adsabs/AstroCLIMB huggingface dataset:
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: Stdfit of the SFD, Planck2014-R, Planck2014-Tau, and Planck2019–Tau maps as a function of reddening. The color of the dots indicates k err. In each panel, the dots are divided into different bins. The bin width is 0.01/0.1 mag when the extinction value is smaller/larger than 0.1 mag. For each panel, the yellow crosses represent the median values, the gray line represents a second-order polynomial fitting to the yellow crosses, and the black dashed line is obtained by shifting the gray line up by 2σ of the fitting. The dots above the black dashed lines are excluded.
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: Correction factor k as a function of ﹩E{\left(B-V\right)}_{\mathrm{map}}﹩ in different sky areas. Panels from left to right show the SFD, Planck2014-R, Planck2014-Tau, and Planck2019–Tau maps, respectively. For each panel, the sky area is labeled on the top, and the red crosses mark the median values. The trends with ﹩E{\left(B-V\right)}_{\mathrm{map}}﹩ are different between different areas for all the maps.
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: All-sky maps of k (or ﹩{k}^{{\prime} }﹩) (top), k fit (or ﹩{k}_{\mathrm{fit}}^{{\prime} }﹩) (middle), and the fitting residual Δk (or ﹩{\rm{\Delta }}{k}^{{\prime} }﹩) (bottom) for different reddening maps. Columns from left to right show the SFD, Planck2014-R, Planck2014-Tau, and Planck2019–Tau maps, respectively.
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: Typical dispersion values of the differences between ﹩E{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{\mathrm{LAMOST}}﹩ and ﹩E{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{\mathrm{map}}﹩ plotted against ﹩E({G}_{\mathrm{BP}}\,-{{G}_{\mathrm{RP}})}_{\mathrm{LAMOST}}﹩. The orange, blue, green, and pink dots represent results for the SFD, Planck2014-R, Planck2014-Tau and Planck2019–Tau dust maps, respectively.
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: Top row: dependence of ﹩{k}^{{\prime} }﹩ on dust temperature and spectral index for the Planck2014-Tau map. Second row: fitting residuals. Third row: fitting residuals as a function of dust temperature. Bottom row: fitting residuals as a function of spectral index. The first column shows the results of all pixels. The other four columns show the results of pixels in four different reddening ranges. One-fifth of all pixels are randomly selected to plot the results.
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: Comparisons between the fitting residuals Δk (or ﹩{\rm{\Delta }}{k}^{{\prime} }﹩) of the SFD, Planck2014-R, Planck2014-Tau, and Planck2019–Tau maps. The correlation coefficients R are labeled.
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: Top row: dependence of k on dust temperature and reddening for the SFD and Planck2014-R maps. Second row: fitting residuals. Third row: fitting residuals as a function of dust temperature. Bottom row: fitting residuals as a function of reddening. One-fifth of all pixels are randomly selected to plot the results.
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: All-sky distributions of ﹩E{\left(B-V\right)}_{\mathrm{LAMOST}}﹩ (left) and ﹩E{\left(B-V\right)}_{\mathrm{map}}﹩ (right). The panels top to bottom show the SFD, Planck2014-R, Planck2014-Tau, and Planck2019–Tau maps, respectively. Note the four maps on the left are different due to different reddening coefficients used.(The data used to create this figure are available.)
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: Histogram distributions of ﹩E{\left(B-V\right)}_{\mathrm{LAMOST}}-E{\left(B-V\right)}_{\mathrm{map}}﹩ (left) and k (right). The panels top to bottom show the SFD, Planck2014-R, Planck2014-Tau, and Planck2019–Tau maps, respectively.
Paper: Validations and Corrections of the SFD and Planck Reddening Maps Based on LAMOST and Gaia Data
Authors: Yang Sun, Haibo Yuan, Bingqiu Chen
Figure caption: Same as Figure 15 but for the Planck2019–Tau map.
Paper: Scalar Quadratic Maximum-likelihood Estimators for the CMB Cross-power Spectrum
Authors: Jiming Chen, Shamik Ghosh, Wen Zhao
Figure caption: Plot of the results for TE-mode power-spectrum estimates for the realistic ground-based CMB experiment. The observed sky is simulated at NSIDE = 512 with ﹩{{\ell }}_{\max }﹩ = 1024 and the noise level is set to 3μ K-arcmin. The input TE-mode power spectrum is shown with the black curve. The classic QML method results are shown with orange line, and QML-SZ method results are shown with green curve. These results are computed at NSIDE = 32. We also show PCL estimator results, obtained with NaMaster, with δ  c  = 10° C2 apodization, with blue line. The gray region denotes the analytical approximation of the error bounds. The data points are the mean of 1000 estimates, and the error bars are given by the standard deviation of the estimates.
