adsabs/AstroCLIMB huggingface dataset:
Paper: Early Results from GLASS-JWST. XI. Stellar Masses and Mass-to-light Ratio of z > 7 Galaxies
Authors: P. Santini, A. Fontana, M. Castellano, N. Leethochawalit, M. Trenti, T. Treu, D. Belfiori, S. Birrer, A. Bonchi, E. Merlin, C. Mason, T. Morishita, M. Nonino, D. Paris, G. Polenta, P. Rosati, L. Yang, K. Boyett, M. Bradac, A. Calabrò, A. Dressler, K. Glazebrook, D. Marchesini, S. Mascia, T. Nanayakkara, L. Pentericci, G. Roberts-Borsani, C. Scarlata, B. Vulcani, Xin Wang
Figure caption: Upper panel: observed (i.e., uncorrected for incompleteness and lensing) cosmic SMD from this study (large solid black circles). Gray thin open symbols show a collection of results from the literature (see legend; Duncan et al. 2014; Oesch et al. 2014; Grazian et al. 2015; Song et al. 2016; Bhatawdekar et al. 2019; Kikuchihara et al. 2020; Stefanon et al. 2021). The salmon-shaded bar shows the range encompassed by indirect measurements of the SMD obtained by converting the 1500 Å luminosities through several mass–luminosity relations from the literature, as well as from the average value measured in this study. Lower panel: ratio of the SMD indirectly inferred by converting 1500 Å luminosities and the one directly obtained from measured stellar masses. We considered the mass–luminosity relations of Kikuchihara et al. (2020) (green squares), Bhatawdekar et al. (2019) (orange triangles), and Stefanon et al. (2021) (blue diamonds), and the average value of the M/L calculated in each of the redshift bins from our data (black circles).
Paper: Deciphering the ∼18 TeV Photons from GRB 221009A
Authors: Sarira Sahu, B. Medina-Carrillo, G. Sánchez-Colón, Subhash Rajpoot
Figure caption: Using the effective area of the LHAASO-WCDA detector, the VHE spectrum for GRB 221009A is given for different values of the spectral index δ by fixing N  γ  = 5500. The intrinsic flux for each δ is also shown. The LHAASO sensitivity curve with 2000 s exposure is also shown. The vertical line corresponds to 18 TeV photon energy. The shaded region is the ±50% relative energy resolution of LHAASO-WCDA for E  γ  ≃ 18 TeV.
Paper: Deciphering the ∼18 TeV Photons from GRB 221009A
Authors: Sarira Sahu, B. Medina-Carrillo, G. Sánchez-Colón, Subhash Rajpoot
Figure caption: The percentage of chance probability for N  γ  ≥ 1 for E  γ  = 18 TeV is plotted as a function of σ.
Paper: Deciphering the ∼18 TeV Photons from GRB 221009A
Authors: Sarira Sahu, B. Medina-Carrillo, G. Sánchez-Colón, Subhash Rajpoot
Figure caption: Same as Figure 1 but using the detector area of LHAASO-KM2A, and the shaded region here is the ±36% relative energy resolution of LHAASO-KM2A for E  γ  ≃ 18 TeV.
Paper: Missing for 20 yr: MeerKAT Redetects the Elusive Binary Pulsar M30B
Authors: Vishnu Balakrishnan, Paulo C. C. Freire, S. M. Ransom, Alessandro Ridolfi, E. D. Barr, W. Chen, Vivek Venkatraman Krishnan, D. Champion, M. Kramer, T. Gautam, Prajwal V. Padmanabh, Yunpeng Men, F. Abbate, B. W. Stappers, I. Stairs, E. Keane, A. Possenti
Figure caption: Bottom panel: high-S/N polarization pulse profile of M30B obtained by summing phase-connected observations between 05U and 08U recorded in the UHF band. The black line represents the total intensity, red and blue lines display the linear and circular polarization pulse profile, respectively. Top panel: measurements of position angle (PA) in degrees above 4σ of the linear polarization.
