adsabs/AstroCLIMB huggingface dataset:
Paper: Far-ultraviolet Flares on Accreting Protostars: Weak and Classical T Tauri Stellar Pair Analysis
Authors: P. C. Hinton, Kevin France, Maria Gracia Batista, Javier Serna, Jesús Hernández, Hans Moritz Günther, Adam F. Kowalski, P. Christian Schneider
Figure caption: Each top panel shows the unadjusted data in blue, the slope-adjusted data in magenta, and the fit line in red. The slope-adjusted data are the unadjusted data corrected for the slope in the red line. Each bottom panel shows only the slope-adjusted data, with statistical levels (3σ: dashed orange; 5σ: solid red) computed ignoring potential flares. The plot title shows the target star, the HST ID, and the hot accretion line being analyzed.
Paper: Bayesian Accretion Modeling: Axisymmetric Equatorial Emission in the Kerr Spacetime
Authors: Daniel C. M. Palumbo, Zachary Gelles, Paul Tiede, Dominic O. Chang, Dominic W. Pesce, Andrew Chael, Michael D. Johnson
Figure caption: Summary of the equatorial emission model. Left: emission model viewed from above, which is defined by an axisymmetric magnetic field ( B ) and local fluid velocity ( β ) that are given with respect to the local zero angular momentum observer tetrad. The magnetic field direction is determined by a pair of spherical angles (η, ι), while the velocity vector lies in the equatorial plane with a magnitude β and angle χ with respect to the local radial direction. The emissivity has a radial profile ﹩{ \mathcal J }(r)﹩, which we typically model as a double power law defined by a characteristic emission radius R and a pair of indices (p 1, p 2). Right: side view showing null geodesics that reach a distant observer at viewing inclination θ o with respect to the angular momentum axis of the black hole and accretion flow. The black hole parameters (θ g, a *) affect the image through gravitational lensing, redshift, and frame dragging, while the positional angle corresponds to a trivial image rotation. For simplicity, the geodesics shown correspond to a Schwarzschild black hole (a * = 0).
Paper: Bayesian Accretion Modeling: Axisymmetric Equatorial Emission in the Kerr Spacetime
Authors: Daniel C. M. Palumbo, Zachary Gelles, Paul Tiede, Dominic O. Chang, Dominic W. Pesce, Andrew Chael, Michael D. Johnson
Figure caption: Partial triangle plots of posteriors on parameters of interest in a fit of the model to itself using closure quantities from 2017 Event Horizon Telescope (EHT) coverage of M 87*. In red, a model containing only the n = 0 image is fit to itself; in blue, a model containing both the n = 0 and n = 1 image is fit to itself. True values are shown in black. The underlying true model has θ g = 3.83 μas, a * = −0.75, θ o = 17°, PA = 288°, β = 0.5, χ = −π/2, ι = π/3, α  ν  = 1, α  ζ  = 1, R = 4.5, p 1 = 5, and p 2 = 5, all of which are fit. Full posteriors are in the Appendix. For this coverage, addition of the n = 1 image softens the degeneracy between black hole mass and emission radius in the fitted results but is still insufficient to constrain spin. Here and in all other triangle plots, contours show 0.5σ, 1σ, 1.5σ, and 2σ levels.
Paper: Bayesian Accretion Modeling: Axisymmetric Equatorial Emission in the Kerr Spacetime
Authors: Daniel C. M. Palumbo, Zachary Gelles, Paul Tiede, Dominic O. Chang, Dominic W. Pesce, Andrew Chael, Michael D. Johnson
Figure caption: Comparison of time-averaged images of Magnetically Arrested Disk (MAD) general relativistic magnetohydrodynamic (GRMHD) simulations of various spins with R high = 20 and the corresponding best-fit model image with ﹩{n}_{\max }=1﹩ from a maximization of the normalized cross-correlation ρ NX. The bottom row shows residuals, where blue indicates that the model fit exceeds the GRMHD image, and red indicates the opposite; residuals are expressed as a fraction of the peak Stokes I flux of the GRMHD image. Model images are annotated at the top left with the best-fit ρ NX and at the bottom left with the inferred black hole and viewing parameters.
