adsabs/AstroCLIMB huggingface dataset:
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Marginalized posterior covariance between H 0 and the metallicity term, Z  W , for the three two-anchor cases and the baseline fit. The metallicity term is well constrained, with a substantial tightening owing to the differential DEB distance between the two clouds (LMC and SMC) from Graczyk et al. (2020). The term has little correlation with H 0 because the anchor abundances span the range in the SN hosts, but this term provides for the consistency between the anchors.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Display of 67 fits in 12 categories of alternatives or extensions to the baseline as shown in Table 5.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Extended MCMC sampling of the posterior for H 0 to measure out to the ±5σ confidence level. The upper panel shows the probability density for the baseline from SH0ES and from the Planck Collaboration et al. (2020) chains. The bottom panel shows the log of the probability density to improve the ability to see the tails. We note some asymmetry to the distribution, with intervals on the low-H 0 side a little smaller than that on the high side, as the measurements are Gaussian in magnitude and in 5 log H 0, hence slightly skewed in H 0.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Comparison of each geometric anchor distance with its expected value based only on the Cepheids it hosts and the distance ladder calibrated by the geometric distance of the other two anchors. The green histograms are MCMC samples from Fits 13, 14, and 15 showing the expected distance of an anchor whose independent distance was excluded from the analysis. The independent measurement (blue curve) and prediction (green) are in good agreement in all cases to <1σ.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Host distance (μ host) covariance matrix. This is the covariance for the baseline set of 37 hosts derived only from the first two rungs and without the use of any SN Ia data. The nonzero off-diagonal terms result from common anchors, common parameters of the Cepheid P–L relation, and covariance of the metallicity scale. The systematic uncertainty in all host distances may be measured from the square root of the level of the off-diagonal elements and is 0.019 mag, or 0.9% in distance.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Simultaneous measurement of H 0 and expansion history. Here the expansion history is fit with a single free parameter, q 0, though as discussed in the text, it can be fit with any form of H(z) using the set of μ host and a set of consistently standardized SNe Ia in these hosts and in the Hubble flow.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: MCMC sampling of the χ 2 statistic of the global fit showing all free parameters except the individual host distances. Contours are 1σ, 2σ, and 3σ confidence regions. We find that the means and uncertainties agree very well with the analytical minimization of χ 2.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Measuring the reddening ratio R in each host. For each host we subtract the intrinsic period–color relation as given in the text to provide E(V − I) and correct the H-band magnitudes for the P–L relation (period and metallicity). The ideal case, M31, has a large span of extinction (because it is highly inclined) and small measurement errors (because it is nearby) to produce a good constraint on the slope, R, whether we consider errors in only the dependent variable (red line and dotted for uncertainty) or both axes (green line). R = 0 is shown as a black line. NGC 5643 is one of the two nearest SN Ia hosts and has the most Cepheids; it yields some constraint on R along with M101. In contrast, the rest of the SN hosts have data similar to UGC 9391, which produces an uninformative constraint on R and shows a large difference in its value and uncertainty by ignoring uncertainties in both axes. The lower right shows the bootstrap resampling for all hosts, with a different color for each, showing that a meaningful constraint is only seen for the few nearest cases, with the others relatively flat. The measurable cases are consistent with the MW R shown as a black dashed line, as are the sum of all SN hosts. Ignoring errors in E(V − I) underestimates R and its uncertainty, as discussed in the text.