adsabs/AstroCLIMB huggingface dataset:
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Distance from ASCC 79 in the plane of the sky against velocity along that separation vector for Cir-E members. The dashed line separates the two velocity components, Cir-Eb and Cir-Ea. We include the fit to the expansion trend in the CirCe Region from Figure 10 of R. Kerr et al. (2025) for reference.
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Left panels: the light curve, models, and residuals of OGLE-2018-BLG-0421 around the anomalous region. The residuals of each model are shown in separate panels with their χ2. Right panels: caustics and trajectories of 2L1S models for OGLE-2018-BLG-0421. The red curves are the caustics, and the black lines with arrows are the trajectories of the source-to-lens motion. The dashed circles mark the finite-source sizes ρ.
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Left panels: the light curve, models, and residuals of KMT-2019-BLG-0578 around the anomalous region. The residuals of each model are shown in separate panels, and their χ2 are presented. The two 2L1S models are visually identical; thus, only one (C) is presented. Right panels: caustics and trajectories of 2L1S models for KMT-2019-BLG-0578. The curves are the caustics, and the lines with arrows are the trajectories of the source-to-lens motion.
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: The 2L1S grid search χ2 distribution for OGLE-2018-BLG-0421 in ﹩(\mathrm{log}s,\mathrm{log}q,\alpha ,\mathrm{log}\rho )﹩ space (α is units of degrees). The colors are coded by the Δχ2. The recognized local minima within 10σ are labeled with their names.
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Same as Figure 2 but for events with newly identified planet-like signals.
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Flow chart of the anomaly search.
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Color–magnitude diagrams (CMDs) for the four new candidate planetary events. The black dots are the field stars within ﹩{2}^{{\prime} }\times {2}^{{\prime} }﹩ of each lensed source. The green dots stars are from HST observations toward Baade’s window (J. A. Holtzman et al. 1998) and have been offset to match the RC centroid. Colors and magnitudes are calibrated to OGLE-III (M. K. Szymański et al. 2011).
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Left panels: the light curves, models, and residuals for MOA-2022-BLG-038 around the anomalous region. The residuals of each model are shown in separate panels, and their χ2 are presented. Right panel: caustics and trajectories of 2L1S models for MOA-2022-BLG-038. The curves are the (planetary) caustics, and the lines with arrows are the trajectories of the source-to-lens motion. The magenta circle marks the source size ρ.
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: The ﹩(\mathrm{log}s,\mathrm{log}q)﹩ distribution of the newly discovered (pink) and recovered (blue) clear planets in the sample.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: We present the triaxial ellipsoid and contact binary models that best fit the observed lightcurve. We selected a couple of screenshots to visualize the object’s rotation at a rotational phase (φrot) of 0, 0.25, 0.50, 0.75, and 1 covering one full rotation. The overplotted continuous lines correspond to the best predicted lightcurves assuming a triaxial ellipsoid (blue) and a contact binary (red) fitting our observed lightcurve (gray circles corresponding to the observed data presented in Section 3.2). Lightcurves are plotted over two full rotation (i.e., rotational phase, φrot between 0 and 2.).
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: The most significant peak of the Lomb periodogram is located at 2.75 cycles/day (Plot a)). However, because of the lightcurve’s asymmetry and large amplitude, we select the double-peaked periodicity of 17.43 ± 0.06 hr (Plot b)). The overplotted Fourier series fit (black continuous line) is unable to match the data inferring that the lightcurve is not sinusoidal (Plot c)). The lightcurve is plotted over two rotations (i.e., rotational phase between 0 and 2) for an improved visualization of the cyclical brightness variation.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Phase coverage of observations for WASP-80b. The units of the axes are arbitrary. The observation dates are in UT and written as YYMMDD. The arrow in the Top-Down View designates the line of sight from Earth.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: An example H﹩{}_{3}^{+}﹩ model with log10(VMR) = −4.0 generated for cross correlation with the data, as described in Section 4.2.1. The blue section covers the wavelength range of our data. The models are sampled at a resolution of R ≈ 500,000 but are convolved with NIRSPEC’s instrument resolution of R ≈ 75,000. The planetary continuum is subtracted to yield the line contrast relative to the stellar continuum. The flux ratio is then Doppler shifted and interpolated onto the same wavelength grid as the data before cross correlation.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: PCA-cleaned data from 210913 with different number of principal components removed. The top panel shows the data cube input, where each horizontal cut of the cube is an individual spectrum. The telluric features with transmittance <80% are masked out. The bottom two panels show the remaining spectral cube after removing 1 and 6 principal components, thus removing the telluric and stellar features.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Average residuals of the PCA for WASP-80b, i.e., the average spectra with telluric features and stellar spectrum removed. This should just leave behind only the exoplanet spectrum. All spectra have been doppler shifted to the planet’s reference frame before averaging. Each panel is centered on an H﹩{}_{3}^{+}﹩ emission line at the transitions R(3,3), R(2,2), Q(1,0), Q(2,1), and Q(3,0). There are no clear H﹩{}_{3}^{+}﹩ emission features at these wavelengths.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Pressure–temperature profiles used in the generation of the exoplanet models, as described in Section 4.2.1.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Autocorrelation for WASP-80b. The spectra were aligned to the planet’s reference frame such that any correlated planet signatures would appear as a peak at a shift of 0 μm. However, no signal is seen in the autocorrelation.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Cross-correlation results for WASP-80b for each of the six model abundances. In each case, the dashed white lines represent the expected location of any H﹩{}_{3}^{+}﹩signature. However, no features are identified at a detection threshold of S/N > 3.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Same as Figure 1 but for WASP-69b. The orbit of WASP-69b is more inclined than WASP-80b.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Same as Figure 4 but for WASP-69b.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Same as Figure 8 but for WASP-69b.