Paper: Bayesian Accretion Modeling: Axisymmetric Equatorial Emission in the Kerr Spacetime
Authors: Daniel C. M. Palumbo, Zachary Gelles, Paul Tiede, Dominic O. Chang, Dominic W. Pesce, Andrew Chael, Michael D. Johnson
Figure caption: Example model images (first column) and their factorization into four underlying quantities: synchrotron emissivity (second column), combined Doppler and gravitational redshift (third column), emissivity profile (fourth column), and optically thin path length factor. The relative brightness here and in all other figures is normalized in individual panels. Underlying model parameters are θ g = 3.8 μas, a * = −0.5, θ o = 45°, β = 0.5, χ = −3π/4, ι = π/3. The emissivity profile has R = 4.5 M, p 1 = p 2 = 3. Top and bottom rows show quantities for the n = 0 and n = 1 images, with increasing n corresponding to subsequent half-orbits of light around the black hole.
Paper: Bayesian Accretion Modeling: Axisymmetric Equatorial Emission in the Kerr Spacetime
Authors: Daniel C. M. Palumbo, Zachary Gelles, Paul Tiede, Dominic O. Chang, Dominic W. Pesce, Andrew Chael, Michael D. Johnson
Figure caption: Same as Figure 3 but for Standard and Normal Evolution (SANE) simulations with R high = 160, for which the majority of emission is far above the Kerr midplane, violating the assumptions of our toy model.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Top: number of heating sources per GMC. Unclassified, supernovae remnants, and H II regions are from Ulvestad & Antonucci (1997), while super hot cores are from Rico-Villas et al. (2020). Note that the super hot core source measurements sample only the inner portion of the NGC 253 CMZ, which includes GMCs 3–6. Bottom: median modeled volume density (green squares) and CRIR (purple circles) values for each GMC. Error bars indicate the 16th–84th percentile of the posterior distributions.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Violin plots derived from modeled HCN/HNC abundance ratios for all GMCs using the most likely 67% of models. Purple violins indicate the smoothed kernel density estimations of the ratio distributions for each GMC. White dots at the center of each violin indicate the median values of the HCN/HNC ratios derived from UCLCHEM's abundance estimates. The thick gray vertical bars within each violin show the interquartile ranges of the UCLCHEM data sets, and the thin gray lines illustrate the two outer quartiles.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 6.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 1.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Top: HCN/HNC abundance ratio as a function of CRIR. Bottom: distribution of Spearman coefficients for a simulated Gaussian data set derived from our modeled HCN/HNC abundance ratios, CRIRs, and their uncertainties. The given value of ρ represents the median of the distribution.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: PDR modeling results from UCLPDR for gas temperature as a function of volume density and CRIR. White boxes indicate the areas of the plot relevant to the conditions in the outer and inner GMCs, and white dots note the specific locations of GMCs 1 and 6.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Observed (triangles and squares) vs. modeled (shaded bars) flux for HCN (red) and HNC (blue). Observed error bars indicate the 1σ uncertainty range. Shaded rectangles show the inner 67% (∼16th–84th percentile) of our modeled flux distributions.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 2.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 4.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 3.
Paper: New Identifications and Multiwavelength Properties of Extragalactic Fermi Gamma-Ray Sources in the SPT-SZ Survey Field
Authors: Lizhong Zhang, 力中 张, Joaquin D. Vieira, Marco Ajello, Matthew A. Malkan, Melanie A. Archipley, Joseph Capota, Allen Foster, Greg Madejski
Figure caption: The 2500 deg2 SPT-SZ survey (Everett et al. 2020). In this region, gray points mark all SPT sources in Everett et al. (2020), green circles represent the position of the previously unassociated 4FGL sources that have SPT counterparts (40), blue circles represent the already-associated 4FGL sources (211), and red circles represent the remaining still-unidentified 4FGL sources (31).
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 10.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 5.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 7.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 9.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Modeling results for GMC 8.
Paper: Lanthanide Features in Near-infrared Spectra of Kilonovae
Authors: Nanae Domoto, Masaomi Tanaka, Daiji Kato, Kyohei Kawaguchi, Kenta Hotokezaka, Shinya Wanajo
Figure caption: Top: Sobolev optical depth of bound–bound transitions calculated with the hybrid line list (Section 2.3) including Th III lines (light blue) taken from the VALD database (λ < 10000 Å) and the NIST database (λ ≥ 10000 Å) at t = 1.5 days under the condition of ρ = 10−14 g cm−3 and T = 5000 K.Bottom: comparison between the synthetic spectra including Th III lines (blue) and the observed spectra of AT2017gfo (gray, Pian et al. 2017; Smartt et al. 2017) at t = 1.5, 2.5, and 3.5 days after the merger (dark to light colors). The light-blue curves are the same as the blue curves in Figure 8.