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Histogram of the 42 SN Ia absolute magnitudes of SNe Ia calibrated from Cepheids in 37 hosts. The 9 SNe Ia in 7 hosts for which a TRGB distance is available from both EDD and CCHP are shown in green (calibrated here with Cepheids), and the 33 SNe Ia in 30 hosts without a TRGB measure from both in blue (calibrated here with Cepheids). The difference in their means of 0.08 ± 0.05 mag is consistent with the shot noise of the SN samples as discussed in Section 7.2, and combined with other differences between the TRGB calibrator set (lines 6–8) produce a net difference in H 0 of 1 km s−1 Mpc−1 (0.03 ± 0.05 mag) as shown in Table 8, which is less than 1σ from the shot noise of the two samples.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Mean differences between Cepheid photometry and distance-ladder fit versus the local background measured by artificial stars (in units of the Cepheid magnitudes), binned in equal numbers of Cepheids. Red is for Cepheids in SN Ia hosts and green for Cepheids in the anchor NGC 4258, with vertical lines indicating the mean background of each set. An underestimate of Cepheid backgrounds in SN Ia hosts at a level of 0.2 mag for the mean Cepheid background or an overestimate of Cepheid backgrounds in NGC 4258 by 0.2 mag for the mean Cepheid (indicated), or half that level for both simultaneously, would be required to solve the tension, but these possibilities are inconsistent with the data, which are consistent with no overestimates or underestimates for either set. Furthermore, it is hard to imagine how an overestimate or underestimate would not similarly affect (and therefore cancel) Cepheids in both NGC 4258 and SN Ia hosts.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Cepheid distances from this work and TRGB distances from the CCHP (F21) and the EDD (Anand et al. 2021) groups to the same SN hosts calibrated by the same geometric anchor distance to NGC 4258, all measured with HST. The seven hosts indicated are all of those measured by these three groups. In blue we show four more-distant hosts measured by Jang & Lee (2017) for which evidence of a TRGB was not detected by Anand et al. (2021). The Cepheid and TRGB distances are consistent, allowing us to combine them (including for three additional TRGB hosts: NGC 1316, 1404, and 4526) simultaneously in Fits 31 and 32.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Comparison of oxygen abundance gradients in the MW inferred by spectra of Cepheids (blue) and from the PP04 calibration of H II regions (black) with data sources indicated in the plot. The mean levels are found to be consistent to σ < 0.1 dex, and we propagate systematic differences in scales in the covariance matrix (as discussed in the text).
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: SN Ia and host properties for the calibrator sample (green) and three Hubble-flow samples. The color (left panel) and light-curve shape (middle) distributions are in good agreement as discussed in the text, particularly for the baseline sample (Lo-z Spiral, orange) whose quality cuts limits are ∣c∣ < 0.15 and ∣x1∣ < 2. The right panel shows the host mass including a truncation of the Lo-z sample (dashed line) with values for this and other host properties in Table 9.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Spectra (scaled f  λ ) of all 42 SNe Ia in the calibrator sample, color-coded by their deepSIP score calibrated to the photometric parameter, Δm 15. As discussed in the text, we find all calibrator SNe to be in the normal range. Peculiar objects SN 1991T and SN 1991bg bracket the extremes and are shown for comparison.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Comparison of PSF photometry (with backgrounds from artificial stars) for Cepheids in SN hosts (black) and NGC 4258 (blue) used here and basic small-aperture photometry with backgrounds from the mean pixel in a local annulus as discussed in the text.
Paper: A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
Authors: Adam G. Riess, Wenlong Yuan, Lucas M. Macri, Dan Scolnic, Dillon Brout, Stefano Casertano, David O. Jones, Yukei Murakami, Gagandeep S. Anand, Louise Breuval, Thomas G. Brink, Alexei V. Filippenko, Samantha Hoffmann, Saurabh W. Jha, W. D'arcy Kenworthy, John Mackenty, Benjamin E. Stahl, WeiKang Zheng
Figure caption: Comprehensive error budgets for six iterations of the SH0ES measurement of H 0 including this one (2022) and the Key Project from 2001 (Freedman et al. 2001). The greatest improvement here is realized by the increase in the number of SN calibrators, to decrease all terms to <1%. The combined error is indicated by horizontal dashed lines.
