adsabs/AstroCLIMB huggingface dataset:
Paper: Physics-informed Machine Learning for Modeling Turbulence in Supernovae
Authors: Platon I. Karpov, Chengkun Huang, Iskandar Sitdikov, Chris L. Fryer, Stan Woosley, Ghanshyam Pilania
Figure caption: Performance metrics of the PIML vs. gradient subgrid models. The top panel shows the ratio of the total turbulent pressure calculated from the model prediction to the target dynamic 3D DNS CCSN data; the middle panel shows the KS statistic; and the bottom panel shows the variance. In total, metrics at 10 checkpoints equally separated in time are presented in the plots.
Paper: Physics-informed Machine Learning for Modeling Turbulence in Supernovae
Authors: Platon I. Karpov, Chengkun Huang, Iskandar Sitdikov, Chris L. Fryer, Stan Woosley, Ghanshyam Pilania
Figure caption: A box filter with a Gaussian kernel (σ = 9) was used to filter the data. The figure shows a slice of sampled u  x , down to (116,116,116); the filter was applied prior to sampling. Left: original; right: filtered.
Paper: Physics-informed Machine Learning for Modeling Turbulence in Supernovae
Authors: Platon I. Karpov, Chengkun Huang, Iskandar Sitdikov, Chris L. Fryer, Stan Woosley, Ghanshyam Pilania
Figure caption: An example of the difference that a magnetic field can bring to the turbulence stress distribution. The data have been taken from JHTDB MHD and HD data sets (Li et al. 2008).
Paper: Physics-informed Machine Learning for Modeling Turbulence in Supernovae
Authors: Platon I. Karpov, Chengkun Huang, Iskandar Sitdikov, Chris L. Fryer, Stan Woosley, Ghanshyam Pilania
Figure caption: Model schematics to calculate the Reynolds stress (τ  ij ) components.
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Top panel: observed central wavelengths of ELGs’ emission lines λ obs vs. Δm NB816 before NB correction. Middle panel: λ obs vs. Δm NB816 after NB correction. Bottom panel: distribution of λ obs for Hα, [O III], and [O II] emitters. The light blue regions mark the wavelength range of 8127–8205 Å, which is used to select ELGs as the final ELG sample for the variability test. The red dashed lines show the variability cut of ∼0.2 mag. ELGs selected by HSC and SC are marked in open circles and open triangles, respectively. Var-ELGs are marked in solid symbols. AGN selected via X-ray, mid-infrared, radio-excess, and emission-line diagnostic methods are marked in stars. The colors shown here are consistent with those in Figure 3. The transmission curves of the SC NB816 (gray solid line) and the HSC NB816 (black solid line) filters are also overlapped in these figures to display the fake variable effect caused by the wing of an NB filter.
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Redshift distributions of ELG candidates selected with SC (left panel) and HSC (right panel). The distributions of photometric redshifts (COSMOS2015; Laigle et al. 2016) and spectroscopic redshifts (see Section 2.3, fourth paragraph for details) of ELG candidates are marked in pink and gray histograms, respectively. The spectroscopically confirmed Hα, [O III], and [O II] emitters are marked in red, blue, and green colors, respectively.
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Color–magnitude diagram for selecting candidate ELGs based on the NB816 and i′/i magnitude with SC (left panel) and HSC (right panel), respectively. The black dots represent all nonsaturated sources. Pink dots represent ELG candidates selected. The black dashed lines mark the magnitude excess for an observed line EW cut of 28 Å. Furthermore, the gray circles marked in the left panel are the saturated sources in the SC i′-band image because of the much lower saturation magnitude in the SC i′-band (i′SC,satur = 20.0) than the HSC i band (i HSC,satur = 18.6).