Paper: Scalar Quadratic Maximum-likelihood Estimators for the CMB Cross-power Spectrum
Authors: Jiming Chen, Shamik Ghosh, Wen Zhao
Figure caption: Normalized covariance matrices ﹩{{ \mathcal C }}_{{\ell },{\ell }^{\prime} }=\mathrm{cov}({\hat{C}}_{{\ell }},{\hat{C}}_{{\ell }^{\prime} })/\sqrt{\mathrm{var}({\hat{C}}_{{\ell }})\mathrm{var}({\hat{C}}_{{\ell }^{\prime} })}﹩ of the QML methods for the space-based experiment. The matrices are obtained from estimates of 1000 simulations for the classic QML estimator (left) and for QML-SZ estimator (right).
Paper: Scalar Quadratic Maximum-likelihood Estimators for the CMB Cross-power Spectrum
Authors: Jiming Chen, Shamik Ghosh, Wen Zhao
Figure caption: Normalized covariance matrices ﹩{{ \mathcal C }}_{{\ell },{\ell }^{\prime} }=\mathrm{cov}({\hat{C}}_{{\ell }},{\hat{C}}_{{\ell }^{\prime} })/\sqrt{\mathrm{var}({\hat{C}}_{{\ell }})\mathrm{var}({\hat{C}}_{{\ell }^{\prime} })}﹩ of the QML methods for the ground-based experiment. The matrices are obtained from estimates of 1000 simulations for classic QML estimator (left) and for QML-SZ estimator (right).
Paper: The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way
Authors: Patryk Iwanek, Igor Soszyński, Szymon Kozłowski, Radosław Poleski, Paweł Pietrukowicz, Jan Skowron, Marcin Wrona, Przemysław Mróz, Andrzej Udalski, Michał K. Szymański, Dorota M. Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Milena Ratajczak
Figure caption: Three examples of Miras from our collection, observed in the BLG fields, with light curves containing a different number of epochs. Top row: a well-covered light curve of Mira OGLE-BLG-LPV-126082. The observations consist of 19,169 epochs that span 23 yr (from 1997 to 2020). Middle row: a medium-covered light curve of Mira OGLE-BLG-LPV-057864. The observations consist of 1593 epochs that span 19 yr (from 2001 to 2020). Bottom row: a poorly covered light curve of Mira OGLE-BLG-LPV-262970. The observations consist of 119 epochs that span 2 yr (from 2018 to 2020). The left-hand-side panels show unfolded light curves, while the right-hand-side panels show phase-folded light curves with pulsation periods P (provided above the plots). The dates at the tops of the unfolded light curves mark the year when the observations started and the year of the last used observations. The phases of the OGLE project are marked with different colors (red, green, and blue). For each star, we also provide the 60″ × 60″ finding chart, oriented with north up and east to the left. Each Mira is at the center of the finding chart, and is marked with a white cross.
Paper: The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way
Authors: Patryk Iwanek, Igor Soszyński, Szymon Kozłowski, Radosław Poleski, Paweł Pietrukowicz, Jan Skowron, Marcin Wrona, Przemysław Mróz, Andrzej Udalski, Michał K. Szymański, Dorota M. Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Milena Ratajczak
Figure caption: Three examples of Miras from our collection, observed in the GD fields, with light curves containing a different number of epochs. Top row: a well-covered light curve of Mira OGLE-GD-LPV-001623. The observations consist of 1307 epochs that span 7 yr (from 2013 to 2020). Middle row: a medium-covered light curve of Mira OGLE-GD-LPV-001263. The observations consist of 180 epochs that span 7 yr (from 2013 to 2020). Bottom row: a poorly covered light curve of Mira OGLE-GD-LPV-021201. The observations consist of 55 epochs than span 2 yr (from 2018 to 2020). The left-hand-side panels show unfolded light curves, while the right-hand-side panels show phase-folded light curves with pulsation periods P (provided above the plots). The dates at the tops of the unfolded light curves mark the year when the observations started and the year of the last used observations. The fourth phase of the OGLE project is marked with blue. For each star, we also provide the 60″ × 60″ finding chart, oriented with north up and east to the left. Each Mira is at the center of the finding chart, and is marked with a white cross.