Paper: Missing for 20 yr: MeerKAT Redetects the Elusive Binary Pulsar M30B
Authors: Vishnu Balakrishnan, Paulo C. C. Freire, S. M. Ransom, Alessandro Ridolfi, E. D. Barr, W. Chen, Vivek Venkatraman Krishnan, D. Champion, M. Kramer, T. Gautam, Prajwal V. Padmanabh, Yunpeng Men, F. Abbate, B. W. Stappers, I. Stairs, E. Keane, A. Possenti
Figure caption: Beam-tiling pattern at the start of the TRAPUM observation of M30 recorded in the UHF band on 2021 January 22. The boundary of the ellipse plotted here corresponds to 50% of the maximum power level. The beam pattern was generated using MOSAIC. The boundaries of the core and half-light radius have been obtained from the Harris (2010) catalog, which are marked as dashed and dashed–dotted lines, respectively. Overlaid on the plots in red are the two known pulsars within this cluster both of which were reported in Ransom et al. (2004). While M30A was discovered and regularly monitored since then, M30B remained undetected since the discovery detection and has now finally been confirmed, localized, and solved using TRAPUM. The inset shows a zoomed-out version of the same plot.
Paper: Missing for 20 yr: MeerKAT Redetects the Elusive Binary Pulsar M30B
Authors: Vishnu Balakrishnan, Paulo C. C. Freire, S. M. Ransom, Alessandro Ridolfi, E. D. Barr, W. Chen, Vivek Venkatraman Krishnan, D. Champion, M. Kramer, T. Gautam, Prajwal V. Padmanabh, Yunpeng Men, F. Abbate, B. W. Stappers, I. Stairs, E. Keane, A. Possenti
Figure caption: Mass–mass diagram of M30B assuming GR obtained from pulsar timing. In the left plot, we show the mass of the companion M c vs. the cosine of the inclination angle. The gray region here is excluded by the requirement that M p > 0. On the right, we present M c vs. the mass of the pulsar M p. The gray region is excluded by the mass function and orbital geometry (i.e., ﹩\sin i\leqslant 1﹩). The black triplet of lines shows the regions consistent with the measurement of the advance of periastron ﹩\dot{\omega }﹩ along with their 1σ uncertainty. As we can see, from these measurements we can derive an upper limit for M p and a lower limit for M c.
Paper: Missing for 20 yr: MeerKAT Redetects the Elusive Binary Pulsar M30B
Authors: Vishnu Balakrishnan, Paulo C. C. Freire, S. M. Ransom, Alessandro Ridolfi, E. D. Barr, W. Chen, Vivek Venkatraman Krishnan, D. Champion, M. Kramer, T. Gautam, Prajwal V. Padmanabh, Yunpeng Men, F. Abbate, B. W. Stappers, I. Stairs, E. Keane, A. Possenti
Figure caption: Postfit timing residuals of PSR J2140−2311B as a function of time and orbital phase using the DD Binary model. Colors indicate different telescopes and backends used to obtain the TOAs.
Paper: The First Flare Observation with a New Solar Microwave Spectrometer Working in 35–40 GHz
Authors: Fabao Yan, Zhao Wu, Ziqian Shang, Bing Wang, Lei Zhang, Yao Chen
Figure caption: Various data sets obtained from 03:52 UT to 03:58 UT: (a) the CBS dynamic spectrum; (b) the CBS microwave flux density; (c) the NoRP microwave flux density, (d) the GOES SXR derivatives and Konus-Wind (KW-Sun) HXR profiles, and (e) the polarization degree (blue) of the NoRP data at 35 GHz, and the ratio (black) of the NoRP data at 35 GHz to the CBS data at 35.25 GHz. Vertical lines mark the separations between the preimpulsive, impulsive, and decay stages. Vertical arrows in panel (b) denote 13 representative moments of the flare evolution, spectra at these moments are presented in Figure 4.
Paper: The First Flare Observation with a New Solar Microwave Spectrometer Working in 35–40 GHz
Authors: Fabao Yan, Zhao Wu, Ziqian Shang, Bing Wang, Lei Zhang, Yao Chen
Figure caption: Evolution of the spectral parameters from 03:54 UT to 03:56 UT: (a) the fitted optically thick and thin spectral indices (α tk and α tn) are plotted as black asterisks and red squares, respectively. The CBS spectral index (α C) is overplotted as blue triangles; (b) the turnover frequency and the corresponding intensity (ν  t  and I  t ) are plotted as black asterisks and red squares, respectively; (c) the power-law fitting of I  t  vs. ν  t  with the combined NoRP and CBS data at moments with the turnover frequency being less than 35 GHz.
