magenta line marks the ﹩{R}_{{\rm{BB}}}\propto {T}_{{\rm{BB}}}^{-2}﹩ relation, anchored at the median Lexcess value for each source.
Paper: The Near-ultraviolet Spectra of FU Orionis Accretion Disks
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Gregory J. Herczeg, Kevin France
Figure caption: The G230L spectrum of BP Tau (black) compared with the median (brown line) and range (brown filled region) of G230L spectra of 50 CTTSs in the ULLYSES sample. The gray lines mark the locations of the NUV emission lines discussed in Section 4. Notice that there is no sign of the Fe II] emission feature at 2505 in either BP Tau or the ULLYSES sample.
Paper: The Near-ultraviolet Spectra of FU Orionis Accretion Disks
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Gregory J. Herczeg, Kevin France
Figure caption: The STIS G230L spectra of the six FUOrs and the CTTS BP Tau for reference. The spectra are sorted top-to-bottom in order of decreasing signal-to-noise. The gray vertical lines mark the locations of the emission features discussed in Section 4.
Paper: The Near-ultraviolet Spectra of FU Orionis Accretion Disks
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Gregory J. Herczeg, Kevin France
Figure caption: Spectrally averaged spatial cuts in the 2D spectra of V1057 Cyg (left), HBC 722 (middle), and BBW 76 (right). The spectral averaging was over ∼75 Å and the legend shows the mean wavelength of each bin.
Paper: Early Evidence for Polar Orbits of Sub-Saturns around Hot Stars
Authors: Emma Dugan, Xian-Yu Wang, Agustin Heron, Hareesh Gautham Bhaskar, Malena Rice, Cristobal Petrovich, Songhu Wang
Figure caption: Spectral energy distribution, TESS transit photometry, out-of-transit radial velocities, and RM effect modeling for TOI-1135. The upper panel in each plot shows the observational data sets along with the corresponding best-fit model from the EXOFASTv2 global modeling (solid red line). The resulting RM signal-to-noise ratio (D. Kipping & X.-Y. Wang 2024) is 8.1. The lower panel in each plot displays the residuals.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: XRISM Constraints on Unidentified X-Ray Emission Lines, Including the 3.5 keV Line, in the Stacked Spectrum of 10 Galaxy Clusters
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Jean-Paul Breuer, Priyanka Chakraborty, Stefano Ettori, Andrew Fabian, Annie Heinrich, Marie Kondo, Julie HLavacek-Larrondo, Hannah McCall, Paul Nulsen, Tom Rose, Helen Russell, Arnab Sarkar, Evan Scannapieco, Kazunori Suda, Ming Sun, Prathamesh Tamhane, Nhut Truong, Norbert Werner, Congyao Zhang
Figure caption: The stacked spectra in the 1.97–3 keV and 4–6.5 keV ranges, with the best-fit two bapec model shown in the green curve. The same as Figure 1, black, red, and blue show the full cluster sample, hot subsample, and cool subsample respectively. For clarity, the hot cluster spectrum is lowered by a factor of 2, and the cool cluster spectrum is lowered by a factor of 3. Detected atomic lines are also labeled.
Paper: Cosmological Constraints on Nonphantom Dynamical Dark Energy with DESI Data Release 2 Baryon Acoustic Oscillations: A 3σ+ Lensing Anomaly
Authors: Shouvik Roy Choudhury, Teppei Okumura, Keiichi Umetsu
Figure caption: The left panel shows the 1D posterior distributions of Alens for various data combinations. The right panel shows its 2D correlation plots with the S8 parameter. We note that dataset combinations with WL included lead to a 3σ+ lensing anomaly due to the strong negative correlation with S8. Even without the WL data, the lensing anomaly is 2σ+.
