adsabs/AstroCLIMB huggingface dataset:
Paper: Solar Wind Charge Exchange Soft X-Ray Emissions in the Magnetosphere during an Interplanetary Coronal Mass Ejection Compared to Its Driven Sheath
Authors: Yingjie Zhang, Tianran Sun, Chi Wang, Li Ji, Jennifer. A. Carter, Steve Sembay, Dimitra Koutroumpa, Ying D. Liu, Guiyun Liang, Wenhao Liu, Wei Sun, Xiaowei Zhao
Figure caption: Images from individual EPICs in the energy range of 0.3–2.0 keV. The small white circles with red slashes represent point sources to be removed. The large green circle indicates the extracted region used for analysis.
Paper: Isotropization and Evolution of Energy-containing Eddies in Solar Wind Turbulence: Parker Solar Probe, Helios 1, ACE, WIND, and Voyager 1
Authors: Manuel Enrique Cuesta, Rohit Chhiber, Sohom Roy, Joshua Goodwill, Francesco Pecora, Jake Jarosik, William H. Matthaeus, Tulasi N. Parashar, Riddhi Bandyopadhyay
Figure caption: Radial distributions of alignment angle ΘBV for PSP and ΘBR for ACE, WIND, and Voyager 1. PSP interval sizes are 1 and 3 hr for heliocentric distances R < 0.3 au and 0.3 au < R < 1 au, respectively. Single day intervals are used for ACE, WIND, and Voyager 1 for R ≥ 1 au. Interval count of each bin is keyed to the color bar. White bins denote zero count.
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Thick points are the number of objects in the lowest luminosity sample of Danieli et al. (2022) per radial bin. The projected radius is taken as ﹩\left\langle {r}_{\perp }\right\rangle ={\int }_{{r}_{1}}^{{r}_{2}}{\rm{\Sigma }}({r}_{\perp }){r}_{\perp }{d}^{2}{r}_{\perp }/{\int }_{{r}_{1}}^{{r}_{2}}{\rm{\Sigma }}({r}_{\perp }){d}^{2}{r}_{\perp }\approx (2/3)({r}_{2}^{3}-{r}_{1}^{3})/({r}_{2}^{2}-{r}_{1}^{2})﹩, taking Σ ≈ constant per bin with r 1 and r 2 inner and outer radii of each bin. The contamination background (BG) is shown in points with error bars ± standard deviation. The contamination is universal among different bins because we chose the bins to have an equal area. The solid line is the sum of the expected contamination (﹩\left\langle \mathrm{BG}\right\rangle ﹩) and a Sérsic profile with n = 0.61 and R  e  = 2.3 kpc, slightly more extended than the Stars in UDG1 (since bins are of equal area, the Sérsic surface density can be adopted immediately).
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Left: the same as upper panels of Figure 5, for a “simulation” that is the mock GC data discussed in the text—without any time integration—such that it presents no mass segregation. Right: a histogram of the slope of line in ﹩{log}({r}_{\perp })﹩ vs. m ⋆—a test statistic μ, essentially—for mock data of GCs in UDG1 all drawn from the same radial distribution (“homogeneous”). The vertical dashed line shows this test statistic for the data (μ data) of UDG1. The probability p(μ < μ data = 0.008.
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: A modified GC sample with relaxed photometric selection criteria, as explained in the text. The “very red object” refers to an object whose color (F475W − F606W = 0.98 mag) differs by about 20 standard deviations than similar other spectroscopically confirmed GCs (F475W − F606W = 0.39 ± 0.03 mag).
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Like Figure 5, but with unregulated DF (“DF U.R.”), i.e., without turning off DF at any radius, either due to core stalling conditions r < 0.3R  e  or the enclosed mass condition M halo − M GCs/2 < 0.
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: A simulation batch where dynamical friction is turned off, using the Stars model, as explained in Section 3. The interaction between GCs causes the mass segregation. Of course, the segregation depends on the GC mass function, which we take to be the sample of 33 observed GCs (Danieli et al. 2022).