Paper: Return of 4U 1730–22 after 49 yr Silence: The Outburst Properties Observed by NICER and Insight-HXMT
Authors: Yu-Peng Chen, Shu Zhang, Shuang-Nan Zhang, Long Ji, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Time evolution of best-fitting parameters for the best-fitting models tbabs*thcomp*bbody (black) and tbabs*thcomp*(diskbb) (red and green) from 4U 1730–22 during its 2021 and 2022 outbursts, including the bolometric flux F, the optical depth τ, the electron temperature T e, the cover factor f sc, and the accretion disk/blackbody temperature kT disk/kT bb and the inner disk radius/blackbody radius R diskb/R bb at a distance of 7.56 kpc and in the face-on scenario (inclination angle θ = 0). The black markers represent the parameters derived from tbabs*thcomp*bbody in the onset and extinction time of the outbursts observed by NICER. The green and red colors indicate the parameters derived from tbabs*thcomp*(diskbb) observed by NICER and the joint observations of NICER and Insight-HXMT, respectively. The “propeller effect” time is marked by a blue line.
Paper: The First Flare Observation with a New Solar Microwave Spectrometer Working in 35–40 GHz
Authors: Fabao Yan, Zhao Wu, Ziqian Shang, Bing Wang, Lei Zhang, Yao Chen
Figure caption: Spectra obtained by fitting the combined NoRP and CBS data at selected moments of T 1 − T 13. The asterisks and squares represent the NoRP and CBS data, respectively. The spectral parameters, including the spectral indices α tk, α tn, and ν  t  are given in each panel. The filled circles denote the location of ν  t .
Paper: Return of 4U 1730–22 after 49 yr Silence: The Outburst Properties Observed by NICER and Insight-HXMT
Authors: Yu-Peng Chen, Shu Zhang, Shuang-Nan Zhang, Long Ji, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Illustration of the central region of an NS–LMXB in the high/soft state before the propeller effect (left), just after the propeller effect (middle), and the tail of the outburst (right). Before the propeller effect, the accretion disk extends to the NS surface; just after that the accretion disk is truncated near the corotation radius and partial material leaks to the NS surface; and at the end of the outburst, there is a scenario of the magnetospheric accretion and the spherical corona.
Paper: The First Flare Observation with a New Solar Microwave Spectrometer Working in 35–40 GHz
Authors: Fabao Yan, Zhao Wu, Ziqian Shang, Bing Wang, Lei Zhang, Yao Chen
Figure caption: The AIA 131 Å (left) and 171 Å (right) images of the partially occulted X2.2 flare. The black arrows in (a) and (c) point at the expanding arcade loops during the preimpulsive stage, and the red ones in (e) and (f) point at the erupting large-scale loop system.
Paper: The First Flare Observation with a New Solar Microwave Spectrometer Working in 35–40 GHz
Authors: Fabao Yan, Zhao Wu, Ziqian Shang, Bing Wang, Lei Zhang, Yao Chen
Figure caption: Overview of the X2.2 flare observed by GOES, NoRP, and CBS on 2022 April 20: (a) the SXR fluxes (solid) and their time derivatives (dashed) observed at 1–8 Å (black) and 0.5–4 Å (red) by GOES; (b) the microwave flux density observed by NoRP at 9.4 (black), 17 (blue), and 35 (red) GHz; (c) the microwave flux density observed by CBS at 35.25 (black), 37.25 (blue), and 39.25 (red) GHz.
Paper: Return of 4U 1730–22 after 49 yr Silence: The Outburst Properties Observed by NICER and Insight-HXMT
Authors: Yu-Peng Chen, Shu Zhang, Shuang-Nan Zhang, Long Ji, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Time evolution of best-fitting parameters for the best-fitting models tbabs*thcomp*bbody (black) and tbabs*thcomp*(bbody+diskbb) (red and green) from 4U 1730–22 during its 2021 and 2022 outbursts, including the bolometric flux F, the optical depth τ, the electron temperature T e, the cover factor f sc, the accretion disk/blackbody temperature kT disk/kT bb, and the inner disk radius/blackbody radius R diskb/R bb at a distance of 7.56 kpc and in the face-on scenario (inclination angle θ = 0). The black markers represent the parameters derived from tbabs*thcomp*bbody in the onset and extinction time of the outbursts observed by NICER. Green and red colors indicate the parameters derived from tbabs*thcomp*(bbody+diskbb) (with fixed blackbody parameters derived from the aforementioned spectral fitting of the onset of the outburst) observed by NICER and the jointed observations of NICER and Insight-HXMT, respectively. The “propeller effect” time is marked by a blue line.
