adsabs/AstroCLIMB huggingface dataset:
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Chemical abundance determination for lithium (upper left), scandium (upper right), strontium (lower left), and barium (lower right). The points represent the NEID combined spectrum, the black lines are the best fits, and the red lines are synthetic spectra with varying abundances for each element. Also shown are synthetic spectra without the presence of each element (gray line). The right panels show the χ 2 minimization routine for each synthetic spectra shown in the left panels. The x-axis is centered on the best-fit value (represented by the gray square) and also shown are ±0.05 dex marks for reference.
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Left panels: carbon abundance determination via spectral synthesis for two 2.5 Å wide sections of the CH G band. The points represent the NEID combined spectrum, the black line is the best fit, and the red lines are synthetic spectra with varying carbon abundances. Also shown is a synthetic spectrum without carbon (gray line). Right panels: χ 2 minimization routine for each synthetic spectrum shown in the left panels. The x-axis is centered on the best-fit value (represented by the gray square) and also shown are ±0.1 and ±0.2 dex marks for reference.
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Distribution of percent differences in equivalent width (EW, in milliangstrom) for the 138 absorption features in common with the H. Ito et al. (2013) analysis. The mean and median differences are shown in the upper left. The red and yellow insets show the lines with the largest percent differences, highlighting the continuum placement in each case (NEID on the left, HDS on the right). See text for further details.
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Normalized flux as a function of wavelength (in Å) for selected regions of the NEID spectra, highlighting a few absorption features of interest for stellar parameter and chemical abundance calculations. The solid black line represents the combined spectra and the white lines show the range of normalized fluxes for the individual exposures.
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Top: Radial velocities for BD+44°493 from the literature (left) and from NEID (right). Individual measurements and references can be found in Tables 2 and A1. Bottom: zoom-in for the NEID radial velocities, with the median and median absolute deviation values annotated. The thickness of the horizontal line is proportional to 1σ.
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Upper-limit estimation for the europium abundance in BD+44°493, using the absorption feature at 4205 Å. Points and lines are similar to the ones in Figures 3 and 4. See text for further details.
Paper: Evolution of Cataclysmic Variables with Binary-driven Mass Loss during Nova Eruptions
Authors: Wen-Shi Tang, Xiang-Dong Li, Zhe Cui
Figure caption: Comparison of the measured ΔP/P (colored circles) in the unit of parts-per-million (ppm) and theoretical predictions (black squares). The color bar represents the inferred mass-loss fraction in the form of BDML. In the upper and low panels, the ΔP values are positive and negative, respectively. The two green lines in the upper panel represent the predictions in the FW model with ΔM ign = 10−6 and 10−4 M ⊙, respectively. The dashed lines connect the observed and theoretical values for given sources. The observed data are taken from B. E. Schaefer (2023).
Paper: Evolution of Cataclysmic Variables with Binary-driven Mass Loss during Nova Eruptions
Authors: Wen-Shi Tang, Xiang-Dong Li, Zhe Cui
Figure caption: Influence of f dt on the evolution of CVs in the FW+BDML model. The initial parameters are M WD,i = 0.6 M ⊙, M 2,i = 0.5 M ⊙, and P orb,i = 0.2 days. Here ﹩{\dot{J}}_{\mathrm{MB}}﹩ is the angular-momentum-loss rate of magnetic braking. The different colored lines correspond to different values of f dt: f dt = 0.03 (blue), 0.05 (yellow), 0.1 (green), and 1.0 (cyan).
