adsabs/AstroCLIMB huggingface dataset:
Paper: Quasi-thermal Noise Spectroscopy Analysis of Parker Solar Probe Data: Improved Electron Density Model for Solar Wind
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, Marc Pulupa, Stuart D. Bale
Figure caption: Comprehensive display of electron density measurements from the initial 15 encounters of the Parker Solar Probe mission, covering radial distances from the Sun between 13 and 100 R ☉. Each panel pertains to an individual encounter, representing a timeframe of 7 days before and after the closest approach to the Sun (perihelion). The color-coded markers indicate the electron density measurements, with the color scale signifying different encounter groups based on their perihelion distances.
Paper: Quasi-thermal Noise Spectroscopy Analysis of Parker Solar Probe Data: Improved Electron Density Model for Solar Wind
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, Marc Pulupa, Stuart D. Bale
Figure caption: Example analysis from Encounter 15. (a) and (b) Frequency ranges denoted by dotted lines for channel 0 and 1, respectively. (c) and (d) Spectra in the frequency range of interest and narrower intensity range with black circles denoting actual data points measured by RFS/LFR.
Paper: Quasi-thermal Noise Spectroscopy Analysis of Parker Solar Probe Data: Improved Electron Density Model for Solar Wind
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, Marc Pulupa, Stuart D. Bale
Figure caption: Comparison of relative differences between the three density models and the QTN data below 50 R ☉, illustrating the accuracy of the derived power-law model. The shaded regions beneath the histograms signify the FWHM. Magenta lines depict Gaussian fits using data points above the FWHM, with the associated parameters provided in the legend.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: Grotrian term diagram of Y II. The ionization energy is shown by the solid horizontal line. The dashed lines indicate the transitions where the investigated spectral lines arise.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: Grotrian term diagram of Y I. The ionization energy is shown by the solid horizontal line. The dashed lines indicate the transitions, where the investigated spectral lines arise.
Paper: Magnetic Structures and Turbulence in SN 1006 Revealed with Imaging X-Ray Polarimetry
Authors: Ping Zhou, Dmitry Prokhorov, Riccardo Ferrazzoli, Yi-Jung Yang, Patrick Slane, Jacco Vink, Stefano Silvestri, Niccolò Bucciantini, Estela Reynoso, David Moffett, Paolo Soffitta, Doug Swartz, Philip Kaaret, Luca Baldini, Enrico Costa, C.-Y. Ng, Dawoon E. Kim, Victor Doroshenko, Steven R. Ehlert, Jeremy Heyl, Frédéric Marin, Tsunefumi Mizuno, Melissa Pesce-Rollins, Carmelo Sgrò, Toru Tamagawa, Martin C. Weisskopf, Fei Xie, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Giorgio Matt, Ikuyuki Mitsuishi, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger W. Romani, Gloria Spandre, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Kinwah Wu, Silvia Zane
Figure caption: Field of view of the two IXPE observations overlaid on the XMM-Newton 2–8 keV image of SN 1006 (Li et al. 2016). The plus sign denotes the SNR center (15h02m51.ˢ7, ﹩-41^\circ 56^{\prime} 33^{\prime\prime} ﹩, J2000) located by Reynolds & Gilmore (1986) and Winkler & Long (1997).