Paper: Third and Fourth Harmonics of Electromagnetic Emissions by a Weak Beam in a Solar Wind Plasma with Random Density Fluctuations
Authors: C. Krafft, P. Savoini
Figure caption: Homogeneous plasma (ΔN = 0) at asymptotic time ω  p  t = 8760; ((a)-(f)): wave spectra in the plane (k  x , k  y ); (g): resonance conditions in the plane (k  x , k  y ). (a) ∣E  xk ∣2 at ω  k  ≃ ω  p , with Langmuir waves ﹩{ \mathcal L },{ \mathcal L }^{\prime\prime} ﹩ (k  x  > 0) and ﹩{{ \mathcal L }}^{{\prime} }﹩ (k  x  < 0). (b) ∣E  xk ∣2 at ω  k  ≃ 2ω  p , with electric field contribution to ﹩{{ \mathcal H }}_{2}﹩ (central ring) and electrostatic harmonics ﹩{{ \mathcal L }}_{2}﹩ (k 2x  > 0) and ﹩{{ \mathcal L }}_{2}^{{\prime} }﹩ (﹩{k}_{2x}^{{\prime} }\lt 0﹩). (c) ∣B  zk ∣2 at ω  k  ≃ 3ω  p : wave ﹩{{ \mathcal H }}_{3}﹩. (d) ∣B  zk ∣2 at ω  k  ≃ 4ω  p : wave ﹩{{ \mathcal H }}_{4}﹩. (e) ∣E  xk ∣2 at ω  k  ≃ 3ω  p , with electric field contribution to ﹩{{ \mathcal H }}_{3}﹩ (central ring) and electrostatic harmonics ﹩{{ \mathcal L }}_{3}﹩ (k 3x  > 0) and ﹩{{ \mathcal L }}_{3}^{{\prime} }﹩                    ﹩({k}_{3x}^{{\prime} }\lt 0﹩). (f) ∣E  xk ∣2 at ω  k  ≃ 4ω  p , with electric field contribution to ﹩{{ \mathcal H }}_{4}﹩ (central ring) and electrostatic harmonics ﹩{{ \mathcal L }}_{4}﹩ (k 4x  > 0) and ﹩{{ \mathcal L }}_{4}^{{\prime} }﹩ (﹩{k}_{4x}^{{\prime} }\lt 0﹩). (g) Angle θ 3 (﹩\cos {\theta }_{3}={k}_{3x}/{k}_{3}﹩) in degrees, as a function of k  x  and k  y  of the Langmuir waves ﹩{{ \mathcal L }}_{1}={ \mathcal L },{{ \mathcal L }}^{{\prime} },{ \mathcal L }^{\prime\prime} ﹩, showing the loci where wavenumber resonance conditions are satisfied for ﹩{{ \mathcal H }}_{2}+{{ \mathcal L }}_{1}\to {{ \mathcal H }}_{3}﹩. All variables are normalized. (a)–(f): logarithmic scales; (g): linear scale.
Paper: Lyα Halos around [O III]-selected Galaxies in HETDEX
Authors: Maja Lujan Niemeyer, William P. Bowman, Robin Ciardullo, Max Gronke, Eiichiro Komatsu, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Karl Gebhardt, Caryl Gronwall, Gary J. Hill, Chenxu Liu, Erin Mentuch Cooper, Donald P. Schneider, Sarah Tuttle, Gregory R. Zeimann
Figure caption: Top: median Lyα SB profile of 1034 [O III] galaxies (blue circles) compared to the redshift-adjusted profile of all LAEs (red squares) and the profile of the LAEs at z < 2.35 (green diamonds). The LAE profiles are slightly shifted along the x-axis for better visibility. The star profile in the [O III] galaxy observations at z = 2.1 and that in the LAE observations at z = 2.5 are shown as light gray and dark gray areas, respectively. The cyan area shows the estimated virial radius of the host dark matter halos of the [O III] galaxies. The dotted and dashed lines show the best-fit PSF-plus-power-law model. Bottom: significance of the difference between the profiles, i.e., the difference between the [O III] profile and the LAE profiles divided by the uncertainties added in quadrature, with the same symbols as above.