Paper: The JCMT BISTRO Survey: The Magnetic Fields of the IC 348 Star-forming Region
Authors: Youngwoo Choi, Woojin Kwon, Kate Pattle, Doris Arzoumanian, Tyler L. Bourke, Thiem Hoang, Jihye Hwang, Patrick M. Koch, Sarah Sadavoy, Pierre Bastien, Ray Furuya, Shih-Ping Lai, Keping Qiu, Derek Ward-Thompson, David Berry, Do-Young Byun, Huei-Ru Vivien Chen, Wen Ping Chen, Mike Chen, Zhiwei Chen, Tao-Chung Ching, Jungyeon Cho, Minho Choi, Yunhee Choi, Simon Coudé, Antonio Chrysostomou, Eun Jung Chung, Sophia Dai, Victor Debattista, James Di Francesco, Pham Ngoc Diep, Yasuo Doi, Hao-Yuan Duan, Yan Duan, Chakali Eswaraiah, Lapo Fanciullo, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Tetsuo Hasegawa, Martin Houde, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Doug Johnstone, Janik Karoly, Vera Könyves, Ji-hyun Kang, Miju Kang, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Jongsoo Kim, Shinyoung Kim, Gwanjeong Kim, Kyoung Hee Kim, Mi-Ryang Kim, Kee-Tae Kim, Hyosung Kim, Florian Kirchschlager, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Chang Won Lee, Hyeseung Lee, Chin-Fei Lee, Jeong-Eun Lee, Sang-Sung Lee, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Sheng-Jun Lin, Hong-Li Liu, Tie Liu, Sheng-Yuan Liu, Junhao Liu, Steven Longmore, Xing Lu, A-Ran Lyo, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Takashi Onaka, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Jonathan Rawlings, Mark Rawlings, Brendan Retter, John Richer, Andrew Rigby, Hiro Saito, Giorgio Savini, Masumichi Seta, Ekta Sharma, Yoshito Shimajiri, Hiroko Shinnaga, Archana Soam, Mehrnoosh Tahani, Motohide Tamura, Ya-Wen Tang, Xindi Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jia-Wei Wang, Anthony Whitworth, Jintai Wu, Jinjin Xie, Meng-Zhe Yang, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Guoyin Zhang, Yapeng Zhang, Chuan-Peng Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, David Eden, Stewart Eyres, Sam Falle, Valentin J. M. Le Gouellec, Frédérick Poidevin, Sven van Loo
Figure caption: Positions of HH 211 MMS and IC 348 MMS (or IC 348 SMM2) in the IC 348 star-forming region at the total intensity map of 850 μm. Cyan and white contours are at total intensities of 0.3 and 0.05 Jy beam−1, respectively, representing the core and filament regions. The beam and the spatial scale bar are shown in the lower left and right corners, respectively.
Paper: The JCMT BISTRO Survey: The Magnetic Fields of the IC 348 Star-forming Region
Authors: Youngwoo Choi, Woojin Kwon, Kate Pattle, Doris Arzoumanian, Tyler L. Bourke, Thiem Hoang, Jihye Hwang, Patrick M. Koch, Sarah Sadavoy, Pierre Bastien, Ray Furuya, Shih-Ping Lai, Keping Qiu, Derek Ward-Thompson, David Berry, Do-Young Byun, Huei-Ru Vivien Chen, Wen Ping Chen, Mike Chen, Zhiwei Chen, Tao-Chung Ching, Jungyeon Cho, Minho Choi, Yunhee Choi, Simon Coudé, Antonio Chrysostomou, Eun Jung Chung, Sophia Dai, Victor Debattista, James Di Francesco, Pham Ngoc Diep, Yasuo Doi, Hao-Yuan Duan, Yan Duan, Chakali Eswaraiah, Lapo Fanciullo, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Tetsuo Hasegawa, Martin Houde, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Doug Johnstone, Janik Karoly, Vera Könyves, Ji-hyun Kang, Miju Kang, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Jongsoo Kim, Shinyoung Kim, Gwanjeong Kim, Kyoung Hee Kim, Mi-Ryang Kim, Kee-Tae Kim, Hyosung Kim, Florian Kirchschlager, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Chang Won Lee, Hyeseung Lee, Chin-Fei Lee, Jeong-Eun Lee, Sang-Sung Lee, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Sheng-Jun Lin, Hong-Li Liu, Tie Liu, Sheng-Yuan Liu, Junhao Liu, Steven Longmore, Xing Lu, A-Ran Lyo, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Takashi Onaka, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Jonathan Rawlings, Mark Rawlings, Brendan Retter, John Richer, Andrew Rigby, Hiro Saito, Giorgio Savini, Masumichi Seta, Ekta Sharma, Yoshito Shimajiri, Hiroko Shinnaga, Archana Soam, Mehrnoosh Tahani, Motohide Tamura, Ya-Wen Tang, Xindi Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jia-Wei Wang, Anthony Whitworth, Jintai Wu, Jinjin Xie, Meng-Zhe Yang, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Guoyin Zhang, Yapeng Zhang, Chuan-Peng Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, David Eden, Stewart Eyres, Sam Falle, Valentin J. M. Le Gouellec, Frédérick Poidevin, Sven van Loo
Figure caption: Left: filament skeleton of the IC 348 star-forming region. Right: position angles of the filament at individual positions of the filament skeleton.
