adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: Best-fit models to the JWST spectrum of WD J1922+0233. The solid blue line displays the best fit for a grid of models using the M. Abel et al. (2012) opacities for H2–He CIA, while the dashed orange line is for a grid of models using the U. G. Jørgensen et al. (2000) H2–He CIA.
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: NIRSpec and MIRI spectra of the three IR-faint white dwarfs observed as part of our program. Both spectra are merged at 5 μm. Photometry data from the literature are shown for comparison (H. C. Harris et al. 1999; M. Kilic et al. 2006, 2009; M. F. Skrutskie et al. 2006; K. C. Chambers et al. 2016).
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: Model comparison of MPB and BS at X = –4 R  M . All results set B  X  = B  Y  = 0, B  Z  = 5 nT(λ = 0°), and P  d  = 1.06 nPa. The black lines are the result of this paper, and the red lines, pink lines, blue dotted–dashed lines, and green dashed lines correspond to results from R. Ramstad et al. (2017), M. Wang et al. (2020, 2022), D. Vignes et al. (2000), and N. J. T. Edberg et al. (2008).
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: Panel (a): northward component IMF; red, blue, and green lines correspond to λ = 0°, 15°, and 30°, respectively. Panel (b): southward component IMF; red, blue, and green lines correspond to λ = 150°, 165°, and 180°, respectively. The black line represents the outline of Mars, and the dots represent the center points, with colors corresponding to the clock angle. Panel (c): the relationship between the Z value of the MPB center coordinates and the IMF clock angle.
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: The dependence of MPB elliptical fitting parameters a (squares in panel (a)), b (circles in panel (b)), and e (down triangles in panel (c)). Red, blue, and green lines represent results in λ = 0°, λ = 90°, and average value across all angles, respectively.
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: The relationship of θ and Δangle with IMF clock angle at X = –4 R  M . The black line is the fitting Equation (8) in Panel (a) and Equation (9) in Panel (b). The blue square represents MPB and the red circle represents BS.
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: The dependence of MPB elliptical fitting parameters a (squares in panel (a)), b (circles in panel (b)), and e (down triangles in panel (c)). Red, blue, and green lines represent results at X = –3, –4 and –5 R  M , respectively.
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: The fitting results of MPB and BS tail cross sections at X = –4 R  M  under different IMF clock angles. The solid arrows represent the elongated direction of the fitting ellipse, and the dashed arrows represent the IMF clock angle. The red, blue, and green colors correspond to λ = 15°, 45°, and 75°, respectively.
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: The dependence of BS elliptical fitting parameters a (squares in panel (a)), b (circles in panel (b)), and e (down triangles in panel (c)). Red, blue, and green lines represent results at X = –3, –4, and –5 R  M , respectively.
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: Tail cross section of MPB and BS at X = –4 R  M . The background color represents the solar wind velocity in panel (a) and panel (b), and it represents the magnetic field intensity in panel (c) and panel (d). The arrow shows the IMF clock angle direction (0° in panels (a) and (c), 45° in panels (b) and (d)). The red line represents the outcome of the ellipse fitting, and the black dot represents the automatic recognition boundary position.
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: The dependence of BS elliptical fitting parameters a (squares in panel (a)), b (circles in panel (b)), and e (down triangles in panel (c)). Red, blue, and green lines represent results in λ = 0°, λ = 90°, and average value across all angles, respectively.
Paper: Spectral Study of Very-high-energy Gamma Rays from SS 433 with HAWC
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, E. De la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, S. Fraija, J. A. García-González, A. Gonzalez Muñoz, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, A. Lara, W. H. Lee, J. Lee, C. de León, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, L. Nellen, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: Significance maps above 1 TeV. (a) A pretrial significance map of the SS 433 region with labels from A. A. Abdo et al. (2007), B. Bartoli et al. (2013), A. U. Abeysekara et al. (2018), and Z. Cao et al. (2021, 2024). (b) A pretrial significance map zoomed in closely around SS 433. The map shows excess after the model fit but only removes background sources for the visualization of the SS 433 jet lobes. The green contour lines indicate the observational results from ROSAT (W. Brinkmann et al. 1996), and the white contour lines are the 5σ contour lines as observed by this work. The X-ray emission regions “e1,” “e2,” and “e3” for the east lobe and “w1” and “w2” for the west lobe have also been indicated (S. Safi-Harb & H. Ögelman 1997). The red cross marks the known location of the binary SS 433. The purple and cyan stars indicate the best-fit locations from this work. The red ring in each panel indicates the angular resolution.