Paper: Magnetic Structures and Turbulence in SN 1006 Revealed with Imaging X-Ray Polarimetry
Authors: Ping Zhou, Dmitry Prokhorov, Riccardo Ferrazzoli, Yi-Jung Yang, Patrick Slane, Jacco Vink, Stefano Silvestri, Niccolò Bucciantini, Estela Reynoso, David Moffett, Paolo Soffitta, Doug Swartz, Philip Kaaret, Luca Baldini, Enrico Costa, C.-Y. Ng, Dawoon E. Kim, Victor Doroshenko, Steven R. Ehlert, Jeremy Heyl, Frédéric Marin, Tsunefumi Mizuno, Melissa Pesce-Rollins, Carmelo Sgrò, Toru Tamagawa, Martin C. Weisskopf, Fei Xie, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Giorgio Matt, Ikuyuki Mitsuishi, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger W. Romani, Gloria Spandre, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Kinwah Wu, Silvia Zane
Figure caption: IXPE images of the northeastern shell of SN 1006 in the 2–4 keV band. Upper left: Stokes I image with a pixel size of 10″. Upper right: polarized signal (﹩\sqrt{{Q}^{2}+{U}^{2}};﹩ right) image binned with a pixel size of ﹩1\buildrel{\,\prime}\over{.} 5﹩. Lower left: PD distribution for pixels with Stokes I >158 counts (to mask out pixels with low X-ray brightness), overlaid with magnetic vectors and their 1σ errors. The blue and red vectors correspond to pixels with a pretrial significance of 2σ–3σ and >3σ, respectively. The length of the magnetic vectors scales with the polarized degree. Lower right: the posttrial confidence level for the detection of the polarized signal. The white contours show the Stokes I levels.
Paper: Magnetic Structures and Turbulence in SN 1006 Revealed with Imaging X-Ray Polarimetry
Authors: Ping Zhou, Dmitry Prokhorov, Riccardo Ferrazzoli, Yi-Jung Yang, Patrick Slane, Jacco Vink, Stefano Silvestri, Niccolò Bucciantini, Estela Reynoso, David Moffett, Paolo Soffitta, Doug Swartz, Philip Kaaret, Luca Baldini, Enrico Costa, C.-Y. Ng, Dawoon E. Kim, Victor Doroshenko, Steven R. Ehlert, Jeremy Heyl, Frédéric Marin, Tsunefumi Mizuno, Melissa Pesce-Rollins, Carmelo Sgrò, Toru Tamagawa, Martin C. Weisskopf, Fei Xie, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Giorgio Matt, Ikuyuki Mitsuishi, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger W. Romani, Gloria Spandre, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Kinwah Wu, Silvia Zane
Figure caption: Stokes I image with regions and the polar plots of these regions in the 2–4 keV band. In the first panel, the regions delineated with solid and dashed lines correspond to the source and background regions, respectively. Each polar plot shows the PD (%) and PA in radial and position angle coordinates, respectively, with the background subtracted. The best-fit PD and PA values are denoted by black dots. The 50%, 90%, 99%, and 99.9% confidence levels (based upon χ 2 on two degrees of freedom) are coded in red, orange, green, and blue, respectively.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: Comparison of the CH2DOH line frequencies (a) between our measurement (Freq.(this work)) and calculation (Freq.(JPL)), and (b) between our measurement and the measurement reported by Pearson et al. (2012; Freq.(Pearson et al.)). The red circles, blue triangles, and green rhombuses indicate the Q-branch (K  a  = 2 − 1) for e 0, e 1, and o 1, respectively.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: Spectra of CH2DOH. The upper panel is the measured spectrum, where line intensities are multiplied by a scaling factor of 1.053. The lower panel is the calculated spectrum based on the JPL database, where the temperature and the column density are 296.1 ± 1.2 K and ﹩({2.32}_{-0.02}^{+0.03})\times {10}^{16}﹩ cm−2, respectively, and the FWHM line width is fixed to 0.6 MHz.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: Time variation in the gas pressure in the cell, where the time of cell closure is set to zero. The introduction of CH3OH gas into the cell is completed at 2 minutes. The gray square points show the measured pressure. The red filled circles show the pressure after the subtraction of the leak effect.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: Comparison between the CH3OH line intensities determined by the experiment and those listed in the CDMS. The dotted lines indicate a range of the experimental error of ±6%. Note that partially overlapped two lines are fitted with a double-Gaussian function as described by Ohno et al. (2022), and the integrated intensity for each line is calculated from the peak intensity and the line width with a correction factor of 1.05 for the contribution of the skirt component.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: Typical line shape of CH2DOH measured with SUMIRE. The solid and dashed lines show the measured spectrum and the result of the Gaussian fitting, respectively.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: Ratios between the S μ 2 values derived in this study and those listed in the JPL database for the b-type Q-branches in CH2DOH. The K  a  = 1 − 0 series lines of o 1 are outside the measurable frequency range.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: Ratios between the S μ 2 values derived in this study and those listed in the JPL database for the c-type Q-branches in CH2DOH.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: Ratios between the S μ 2 values derived in this study and those listed in the JPL database for the a-type R-branches in CH2DOH.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: Best NLTE fits (continuous red curve) to the solar flux line profiles (black circles) of Y I 4128, 4674, 6435 Å and Y II 4124, 4374, 4398, 4883, 4900, 5087, 5200, 5205, 5289 Å. For each line, the LTE profile (dashed blue curve) was computed with the yttrium abundance obtained from the NLTE analysis.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: Stellar NLTE yttrium-to-iron abundance ratios as a function of metallicity for 65 stars; and the [Y/Fe]–[Fe/H] ratio for the solar neighborhood models with s-process only (dashed line) and with s- and r-processes (solid line) from Kobayashi et al. (2020). Different symbols correspond to different stellar populations, namely, the thin disk (open circles), the thick disk (filled circles), and the halo (asterisks).