Paper: The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way
Authors: Patryk Iwanek, Igor Soszyński, Szymon Kozłowski, Radosław Poleski, Paweł Pietrukowicz, Jan Skowron, Marcin Wrona, Przemysław Mróz, Andrzej Udalski, Michał K. Szymański, Dorota M. Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Milena Ratajczak
Figure caption: Two examples of stars that were classified as Miras by Soszyński et al. (2013), but whose amplitudes change significantly over time and fluctuate around 0.8 mag. Such stars were reclassified from Miras to SRVs and excluded from the sample. The left-hand-side panels show unfolded light curves, while the right-hand-side panels show phase-folded light curves with pulsation periods P (provided above the plots). The dates at the tops of the unfolded light curves mark the years when the observations started and the year of the last used observations. The individual phases of the OGLE project are marked with different colors.
Paper: The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way
Authors: Patryk Iwanek, Igor Soszyński, Szymon Kozłowski, Radosław Poleski, Paweł Pietrukowicz, Jan Skowron, Marcin Wrona, Przemysław Mróz, Andrzej Udalski, Michał K. Szymański, Dorota M. Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Milena Ratajczak
Figure caption: Distribution of Miras (black points) in the Galactic coordinates. Our catalog contains 40,356 Mira-type variables in the BLG and 25,625 in the GD. The gray area shows the OGLE-IV footprint of the Milky Way.
Paper: The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way
Authors: Patryk Iwanek, Igor Soszyński, Szymon Kozłowski, Radosław Poleski, Paweł Pietrukowicz, Jan Skowron, Marcin Wrona, Przemysław Mróz, Andrzej Udalski, Michał K. Szymański, Dorota M. Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Milena Ratajczak
Figure caption: Distributions of the I-band mean magnitudes (top left), V-band mean magnitudes (top right), pulsation periods (bottom left), and I-band amplitudes (bottom right) for the Miras in the BLG (gray histograms) and GD fields (red dashed histograms).
Paper: The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way
Authors: Patryk Iwanek, Igor Soszyński, Szymon Kozłowski, Radosław Poleski, Paweł Pietrukowicz, Jan Skowron, Marcin Wrona, Przemysław Mróz, Andrzej Udalski, Michał K. Szymański, Dorota M. Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Milena Ratajczak
Figure caption: 14 examples of Mira stars from our catalog that were observed from 1997, i.e., the beginning of the OGLE-II phase, until 2020 March. The left-hand-side panels show unfolded light curves, while the right-hand-side panels show phase-folded light curves with pulsation periods P (provided above the plots). The dates at the tops of the unfolded light curves mark the year when the observations started and the year of the last used observations. The individual phases of the OGLE project are marked with different colors (red, green, and blue).
Paper: The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way
Authors: Patryk Iwanek, Igor Soszyński, Szymon Kozłowski, Radosław Poleski, Paweł Pietrukowicz, Jan Skowron, Marcin Wrona, Przemysław Mróz, Andrzej Udalski, Michał K. Szymański, Dorota M. Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Milena Ratajczak
Figure caption: The same as Figures 5 and 6, but 14 other Miras are presented.
Paper: The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way
Authors: Patryk Iwanek, Igor Soszyński, Szymon Kozłowski, Radosław Poleski, Paweł Pietrukowicz, Jan Skowron, Marcin Wrona, Przemysław Mróz, Andrzej Udalski, Michał K. Szymański, Dorota M. Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Milena Ratajczak
Figure caption: The same as Figure 5, but 14 other Miras are presented.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of the apparent speeds of all moving knots (left), and weighted average of the apparent speed for each source (right) detected in FSRQs (top), BL Lac objects (middle), and RGs (bottom).