Paper: The JCMT BISTRO Survey: The Magnetic Fields of the IC 348 Star-forming Region
Authors: Youngwoo Choi, Woojin Kwon, Kate Pattle, Doris Arzoumanian, Tyler L. Bourke, Thiem Hoang, Jihye Hwang, Patrick M. Koch, Sarah Sadavoy, Pierre Bastien, Ray Furuya, Shih-Ping Lai, Keping Qiu, Derek Ward-Thompson, David Berry, Do-Young Byun, Huei-Ru Vivien Chen, Wen Ping Chen, Mike Chen, Zhiwei Chen, Tao-Chung Ching, Jungyeon Cho, Minho Choi, Yunhee Choi, Simon Coudé, Antonio Chrysostomou, Eun Jung Chung, Sophia Dai, Victor Debattista, James Di Francesco, Pham Ngoc Diep, Yasuo Doi, Hao-Yuan Duan, Yan Duan, Chakali Eswaraiah, Lapo Fanciullo, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Tetsuo Hasegawa, Martin Houde, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Doug Johnstone, Janik Karoly, Vera Könyves, Ji-hyun Kang, Miju Kang, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Jongsoo Kim, Shinyoung Kim, Gwanjeong Kim, Kyoung Hee Kim, Mi-Ryang Kim, Kee-Tae Kim, Hyosung Kim, Florian Kirchschlager, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Chang Won Lee, Hyeseung Lee, Chin-Fei Lee, Jeong-Eun Lee, Sang-Sung Lee, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Sheng-Jun Lin, Hong-Li Liu, Tie Liu, Sheng-Yuan Liu, Junhao Liu, Steven Longmore, Xing Lu, A-Ran Lyo, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Takashi Onaka, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Jonathan Rawlings, Mark Rawlings, Brendan Retter, John Richer, Andrew Rigby, Hiro Saito, Giorgio Savini, Masumichi Seta, Ekta Sharma, Yoshito Shimajiri, Hiroko Shinnaga, Archana Soam, Mehrnoosh Tahani, Motohide Tamura, Ya-Wen Tang, Xindi Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jia-Wei Wang, Anthony Whitworth, Jintai Wu, Jinjin Xie, Meng-Zhe Yang, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Guoyin Zhang, Yapeng Zhang, Chuan-Peng Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, David Eden, Stewart Eyres, Sam Falle, Valentin J. M. Le Gouellec, Frédérick Poidevin, Sven van Loo
Figure caption: Left: linear polarization angles and fractions in the IC 348 star-forming region detected in 850 μm dust continuum. The length of each segment is proportional to the polarization fraction, and the reference length is shown in the lower right corner. Right: magnetic field orientations in the IC 348 star-forming region obtained by 90° rotations of the linear polarization angles. Segment lengths are uniform to have the field directions better presented. The background image is the 850 μm total intensity, and the beam size is shown in the lower left corner of both panels.
Paper: Evolution of Cataclysmic Variables with Binary-driven Mass Loss during Nova Eruptions
Authors: Wen-Shi Tang, Xiang-Dong Li, Zhe Cui
Figure caption: Similar to Figure B1 but for M WD,i = 1.0 M ⊙. In the upper and lower M 2,i = 1.0 M ⊙, P orb,i = 0.4 days, and M 2,i = 0.6 M ⊙, P orb,i = 0.4 days, respectively. The blue and yellow lines represent the results with f dt = 0.5 and 1.0, respectively.
Paper: Evolution of Cataclysmic Variables with Binary-driven Mass Loss during Nova Eruptions
Authors: Wen-Shi Tang, Xiang-Dong Li, Zhe Cui
Figure caption: Example evolution that displays the influence of reaccretion of the nova ejecta by the companion with ﹩{\gamma }_{\mathrm{re}}=0.5﹩. The steel blue and orange lines show the cases with ﹩{\gamma }_{\mathrm{re}}=0﹩ and 0.5, respectively.
Paper: Evolution of Cataclysmic Variables with Binary-driven Mass Loss during Nova Eruptions
Authors: Wen-Shi Tang, Xiang-Dong Li, Zhe Cui
Figure caption: Distribution of CVs in the donor radius–orbital period diagram. The color bar denotes the probability density that CVs appear in a specific pixel. The left and right panels show the results in the FW+BDML model and the FW model, respectively. The purple stars represent the observed sources from M. McAllister et al. (2019).