Paper: Return of 4U 1730–22 after 49 yr Silence: The Outburst Properties Observed by NICER and Insight-HXMT
Authors: Yu-Peng Chen, Shu Zhang, Shuang-Nan Zhang, Long Ji, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Hardness–intensity diagram for NICER observations. Hardness is defined as the NICER count rate ratio in the (2.5–10 keV)/(1.7–2.5 keV) bands; intensity is defined as the count rate of NICER in 0.4–10 keV. Each point in the diagram represents one obsid with an exposure time of ∼1000–5000 s. The black points and red points represent the outbursts in 2021 and 2022, respectively. For the outburst in 2021, it began at the bottom left and evolved in a counterclockwise loop, as shown with the gray arrow. For the outburst in 2022, the NICER observations missed the outburst’s onset and the first observation is located at the top right and evolved in a counterclockwise direction, ending at the bottom left, as shown with the red arrow. The “propeller effect” time is marked by the blue arrow. The black and red points in the green box indicate the onset of the outburst in 2021 and the extinction of the outburst in 2022, which are <40 cts s−1 and stacked and fitted, respectively.
Paper: Return of 4U 1730–22 after 49 yr Silence: The Outburst Properties Observed by NICER and Insight-HXMT
Authors: Yu-Peng Chen, Shu Zhang, Shuang-Nan Zhang, Long Ji, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Top panel: daily light curves of 4U 1730–22 by MAXI (2–20 keV, black) during the outbursts in 2021 and 2022. Middle panel: net light curves of 4U 1730–22 by LE (1–10 keV, red) and ME (8–30 keV, green) which are rebinned by one obsid (∼10,000 s). Bottom panel: net light curves of 4U 1730–22 by NICER (0.3–12 keV, its full energy band) that are rebinned by one obsid (∼3000 s). Please note the error bars of the light curves of LE, ME, and NICER are smaller than the size of the symbols, and the NICER light curves are plotted in a diagram of log count rate vs. time. The “propeller effect” time is marked by a blue line. The data points in the green box indicate the obsids with count rate <40 cts s−1 at the onset of the outburst in 2021 and the extinction of the outburst in 2022, which are stacked and fitted, respectively; the derived model parameters from the two stacked specta are shown in Table 1.
Paper: Return of 4U 1730–22 after 49 yr Silence: The Outburst Properties Observed by NICER and Insight-HXMT
Authors: Yu-Peng Chen, Shu Zhang, Shuang-Nan Zhang, Long Ji, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Left panel: the results of the spectral fits with data from NICER (black), LE (red), and ME (green) at the peak flux of the outburst in 2021 by cons*tbabs*thcomp*(bb+diskbb) with fixed blackbody parameters derived from the spectral fitting results of the onset of the outburst. Right panel: the results of the spectral fits with NICER data at the end of the outburst in 2022 by tbabs*thcomp*bb.
Paper: Return of 4U 1730–22 after 49 yr Silence: The Outburst Properties Observed by NICER and Insight-HXMT
Authors: Yu-Peng Chen, Shu Zhang, Shuang-Nan Zhang, Long Ji, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: The results of the spectral fits of the obsid 4639010184 (left) and obsid 4639010185 (right), i.e., the two obsids at the transition time when the “propeller effect” occurred at the decay phase of the outburst in 2022 by tbabs*thcomp*(bb+diskbb).