Paper: Spectral Study of Very-high-energy Gamma Rays from SS 433 with HAWC
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, E. De la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, S. Fraija, J. A. García-González, A. Gonzalez Muñoz, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, A. Lara, W. H. Lee, J. Lee, C. de León, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, L. Nellen, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: Significance maps around the SS 433 jet lobes for different energy ranges. The background sources have been subtracted. The red circle in each panel indicates the angular resolution of the bin that includes the most number of events for the given energy range. (a) Shows the significance map corresponding to 1–10 eV. The green contour indicates the 3σ level in the HAWC data. The black contour indicates the 3σ level in the H.E.S.S. data at energies 2.5–10 TeV. (b) Shows the significance map corresponding to above 10 TeV. The green contour indicates the 4σ level in the HAWC data at energies above 10 TeV. The black contour indicates the 4σ level in the H.E.S.S. data at energies above 10 TeV. (c) Shows the significance map corresponding to above 18 TeV. The green contour indicates the 4σ level in the HAWC data. The black contour indicates the 4σ level in the H.E.S.S. data at energies above 10 TeV (H. E. S. S. Collaboration et al. 2024).
Paper: Spectral Study of Very-high-energy Gamma Rays from SS 433 with HAWC
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, E. De la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, S. Fraija, J. A. García-González, A. Gonzalez Muñoz, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, A. Lara, W. H. Lee, J. Lee, C. de León, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, L. Nellen, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: The spectral energy distribution of the gamma-ray emission site in the SS 433 east (top) and west (bottom) lobes measured by HAWC (this work; orange), Fermi-LAT (K. Fang et al. 2020; light blue markers), H.E.S.S. (H. E. S. S. Collaboration et al. 2024; navy square markers), and VERITAS (P. Kar 2017; brown upper limit). Models are shown for reference, including M. M. Reynoso & A. M. Carulli (2019, parameter 3a; light gray dotted curve), T. Sudoh et al. (2020; dark gray dashed–dotted curves), K. Fang et al. (2020; gray shaded regions), S. S. Kimura et al. (2020, scenario D; light gray dashed curve), and H. E. S. S. Collaboration et al. (2024; gray dashed curve).
Paper: Spectral Study of Very-high-energy Gamma Rays from SS 433 with HAWC
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, E. De la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, S. Fraija, J. A. García-González, A. Gonzalez Muñoz, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, A. Lara, W. H. Lee, J. Lee, C. de León, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, L. Nellen, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: The best-fit power-law spectra of the SS 433 lobes. Information on each data point corresponding to energy bins is presented in Appendix C. The shaded region represents the 1σ statistical error band. The red data point at 20 TeV represents the best-fit result at e1 (w1) for the east (west) lobe from A. U. Abeysekara et al. (2018).
Paper: Spectral Study of Very-high-energy Gamma Rays from SS 433 with HAWC
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, E. De la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, S. Fraija, J. A. García-González, A. Gonzalez Muñoz, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, A. Lara, W. H. Lee, J. Lee, C. de León, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, L. Nellen, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: Significance maps of the results from the source search pipeline. The lower labels indicate the sources found by this analysis. (a) HAWC data map. (b) Model map. (c) Residual map.
Paper: Spectral Study of Very-high-energy Gamma Rays from SS 433 with HAWC
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, E. De la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, S. Fraija, J. A. García-González, A. Gonzalez Muñoz, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, A. Lara, W. H. Lee, J. Lee, C. de León, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, L. Nellen, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: A one-dimensional significance histogram of the final residual map shown in Figure 2(c).