Paper: Lyα Halos around [O III]-selected Galaxies in HETDEX
Authors: Maja Lujan Niemeyer, William P. Bowman, Robin Ciardullo, Max Gronke, Eiichiro Komatsu, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Karl Gebhardt, Caryl Gronwall, Gary J. Hill, Chenxu Liu, Erin Mentuch Cooper, Donald P. Schneider, Sarah Tuttle, Gregory R. Zeimann
Figure caption: Median Lyα SB profiles of differently separated subsamples. Except for the bottom right, each panel includes the subsample above (upward-facing magenta triangles) and below (downward-facing green triangles) the median of one property. The bottom-right panel shows the subsample above and below the linear SFR–M ⋆ relation. The bottom part of each panel shows the significance of the difference between the two profiles.
Paper: Lyα Halos around [O III]-selected Galaxies in HETDEX
Authors: Maja Lujan Niemeyer, William P. Bowman, Robin Ciardullo, Max Gronke, Eiichiro Komatsu, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Karl Gebhardt, Caryl Gronwall, Gary J. Hill, Chenxu Liu, Erin Mentuch Cooper, Donald P. Schneider, Sarah Tuttle, Gregory R. Zeimann
Figure caption: Comparison of the surface luminosity profile of the [O III] galaxies (blue circles) and that of the LAEs (red squares) with LAEs at z = 3−4 (WI+18; Wisotzki et al. 2018), LAEs at z = 2.2 and z = 3.3 (KI+21; Kikuchihara et al. 2022), LBGs with net Lyα emission and absorption at z = 2.65 (ST+11; Steidel et al. 2011), and LBGs at z = 3.56 (KU+22; Kusakabe et al. 2022). The dotted profiles are convolved with the VIRUS PSF.
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption: Broadband light curves for models m15ni175 (thick curves) and m15ni2 (dashed curves), together with SN 2021yja. Crosses represent the observations taken from Hosseinzadeh et al. (2022), and circles represent data taken from Vasylyev et al. (2022). The statistical uncertainties of the observations are smaller than the data points. Time “0” corresponds to the explosion epoch introduced by Hosseinzadeh et al. (2022). The synthetic curves are shifted by −8 days to match the early phase and the end of the plateau.
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption:  UVW1 and Ugri broadband magnitudes for the best-fit model “best” (dashed curves) and the model “sharp” with the compact CSM (solid curves), and SN 2021yja.
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption: Cumulative distribution of the time between the onset of mass transfer and core collapse, ﹩\mathrm{log}({\rm{\Delta }}{t}_{\mathrm{RLOF}-\mathrm{CC}}﹩ yr −1), estimated for a 20 M ⊙ RSG progenitor evolving in a binary with a 1/10 as a massive companion, shown for different metallicities.
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption: Pseudo-bolometric (solid), bolometric (dotted), and X-ray–EUV (dashed), light curves for model m15ni175 (red), along with the “bolometric” data of SN 2021yja (circles). We show the basic model m15 in black for reference and to demonstrate the effect of interaction.
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption: Photospheric-velocity evolution for models m15ni175 and m15ni2 and for SN 2021yja. Crosses represent velocities obtained from fits to the iron line in Hosseinzadeh et al. (2022), and circles represent velocities from spectral modeling in Vasylyev et al. (2022).
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption: Density structures of the best-fit (“best”) model and the model with the sharper density gradient in the CSM (“sharp”).
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption: Chemical structure of model m15ni175. We show selected elements: hydrogen (green), helium (magenta), oxygen (red), and radioactive nickel (blue).
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption: Density structures of the models with CSM structures specified in Table 1. The profiles of the models “extended 1” (−0.2), “extended 3” (−0.4), “Shell 1” (+0.2), “Shell 2” (+0.4), and “Shell 3” (−0.2) are shown with different offsets (specified in parentheses) for clarity.
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption: Density structure of model m15ni175.