adsabs/AstroCLIMB huggingface dataset:
Paper: A Study of Slow-mode Shocks in the Near-Earth Magnetotail with MMS Observations and Hybrid Simulations
Authors: Nehpreet K. Walia, Kanako Seki, Takanobu Amano, Naritoshi Kitamura, Yoshifumi Saito, Tara Ahmadi, Daniel J. Gershman, Craig J. Pollock, Barbara L. Giles, Stephen A. Fuselier, Christopher T. Russell, James L. Burch
Figure caption: Distribution of total crossings (gray) vs. slow-mode shock events (blue) showing the percentage of downstream points where ﹩{\boldsymbol{\varepsilon }}\leqslant ﹩ 0 (firehose unstable region).
Paper: A Study of Slow-mode Shocks in the Near-Earth Magnetotail with MMS Observations and Hybrid Simulations
Authors: Nehpreet K. Walia, Kanako Seki, Takanobu Amano, Naritoshi Kitamura, Yoshifumi Saito, Tara Ahmadi, Daniel J. Gershman, Craig J. Pollock, Barbara L. Giles, Stephen A. Fuselier, Christopher T. Russell, James L. Burch
Figure caption: Fourier power spectra of Vy  for high beta, ﹩\beta ﹩ = 0.2 (blue), medium beta, ﹩\beta ﹩ = 0.01 (orange), and low beta, ﹩\beta ﹩ = 0.001 (green) at ﹩y/{\lambda }_{i}﹩ = 0.
Paper: X-Ray Spectroscopy of the Dwarf Nova Z Chamaeleontis in Quiescence and Outburst Using the XMM-Newton Observatory
Authors: Şölen Balman, Eric M. Schlegel, Patrick Godon, Jeremy J. Drake
Figure caption: Left: the quiescent EPIC pn and MOS1 and MOS2 spectra of Z Cha simultaneously fit with the (tbabs × CEVMKL) model. Middle: the EPIC spectra simultaneously fit with the composite model of (pcfabs × (CEVMKL + power)). Right: the spectra fit using the composite model (pcfabs × zxipcf × VNEI). In the panels, the dotted lines show the contribution of the different model components. The lower panels show the residuals in standard deviations (in σ).
Paper: X-Ray Spectroscopy of the Dwarf Nova Z Chamaeleontis in Quiescence and Outburst Using the XMM-Newton Observatory
Authors: Şölen Balman, Eric M. Schlegel, Patrick Godon, Jeremy J. Drake
Figure caption: Simultaneously fitted EPIC spectra with the model (tbabs × CEVMKL). The plots show the fit quality and residuals around the iron complex at 6–7 keV. The residuals on the left reveal an apparent H-like iron absorption line. The iron abundance is thawed in the fitting process. The right panel is a fit using the warmabs model—partially ionized (photoionized) absorber—where the absorption line is well accommodated by the absorber model (see Section 5.2).
Paper: X-Ray Spectroscopy of the Dwarf Nova Z Chamaeleontis in Quiescence and Outburst Using the XMM-Newton Observatory
Authors: Şölen Balman, Eric M. Schlegel, Patrick Godon, Jeremy J. Drake
Figure caption: The quiescent X-ray light curve of Z Cha obtained using the XMM-Newton EPIC pn data. The figure shows the locations of the X-ray/optical eclipses in the X-ray light curve. A bin size of 1 s is used in accordance with the source count rate of 1.1 c s−1, which yields approximately one photon per bin in the figure. A light orange color bar, indicating the X-ray eclipse duration of 324 s (from mid-ingress to mid-egress), calculated by A. A. Nucita et al. (2011), is approximately overlaid on the plots.
Paper: X-Ray Spectroscopy of the Dwarf Nova Z Chamaeleontis in Quiescence and Outburst Using the XMM-Newton Observatory
Authors: Şölen Balman, Eric M. Schlegel, Patrick Godon, Jeremy J. Drake
Figure caption: Fits to the outburst EPIC pn and MOS1 and MOS2 spectra of Z Cha. All three EPIC spectra are fit simultaneously with the (tbabs × (BBODY + GAUSS + CEVMKL + power)) model on the left. The middle panel shows the EPIC spectra simultaneously fit with the composite model of (pcfabs × pcfabs × zxipcf × CEVMKL). The right panel shows the same fit spectra using the composite model (pcfabs × pcfabs × (CEVMKL + power)). In the panels, the dotted lines show the contributions of the different model components. The lower panels show the residuals in standard deviations (σ).