Paper: Cosmological Constraints on Nonphantom Dynamical Dark Energy with DESI Data Release 2 Baryon Acoustic Oscillations: A 3σ+ Lensing Anomaly
Authors: Shouvik Roy Choudhury, Teppei Okumura, Keiichi Umetsu
Figure caption: The left, middle, and right panels show the 1D posterior distributions of ∑mν, Neff, and H0 (km s−1Mpc−1), respectively, for various data combinations. The dashed vertical line in the middle panel corresponds to the standard model value of Neff = 3.044.
Paper: XRISM Constraints on Unidentified X-Ray Emission Lines, Including the 3.5 keV Line, in the Stacked Spectrum of 10 Galaxy Clusters
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Jean-Paul Breuer, Priyanka Chakraborty, Stefano Ettori, Andrew Fabian, Annie Heinrich, Marie Kondo, Julie HLavacek-Larrondo, Hannah McCall, Paul Nulsen, Tom Rose, Helen Russell, Arnab Sarkar, Evan Scannapieco, Kazunori Suda, Ming Sun, Prathamesh Tamhane, Nhut Truong, Norbert Werner, Congyao Zhang
Figure caption: Similar to Figure 3 but in the 6.5–7.0 keV and 7.0–9.4 keV ranges.
Paper: Photon Orbit Signatures in Spectra of Black Hole Accretion Disks
Authors: Daniel C. M. Palumbo, George N. Wong, Angelo Ricarte
Figure caption: Dependence of the photon ring spectral feature on inclination and electron density in a RIAF model of Sgr A*. Left: 230 GHz images of the same model at 30° and 70° inclination, with a fixed peak number density of 3 × 108 cm−3. Middle: spectral index maps at 230–235 GHz at each inclination. Right: spectra of the decomposed model at each inclination, varying the electron number density. The black star indicates the 230 GHz, 2.4 Jy value at the density used in the left figures.
Paper: Photon Orbit Signatures in Spectra of Black Hole Accretion Disks
Authors: Daniel C. M. Palumbo, George N. Wong, Angelo Ricarte
Figure caption: Spectral feature in ray-traced GRMHD, corresponding to a MAD a = 0.5 Rhigh = 160 model of M87*. Left: total intensity map. Center: spectral index map at 230 GHz revealing the elevated spectral index in the photon ring. Right: instantaneous spectrum, where the gray vertical band demarcates 230–345 GHz, and a circle marks the maximum of each contribution.
Paper: Photon Orbit Signatures in Spectra of Black Hole Accretion Disks
Authors: Daniel C. M. Palumbo, George N. Wong, Angelo Ricarte
Figure caption: Survey of power-law index p for the direct and indirect image magnetic field incidence angles θB,0 = 15° and θB,1 = 45° as shown in Figure 2. Steeper power laws increase the relative contribution of the photon ring, leading to substructure in the spectrum of the polarization fraction.
Paper: Discovery of a 9.67 s Pulsar in an Ultraluminous X-Ray Source in NGC 4631 with XMM-Newton
Authors: Lorenzo Ducci, Sandro Mereghetti, Fabio Pintore, Sinan Allak, Andrea Santangelo, Manami Sasaki, Patrick Kavanagh
Figure caption:  ﹩{Z}_{1}^{2}﹩ test computed for the pn data of X−8, in the energy range 0.2–12 keV.
Paper: Discovery of a 9.67 s Pulsar in an Ultraluminous X-Ray Source in NGC 4631 with XMM-Newton
Authors: Lorenzo Ducci, Sandro Mereghetti, Fabio Pintore, Sinan Allak, Andrea Santangelo, Manami Sasaki, Patrick Kavanagh
Figure caption: EPIC images of the field around ULXs X−2 and X−8 in three energy bands. The images are a combination of pn, MOS1, and MOS2 data using the SAS emosaic task. The circles indicate the 95% positional uncertainty for each source (X−2: 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩7; X−8: 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩97).