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Mid-infrared color–color diagram for AGN selection. ELGs and var-ELGs with IRAC detections in all four bands are marked in gray dots and squares, respectively. Four out of five var-ELGs have all four bands detection, and none of them are MIR AGN. X-ray selected AGN and star-forming galaxies are marked in blue stars and blue triangles, respectively. AGN selected by Delvecchio et al. (2017) via the radio-excess method are marked in red circles. AGN selected via the BPT diagnostic are marked in green diamonds. The sources within the dotted-line region are regarded as MIR AGN (Stern et al. 2005).
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Two-epoch magnitude differences vs. magnitudes with HSC of ELGs in the NB (left) and BB (right), respectively. Both NB magnitudes and NB-magnitude differences used here are corrected by the NB transmissions. The symbols, lines, and colors here are the same as Figure 4.
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Two-epoch magnitude differences in the NB and BB of our ELGs before and after NB correction (upper panel and lower panel, respectively). The ELGs selected in SC only, in HSC only, and in both SC and HSC are marked as orange squares, blue circles, and green triangles, respectively. The histograms of the magnitude differences are also presented.
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Processing flow on the sample selection of ELGs and variable ELGs.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: Images of NGC 7674 (a) and (b), and MCG-03-04-014 (c) and (d). These example images illustrate region identification, measurement, and classification procedures described in Sections 3 and 4.1. (a) and (c): native-resolution 33 GHz images, as displayed in Figure 2, with black contours outlining the areas of individual radio regions identified as leaf in a single run of Astrodendro. (b): 15–33 GHz spectral index map for NGC 7674 allows for the identification of synchrotron-dominated radio jets with steep spectra (α ∼ −1) and AGNs with flat spectrum (α ∼ 0). Black contours are the same as in panel (a). (d): Archival HST/NICMOS F160W is used to locate the nucleus and off-nuclear star-forming region identified in MCG-03-04-014, as shown in panel (c). In panels (b) and (d), region types classified following the methodology outlined in Section 4.1 are labeled. In each panel, the black ellipse represents the native synthesized beam.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: The distribution of derived properties of regions identified and characterized at native resolutions using Astrodendro. For direct comparison, we only show results derived from 33 GHz measurements, available for 99 native regions, excluding the “Bg” source in IC 0214 and 17 unresolved regions. Left: effective radius R  e . Middle: 33 GHz luminosity L 33. Right: 33 GHz luminosity surface density ﹩{{\rm{\Sigma }}}_{{L}_{33}}﹩. In all three columns, we also show distributions for “AGN” (magenta), “AGN/SBnuc” (green), “SBnuc” (yellow), and “SF” regions (blue), and the corresponding median values (dashed lines), overlaid on the distributions of all 99 native regions (gray). Results for “Jet” and “Ud” regions are not separately shown for simplicity. While all region types are distributed over similar size ranges, “AGN” and “AGN/SBnuc” have higher L 33 and ﹩{{\rm{\Sigma }}}_{{L}_{33}}﹩ than “SF” by an order of magnitude.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: The distribution of brightness temperatures of regions identified at native resolutions at 15 or 33 GHz. Left: values derived from Astrodendro measurements of region areas and flux densities. The distribution for all 133 native regions is shown by the black unfilled histogram. Right: values derived from Gaussian-fitting results using CASA imfit task. The distribution for 116 regions with successful fits is shown by the black filled histogram. In both panels, distributions for “AGN” (magenta), “AGN/SBnuc” (green), “SBnuc” (yellow), and “SF” (blue) are shown separately for comparison, with dashed lines marking the median values. Overall, “AGN” regions have the highest brightness temperatures, and Gaussian-fitting yields higher values, but only one “AGN” (in NGC 1068) exceeds the maximum starburst brightness temperature (∼ 104 K). The measured low brightness temperature for AGNs is likely due to beam dilution.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: Basic properties (Heliocentric velocity and 8–1000 μm IR luminosity) of the GOALS-ES sample. Each system is color-coded by its merger stage, using visual classification by Stierwalt et al. (2013). The sample covers the full range of IR luminosities, distances, and merger stages represented by the GOALS sample of all 201 local U/LIRGs.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: Examples of native-resolution 33 (top) and 15 GHz (bottom) images used in this work. Each image is displayed in linear stretch with bilinear interpolation, and the color bars show the brightness of the radio continuum emission, in the range of 0%–80% of the peak pixel value, in units of mJy beam−1. Synthesized beams (lower left) and scale bars of 100 pc (lower right) are shown.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: Region classification scheme described in Section 4.1 and demonstrated in Figure 3. Descriptions of individual galaxies are provided in Appendix A, including their multiwavelength AGN classifications and the ancillary data sets used. Numbers of native regions classified at each step are shown in brackets. Note that mid-IR (MIR) galaxy “core” sizes are measured by Díaz-Santos et al. (2010).