Paper: X-Ray Spectroscopy of the Dwarf Nova Z Chamaeleontis in Quiescence and Outburst Using the XMM-Newton Observatory
Authors: Şölen Balman, Eric M. Schlegel, Patrick Godon, Jeremy J. Drake
Figure caption: Averaged XMM-Newton RGS 1 and RGS 2 spectra of Z Cha. The left panel shows the high-resolution X-ray spectrum obtained in quiescence fitted with the (pcfabs × CEVMKL) model. The right panel shows the averaged RGS 1 and RGS 2 spectra of Z Cha in outburst fit with the (pcfabs × pcfabs × CEVMKL) composite model. In both panels, the solid lines (in red color) show the fitted model. The lower panels show the residuals in standard deviations (in σ).
Paper: X-Ray Spectroscopy of the Dwarf Nova Z Chamaeleontis in Quiescence and Outburst Using the XMM-Newton Observatory
Authors: Şölen Balman, Eric M. Schlegel, Patrick Godon, Jeremy J. Drake
Figure caption: Optical OM B band (upper left) and X-ray light curve (LC; lower left), as observed by EPIC using XMM-Newton (both LCs are of the outburst). 10 s time binning is used for the B-band LC, while 250 s binning is used for the X-ray LC. The right panels show the LC in the outburst folded at the orbital period of Z Cha (see the text for Ephemerides). 150 and 15 phase bins are used for the B-band and X-ray EPIC mean LCs, respectively.
Paper: X-Ray Spectroscopy of the Dwarf Nova Z Chamaeleontis in Quiescence and Outburst Using the XMM-Newton Observatory
Authors: Şölen Balman, Eric M. Schlegel, Patrick Godon, Jeremy J. Drake
Figure caption: Averaged RGS 1+RGS 2 spectra of Z Cha in outburst. The top left and right panels show identified lines labeled individually. The fitted high-resolution RGS spectrum is in the right panel of Figure 6. The bottom three panels show selected examples of fitted lines with a GAUSS emission model, as displayed in Table 5.
Paper: X-Ray Spectroscopy of the Dwarf Nova Z Chamaeleontis in Quiescence and Outburst Using the XMM-Newton Observatory
Authors: Şölen Balman, Eric M. Schlegel, Patrick Godon, Jeremy J. Drake
Figure caption: Averaged RGS 1+RGS 2 spectra of Z Cha in quiescence. The top panel shows identified lines labeled individually. The fitted high-resolution RGS spectrum is in the left panel of Figure 6. The three bottom panels show selected examples of fitted lines with a GAUSS emission model, as displayed in Table 4.
Paper: Synchrotron Break Frequencies of Mildly to Highly Relativistic Outflows Observed Off-axis
Authors: Gilad Sadeh
Figure caption: Calculated synchrotron spectrum following A. Gruzinov & E. Waxman (1999) for the following parameters {E, n, t, εe, εB, p} = {1055 erg, 1 cm−3, 2 days, 5 × 10−2, 10−4, 2.2} with and without synchrotron cooling. The analytic νm and νc, Equations (7) and (16), are shown by “+” and “x” signs, respectively.
Paper: Synchrotron Break Frequencies of Mildly to Highly Relativistic Outflows Observed Off-axis
Authors: Gilad Sadeh
Figure caption: A schematic illustration of the conditions described in Section 2.
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: The 2D cuts of simulated C(E, Θ, Φ = 0°) observations for plasma with N in = 10 cm−3, E 0,in ∼1 keV flowing along Θ = Φ = 0°, k B T in = 50 eV, and for instrument concept with (a) G F = 1.16 × 10−6 cm2 sr eV/eV and (b) G F = 1.39 × 10−5 cm2 sr eV/eV.
