adsabs/AstroCLIMB huggingface dataset:
Paper: Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies
Authors: R. Chen, D. Scolnic, E. Rozo, E. S. Rykoff, B. Popovic, R. Kessler, M. Vincenzi, T. M. Davis, P. Armstrong, D. Brout, L. Galbany, L. Kelsey, C. Lidman, A. Möller, B. Rose, M. Sako, M. Sullivan, G. Taylor, P. Wiseman, J. Asorey, A. Carr, C. Conselice, K. Kuehn, G. F. Lewis, E. Macaulay, M. Rodriguez-Monroy, B. E. Tucker, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. Gruen, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, O. Lahav, M. Lima, M. March, F. Menanteau, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, G. Tarle, D. Thomas, C. To, D. L. Tucker, T. N. Varga
Figure caption: Distributions of redshift (left) and light-curve parameters c (middle left), x 1 (middle right), and m  B  (right) for the data and simulations. The data are represented by the black points, while the simulations are represented by the blue histograms. The simulation histograms are normalized to the data. The reduced χ 2 value is reported for each parameter. The covariances between parameters are not shown, as they are found to be small.
Paper: Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies
Authors: R. Chen, D. Scolnic, E. Rozo, E. S. Rykoff, B. Popovic, R. Kessler, M. Vincenzi, T. M. Davis, P. Armstrong, D. Brout, L. Galbany, L. Kelsey, C. Lidman, A. Möller, B. Rose, M. Sako, M. Sullivan, G. Taylor, P. Wiseman, J. Asorey, A. Carr, C. Conselice, K. Kuehn, G. F. Lewis, E. Macaulay, M. Rodriguez-Monroy, B. E. Tucker, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. Gruen, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, O. Lahav, M. Lima, M. March, F. Menanteau, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, G. Tarle, D. Thomas, C. To, D. L. Tucker, T. N. Varga
Figure caption: Top: redshift and color bias dependence, with the dashed black line at the color bias of zero, where the subscript “RM” stands for the redMaGiC photometric redshift case. Bottom: the ΛCDM μ bias plotted against the Tripp estimator term for color, with the dashed black line at x = y. Both are shown for data (left) and simulations (right). The color of each point corresponds to the redshift of the SN, as given by the colorbar on the right.
Paper: Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies
Authors: R. Chen, D. Scolnic, E. Rozo, E. S. Rykoff, B. Popovic, R. Kessler, M. Vincenzi, T. M. Davis, P. Armstrong, D. Brout, L. Galbany, L. Kelsey, C. Lidman, A. Möller, B. Rose, M. Sako, M. Sullivan, G. Taylor, P. Wiseman, J. Asorey, A. Carr, C. Conselice, K. Kuehn, G. F. Lewis, E. Macaulay, M. Rodriguez-Monroy, B. E. Tucker, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. Gruen, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, O. Lahav, M. Lima, M. March, F. Menanteau, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, G. Tarle, D. Thomas, C. To, D. L. Tucker, T. N. Varga
Figure caption: Left: the distribution of the redMaGiC (RM) photometric redshifts for all redMaGiC galaxies (dashed black line) compared to the subset with a matched SN (solid red line). Right: the distribution of the z-band magnitudes for all redMaGiC (RM) galaxies (dashed black line) compared to the subset with a matched SN (solid red line). The histograms for all the RM galaxies are scaled to match the sums of the RM galaxies that host SNe.
Paper: Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies
Authors: R. Chen, D. Scolnic, E. Rozo, E. S. Rykoff, B. Popovic, R. Kessler, M. Vincenzi, T. M. Davis, P. Armstrong, D. Brout, L. Galbany, L. Kelsey, C. Lidman, A. Möller, B. Rose, M. Sako, M. Sullivan, G. Taylor, P. Wiseman, J. Asorey, A. Carr, C. Conselice, K. Kuehn, G. F. Lewis, E. Macaulay, M. Rodriguez-Monroy, B. E. Tucker, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. Gruen, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, O. Lahav, M. Lima, M. March, F. Menanteau, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, G. Tarle, D. Thomas, C. To, D. L. Tucker, T. N. Varga
Figure caption: Hubble diagrams for the redshift methods as described in Figure 5, but using data. The number of high-z SNe, as well as the redshift scatter σ Δz/(1+z) and Hubble scatter, are given for each redshift method.