Paper: Lanthanide Features in Near-infrared Spectra of Kilonovae
Authors: Nanae Domoto, Masaomi Tanaka, Daiji Kato, Kyohei Kawaguchi, Kenta Hotokezaka, Shinya Wanajo
Figure caption: Synthetic spectra at t = 2.5 days after the merger for different mass fractions of La (left) and Ce (right). Variation of each element is shown in the legend with the same color used for the spectra. Pink and orange arrows in each panel indicate the position of the notable absorption lines caused by La III and Ce III, respectively. Line segments above and below the spectra indicate spectral slopes for visualization.
Paper: Lanthanide Features in Near-infrared Spectra of Kilonovae
Authors: Nanae Domoto, Masaomi Tanaka, Daiji Kato, Kyohei Kawaguchi, Kenta Hotokezaka, Shinya Wanajo
Figure caption: Comparison between the synthetic spectra (blue) and the observed spectra of AT2017gfo (gray, Pian et al. 2017; Smartt et al. 2017) at t = 1.5, 2.5, and 3.5 days after the merger (dark to light colors). Spectra are vertically shifted for visualization. The gray shade shows the regions of strong atmospheric absorption.
Paper: Lanthanide Features in Near-infrared Spectra of Kilonovae
Authors: Nanae Domoto, Masaomi Tanaka, Daiji Kato, Kyohei Kawaguchi, Kenta Hotokezaka, Shinya Wanajo
Figure caption: Comparison of intensities for NIR Ce III lines between those calculated with theoretical gf-values and those measured by experiments (Johansson & Litzén 1972). Gray dashed and dotted lines correspond to perfect agreement and deviations by a factor of 3, respectively. Blue circles indicate the lines whose theoretical gf-values are underestimated more than a factor of 3.
Paper: Lanthanide Features in Near-infrared Spectra of Kilonovae
Authors: Nanae Domoto, Masaomi Tanaka, Daiji Kato, Kyohei Kawaguchi, Kenta Hotokezaka, Shinya Wanajo
Figure caption: Left: energy diagram for Sr II. Black and red lines show energy levels from the NIST database and the HULLAC results, respectively. Right: comparison of gf-values between the VALD database and the HULLAC results. Gray dashed line corresponds to perfect agreement between them, and dashed–dotted and dotted lines indicate deviations by a factor of 3 and 10, respectively.
Paper: Lanthanide Features in Near-infrared Spectra of Kilonovae
Authors: Nanae Domoto, Masaomi Tanaka, Daiji Kato, Kyohei Kawaguchi, Kenta Hotokezaka, Shinya Wanajo
Figure caption: Comparison of intensities (green circles) for Th III lines between those calculated with gf-values from the VALD database and those measured by experiments (Kramida et al. 2021; Engleman 2003). Gray dashed and dotted lines correspond to perfect agreement and deviations by a factor of 3 and 10, respectively. Red circles indicate the lines whose gf-values are estimated from the measured intensities.
Paper: Lanthanide Features in Near-infrared Spectra of Kilonovae
Authors: Nanae Domoto, Masaomi Tanaka, Daiji Kato, Kyohei Kawaguchi, Kenta Hotokezaka, Shinya Wanajo
Figure caption: Synthetic spectrum (blue curve) and Sobolev optical depth of each transition (vertical lines) at t = 1.5 days. We plot the Sobolev optical depths of spectroscopically accurate lines in the ejecta at v = 0.16 c. The positions of lines are blueshifted according to v = 0.16 c. The temperature in the ejecta at v = 0.16 c is T ∼ 6000 K.
Paper: Lanthanide Features in Near-infrared Spectra of Kilonovae
Authors: Nanae Domoto, Masaomi Tanaka, Daiji Kato, Kyohei Kawaguchi, Kenta Hotokezaka, Shinya Wanajo
Figure caption: The temperature structure of the ejecta at t = 1.5, 2.5, and 3.5 days after the merger.
Paper: Lanthanide Features in Near-infrared Spectra of Kilonovae
Authors: Nanae Domoto, Masaomi Tanaka, Daiji Kato, Kyohei Kawaguchi, Kenta Hotokezaka, Shinya Wanajo
Figure caption: Same as Figure 12, but for Y I.