Paper: Synchrotron Break Frequencies of Mildly to Highly Relativistic Outflows Observed Off-axis
Authors: Gilad Sadeh
Figure caption: The ratio between the analytical estimation from J. Granot & R. Sari (2002) for νm, which is valid in the limit of θ = 0, γ → ∞ , to our extension given in Equation (7) for various Lorentz factors and viewing angles. We use Equation (21) to adjust to the spherical ultrarelativistic strong explosion.
Paper: Synchrotron Break Frequencies of Mildly to Highly Relativistic Outflows Observed Off-axis
Authors: Gilad Sadeh
Figure caption: The ratio between the analytical estimation from I. Linial & R. Sari (2019) for ﹩{\nu }_{c}^{\mathrm{IC}}﹩, which is valid in the limit of θ = 0, γ → ∞ , to our extension given in Equation (20) for various Lorentz factors and viewing angles.
Paper: Synchrotron Break Frequencies of Mildly to Highly Relativistic Outflows Observed Off-axis
Authors: Gilad Sadeh
Figure caption: In dark blue: the allowed parameter space for νm > 0.5 GHz, and ﹩{\theta }_{e}\lt {\sin }^{-1}\left(\tfrac{1}{\gamma }\right)﹩. The black lines represent equal νm curves. We used p = 2.17 and ﹩{\varepsilon }_{e,-1}^{2}{\varepsilon }_{B,-2}^{\tfrac{1}{2}}{n}_{-3}^{\tfrac{1}{2}}=0.07﹩.
Paper: Synchrotron Break Frequencies of Mildly to Highly Relativistic Outflows Observed Off-axis
Authors: Gilad Sadeh
Figure caption: In dark blue: the allowed parameter space for ﹩h{\nu }_{c}^{\mathrm{syn}}\gt 10﹩ keV, θe > 5°, γ ≥ 4, and ﹩{\theta }_{e}\lt {\sin }^{-1}\left(\tfrac{1}{\gamma }\right)﹩. The black lines represent equal ﹩h{\nu }_{c}^{\mathrm{syn}}﹩ curves. We used εB,−2n−3 = 0.01, 3.5 < γ < 6, and t155 = 1.
Paper: Synchrotron Break Frequencies of Mildly to Highly Relativistic Outflows Observed Off-axis
Authors: Gilad Sadeh
Figure caption: The ratio between the analytical estimation from I. Linial & R. Sari (2019) for ﹩{\nu }_{c}^{\mathrm{syn}}﹩, which is valid in the limit of θ = 0, γ → ∞ , to our extension given in Equation (16) for various Lorentz factors and viewing angles.
Paper: Synchrotron Break Frequencies of Mildly to Highly Relativistic Outflows Observed Off-axis
Authors: Gilad Sadeh
Figure caption: In dark blue: the allowed parameter space for ﹩h{\nu }_{c}^{\mathrm{IC}}\gt 10﹩ keV. The black lines represent equal ﹩h{\nu }_{c}^{\mathrm{IC}}﹩ curves. We used εB,−2n−3 = 0.03 and t = 9.
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: Results of the polytropic analysis applied to parameters of a nonvarying plasma. (a) The 2D histograms of the determined γ and (b) the associated P corr per maximum ﹩{C}_{\exp }﹩. (c) The 2D histogram of γ per maximum ﹩{C}_{\exp }﹩ but only for intervals with ∣P corr∣ > 0.7.
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: The 2D histograms of ﹩\tfrac{{N}_{\mathrm{out}}}{{\overline{N}}_{\mathrm{out}}}﹩ and ﹩\tfrac{{T}_{\mathrm{out}}}{{\overline{T}}_{\mathrm{out}}}﹩ as determined by applying the χ 2 minimization to 5000 observation samples with (a) maximum ﹩{C}_{\exp }\sim 5﹩ counts and (b) maximum ﹩{C}_{\exp }\sim 60﹩ counts. In both cases, the occurrence in each ﹩\tfrac{{N}_{\mathrm{out}}}{{\overline{N}}_{\mathrm{out}}}﹩ column is normalized to its maximum value within the column. The red circles correspond to the mean ﹩\tfrac{{T}_{\mathrm{out}}}{{\overline{T}}_{\mathrm{out}}}﹩ within each ﹩\tfrac{{N}_{\mathrm{out}}}{{\overline{N}}_{\mathrm{out}}}﹩ column, while the orange dashed line is the adiabatic model (see the text for more).