Paper: Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies
Authors: R. Chen, D. Scolnic, E. Rozo, E. S. Rykoff, B. Popovic, R. Kessler, M. Vincenzi, T. M. Davis, P. Armstrong, D. Brout, L. Galbany, L. Kelsey, C. Lidman, A. Möller, B. Rose, M. Sako, M. Sullivan, G. Taylor, P. Wiseman, J. Asorey, A. Carr, C. Conselice, K. Kuehn, G. F. Lewis, E. Macaulay, M. Rodriguez-Monroy, B. E. Tucker, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. Gruen, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, O. Lahav, M. Lima, M. March, F. Menanteau, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, G. Tarle, D. Thomas, C. To, D. L. Tucker, T. N. Varga
Figure caption: Hubble diagram from analyzing the simulations for (left) the spec-z from the host galaxy and (right) the redMaGiC photo-zs from the host galaxy. The number of high-z SNe is shown in each panel, as well as the redshift scatter σ Δz/(1+z) and Hubble scatter.
Paper: Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies
Authors: R. Chen, D. Scolnic, E. Rozo, E. S. Rykoff, B. Popovic, R. Kessler, M. Vincenzi, T. M. Davis, P. Armstrong, D. Brout, L. Galbany, L. Kelsey, C. Lidman, A. Möller, B. Rose, M. Sako, M. Sullivan, G. Taylor, P. Wiseman, J. Asorey, A. Carr, C. Conselice, K. Kuehn, G. F. Lewis, E. Macaulay, M. Rodriguez-Monroy, B. E. Tucker, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. Gruen, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, O. Lahav, M. Lima, M. March, F. Menanteau, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, G. Tarle, D. Thomas, C. To, D. L. Tucker, T. N. Varga
Figure caption: Redshift bias and scatter, as defined in Figure 2, but for a random selection of 3000 SNe from simulations.
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: Eddington ratios as a function of the look-back time (t lookback) for luminosity-declining AGN candidates, the parent sample, and [O III] λ5007 bright AGNs. The three look-back times were calculated based on the averaged emitting size of the ADs, dusty tori, and the NLRs. Here the dashed lines and gray area represent the median and scatter of the λ Edd of the parent sample. The differences in the observation time between the SDSS DR7 and WISE observations are taken into account to estimate the t lookback, whose reference time is set on 2022 February 2 (MJD = 59612). The t lookback of the AD and torus for the parent sample are shifted 0.03 dex to the right for clarity.
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: The correlation of the bolometric AGN luminosity estimated from the WISE 12 μm band and [O III] λ5007 emission line. The gray circles represent the parent sample, and the blue filled circles represent the luminosity-declining AGN candidates. The orange dashed line represents the 1:1 line of the two luminosities. For the comparison with other fading/dying AGNs, we showed the location of Arp 187 (blue upper bound), which is one of the most promising dying AGNs (Ichikawa et al. 2016; Ichikawa & Tazaki 2017; Ichikawa et al. 2019a, 2019c), and the location of J0916a (orange upper bound), which is a fading AGN whose fading phase is likely recently started (<102 yr) with strong past outburst activity in the NLR (Chen et al. 2019, 2020a, 2020b). The selection criteria of the luminosity-declining AGN candidates discussed in Section 2.5 are represented by the red dashed line.
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: Luminosities of luminosity-declining AGN candidates (blue filled circles) and the parent sample (gray circles) as a function of redshift. Left: the bolometric luminosity estimated from the observed [O III] λ5007 emission luminosities (L bol,[O III]obs) as a function of redshift. Right: the bolometric luminosity estimated from the 15 μm bands (L bol,15μm) as a function of redshift.
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: The binned distribution of ﹩\mathrm{log}(R)﹩ of the parent sample is represented here by the black circles. The black and blue Gaussian lines represent the ones as a result of the two Gaussian component fitting. The orange line represents the composite of the two components. The red line shows the selection cut for the luminosity-declining AGN candidates at ﹩\mathrm{log}(R)\,=﹩ −1.