Paper: GOALS-JWST: Mid-infrared Spectroscopy of the Nucleus of NGC 7469
Authors: L. Armus, T. Lai, V. U, K. L. Larson, T. Diaz-Santos, A. S. Evans, M. A. Malkan, J. Rich, A. M. Medling, D. R. Law, H. Inami, F. Muller-Sanchez, V. Charmandaris, P. van der Werf, S. Stierwalt, S. Linden, G. C. Privon, L. Barcos-Muñoz, C. Hayward, Y. Song, P. Appleton, S. Aalto, T. Bohn, T. Böker, M. J. I. Brown, L. Finnerty, J. Howell, K. Iwasawa, F. Kemper, J. Marshall, J. M. Mazzarella, J. McKinney, E. J. Murphy, D. Sanders, J. Surace
Figure caption: Atomic and H2 line profiles in the MIRI/MRS nuclear spectrum of NGC 7469. High-ionization lines are shown in panel (a). A comparison of some of the brighter high- and low-ionization lines is shown in panel (b). All lines are continuum-subtracted and have been normalized and shifted to the centroid of the narrow-line peak. Black dotted lines indicate the base level and zero velocity in each case. The high-ionization lines are all asymmetric, with wings that extend up to 1700 km s−1 to the blue. The high-velocity blue wings are not present in the low-ionization lines. A simple two-component Gaussian fit to the 14.3 μm [Ne V] line is shown in panel (c). In this panel, the narrow [Ne V] component is in green, the broad blueshifted component is in violet, and the sum is in red. Also shown, with a blue dotted line, is a Gaussian having a width corresponding to an unresolved line at this wavelength. A number of the H2 emission lines detected in the NGC 7469 nuclear spectrum are shown in panel (d) for comparison. While the H2 lines are resolved, they are all symmetric and narrow.
Paper: GOALS-JWST: Mid-infrared Spectroscopy of the Nucleus of NGC 7469
Authors: L. Armus, T. Lai, V. U, K. L. Larson, T. Diaz-Santos, A. S. Evans, M. A. Malkan, J. Rich, A. M. Medling, D. R. Law, H. Inami, F. Muller-Sanchez, V. Charmandaris, P. van der Werf, S. Stierwalt, S. Linden, G. C. Privon, L. Barcos-Muñoz, C. Hayward, Y. Song, P. Appleton, S. Aalto, T. Bohn, T. Böker, M. J. I. Brown, L. Finnerty, J. Howell, K. Iwasawa, F. Kemper, J. Marshall, J. M. Mazzarella, J. McKinney, E. J. Murphy, D. Sanders, J. Surace
Figure caption: JWST/MIRI mid-infrared spectra of NGC 7469. The top panel (a) is a comparison of the total MIRI/MRS spectrum (blue solid) and the nuclear extraction (red solid) to the Spitzer/IRS low-resolution spectrum (purple dotted) from Stierwalt et al. (2013). All spectra are arbitrarily scaled and presented in the rest frame. Prominent emission lines and PAH features are labeled at the top. Atomic lines covering a wide range of ionization potentials and a number of H2 lines from warm molecular gas are present in the NGC 7469 nuclear spectrum. The PAH features that dominate the total JWST and Spitzer spectra are very weak in the nuclear spectrum, and the high-ionization lines are significantly enhanced relative to the low-ionization lines. The green line at the bottom of the panel indicates the wavelength ranges of individual MIRI/MRS channels. The bottom four panels (b)–(e) highlight four spectral regions of the nuclear spectrum with individual bright emission features labeled. Asymmetric blue wings and broad profiles are evident on many of the high-ionization emission lines, indicative of fast-moving gas associated with a nuclear outflow.
Paper: GOALS-JWST: Mid-infrared Spectroscopy of the Nucleus of NGC 7469
Authors: L. Armus, T. Lai, V. U, K. L. Larson, T. Diaz-Santos, A. S. Evans, M. A. Malkan, J. Rich, A. M. Medling, D. R. Law, H. Inami, F. Muller-Sanchez, V. Charmandaris, P. van der Werf, S. Stierwalt, S. Linden, G. C. Privon, L. Barcos-Muñoz, C. Hayward, Y. Song, P. Appleton, S. Aalto, T. Bohn, T. Böker, M. J. I. Brown, L. Finnerty, J. Howell, K. Iwasawa, F. Kemper, J. Marshall, J. M. Mazzarella, J. McKinney, E. J. Murphy, D. Sanders, J. Surace
Figure caption: False-color JWST NIRCam F150W subarray image of the center of NGC 7469. The image, which is 5.″1 (1.65 kpc) across, shows the bright, central AGN and the surrounding starburst ring, which is resolved into dozens of star-forming knots, interspersed with regions of diffuse emission and dark dust lanes. In the image, two circles are shown that represent the extraction regions for the MIRI total (large yellow circle; 3.″6 diameter) and nuclear (small blue circle; 0.″3 diameter) MRS spectra discussed in the text. The total spectrum includes the AGN and starburst ring. The nuclear spectrum is dominated by the AGN and is the focus of this paper. A scale bar depicting 100 pc in projection is shown at the lower left.
