adsabs/AstroCLIMB huggingface dataset:
Paper: Multistructured Accretion Flow of Sgr A*. II. Signatures of a Cool Accretion Disk in Hydrodynamic Simulations of Stellar Winds
Authors: Mayura Balakrishnan, Christopher M. P. Russell, Lia Corrales, Diego Calderón, Jorge Cuadra, Daryl Haggard, Sera Markoff, Joey Neilsen, Michael Nowak, Q. Daniel Wang, Frederick Baganoff
Figure caption: Left: line profiles generated by plasma simulated in the 0″–1.″5 source region (top) and 1.″5–5″ background region (bottom). Middle and right: predicted counts histograms calculated for HEG +1 (middle) and HEG −1 (right) for the disk (solid curves) and no-disk (dashed curves) plasma scenarios in the stellar wind simulation. We plot the source and background regions in purple and red, respectively. The small differences between the final spectra with and without a cold gas disk are slight and not resolvable with Chandra HETGS, differing only by ∼2.6% at the peaks. We are thereby unable to detect evidence of the ∼104 K disk from X-ray spectroscopy alone.
Paper: Multistructured Accretion Flow of Sgr A*. II. Signatures of a Cool Accretion Disk in Hydrodynamic Simulations of Stellar Winds
Authors: Mayura Balakrishnan, Christopher M. P. Russell, Lia Corrales, Diego Calderón, Jorge Cuadra, Daryl Haggard, Sera Markoff, Joey Neilsen, Michael Nowak, Q. Daniel Wang, Frederick Baganoff
Figure caption: The anticipated NewAthena photon counts spectra for the stellar wind plasma models (red) under both disk (solid) and quasi-steady (dotted–dashed) accretion scenarios in the Fe Kα region. The best-fit RIAF and contours from Paper I are overlaid in blue. The stellar wind model will be differentiable from the RIAF model, and it is possible, with a high signal-to-noise ratio, to detect signatures of the cold disk in the X-ray plasma.
Paper: Multistructured Accretion Flow of Sgr A*. II. Signatures of a Cool Accretion Disk in Hydrodynamic Simulations of Stellar Winds
Authors: Mayura Balakrishnan, Christopher M. P. Russell, Lia Corrales, Diego Calderón, Jorge Cuadra, Daryl Haggard, Sera Markoff, Joey Neilsen, Michael Nowak, Q. Daniel Wang, Frederick Baganoff
Figure caption: The high-resolution quiescent spectrum of Sgr A*, extracted in Corrales et al. (2020), plotted in counts. The top and bottom panels show the data from the HEG +1 and −1 orders, respectively. In this work, we focus on the Fe Kα complex between 6.4 and 7.2 keV. The spectra extracted from the source (out to 1.″5) and background (between 1.″5 and 5″) regions are plotted in black and blue, respectively, and are rebinned to a factor of 3.
Paper: Multistructured Accretion Flow of Sgr A*. II. Signatures of a Cool Accretion Disk in Hydrodynamic Simulations of Stellar Winds
Authors: Mayura Balakrishnan, Christopher M. P. Russell, Lia Corrales, Diego Calderón, Jorge Cuadra, Daryl Haggard, Sera Markoff, Joey Neilsen, Michael Nowak, Q. Daniel Wang, Frederick Baganoff
Figure caption: Final fits to the HEG +1 and −1 source and background regions. The observation is plotted in black, with the best-fit RIAF model in blue and the stellar wind simulations in pink. The residual counts spectrum (observation − model) is plotted below each subplot. The data are binned to a factor of 4 for visual clarity; however, the fitting was performed on the unbinned HEG data. While the models capture the 6.7 keV peak in the source spectrum, most of the observed line structure is not predicted in the simulations.
Paper: Multistructured Accretion Flow of Sgr A*. II. Signatures of a Cool Accretion Disk in Hydrodynamic Simulations of Stellar Winds
Authors: Mayura Balakrishnan, Christopher M. P. Russell, Lia Corrales, Diego Calderón, Jorge Cuadra, Daryl Haggard, Sera Markoff, Joey Neilsen, Michael Nowak, Q. Daniel Wang, Frederick Baganoff
Figure caption: Histograms showing the Cash statistic from the posterior distributions of both the RIAF (blue) and stellar wind (pink) simulation fits.
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Comparison of time-averaged MAD (left) and SANE (right) GRMHD simulations of M87* (top row) with the best-fitting equatorial (second row), dual-cone (third row), and combination (equatorial + dual-cone) models (fourth row). These two simulations are representative of the minimal and maximal emission scale heights that are typically seen in GRMHD simulations of M87*. The best-fitting models are determined by maximizing the normalized cross correlation in the image domain. The text in each panel gives the opening angle of the cone (θ  s ), the viewing inclination (θ o), the black hole spin (a), and the mass-to-distance ratio (θ  g ). The bottom row compares the fitted emissivity functions of our models (colored lines) to the true emissivity of the GRMHD (grayscale). The predicted emissivities are consistent with those of the GRMHD, as is evident by their overlap, which illustrates our model’s ability to perform photogrammetry in black hole spacetimes.