Paper: Cosmological Prediction of the Void and Galaxy Clustering Measurements in the CSST Spectroscopic Survey
Authors: Yingxiao Song, Qi Xiong, Yan Gong, Furen Deng, Kwan Chuen Chan, Xuelei Chen, Qi Guo, Guoliang Li, Ming Li, Yun Liu, Yu Luo, Wenxiang Pei, Chengliang Wei
Figure caption: The multipole power spectra ﹩{P}_{{\ell }}^{\mathrm{gg}}﹩ (green), ﹩{P}_{{\ell }}^{\mathrm{vv}}﹩ (blue), and ﹩{P}_{{\ell }}^{\mathrm{vg}}﹩ (red) with ℓ = 0 at z = 0.3, 0.6, and 0.9 in the simulation. The gray data points with SNR <1 are excluded in the constraint process. The curves are the best fits of the theoretical calculation, and the dotted line indicates that the values are negative. The solid, dashed–dotted, and dashed curves are the total, clustering, and noise terms of the power spectra.
Paper: Could the Recent Rebrightening of the GW170817A Afterglow Be Caused by a Counterjet?
Authors: Ranadeep G. Dastidar, Paul C. Duffell
Figure caption: Density snapshot of our jet–counterjet model using the JET code. Two opposing boosted fireballs are injected, each with a single impulse normalized energy. The jets are evolving through a constant density medium, n ISM = 0.1 cm−3, marked by the gray background. The dashed black circle is for scaling reference, which marks the radial distance r = 1.07 [code units] ≈ 2.53 × 1018 cm. The snapshot is the density profile at a typical time during its evolution.
Paper: Cosmological Prediction of the Void and Galaxy Clustering Measurements in the CSST Spectroscopic Survey
Authors: Yingxiao Song, Qi Xiong, Yan Gong, Furen Deng, Kwan Chuen Chan, Xuelei Chen, Qi Guo, Guoliang Li, Ming Li, Yun Liu, Yu Luo, Wenxiang Pei, Chengliang Wei
Figure caption: Contour maps at 68% and 95% CL and 1D pdfs of the three void-density-profile parameters and void biases constrained by the void autopower spectra (blue) and joint power spectra (red) derived from the simulation. The left, middle, and right panels show the results of α  i , β  i , γ  i , and ﹩{b}_{{\rm{v}}}^{i}﹩ at z = 0.3, 0.6, and 0.9, respectively.
Paper: Cosmological Prediction of the Void and Galaxy Clustering Measurements in the CSST Spectroscopic Survey
Authors: Yingxiao Song, Qi Xiong, Yan Gong, Furen Deng, Kwan Chuen Chan, Xuelei Chen, Qi Guo, Guoliang Li, Ming Li, Yun Liu, Yu Luo, Wenxiang Pei, Chengliang Wei
Figure caption: Contour maps of the six cosmological parameters at 68% and 95% CL for galaxy clustering (green), void clustering (blue), and joint constraints (red) derived from the simulation. The 1D pdf for each parameter is also shown. The gray dotted lines mark the fiducial values of the cosmological parameters.
Paper: Cosmological Prediction of the Void and Galaxy Clustering Measurements in the CSST Spectroscopic Survey
Authors: Yingxiao Song, Qi Xiong, Yan Gong, Furen Deng, Kwan Chuen Chan, Xuelei Chen, Qi Guo, Guoliang Li, Ming Li, Yun Liu, Yu Luo, Wenxiang Pei, Chengliang Wei
Figure caption: Contour maps at 68% and 95% CL and 1D pdfs of ﹩{N}_{{\rm{g}}}^{i}﹩ (left panel), ﹩{N}_{{\rm{v}}}^{i}﹩ (middle panel), and ﹩{N}_{\mathrm{vg}}^{i}﹩ (right panel) at z = 0.3, 0.6, and 0.9 derived from the galaxy power spectrum (green), void power spectrum (blue), and joint power spectra (red) in the simulation, respectively.
Paper: Cosmological Prediction of the Void and Galaxy Clustering Measurements in the CSST Spectroscopic Survey
Authors: Yingxiao Song, Qi Xiong, Yan Gong, Furen Deng, Kwan Chuen Chan, Xuelei Chen, Qi Guo, Guoliang Li, Ming Li, Yun Liu, Yu Luo, Wenxiang Pei, Chengliang Wei
Figure caption: Contour maps at 68% and 95% CL and 1D pdfs of the galaxy bias ﹩{b}_{{\rm{g}}}^{i}﹩ at z = 0.3, 0.6, and 0.9 derived from the galaxy power spectrum (green) and joint power spectra (red) in the simulation, respectively.