Paper: GOALS-JWST: Mid-infrared Spectroscopy of the Nucleus of NGC 7469
Authors: L. Armus, T. Lai, V. U, K. L. Larson, T. Diaz-Santos, A. S. Evans, M. A. Malkan, J. Rich, A. M. Medling, D. R. Law, H. Inami, F. Muller-Sanchez, V. Charmandaris, P. van der Werf, S. Stierwalt, S. Linden, G. C. Privon, L. Barcos-Muñoz, C. Hayward, Y. Song, P. Appleton, S. Aalto, T. Bohn, T. Böker, M. J. I. Brown, L. Finnerty, J. Howell, K. Iwasawa, F. Kemper, J. Marshall, J. M. Mazzarella, J. McKinney, E. J. Murphy, D. Sanders, J. Surace
Figure caption: Emission line properties as a function of ionization and critical density in NGC 7469. The broad line widths and broad-to-narrow component flux ratios are plotted as a function of ionization potential (panels (a) and (c)) and critical density (panels (b) and (d)) for the fine-structure lines in the nuclear spectrum of NGC 7469. The lines show a correlation of broad line width and broad-to-narrow line flux ratio with ionization potential. Linear fits are shown as green dashed lines in panels (a) and (c), excluding the [Mg VII] 5.5 μm line, which is blended with H2.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program): The Magnetic Fields in the Multiphase Interstellar Medium of the Antennae Galaxies 
Authors: Enrique Lopez-Rodriguez, Alejandro S. Borlaff, Rainer Beck, William T. Reach, Sui Ann Mao, Evangelia Ntormousi, Konstantinos Tassis, Sergio Martin-Alvarez, Susan E. Clark, Daniel A. Dale, Ignacio del Moral-Castro
Figure caption: Total and polarized intensities of the Antennae galaxies at wavelengths of 154 μm and 11 cm. Top: I 154 μm (left; colorscale) with overlaid contours starting at ﹩100{\sigma }_{{I}_{154\,\mu {\rm{m}}}}﹩ and increasing in steps of ﹩{2}^{n}\times {\sigma }_{{I}_{154\,\mu {\rm{m}}}}﹩, where n = 6.7, 7.2, 7.7,  ... and ﹩{\sigma }_{{I}_{154\,\mu {\rm{m}}}}\,=\,0.01﹩ mJy arcsec−2. PI 154 μm (right; colorscale) with overlaid contours at ﹩3{\sigma }_{{\mathrm{PI}}_{154\,\mu {\rm{m}}}}﹩ and increasing in steps of n × σ, where n = 3, 3.5, 4,  ... and ﹩{\sigma }_{{\mathrm{PI}}_{154\,\mu {\rm{m}}}}\,=\,0.07﹩ mJy arcsec−2. For both figures, the 154 μm B-field orientations (white lines) with their lengths proportional to P are shown. A legend of 5% polarization, the beam size (red circle), and several physical structures with their outlined mask (see the Appendix) are shown. Middle: I radio (left; colorscale) with overlaid contours in log10 scale starting at ﹩4{\sigma }_{{I}_{\mathrm{Radio}}}﹩ and increasing in steps of ﹩{2}^{n}\times {\sigma }_{{I}_{\mathrm{Radio}}}﹩, where n = 2, 2.5, 3,  ... and ﹩{\sigma }_{{I}_{\mathrm{Radio}}}=0.01﹩ mJy beam−1. PIradio (right; colorscale) with overlaid contours in log10 scale starting at ﹩5{\sigma }_{{\mathrm{PI}}_{\mathrm{Radio}}}﹩ and increasing in steps of ﹩{2}^{n}\times {\sigma }_{{\mathrm{PI}}_{\mathrm{Radio}}}﹩, where n = 5, 7, 9,  ... and ﹩{\sigma }_{{\mathrm{PI}}_{\mathrm{Radio}}}=0.004﹩ mJy beam−1. The lengths of the lines are set to unity to show the B-field orientations. Bottom: overlaid comparison of the B-field orientation (left) and PI (right) at 154 μm (black lines and contours) and 11 cm (white lines and gray contours). For both figures, PI is displayed in colorscale as described above.