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Best-fitting equatorial, dual-cone, and combination (equatorial + dual-cone) models to a time-averaged retrograde R high = 160 MAD GRMHD simulation of Sgr A* viewed at inclinations of 30°, 50°, 70°, and 90° (from left to right). The NxCORR score for all models is above 0.85 and increases as the black hole is viewed more face-on. In addition, the parameters of the best-fitting models are within a few percent of the true parameters for both mass and spin at low-to-modest inclinations. As expected, the dual-cone model (13 parameters) outperforms the equatorial model (12 parameters) despite having only a single additional parameter. In contrast, the combination model (23 parameters) provides only marginal additional improvement despite nearly doubling the number of parameters. Table 4 lists the parameters for each model.
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Schematic depiction of our dual-cone emission model. The full model consists of a Kerr black hole (black sphere) surrounded by synchrotron-emitting plasma (green arrows) confined to a cone of opening angle θ  s  and threaded by a magnetic field ﹩{\boldsymbol{B}}﹩ (red field lines). The magnetic field and plasma are taken to be axisymmetric about the equatorial plane. The emission is concentrated at a characteristic radius, R, with the profile determined by a double power-law distribution with exponents p 1 and p 2 (translucent blue cone). The polarization from the synchrotron radiation is parallel transported along null-geodesics (yellow and orange ticked trajectories) to generate an image on the screen of an observer at radial infinity. The image generated from the model is the sum of multiple subimages corresponding to the different trajectories light can take from the source to the observer.
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Same as Figure 3, but when the ground truth image and model image are both blurred by a 10 μas FWHM Gaussian kernel before comparison. The resulting NxCORR values are higher than for the unblurred case, with excellent fidelity for all model types. However, despite the improved image fidelity at this resolution, the best-fitting parameters have significantly larger discrepancies than for the unblurred fits, showing the strong degeneracies that are present when restricted to the current EHT resolution, especially because the photon ring cannot be distinguished from the direct emission.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Left: fraction of energy flux density reaching the TR. Right: RC potential drop at the TR in kV. From top to bottom: calculations using a cospatial coronal density of 6 × 109 cm–3, 3 × 1010 cm–3, and 1 × 1011 cm−3, respectively. The other parameters used are a loop half-length of ∼12 Mm, a low-energy cutoff of 20 keV, and spectral index δ = 4. The red and black rectangles represent the deduced energy flux densities using the CTTM from W03 and K11, respectively.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: All calculations use 12 Mm, 15 keV, δ = 5. The coronal densities in the top and bottom panels are 6 × 109 cm−3 and 3 × 1010 cm−3, respectively. From left to right: fraction of energy flux density deposited above the TR as a function of injected flux density (x-axis) and coronal temperature (y-axis), runaway fraction at the loop top, the maximum normalized (to the Dreicer field) RC electric field, the total potential drop at the TR, and the thermalization distance from the loop top. Note that the maximum distance plotted is at the TR. Note the different ranges between top and bottom panels: the x-axis covers 10–12 and 10.5–12.5, and the color bars are the same except for the potential drop at the TR.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Electron distributions at various positions along the loop legs in the three cases of Figure 1.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Same as Figures 9 and 8. Parameters used are a loop half-length of 12 Mm and E  c  = 10 keV. Note the different temperature ranges in the top two and bottom two panels.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Same as Figure 10, but with a loop half-length of 12 Mm and low-energy cutoff of 20 keV.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Same as Figure 8, but with 12 Mm, 85 keV, δ = 3. Note the different color bar range in the fraction of energy flux density deposited above the TR.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Overview of the G35 complex in Spitzer 8 μm  emission. The solid and dashed circles correspond to the H II regions and candidates from the WISE catalog by Anderson et al. (2014), respectively, with the symbol size representing the actual size of those objects. The plus symbols identify the positions of ultracompact H II regions from different literature catalogs (Bronfman et al. 1996; Hou & Han 2014; Hu et al. 2016; Kalcheva et al. 2018; Ouyang et al. 2019). The class II methanol masers retrieved from Ladeyschikov et al. (2019) and Nguyen et al. (2022) are marked by open triangles. The solid stars identify the red Midcourse Space Experiment MYSOs (Urquhart et al. 2011) while the open stars identify massive protostars (Li et al. 2018). Six dark clouds mentioned in Section 2 with their names are marked using white dashed rectangles. The white dashed lines approximately delineate boundaries of different clouds. The region of 850 μm continuum for final analysis is limited within a white solid contour of the 20 mJy beam−1 rms level.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Spatial distributions of filaments (red curves) and clumps (colored dots). In (a) the color of the dot corresponds to the value of the clump mass, while in (b) it corresponds to the value of the mass surface density. In both panels, the white plus and cross symbols indicate IR-bright and IR-dark clumps inferred from Spitzer 8 μm images, respectively. The examples of HR clumps, FR clumps, and NFR clumps mentioned in Section 5.1 are marked with arrows.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Detection fraction of simulated sources as a function of peak flux density. Different curves correspond to different FOV analysis, for FOVs 1, 2, and 3 and their sum as the total FOV. The dashed cyan line indicates the 95% detection fraction/flux completeness level. Two dashed gray lines (from left to right) show the 6 rms and 7 rms levels (1 rms = 10 mJy beam−1).