Paper: Efficient and Accurate Force Replay in Cosmological-baryonic Simulations
Authors: Arpit Arora, Robyn Sanderson, Christopher Regan, Nicolás Garavito-Camargo, Emily Bregou, Nondh Panithanpaisal, Andrew Wetzel, Emily C. Cunningham, Sarah R. Loebman, Adriana Dropulic, Nora Shipp
Figure caption: Force reconstruction performance at the present day. First row: relative force residual (﹩{{\boldsymbol{F}}}_{{\rm{res}}}={{\boldsymbol{F}}}_{{\rm{reconstructed}}}/{{\boldsymbol{F}}}_{{\rm{true}}}-1﹩) for DM particles within 50 kpc of the galactic center at the present day for the X-direction in the Y–Z plane (left) the Y-direction in the X–Z plane (center), and the Z-direction in the X–Y plane (right). The multipole model used to reconstruct the forces is truncated with maximum pole orders ﹩{{\ell }}_{\max }={m}_{\max }=4﹩. The black ellipse encloses 90% of the stellar mass in each panel. Second row: histograms of the force residuals shown in each of the above panels. The 16th (red dashed line), 50th (blue dashed line), and 84th (red dashed line) quantiles, as well as the mean and standard deviation obtained from Gaussian fits, are marked for reference. Overall, the forces are reconstructed with under 10% error, with over 95% of the reconstructed forces having less than 4% error.
Paper: Efficient and Accurate Force Replay in Cosmological-baryonic Simulations
Authors: Arpit Arora, Robyn Sanderson, Christopher Regan, Nicolás Garavito-Camargo, Emily Bregou, Nondh Panithanpaisal, Andrew Wetzel, Emily C. Cunningham, Sarah R. Loebman, Adriana Dropulic, Nora Shipp
Figure caption: Variation in performance with different symmetry assumptions, force residual or the fractional variation from the true force distributions of the absolute magnitude of force for DM particles (green) and star particles (orange) within 50 kpc of the galactic center at the present day. The forces are reconstructed using fixed pole order ﹩{\left({\ell },m\right)}_{\max }=4﹩ and different symmetry conditions for the halo and the disk. The corresponding symmetry names and notation are provided in Table 2. The horizontal dotted lines represent the 25th and 75th quartiles of the distributions, while the dashed line represents the 50th quartile.
Paper: Efficient and Accurate Force Replay in Cosmological-baryonic Simulations
Authors: Arpit Arora, Robyn Sanderson, Christopher Regan, Nicolás Garavito-Camargo, Emily Bregou, Nondh Panithanpaisal, Andrew Wetzel, Emily C. Cunningham, Sarah R. Loebman, Adriana Dropulic, Nora Shipp
Figure caption: Performance over a range of orbital periods. Randomly selected reconstructed orbits (blue dashed lines) compared with the original trajectories (black solid lines) of stars from the simulation across Cartesian planes (first three columns from left) in physical coordinates, and in terms of the distance from the host center over time (rightmost column). The orbits are plotted in order of increasing orbital period (listed in the top-left corner in the leftmost panel in each row). The relative position error (see Equation (5)) at the final time step is listed in the top-right corner of the rightmost plot in each row. The method reconstructs orbits accurately across a factor of 20 in orbital periods and 100 in galactocentric distance.
Paper: Constraining the Location of the γ-Ray Emission Region in Radio-loud AGN 3C 380
Authors: Sanna Gulati, Debbijoy Bhattacharya, P. Sreekumar
Figure caption: The cross-correlation plot of the γ-ray and radio time lag analysis.
Paper: Efficient and Accurate Force Replay in Cosmological-baryonic Simulations
Authors: Arpit Arora, Robyn Sanderson, Christopher Regan, Nicolás Garavito-Camargo, Emily Bregou, Nondh Panithanpaisal, Andrew Wetzel, Emily C. Cunningham, Sarah R. Loebman, Adriana Dropulic, Nora Shipp
Figure caption: Example of orbit reconstruction. Real (black solid curve) and reconstructed (blue dashed curve) trajectories for a randomly selected star particle extracted from the simulation and integrated in the time-evolving multipole model from Section 2.2 for approximately 3.8 Gyr up to the present day in the X–Y (left) and R–Z (right) planes. The trajectories exhibit a close match, indicating a strong agreement between the real and reconstructed paths; positions at present day (i.e., the final time step of integration) are marked with a star. Figure 4 shows a sample of five other randomly selected orbits with varying orbital periods. All the trajectories are shown in physical coordinates.