Paper: An Extremely Hot Pulsating Prewhite Dwarf from OGLE
Authors: Paweł Pietrukowicz, Klaus Werner, Mateusz J. Mróz, Milena Ratajczak
Figure caption: OGLE-III I-band time-series data for object OGLE-GD-WD-0001 and results of the frequency analysis: distribution of the observations in time (top panel), cadence of the observations shown as a histogram of time differences between two subsequent exposures (second panel from the top), phase-folded original and prewhitened light curves together with the power spectra (lower panels). The frequency is given in cycles per day.
Paper: An Extremely Hot Pulsating Prewhite Dwarf from OGLE
Authors: Paweł Pietrukowicz, Klaus Werner, Mateusz J. Mróz, Milena Ratajczak
Figure caption: Color–magnitude diagram with the location of the blue object OGLE-GD-WD-0001.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: The measured RM values with 1σ error along the ridge line of Centaurus A. To help better visualize the observed RM variations, the zoom-in plots show the observed EVPA at different IFs at different regions of inflection along the jet and the corresponding FDFs. The 8σ noise threshold used in the FDF is shown using the dashed horizontal line. The locations of jet components are shown as shaded regions (as obtained from our 7.8 GHz frequency). We note that, due to having a larger restoring beam (due to having applied a constant uv-range cutoff at all IFs), we obtain a larger beam in the images used for RM synthesis as compared to the beam size in the 7.8 GHz kinematics study, resulting in RM structures in the central panel spanning beyond the C1 (CJ2) component along the approaching (receding) jet, due to image-based beam convolution effects. The dashed black lines in the zoom-in panels help guide the reader to visualize the slope (Faraday depth) of the Faraday rotation material at a given location along the jet.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: The fitted spectral index (along with 68% high-density intervals) along the ridge line of Centaurus A. Distances are measured from the base of the jet at 7.78  GHz, with positive distance values being along the approaching jet. In the zoom-in plots, we show the corresponding intensity values from each IF at the locations of jet components. Also, as can be seen from the central plot, we consistently get very similar spectral indices across all epochs.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: The distance of the CJ2 component, as measured from the phase center (peak intensity location in the image) of the epoch-wise stacked image, with 95% measurement errors. We also show the fitted core-shift function as the black dashed line, along with 68% and 95% high-density intervals of the fit in different shades of gray.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: The Faraday rotation corrected intrinsic electric field directions in the subparsec-scale jet of Centaurus A. In the background, we show the stacked 4.59 GHz image after having applied the uv-range cutoff described in Section 3.2. As the diagonal axis, we show the angular distance downstream as measured from the jet base at 7.8 GHz. As the electric fields are measured from the epoch-stacked image, they represent the directions of long-term persistent fields in the jet.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: The posterior of the fit apparent speed (β app is fractional light speed of the approaching jet component) and component ejection dates. The vertical green dashed line and the shaded area are the previously obtained values from the literature. Note that, due to components C3 and CJ2 having very slow speeds, we do not obtain any significant ejection date (the posterior is distributed over a very large range of dates).
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: The light curves for all the model components. We also show the historical flux density evolution for the identified components from previous studies.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: The constraints on inclination angle and intrinsic jet speed obtained from the proper motion and brightness ratio of Centaurus A’s approaching jet components. Together, they constrain the inclination angle of Centaurus A to be less than 25◦.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Montage of all images from epoch 1. The contour levels are at noise × 2 n , where n = 1, 2, 3, 4,.... For frequency bands with an asterisk next to the frequency, no reliable EVPA calibration could be performed. The vectors show the EVPA-corrected electric field directions but are not corrected for Faraday rotation.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Same as Figure 12, but for epoch 2.