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: Results of the polytropic analysis applied to parameters of an isobaric plasma (input γ = 0). (a) The 2D histograms of the determined γ and (b) the associated P corr per maximum ﹩{C}_{\exp }﹩. (c) The 2D histogram of γ per maximum ﹩{C}_{\exp }﹩ but only for intervals with ∣P corr∣ > 0.7.
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: Histograms of (a) γ values and (b) the P corr determined from the polytropic analysis of a nonvarying plasma with N in=10 cm−3, E 0,in ∼1 keV, bulk flow vector along Θ = Φ = 0°, k B T in = 50 eV, and instrument G F = 1.16 × 10−6 cm2 sr eV/eV. The gray histograms correspond to all the analyzed subintervals, while the red histograms correspond to subintervals with ∣P corr∣ > 0.7.
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: Normalized statistical uncertainties of the determined plasma parameters, ﹩\tfrac{\sigma ({N}_{\mathrm{out}})}{{\rm{\Delta }}{N}_{\mathrm{out}}}﹩ (black) and ﹩\tfrac{\sigma ({T}_{\mathrm{out}})}{{\rm{\Delta }}{T}_{\mathrm{out}}}﹩ (red), as functions of maximum ﹩{C}_{\exp }﹩ (top axis) and the determined γ (bottom axis).
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: Illustration of number of counts as a function of energy and the fitted distributions for two cases of different levels of statistical uncertainty. (a) A case with significant statistical uncertainty, and (b) a case with reduced statistical uncertainty. The illustration shows the expected counts (black), the values of highly possible outcomes (gray), and two fitted distributions in each panel. The blue curve has a smaller temperature than that of the red distribution.
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: Results of the polytropic analysis applied to isobaric plasma parameters determined by the MLE method. (a) The 2D histograms of the determined γ and (b) the associated P corr per maximum ﹩{C}_{\exp }﹩. (c) The 2D histogram of γ per maximum C exp, only for intervals with ∣P corr∣ > 0.7.
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: Results of the polytropic analysis applied to plasma parameters determined by the the MLE method. The simulations consider a nonvarying plasma. (a) The 2D histograms of the determined γ, and (b) the associated P corr per maximum ﹩{C}_{\exp }﹩. (c) The 2D histogram of γ per maximum Cexp, but only for intervals with ∣P corr∣ > 0.7. The analysis is performed on the exact same plasma and instrument parameters as those used to produce Figure 4 (see text).
Paper: Artificial Polytropic Behavior of Plasmas Determined from the Application of Chi-squared Minimization Analysis to Data with Significant Statistical Uncertainty
Authors: Georgios Nicolaou, George Livadiotis, Charalambos Ioannou
Figure caption: Normalized statistical uncertainties of the plasma parameters determined using the MLE method, (black) ﹩\tfrac{\sigma ({N}_{\mathrm{out}})}{{\rm{\Delta }}{N}_{\mathrm{out}}}﹩ and (red) ﹩\tfrac{\sigma ({T}_{\mathrm{out}})}{{\rm{\Delta }}{T}_{\mathrm{out}}}﹩, as functions of maximum ﹩{C}_{\exp }﹩ and the determined γ.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Photometry of SN 2021foa. Swift UVW1, UVM2, UVW2, Thacher griz, Nickel BVri, and LCO/Sinistro UBVRI, up, gp, rp, ip, z data (AB system) are denoted by symbols and color coded as described in the legend. All light curves are offset by a constant, for clarity. The gray vertical lines mark our spectroscopic data at their respective epochs relative to r max at MJD﹩{}_{{\mathtt{\max }}}=59302.35﹩  days. Event A encompasses the time when the light curve of SN 2021foa shows precursor emission. Uncertainties are smaller than the size of the markers. The green band delimits the phases where a short plateau is observed (from +14 to +22 days). The inset highlights that same phase region.