Paper: Could the Recent Rebrightening of the GW170817A Afterglow Be Caused by a Counterjet?
Authors: Ranadeep G. Dastidar, Paul C. Duffell
Figure caption: Lightcurves for a given set of jet–ISM parameters, but varying the observer angle. The lightcurves for observer angles θ obs = [0.5, 0.15, 0.25, 0.40, 0.55, 0.80, 1.00, 1.20, 1.30, 1.40, 1.57] rad are shown. For θ obs < θ 0(=0.14 rad), we see the lightcurves start with a plateau-like feature. For larger viewing angles (θ obs > θ 0), the lightcurve increases first, due to emissions from the jet limbs. As the jet slows down and spreads, the jet core eventually becomes visible, and the lightcurve peaks. Irrespective of the observer angle, the second rise and peak are due to the counterjet happening almost at the same time around 1000 days. For extreme off-axis angles (θ obs > 1.2 rad), we enter a regime when the forward and counterjets cannot be distinguished from each other. This results in single peak lightcurves. These lightcurves peak at a much later time, closer to the second rebrightening, and fall off sharply almost immediately.
Paper: Could the Recent Rebrightening of the GW170817A Afterglow Be Caused by a Counterjet?
Authors: Ranadeep G. Dastidar, Paul C. Duffell
Figure caption: Lightcurves at 3 GHz (red) and 1 keV (blue) for GRB 170817A as observed from θ obs = 49.°8. The solid circles are data taken from various sources listed in the text. The solid and dashed lines are lightcurves with and without the counterjet, respectively. The clear late-time excess seen in the solid lines, compared to the dashed line, implies the excess emissions come from a counterjet, peaking around 1000 days. The excess flux seen in the data, especially for the 1 keV X-ray band, matches very closely with the counterjet rebrightening within the errors of the observations. But a stronger emission is expected at 3 GHz around the rebrightening time.
Paper: Could the Recent Rebrightening of the GW170817A Afterglow Be Caused by a Counterjet?
Authors: Ranadeep G. Dastidar, Paul C. Duffell
Figure caption: The location of the maximum emitting region at 3 GHz for the off-axis jet of GRB 170817A is plotted. The observer is placed at θ obs = 0.87 rad. Plotted at the top (the solid circles) is the observed physical distance of the merger center to the maximum emitting region on the sky at 3 GHz, from K. P. Mooley et al. (2018a). Plotted below that is the flux map at the different epochs. These show the apparent motion of the flux contributions from the afterglow, along the line joining the merger center and the observer. The solid lines are obtained using the parameters from this paper (Table 1) while the dashed lines are obtained using the Y. Wu & A. MacFadyen (2018) model. The peaks from these plots are used to identify the location of GRB 170817A for that given time.
Paper: Could the Recent Rebrightening of the GW170817A Afterglow Be Caused by a Counterjet?
Authors: Ranadeep G. Dastidar, Paul C. Duffell
Figure caption: Ratios of the timescales when the emissions from the forward jet peak, to that of the counterjet on the y-axis, compared to the observer angle along the x-axis. This is measured at two frequencies/energies: the 3 GHz radio band and 1 keV X-ray band. We find no difference in their dependence on the observer angle, as expected. This temporal ratio follows the empirical scaling law in Equation (22). This is plotted as blue dashed lines. The region of interest is when ﹩{t}_{p}^{j}/{t}_{p}^{{cj}}\sim 175/1234﹩, which is the prospective observer viewing angle θ obs ∼ 0.85 rad, which is also marked with thin black dashed lines. The thick dashed line at θ 0 = 0.09 rad shows the jet opening angle. Due to various shocks and numerical instabilities at the jet wing boundaries, the temporal ratio is slightly different for the X-ray and radio near the jet opening angle. Since θ obs is much greater than the jet opening angle, this numerical effect can be ignored without loss of generality.