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: Comparison of the variability distribution of the ΔW1 for luminosity-declining AGN candidates in blue, the parent sample in black, and additionally the complete AGN catalog of Mullaney et al. (2013; Mul13) containing also type 2 AGNs in gray. The left y-axis shows the number of sources for the parent sample and the catalog of Mullaney et al. (2013; Mul13), and the right axis shows the number for the luminosity-declining AGN candidates.
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: BH mass distribution as a function of redshift. The symbols are the same as in Figure 3.
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: (a–b) Maps of 12CO(J = 2–1/ 1–0) ratios at the two velocity clouds, superposed on the 12CO(J = 1–0) contours (black) and radio continuum shell boundary (magenta). The lowest contour level and the contour intervals for CO are 3 and 2 K km s−1, respectively. The contour level of the radio continuum shell boundary is 40 mJy beam−1. The 12CO(J = 2–1) data were smoothed to match the effective beam size of the 12CO(J = 1–0) data (angular resolution of ∼156″). The gray areas representing that the 12CO(J = 1–0) and/or 12CO(J = 2–1) data show a low significance of ∼5σ or lower. The white rectangles indicate the observed areas of 12CO(J = 2–1) . (c) Averaged 12CO(J = 2–1) (red) and 12CO(J = 1–0) (blue) profiles, which are extracted from the red rectangles as shown in Figures 3(a) and (b). The yellow shaded area represents the velocity range of wing-like profiles (see the text).
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: Integrated intensity maps and position–velocity (p-v) diagrams of 12CO(J = 1–0) (top panels) and H I (middle and bottom panels). The integration range is 8 to 20 km s−1 (left panels) in the velocity for each intensity map; and from 124.°98 to 126.°22 in the R.A. for each p-v diagram. The superposed contours in Figures 4(a) and (c) indicate the radio continuum at 1.4 GHz, whose contour levels are the same as shown in Figure 2. The superposed contours in the bottom panels indicate 12CO(J = 1–0), whose contour levels are 3, 6, 9, 12, 15, 18, and 21 K km s−1 for Figure 4(e); and 0.10, 0.28, 0.46, 0.64, 0.82, 1.00, 1.18, 1.36, 1.54, 1.72, 1.90, and 2.08 K degree for Figure 4(f).
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: Velocity channel distributions of the NANTEN 12CO(J = 1–0) and the ATCA & Parkes H I. The superposed contours are 1.4 GHz radio continuum from ATCA & Parkes (Reynoso et al. 2017). The contour levels are 40, 100, 220, 340, and 460 mJy beam−1. Each panel of CO/H I shows distributions every 4 km s−1 in the velocity range −4 to 20 km s−1. The color bars for CO and H I are shown at the top of the set of panels.
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: (a–b) X-ray hardness ratio maps overlaid with the CO/H I-derived N p(H2 + H I) contours at V LSR = 0–8 km s−1 (left panel) and 8–20 km s−1 (middle panel). The lowest contour level and the contour intervals are 0.8 and 0.8 × 1021 cm−2, respectively. The energy band of the hardness ratio map is 0.36–0.46 keV for the soft-band image and 1.14–1.27 keV for the hard-band image. The gray areas are excluded regions outside the radio continuum shell. The dashed circle in (b) encloses a local spot with a very high hardness ratio. (c) Correlation plots between the hardness ratio and CO/H I-derived N p(H2 + H I). The black and red filled circles represent the data points in the velocity ranges of 0–8 km s−1 and 8–20 km s−1, respectively.
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: (a) Column density maps of the ISM protons N p(H2 + H I) estimated from the 12CO(J = 1–0) and H I integrated intensities. The velocity range of the integrations is 0–8 km s−1. (b) Column density map of N p estimated from A  V  (Dobashi et al. 2005) (hereafter the “N p(A  V )”). The superposed contours indicate the 1.4 GHz radio continuum, as shown in Figure 2. (c) Correlation plots between N p(A  V ) and N p(H2 + H I). The dashed line represents the equality of the two values. All the data sets used here are smoothed with a Gaussian function to the half-power beam width of the A V distribution (∼6′).