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Comparison of the observations of Perseus from S. A. Walker et al. (2018) (top row) with the results of two of our simulations (central and bottom rows), using GGM surface brightness maps. The initial parameters of the two simulations are indicated in the top left corner of the row corresponding to the simulation. All images show GGM maps. The images have been rotated in the merger plane by 90° from the original simulation orientation, to better match the observations.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: Comparison of the observations of Perseus from S. A. Walker et al. (2018) (top row) with the results of one of our simulations (central and bottom rows), using temperature maps. The initial parameters of the simulation are indicated on the top left corner of the bottom row. The large-scale temperature map has been rotated in the merger plane by 90° from the original simulation orientation to better match the observations, as in Figure 16.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: GGM images for different projection angles for the simulation with β = 200, R = 1:5, θ = 30°, and v = 2000 km s−1. The dashed line in each panel marks a circle of radius 700 kpc. All images are shown at 7.5 Gyr after the first pericenter passage.
Paper: On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
Authors: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, Maxim Markevitch
Figure caption: GGM images of the core region for the simulation with β = 200, R = 1:5, θ = 20°, and v = 2000 km s−1. The time indicated in the top left corner of each image is from the first passage.
Paper: JCMT 850 μm Continuum Observations of Density Structures in the G35 Molecular Complex
Authors: Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham Ngoc Diep, Nicolas Peretto, R. K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark G. Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn J. White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Swagat R. Das, Jingwen Wu, Chen Wang
Figure caption: Dust emission maps as traced by 850 μm continuum for the G35 complex. All symbols are the same as those in Figure 1. The beam size of 850 μm  observations is displayed at the bottom left corner.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247
Authors: Luis A. Zapata, Manuel Fernández-López, Patricio Sanhueza, Josep M. Girart, Luis F. Rodríguez, Paulo Cortés, Patrick Koch, Maria T. Beltrán, Kate Pattle, Henrik Beuther, Piyali Saha, Wenyu Jiao, Fengwei Xu, Xing Walker Lu, Fernando Olguin, Shanghuo Li, Ian W. Stephens, Ji-hyun Kang, Yu Cheng, Spandan Choudhury, Kaho Morii, Eun Jung Chung, Jia-Wei Wang, Jihye Hwang, A-Ran Lyo, Q. Zhang, Huei-Ru Vivien Chen
Figure caption: ALMA magnetic field vectors overlaid onto the resulting 1.2 mm continuum emission (Stokes I) from IRAS 16547−4247. The white vector segments trace the polarization percentage. The vector segment is displayed more or less per every beam, using only data with a 2σ cut in the debiasing process. The black contours are from −0.5, 0.5, 1, 5, 10, 20, 40, and 60 times 0.2 mJy beam−1 the rms noise of the image. The red contours are from −5, 5, 10, 20, 40, 60, 80, and 180 times the rms noise of the Very Large Array (VLA) 3.6 cm continuum emission, which is 20 μJy beam−1. The 3.6 cm continuum emission delineates the radio thermal jet with a NW–SE orientation reported by G. Garay et al. (2003) and L. F. Rodríguez et al. (2008). The synthesized beam (half-power contour) of the ALMA continuum image is shown in the bottom right corner. The scale bar on the right represents the peak flux of the ALMA 1.2 mm continuum emission. The dashed lines trace more or less the biconical dusty envelope revealed in this study. The white circle traces the primary beam or the FWHM of 22.″7. The yellow dots trace the positions of the sources reported in Table 1.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247
Authors: Luis A. Zapata, Manuel Fernández-López, Patricio Sanhueza, Josep M. Girart, Luis F. Rodríguez, Paulo Cortés, Patrick Koch, Maria T. Beltrán, Kate Pattle, Henrik Beuther, Piyali Saha, Wenyu Jiao, Fengwei Xu, Xing Walker Lu, Fernando Olguin, Shanghuo Li, Ian W. Stephens, Ji-hyun Kang, Yu Cheng, Spandan Choudhury, Kaho Morii, Eun Jung Chung, Jia-Wei Wang, Jihye Hwang, A-Ran Lyo, Q. Zhang, Huei-Ru Vivien Chen