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: NLTE abundance ratios between the neutron-capture elements. The same symbols are used as in Figure 10.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: Departure coefficients as a function of log τ 5000 for the lower and upper levels of the Y I line at 4128 Å in the model 5777/4.44/0 (upper panel) and for the lower and upper levels of the Y II line at 5087 Å in the model 4600/1.43/−2.55 (bottom panel). The line formation regions are shown by gray shadow vertical lines. Right panels: theoretical line profiles of the investigated lines calculated with LTE and NLTE for the particular atmospheric models.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: Departure coefficients for the Y I levels (left column) and the Y II levels (right column) as a function of log τ 5000 in the model atmospheres with 5777/4.44/0 (top row) and 5780/3.7/−2.46 (bottom row).
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: Yttrium LTE (open symbols) and NLTE (filled symbols) abundances of a few program stars derived from Y I (circles) and Y II (squares) lines in the wide spectral region.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: NLTE abundance corrections as functions of [Fe/H] for selected Y II lines at 4398, 4883, 4900, and 5087 Å for three sets of stellar parameters T eff/log g = 5000/2.0, 5000/4.0, and 6000/4.0. Everywhere, V mic = 2 km s−1 and [Y/Fe] = 0.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: [Y/Fe] LTE (left panel) and NLTE (right panel) ratios obtained from Y I and Y II lines. The error bars correspond to the dispersion in the single line measurements about the mean.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: The fractions of Y I, Y II, and Y III in the model atmospheres with different stellar parameters.
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Seismic mass vs. [C/Fe] (left panel); seismic mass vs. [N/Fe] (right panel) for our CDGs, the previously known wGb stars, underluminous stars from Li et al. (2022), Li-rich giants from Yan et al. (2021), and a large sample of RC stars from Mosser et al. (2014) and Yu et al. (2018) with symbols having the same meaning as in Figure 12. We determine luminosities for the Li-rich giants in the same manner as our CDGs, detailed in Section 3.2. Using this, we estimated the seismic masses of these stars using mass Equation (3). Six of our normal-luminosity-RC CDGs are included in the Li-rich study of Yan et al. (2021). They overlap with the Li-rich giants with a slight offset in seismic mass. The “normal” RC stars show a correlation between mass and nitrogen (and carbon) abundance. This reflects FDU surface pollution from early on in the RGB (e.g., Iben & Renzini 1984). The trend shows fairly sharp edges, allowing us to make a cut in N (or C) that varies with mass (dashed lines). This helps in distinguishing the chemically peculiar stars. To the right of the N line, the stars can be considered N-rich, for their mass. The vertical shaded region at [N/Fe]= +0.8 ± 0.05 dex, denotes the upper limit of our CDG sample's N-enhancement as well as the highest N abundance possible if the ON cycle was activated after all C is burned to N (see the text for details). Solar abundances are from Grevesse et al. (2007).