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Left: Monthly average values of northern (top), southern (middle), and full-disk (bottom) sunspot numbers measured at KO from 1905 to 2016. Right: Same as the left-side plot but for the 13th month smoothed data.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Left: Monthly average values of northern (top), southern (middle), and full-disk (bottom) sunspot group area (μHem) measured at KO from 1905 to 2016. Right: Same as the left-side plot but for the 13th month smoothed data.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: (a) Morlet wavelet spectra of the monthly KO sunspot group area time series in the northern hemisphere. (b) Global power spectra for short-term periods mainly to study the Rieger-group periodicities. (c) Local Morlet wavelet power spectra to investigate the dynamical behaviors of QBOs (1.4 to 4 yr) and other long-term periods including the solar cycle period. (d) Similar to panel (b) for other long-term periods including the Schwabe cycle. The dotted lines in all global wavelet power spectra represent the 95% confidence level.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: (a) Morlet wavelet spectra of the monthly KO sunspot number time series in the northern hemisphere. (b) Global power spectra for short-term periods mainly to study the Rieger-group periodicities. (c) Local Morlet wavelet power spectra to investigate the dynamical behaviors of QBOs (1.4–4 yr) and other long-term periods including the solar cycle period. (d) Similar to panel (b) for other long-term periods including the Schwabe cycle. The dotted lines in all global wavelet power spectra represent the 95% confidence level.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Wavelet plots showing the presence of the ∼22 yr Hale cycle in the hemispheric and full-disk sunspot number data sets.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: The sketches of sunspots, plages, filaments, and prominences are made on the Stonyhurst grid for two different days of observations. Specific colors are used to draw different features. The left-side image is for the date 1937 April 3, and the right side image is for the date 1957 January 21. The B 0 angle and p angle are shown the chart.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Same as Figure 4, but for the whole-disk data.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Same as Figure 4, but for the southern hemisphere.
Paper: Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae
Authors: Réka Könyves-Tóth
Figure caption: Top panel: premaximum spectra of Type W SLSNe-I sorted by phase. The W-shaped absorption feature is apparent near 4000–5000 Å in these spectra; this region is highlighted with purple. Bottom panel: premaximum spectra of Type 15bn SLSNe-I sorted by phase. The wavelength range, where the W-shaped feature is expected, is shaded with green. It is seen that such an absorption blend is missing from all spectra of Type 15bn objects. The narrow emission lines of the host galaxy, as well as the telluric absorption lines, were removed from all spectra before plotting.
Paper: Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae
Authors: Réka Könyves-Tóth
Figure caption: Chemical composition of the examined 27 SLSNe-I. On the vertical axis, the names of the studied SLSNe-I are listed, while the horizontal axis lists the possible identified ions. The horizontal red line divides Type W (above) and Type 15bn (below) SLSNe-I.
Paper: Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae
Authors: Réka Könyves-Tóth
Figure caption: The −22 day phase observed spectrum of SN 2010kd (black) together with its best-fit SYN++ model showing T phot = 15,000 K (red). A lower (T phot  =  13,000 K) and a higher (T phot  =  17,000 K) model is plotted as well with green and blue colors, respectively. The three models share the same global and local parameters with the exception of the photospheric temperature.