Figure caption: ALMA magnetic field vectors overlaid onto the resulting H13CO+(3−2) line moment 0 (upper) and moment 1 maps (lower) from IRAS 16547−4247. The red vector segments trace the polarization percentage. The vector segment is displayed more or less per every beam, using only data with a 2σ cut in the debiasing process (same as Figure 1). In the upper panel, the black contours are from −5, 5, 10, 20, 40, 60, 80, and 180 times the rms noise of the VLA 3.6 cm continuum emission, which is 20 μJy beam−1. The 3.6 cm continuum emission delineates a radio free–free jet with NW–SE orientation reported by G. Garay et al. (2003) and L. F. Rodríguez et al. (2008). The scale bar on the right represents the peak flux of the ALMA H13CO+(3−2) line emission. In the lower panel, the black contours are from −0.5, 0.5, 1, 5, 10, 20, 40, and 60 times 0.2 mJy beam−1 the rms noise of the continuum image. The scale bar on the right represents the the weighted mean radial velocity of the ALMA H13CO+(3−2) line emission. The synthesized beam (half-power contour) of the ALMA line image is shown in the bottom right corner of each panel. The dashed curves trace the multiple bow shocks and outflow cavities discussed in the main text.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247
Authors: Luis A. Zapata, Manuel Fernández-López, Patricio Sanhueza, Josep M. Girart, Luis F. Rodríguez, Paulo Cortés, Patrick Koch, Maria T. Beltrán, Kate Pattle, Henrik Beuther, Piyali Saha, Wenyu Jiao, Fengwei Xu, Xing Walker Lu, Fernando Olguin, Shanghuo Li, Ian W. Stephens, Ji-hyun Kang, Yu Cheng, Spandan Choudhury, Kaho Morii, Eun Jung Chung, Jia-Wei Wang, Jihye Hwang, A-Ran Lyo, Q. Zhang, Huei-Ru Vivien Chen
Figure caption: ALMA magnetic field overlaid onto the resulting HN13C line moment 0 (upper) and moment 1 maps (lower) from IRAS 16547−4247. The red vector segments trace the polarization percentage. The vector segment is displayed more or less per every beam, using only data with a 2σ cut in the debiasing process (same as Figure 1). In the upper panel, the black contours are from −5, 5, 10, 20, 40, 60, 80, and 180 times the rms noise of the VLA 3.6 cm continuum emission, which is 20 μJy beam−1. The 3.6 cm continuum emission delineates a radio free–free jet with NW–SE orientation reported by G. Garay et al. (2003) and L. F. Rodríguez et al. (2008). The scale bar on the right represents the peak flux of the ALMA HN13C line emission. In the lower panel, the black contours are from −0.5, 0.5, 1, 5, 10, 20, 40, 60, and 80 times 0.2 mJy beam−1 of the ALMA 1.2 mm continuum emission. The scale bar on the right represents the radial velocity of the ALMA HN13C line emission. The synthesized beam (half-power contour) of the ALMA line image is shown in the bottom right corner of each panel. The dashed lines trace more or less the biconical dusty envelope revealed in this study.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247
Authors: Luis A. Zapata, Manuel Fernández-López, Patricio Sanhueza, Josep M. Girart, Luis F. Rodríguez, Paulo Cortés, Patrick Koch, Maria T. Beltrán, Kate Pattle, Henrik Beuther, Piyali Saha, Wenyu Jiao, Fengwei Xu, Xing Walker Lu, Fernando Olguin, Shanghuo Li, Ian W. Stephens, Ji-hyun Kang, Yu Cheng, Spandan Choudhury, Kaho Morii, Eun Jung Chung, Jia-Wei Wang, Jihye Hwang, A-Ran Lyo, Q. Zhang, Huei-Ru Vivien Chen
Figure caption: Left panel: ALMA polarization intensity map overlaid with the 1.2 mm continuum emission from IRAS 16547−4247. Right panel: same as the left panel but showing the ALMA Polarization Fraction. In both panels, the black contours are from −0.5, 0.5, 1, 5, 10, 20, 40, and 60 times 0.2 mJy beam−1 the rms noise of the image. The synthesized beam (half-power contour) of the ALMA continuum image is shown in the bottom right corner. The scale bar on the right represents the debiased polarization intensity and polarization fraction. These maps were constructed with a threshold of 2σ for the polarization.