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Schematic representation of the possible steps in a HeWD plus RGB star merger leading to the formation of a red clump star with a carbon-poor and nitrogen-rich surface. This illustration is based on Figure 5 in Postnov & Yungelson (2014) and Figure 2 in Zhang & Jeffery (2013).
Paper: Turbulent Structure in Supernova Remnants G46.8−0.3 and G39.2−0.3 from THOR Polarimetry
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Ralf S. Klessen, Michael Rugel, Juan D. Soler
Figure caption: (a) Map of σ  ϕ  for SNR G39.2−0.3. Contour levels are 20, 30, 55, 80, 110, and 140 mJy beam−1 from THOR+VGPS Stoke I at 21 cm. Subregions with a purple border indicate two-component Faraday rotation from Shanahan et al. (2022) and are not included when QU fitting using a model of single-component Faraday rotation with Burn depolarization. (b) Effelsberg polarization intensity map of G39.2−0.3 at6 cm with Stokes I contours at 0.5, 1.0, 2.0, 3.0, and 4.0 K. The red circles identify regions where we compare THOR polarization to Effelsberg polarization. The size of the red circles correspond to the Effelsberg beam of 2.′5. The coordinates of each region are given in Table 1.
Paper: Turbulent Structure in Supernova Remnants G46.8−0.3 and G39.2−0.3 from THOR Polarimetry
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Ralf S. Klessen, Michael Rugel, Juan D. Soler
Figure caption: (a) Map of σ  ϕ  for SNR G46.8−0.3. Contour levels are 14, 19, 24, 29, 34, and 39 mJy beam−1 from THOR+VGPS Stoke I at 21 cm. Subregions with a purple border indicate two-component Faraday rotation from Shanahan et al. (2022) and are not included when QU fitting using a model of single-component Faraday rotation with Burn depolarization. (b) Effelsberg polarization intensity map of G46.8−0.3 at 6 cm with Stokes I contours at 0.2, 0.4, 0.6, 0.8, 1.0, 1.2, and 1.4 K. The red circles identify regions where we compare THOR polarization to Effelsberg polarization. The size of the red circles correspond to the Effelsberg beam of 2.′5. The coordinates of each region are given in Table 1.
Paper: Turbulent Structure in Supernova Remnants G46.8−0.3 and G39.2−0.3 from THOR Polarimetry
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Ralf S. Klessen, Michael Rugel, Juan D. Soler
Figure caption: Observed and corrected SFs for SNRs G46.8−0.3 (a) and G39.2−0.3 (b). The colored solid lines are power-law fits to the SNR SFs. The black solid lines are power-law fits to the simulated point-source (individual pixel) SFs, which have been extended to where they equal the median of the simulation box plot. The box plots are generated from the distribution of ﹩2{\sigma }_{\phi }^{2}﹩ for the SNR (colored) and the simulation (black). The red lines in the box plots are the median of each ﹩2{\sigma }_{\phi }^{2}﹩ distribution, the bottom and top of the box are the first and third quartiles, respectively, and the whiskers extend to the maximum and minimum values in the distribution. The vertical dashed lines represent the THOR beam of 16″. The SFs are discussed in Section 4.1 and the box plots are discussed in Section 4.2.
Paper: Turbulent Structure in Supernova Remnants G46.8−0.3 and G39.2−0.3 from THOR Polarimetry
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Ralf S. Klessen, Michael Rugel, Juan D. Soler
Figure caption: SFs for EGRSs and the corrected SNR SFs. The solid and dashed black lines are power-law fits to the EGRS at θ > 0.°57 and θ < 1.°25, respectively. The purple and green solid lines are power-law fits to the corrected SFs of G46.8−0.3 and G39.2−0.3, respectively. The shaded red region is the approximate SF for Galactic Faraday rotation in the foreground of the SNRs. The yellow crosses are derived from the ATNF pulsar catalog (Manchester et al. 2005). Each cross represents a pair of pulsars with an angular separation of θ and an amplitude derived with Equation (5) with N = 1. The blue squares, from left to right, indicate the median values for angular scales 0.°1 < θ ≤ 1°, 1° < θ ≤ 3°, and 3° < θ ≤ 10°.