Paper: Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae
Authors: Réka Könyves-Tóth
Figure caption: Early premaximum spectra of Type W SLSNe-I . The observed spectra are plotted with black, while red color indicates the best-fit models obtained in SYN++. The single-ion contributions to the overall model (purple lines) are shifted vertically for clarification.
Paper: Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae
Authors: Réka Könyves-Tóth
Figure caption: Early premaximum spectra of Type 15bn SLSNe-I. The observed spectra (black lines) are plotted together with their best-fit SYN++ model (green lines). The contribution of the identified elements to the overall model spectra are shown with orange color, shifted vertically for clarification.
Paper: Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae
Authors: Réka Könyves-Tóth
Figure caption: Near-maximum spectra of Type W SLSNe-I with the same color-coding as Figure 2.
Paper: Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae
Authors: Réka Könyves-Tóth
Figure caption: Photospheric velocities as a function of photospheric temperatures of the 27 studied SLSNe-I obtained from SYN++ modeling. Type W SLSNe-I are plotted with red dots, while Type 15bn objects are shown with green dots.
Paper: Premaximum Spectroscopic Diversity of Hydrogen-poor Superluminous Supernovae
Authors: Réka Könyves-Tóth
Figure caption: Near-maximum spectra of Type 15bn SLSNe-I . The color-coding is the same as in Figure 4.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Examples of the ﹩\sin \,(2{\ell })﹩ form of the RM at intermediate positive latitudes. On the upper panel are profiles made from averaging the latitude range +35° < b < + 40°, with the GMIMS (DRAO) data shown in blue and the extragalactic (ExGal) RM grid (Hutschenreuter et al. 2022) shown in red. Error bars on the points show ±1σ of the distributions of values in each bin. The least-squares fit parameters are shown (Equation (1), see Table 1). In the lower panel is a similar pair of averages for +40° < b < + 45°. In each panel, the scatter plot on the right shows the correlation between the median values from GMIMS (x-axis) and the extragalactic sample. The Pearson correlation coefficient (R) is indicated, along with the slope of the best linear fit, shown with the red line.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Correlation slopes and amplitude ratios for the ﹩\sin \,(2{\ell })﹩ terms at midlatitudes. Slopes are plotted for latitudes having R > 0.5 only. Amplitude ratios are plotted only for +15 < b < + 50, for which all but one of the values of C 2 are greater than 5σ in both surveys. (The exceptions are latitudes 25°–30° in the GMIMS survey that have C 2 = 18.0 ± 4.0 rad m−2, i.e., 4.5σ, and latitudes 45°–50° in the extragalactic survey that have C 2 = 7.9 ± 1.6 rad m−2, i.e., 4.9σ.) The blue lines indicate the range of slopes expected for a uniform, Faraday thin slab. Values above 2 can arise in various ways, e.g., the diffuse emission is beginning to show depth depolarization. Values close to 1 suggest that the diffuse emission is behind most of the magnetoionic medium that causes the Faraday rotation in the extragalactic sample. A field reversal along the line of sight could explain values of the slope less than 1.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: The fitted phases of the ﹩\sin \,{\ell }﹩ and ﹩\sin \,(2{\ell })﹩ functions, i.e., ϕ 1 and ϕ 2 in Equation (1). In the northern hemisphere, ϕ 2 from both the GMIMS and the extragalactic fits are shown, in blue and red respectively. In the south, the extragalactic fits give ϕ 1 ≃ π. In the figure, we subtract π to get the black points on the same scale as the ϕ 2 values in the north. Note that both the error bars and the range of values for ϕ 1 naturally have about twice the range as for ϕ 2 because of the factor of 2 in the third term on the right of Equation (1). The conditions for including points on the plot are that R > 0.5 and the error in ϕ is small, i.e., σ  ϕ2 < 0.075 radians or σ  ϕ1 < 0.15 radians.