Paper: Spectropolarimetry of the Thermonuclear Supernova SN 2021rhu: High Calcium Polarization 79 Days after Peak Luminosity
Authors: Yi Yang, 轶 杨, Huirong Yan, Lifan Wang, J. Craig Wheeler, Dietrich Baade, Howard Isaacson, Aleksandar Cikota, Justyn R. Maund, Peter Hoeflich, Ferdinando Patat, Steven Giacalone, Malena Rice, Dakotah B. Tyler, Divya Mishra, Chris Ashall, Thomas G. Brink, Alexei V. Filippenko, Llíus Galbany, Kishore C. Patra, Melissa Shahbandeh, Sergiy S. Vasylyev, Jozsef Vinkó
Figure caption: Evolution of the intrinsic polarization of SN 2021rhu. For each epoch, the degree of polarization is presented (red histogram) with 40 Å binning, together with the full-resolution and arbitrarily scaled flux spectrum (black line). Ca II NIR3 features at all epochs are labeled with their velocities (v Ca) calculated with λ 0,Ca = 8570 Å (Section 3.1). Vertical light-green lines indicate the locations of the three components of Ca II NIR3. The two vertical green dashed lines trace the evolution of the Ca II H and K and the Ca II NIR3 velocities. Vertical purple lines identify the Si II λ5976 and Si II λ6355 features at days −7 and +0. The Ca and Si velocities were determined from the absorption minima corresponding to λ 0,Ca and Si II λ6355, respectively. The degree of polarization across both Ca II NIR3 and Ca II H and K shows a substantial increase at later epochs.
Paper: Spectropolarimetry of the Thermonuclear Supernova SN 2021rhu: High Calcium Polarization 79 Days after Peak Luminosity
Authors: Yi Yang, 轶 杨, Huirong Yan, Lifan Wang, J. Craig Wheeler, Dietrich Baade, Howard Isaacson, Aleksandar Cikota, Justyn R. Maund, Peter Hoeflich, Ferdinando Patat, Steven Giacalone, Malena Rice, Dakotah B. Tyler, Divya Mishra, Chris Ashall, Thomas G. Brink, Alexei V. Filippenko, Llíus Galbany, Kishore C. Patra, Melissa Shahbandeh, Sergiy S. Vasylyev, Jozsef Vinkó
Figure caption: Spectropolarimetry of SN 2021rhu observed on day −7. The five panels (from top to bottom) present (a) the scaled flux spectrum; (b, c) the normalized Stokes parameters Q and U, respectively; (d) the polarization spectrum (p); and (e) the polarization position angle (PA). The diagrams in panels (b)–(d) represent the polarization after ISP correction. PAs in panel (e) are presented before subtracting the ISP. The data have been rebinned to 40 Å, while the Stokes Q and U parameters approximately sampled with the detector pixel size are indicated by gray histograms in panels (b)–(c).
Paper: Spectropolarimetry of the Thermonuclear Supernova SN 2021rhu: High Calcium Polarization 79 Days after Peak Luminosity
Authors: Yi Yang, 轶 杨, Huirong Yan, Lifan Wang, J. Craig Wheeler, Dietrich Baade, Howard Isaacson, Aleksandar Cikota, Justyn R. Maund, Peter Hoeflich, Ferdinando Patat, Steven Giacalone, Malena Rice, Dakotah B. Tyler, Divya Mishra, Chris Ashall, Thomas G. Brink, Alexei V. Filippenko, Llíus Galbany, Kishore C. Patra, Melissa Shahbandeh, Sergiy S. Vasylyev, Jozsef Vinkó
Figure caption: Similar to Figure 2, but for day +0 at higher spectral resolution. The data have been rebinned to 8 Å. For comparison, low-resolution data obtained at the same epoch rebinned to 40 Å are shown by the brown thick histograms in panels (b)–(d). The vertical solid green lines in panels (a) and (d) represent the minimum of the total-flux absorption line at 12,000 km s−1. The left and right vertical dashed lines in panel (d) mark the two polarization peaks at 13,500 and 9600 km s−1, respectively. The gray shaded area identifies a region with a major telluric feature.
Paper: Spectropolarimetry of the Thermonuclear Supernova SN 2021rhu: High Calcium Polarization 79 Days after Peak Luminosity
Authors: Yi Yang, 轶 杨, Huirong Yan, Lifan Wang, J. Craig Wheeler, Dietrich Baade, Howard Isaacson, Aleksandar Cikota, Justyn R. Maund, Peter Hoeflich, Ferdinando Patat, Steven Giacalone, Malena Rice, Dakotah B. Tyler, Divya Mishra, Chris Ashall, Thomas G. Brink, Alexei V. Filippenko, Llíus Galbany, Kishore C. Patra, Melissa Shahbandeh, Sergiy S. Vasylyev, Jozsef Vinkó
Figure caption: Same as Figure 2, but for day +0.