Paper: Discovery of a 9.67 s Pulsar in an Ultraluminous X-Ray Source in NGC 4631 with XMM-Newton
Authors: Lorenzo Ducci, Sandro Mereghetti, Fabio Pintore, Sinan Allak, Andrea Santangelo, Manami Sasaki, Patrick Kavanagh
Figure caption: Combined XMM-Newton EPIC image of NGC 4631 in the 0.3–10 keV band from the 2025 July observation. The locations of known ULXs and the new ULX X−8 are marked.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: Emission profiles of the Lyα lines detected with VLT/MUSE and the absorption profile of the Mg II absorber observed by Magellan/FIRE along the J1306+0356 sight line at z = 4.8651, shown in velocity space. The upper panel shows the spectra of the two LAEs, which are at distances of 201 kpc (red) and 197 kpc (blue) from the absorbing gas, respectively. LAE1 is centered at z = 4.867, at the peak of the strongest component. The gray dashed lines indicate the potential subcomponents of LAE1. The shaded regions indicate the wavelength interval used to compute the EW of the Lyα lines. For LAE1, the blue bump is tentative, therefore we do not include it in the EW measurement. The lower panels show the Mg II λ2796 and Mg II λ2803 lines, respectively, with the blue dashed line representing the zero-point at z = 4.8651, where the first major subcomponents are located. Complete Voigt profile fitting of the two systems is provided in Table A1 and Appendix Figure A4.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: Left: spatial distribution of the absorbing gas along J1306+0356 (located at the center of the VLT/MUSE cube) and the two LAEs, which are offset by ∼200 kpc from the gas. The background image is the variance-weighted white-light image generated by MUSELET (for details, see Section 2.6). Narrowband images of the two detected LAEs are presented. The absorbing gas structure is composed of two VSMG II systems, with a total velocity width Δv greater than 1000 km s−1. Right: spatial distribution of the absorbing gas along the J0305–3150 sight line (upper right corner) and the host galaxy, as detected with JWST/NIRCam data. The red dashed line is the fitted galaxy major axis.
Paper: Disturbed Cold Gas in Galaxy and Structure Formation
Authors: Siwei Zou, Robert A. Simcoe, Patrick Petitjean, Céline Péroux, Jaclyn B. Champagne, Feige Wang, Jinning Liang, Fangzhou Jiang, Zihao Li, Wen Sun, Xiaohui Fan, Jinyi Yang, Luis C. Ho, Xiaojing Lin, Jianan Li, Jianwei Lyu, Lile Wang, Weizhe Liu, Emanuele Paolo Farina, Xiangyu Jin, Cheng Cheng
Figure caption: The absorption profiles of the VSMG II at z = 2.5662, along with the 1D spectrum of the detected galaxy, which is 4﹩\mathop{.}\limits^{\unicode{x02033}}﹩65 (38 kpc) away from the absorber. The galaxy shows He I (with a Gaussian fit), [S III], and Paschen emission lines at z = 2.5643 in the JWST NIRCam F356W band. The zero-point is centered on the strongest Mg II subcomponent (the same in each panel).
Paper: Preperihelion Development of Interstellar Comet 3I/ATLAS
Authors: David Jewitt, Jane Luu
Figure caption: Composite preperihelion lightcurve of 3I/ATLAS with error bars omitted for clarity. The solid line shows heliocentric index n = 3.8 while the dashed lines above and below it represent the ±1σ uncertainties on n. Error bars are omitted for clarity of presentation.
Paper: Preperihelion Development of Interstellar Comet 3I/ATLAS
Authors: David Jewitt, Jane Luu
Figure caption: Sample images showing the morphological development of 3I/ATLAS. The image dates and heliocentric distances of the comet are shown in each panel, as is a 10″ scale bar. Sunward is west. The location of the brightest pixel is marked with a red dot, showing that the dust is extended asymmetrically toward the west in the early data, reversing to the east as the radiation pressure-swept tail develops in the later data. See Table 1 for additional details.