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Host-galaxy frame brightness temperature distributions of the core (left) and noncore (knots, right) features between 2013 January and 2018 December. Unshaded regions of the distributions represent components with lower limits to ﹩{T}_{{\rm{b}},\mathrm{obs}}^{{\rm{s}}}﹩. The bin sizes are neither linear nor logarithmic. Values in parentheses are the number of T b,obs measurements of components for each subclass, including lower limits.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Median core component host-galaxy frame brightness temperature distributions of blazars in the VLBA-BU-BLAZAR sample, as determined through survival analysis. The bin sizes are neither linear nor logarithmic.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Median knot component host-galaxy frame brightness temperature distributions of blazars in the VLBA-BU-BLAZAR sample, as determined through survival analysis. The bin sizes are neither linear nor logarithmic.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Total intensity images of the VLBA-BU-BLAZAR sample at 43 GHz with uniform weighting. Parameters of all images are listed in Table 4. Contours decrease by a factor of ﹩\sqrt{2}﹩ from the peak flux density. Black circles on the images indicate the jet features according to the model fits. The shaded ellipse in the bottom-left corner represents the restoring beam.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of the differences between the velocity vector, Φ, and the jet axis, 〈Θjet〉, in FSRQs (top), BL Lac objects (middle), and RGs (bottom).∣Φ − 〈Θjet〉∣ > 90° indicates slow or upstream motion of the knot segment.
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: Cumulative distribution of differences between jet directions in the same AGN determined at frequency pairs with the largest numbers of overlapping objects: 2–8 GHz, 5–8 GHz, 8–15 GHz. Additionally, we show the comparison of 15 GHz measurements to those estimated within the MOJAVE program (Lister et al. 2019 uses the same 15 GHz observations).
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: An example of the piecewise linear fitting procedure described in Section 2.2 for the knot C35 of the FSRQ 1253–055. The three panels represent the total distances from the core along the (a) radial R-axis, (b) X-axis (relative R.A.), and (c) Y-axis (relative decl.). The red lines represent the piecewise linear fits to the data, while the gray dotted lines indicate break-point dates. The fit line in (a) is constructed from the combination of the fits in (b) and (c). The estimated epoch of ejection, t ◦, is shown in (a) as a horizontal red line. See the text for details.
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: Comparison of the average formal model-fitting uncertainty ﹩\overline{{\sigma }_{\mathrm{PA}}}﹩ derived from individual single-epoch measurements with the intraband scatter std(PA). Only AGNs with at least 10 measurements at the corresponding frequency are shown here. The majority of the points lie below the top dotted line: the scatter is less than 5 times the formal uncertainty for about 90% of the objects.
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: Distribution of jet direction differences: same as Figure 9, but for measurements performed in two other works, Plavin et al. (2019a) (top) and Blinov et al. (2020) (bottom).
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: VLBI images of the same AGN at 8 and 2 GHz. The lower-frequency jet direction was flipped following the criteria outlined in Section 3. The residual difference between these directions is attributed to apparent jet bending.
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: VLBI images illustrating the jet direction determination at the shortest angular scales possible. Note the arrow length that corresponds to the separation between the two model components. Left: an example of a straight jet. Middle: the jet is not visible at the restored image, but our visibility-based approach successfully detects it. See the right panel showing the same AGN observed at a higher frequency: the jet orientation is in agreement.
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: VLBI images of the two AGNs where we had to explicitly flip the jet direction due to the available information from specific detailed studies. See the discussion in Section 4.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Timescale of variability of the size vs. that of the flux density for superluminal knots in our sample. “Reliable” estimates of τ a (for which ﹩{\tau }_{{\rm{a}}}\geqslant 2{\sigma }_{{\tau }_{{\rm{a}}}}﹩) are shown in black, while those that do not meet the reliability criterion are shown in red. The solid line marks the approximate relation for an optically thin shock with α ∼ 0.7 (Marscher & Gear 1985). Error bars are omitted for visual clarity.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Left: distribution of the projected distances from the core to the stationary features in our sample. Right: trajectories of the stationary features A1 in 0528+134 (FSRQ, red circles), A2 in 1749+096 (BL, blue squares), and A1 in 0430+052 (RG, green triangles) with respect to the core, A0 (the black cross at position (0,0)). The solid lines show 2σ confidence ellipses used to characterize the dispersion and orientation of the knot motion.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Histograms of relative knot accelerations (left) parallel and (right) perpendicular to the jet axis for all sources, separated by distance from the 43 GHz core. Red vertical lines in all panels indicate the median acceleration, while the gray dotted vertical lines indicate no acceleration.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of the differences between the major axis orientation angles, ϖ, and 〈Θjet〉, in FSRQs (top), BL Lac objects (middle), and RGs (bottom). See the text for details.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Left: distances from the 43 GHz core to the acceleration region and stationary feature closest to that acceleration region. The vertical segments of data correspond to sources that contain multiple knots with acceleration zones beyond the last stationary feature. The gray shaded region delineates the portion of the figure that is expanded for better viewing in the right panel. Error bars are shown in gray in both panels.