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption:  R-/r-band light-curve comparison of interacting SNe IIn/Ibn. Light curves are shown for SNe 2005la (A. Pastorello et al. 2008b), 2011hw (N. Smith et al. 2012a; A. Pastorello et al. 2015a), iPTF15akq (G. Hosseinzadeh et al. 2017), 2020bqj (E. C. Kool et al. 2021), 2021foa (A. Reguitti et al. 2022), 2009ip-like SNe 2009ip (M. Fraser et al. 2013; A. Pastorello et al. 2013), 2016jbu (C. D. Kilpatrick et al. 2018; S. J. Brennan et al. 2022b) and 2016bdu (A. Gal-Yam et al. 2007; A. Pastorello et al. 2018), including the SNe Ibn 2006jc (A. Pastorello et al. 2007) and SN 2023fyq (S. J. Brennan et al. 2024a; Y. Dong et al. 2024). All data are denoted by symbols and color coded according to the legend. The gray-shaded region corresponds to the SNe Ibn template of G. Hosseinzadeh et al. (2017, H17). The green-shaded area is the weighted mean ±σ of the photometric sample of SNe Ibc in M. R. Drout et al. (2011, D11). The reference epoch of SN 2016jbu is with respect to V-band maximum. Vertical lines delimit the event A of SN 2021foa in Figure 1.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Low and medium (XSH; VLT/X-shooter) resolution optical spectra of SN 2021foa (Section 2.2, Table A2). Black, dashed vertical lines indicate the rest-frame wavelength of the strongest lines observed in SN 2021foa, mostly H I and He I lines. For visualization purposes, we smoothed all the spectra with a rolling Gaussian with a kernel size of ∼15 Å.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Low and medium (XSH; VLT/X-shooter) resolution NIR spectra of SN 2021foa (see Section 2.2, Table A2). For visualization purposes, the X-shooter spectra were trimmed from 2.2 to 2.5 μm due to low signal-to-noise in that region. All spectra were smoothed with a rolling Gaussian with a kernel size of ∼15 Å.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Upper, middle, and bottom panels show the evolution of the radius (R BB), temperature (T BB), and bolometric luminosity (L bol) of SN 2021foa (magenta) and SN 2009ip (yellow) obtained through BB fits to the SED of SN 2021foa using extrabol (filled squares) and SuperBol (filled circles; M. Nicholl 2018). The green-shaded area represents the epochs of the short plateau in the light curves (see Figure 1).
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Modeling of the Hα profiles. Zero velocity corresponds to the rest wavelength of Hα line. The first two epochs were fitted using a combination of a Gaussian and Lorentzian profile (red, green), while the spectra from −3 to +51 days are fit by three Gaussians, accounting for the narrow and broader emission (green and red), and the absorption (purple). For the medium-resolution spectra (+66, +95, and +129 days), an additional Gaussian component has been added to fit the profile (turquoise). Blue- and red-dashed vertical lines mark the velocities of the rest-frame wavelength of Hα and He I 6678 Å, respectively.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: SN and dust fit to VLT/X-shooter spectra at +66 days (upper panel), +95 days (middle panel), and +129 days (lower panel). The SN hot BB function (green curves—dominant below ≈8000 Å) is fit simultaneously with an MBB function to describe the NIR dust emission (red curves) to the observed spectra (black). The blue curves show the sum of the two individual components. Filled cyan rectangles illustrate the spectral regions excluded for the fit due to the large number of emission lines.
Paper: SN 2021foa: The “Flip-flop” Type IIn/Ibn Supernova
Authors: D. Farias, C. Gall, G. Narayan, S. Rest, V. A. Villar, C. R. Angus, K. Auchettl, K. W. Davis, R. J. Foley, A. Gagliano, J. Hjorth, L. Izzo, C. D. Kilpatrick, H. M. L. Perkins, E. Ramirez-Ruiz, C. L. Ransome, A. Sarangi, R. Yarza, D. A. Coulter, D. O. Jones, N. Khetan, A. Rest, M. R. Siebert, J. J. Swift, K. Taggart, S. Tinyanont, P. Wrubel, T. J. L. de Boer, K. E. Clever, A. Dhara, H. Gao, C.-C. Lin
Figure caption: Collection of light curves of SN 2021foa in several bands reported in this work and A. Reguitti et al. (2022). Color symbols are the photometric data. Light and bold color lines are 1000 sampled MOSFiT light curves from the posterior distribution for the shell (s = 0) and wind-like CSM configuration (s = 2), respectively.