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: Enlarged views of the northeastern shell (top panels), and the eastern shell (bottom panels) as indicated by the dashed white rectangles in Figure 4(a). The distribution of the 12CO(J = 2–1) contours are superposed on the radio continuum images (left panels), X-ray images (middle panels), and Hα images (right panels; Parker et al. 2005). The lowest contour level and the contour intervals are 1.0 and 1.0 K km s−1, respectively. The integration velocity range is 8–12 km s−1 for the top panels and 12–20 km s−1 for the bottom panels.
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: Maps of (a) 1.4 GHz radio continuum from ATCA & Parkes (Reynoso et al. 2017), (b) XMM-Newton & Chandra X-ray flux (0.5–7.0 keV), and (c) gamma-rays above 10 GeV toward Puppis A (Xin et al. 2017). The superposed contours are the gamma-rays, and the contour levels are 3, 4, 5, 6, 7, 8, and 9σ.
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: Type III radio burst observed with (a) WIND/WAVES, (b) STEREO A/WAVES (S/WAVES), (c) PSP/FIELDS, and (d) LOFAR. The radio burst is observed at LOFAR, S/WAVES, and WIND/WAVES at ∼12:45 UT as they are all located at a distance of ∼1 au from the Sun, while it was observed 6 minutes earlier by PSP due to its closer proximity to the Sun at ∼50  R ⊙. Using a PSP–Earth light travel time, PSP’s dynamic spectrum has been shifted by +385.80 s to match the one of LOFAR. An additional zoom out panel shows GOES X-ray flux for several hours either side of the burst in energy channels 0.5–4.0 Å (blue) and 1.0–8.0 Å (red).
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: Maps of (a) NANTEN 12CO(J = 1–0) integrated intensity (Moriguchi et al. 2001), (b) Planck dust opacity, and (c) Planck dust temperature (Planck Collaboration et al. 2014). The integration velocity range of CO is from −10 to 80 km s−1. The superposed black contours in Figures 10(a) and 10(b) indicate the CO intensity, whose contour levels are from 6 K km s−1, with 6 K km s−1 intervals. The dashed contours in Figure 10(c) represent a dust temperature of 17.5 K. The remaining superposed contours indicate the 1.4 GHz radio continuum, and the contour levels are the same as shown in Figure 2.
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: HMI magnetogram showing AR 12738 located near the east limb of the Sun (48°E). During PSP encounter 2, this AR was associated with a long-duration type III storm and noise storm (Cattell et al. 2021; Krupar et al. 2020; Pulupa et al. 2020).
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: Radial profiles of the radio continuum, centered at (α, δ) = (125.°59, −43.°03). The black steps with filled circles indicate the average values of the radio continuum in each annulus. The dashed line represents the three-dimensional Gaussian distribution and the solid line represents its projected distribution derived by least-squares fitting (see the text). The vertical dashed lines indicate the best-fit values of the radius and range of the shell thickness.
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: (a–c) Distributions of the ISM proton column densities (a) N p(H2), (b) N p(H I), and (c) N p(H2 + H I). The velocity range of the integrations is 8–20 km s−1 for each map. (d) Gamma-ray distribution above 10 GeV, as shown in Figure 1.
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: Correlation plot between the 12CO(J = 1–0) integrated intensity W(CO10) and the proton column density N p derived using the Planck dust opacity and Equation (A1). The typical error is shown in the right bottom corner. The linear regression found by χ 2 fitting is shown by the solid green line. The shaded area represents the errors of the fitting (see the text).
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: PSP/RFS radio spectrogram for 2019 April 9th. Each vertical stripe is a type III burst. The ∼12:40 UT burst studied in this paper is indicated by the red box annotating the figure. The broadband signatures at lower frequencies are due to variations in the in situ electron plasma parameters (Moncuquet et al. 2020; Liu et al. 2021).
Paper: Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Puppis A
Authors: M. Aruga, H. Sano, Y. Fukui, E. M. Reynoso, G. Rowell, K. Tachihara
Figure caption: Correlation plot between the age of SNRs and the total energy of the cosmic-ray protons W p (Sano et al. 2021a, 2022). The green line indicates the linear regression of the double-logarithmic plot by applying least-squares fitting to the data points representing the ages of SNRs below 6 kyr.