Paper: Constraining the Location of the γ-Ray Emission Region in Radio-loud AGN 3C 380
Authors: Sanna Gulati, Debbijoy Bhattacharya, P. Sreekumar
Figure caption: Left panel: multiband light curve of 3C 380 using Swift and Fermi observations. The γ-ray light curve is monthly averaged. Right panel: the monthly averaged γ-ray light curve plotted with the VLBA total flux density. The gray shaded box highlights the γ-ray flare.
Paper: Constraining the Location of the γ-Ray Emission Region in Radio-loud AGN 3C 380
Authors: Sanna Gulati, Debbijoy Bhattacharya, P. Sreekumar
Figure caption: SED of 3C 380 during the preflaring period (AstroSat time) and flaring period (Swift time). The average γ-ray flux/UL and IR data of the steady state are plotted for a visual comparison.
Paper: Constraining the Location of the γ-Ray Emission Region in Radio-loud AGN 3C 380
Authors: Sanna Gulati, Debbijoy Bhattacharya, P. Sreekumar
Figure caption: Average (non-flaring) SED of 3C 380. The archival radio data, plotted in filled gray circles, is taken from ASDC. The mid- and far-IR data, plotted in open dark red circles, is taken from NED.
Paper: Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. III. Eddington Ratio Dependence on the Structures of Dusty and Dust-free Outflows
Authors: Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura
Figure caption: Radial profiles comparing the radiation-driven wind at ﹩\mathrm{log}\,{\gamma }_{\mathrm{Edd}}=0﹩ (left-hand side) and the thermal wind at ﹩\mathrm{log}\,{\gamma }_{\mathrm{Edd}}=-3﹩ for various angles, θ = 20 (dotted line), θ = 40 (dashed line), and θ = 60 (solid line). These profiles are obtained by averaging snapshots over the period of 4180 < t < 5573 yr, equivalent to 50 rotational times at R = 0.01 pc. Panels (a)–(d) on the right-hand side show the outflow velocity, sound speed, number density, and Mach number, respectively. The red solid lines in panels (a) denote the escape velocity, while panels (c) indicate the scaling with p = 2 of n(r) ∝ r −p .
Paper: Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. III. Eddington Ratio Dependence on the Structures of Dusty and Dust-free Outflows
Authors: Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura
Figure caption: (a) Obscuring fraction f obs of the numerical results as a function of the Eddington ratio for N H = 1024 cm−2 (blue) and N H = 1022 cm−2 (red). Filled circle symbols with solid lines represent the dust-free gas, and filled square symbols with dotted lines represent the dusty gas. (b) Comparison of the obscuring fraction between the numerical results for the dusty gas (red) for N H = 1022 cm−2 and observations: Gray square symbols with bars represent the median with ±1σ percentile of the observed IR sources combining the obscuring fraction f obs,IR K. Ichikawa et al. (2019). The Eddington ratios for each object are based on the results by M. J. Koss et al. (2021). (c) Same as (b), but for the dust-free gas. The black circle symbols with bars represent the observed X-ray data (C. Ricci et al. 2017).
Paper: Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. III. Eddington Ratio Dependence on the Structures of Dusty and Dust-free Outflows
Authors: Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura
Figure caption: The top panel is a typical radial profile of the outflow based on the analytical solution for ﹩\mathrm{log}{\gamma }_{\mathrm{Edd}}=0﹩. The bottom panel indicates the region of the dominated force and the typical radii on the ﹩\mathrm{log}r﹩–﹩\mathrm{log}{\gamma }_{\mathrm{Edd}}﹩ plane. Three dominant forces are delineated: acceleration by gas pressure (blue) and by dust-radiation force (orange), and deceleration by gravity (gray). These regions are distinguished by the dust sublimation radius (red solid line) and the critical point (black solid line). The dust-radiation force is also dependent on ΓEdd,d (dashed line), representing the optically thin case of A. C. Fabian et al. (2008). The right-hand side summarizes the processes and equations related to the analytic solutions.