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Like Figure 5, but r merger = 10 pc (top) and r merger = 35 pc (bottom).
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Like Figure 5, but with n GC = 2, i.e., a relatively cuspy GC distribution.
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Like Figure 5, but ϵ = 4 pc (top) and ϵ = 12 pc (bottom).
Paper: 3D Hydrodynamical Simulations of Helium-ignited Double-degenerate White Dwarf Mergers
Authors: Niranjan C. Roy, Vishal Tiwari, Alexey Bobrick, Daniel Kosakowski, Robert Fisher, Hagai B. Perets, Rahul Kashyap, Pablo Lorén-Aguilar, Enrique García-Berro
Figure caption: Temporal evolution of nucleosynthetic abundances where mass fractions shown are normalized to the final value for each isotope.
Paper: 3D Hydrodynamical Simulations of Helium-ignited Double-degenerate White Dwarf Mergers
Authors: Niranjan C. Roy, Vishal Tiwari, Alexey Bobrick, Daniel Kosakowski, Robert Fisher, Hagai B. Perets, Rahul Kashyap, Pablo Lorén-Aguilar, Enrique García-Berro
Figure caption: Evolution of key hydrodynamic and nucleosynthetic quantities through the Z = 0 midplane during and after the helium detonation on the accretor. From top to bottom, the temperature, mass density, 4He, and 44Ti mass densities are shown at times t = (4.2, 6.1, 7.9) s, at a resolution of 17 km.
Paper: 3D Hydrodynamical Simulations of Helium-ignited Double-degenerate White Dwarf Mergers
Authors: Niranjan C. Roy, Vishal Tiwari, Alexey Bobrick, Daniel Kosakowski, Robert Fisher, Hagai B. Perets, Rahul Kashyap, Pablo Lorén-Aguilar, Enrique García-Berro
Figure caption: Density (white) and pressure (lime) contours overlaid on 2D temperature slice plots along the X = 0 (top row) midplane, and corresponding planes along the Y (middle row) and Z (bottom row) at times (4.2, 5.4, 6.1) s for a resolution of 17 km.
Paper: 3D Hydrodynamical Simulations of Helium-ignited Double-degenerate White Dwarf Mergers
Authors: Niranjan C. Roy, Vishal Tiwari, Alexey Bobrick, Daniel Kosakowski, Robert Fisher, Hagai B. Perets, Rahul Kashyap, Pablo Lorén-Aguilar, Enrique García-Berro
Figure caption: Evolution of global maximum temperature, kinetic energy (excluding rotational kinetic energy), and total 4He budget in the computational domain. This plot shows the initial helium detonation at t = 4.1 s and the subsequent collision of detonation fronts at t ∼ 6 s.
Paper: A Speed Bump: SN 2021aefx Shows that Doppler Shift Alone Can Explain Early Excess Blue Flux in Some Type Ia Supernovae
Authors: C. Ashall, J. Lu, B. J. Shappee, C. R. Burns, E. Y. Hsiao, S. Kumar, N. Morrell, M. M. Phillips, M. Shahbandeh, E. Baron, K. Boutsia, P. J. Brown, J. M. DerKacy, L. Galbany, P. Hoeflich, K. Krisciunas, P. Mazzali, A. L. Piro, M. D. Stritzinger, N. B. Suntzeff
Figure caption: (Top left): illustration of how changing the velocity of the −17.3 days spectrum can affect the u-band and B-band synthetic magnitudes. The scale on the right denotes the velocity shift, where 30,000 km s−1, is the velocity of the observed spectra. (Middle left): similar to the top left panel but with the spectrum of SN 2009ig at −14.2 days (Foley et al. 2012). In this panel we also present the magnitude change in the swift U  band. (Bottom left): similar to the top left panel but with the spectrum of SN 2011fe at −13.3 days (Mazzali et al. 2014) taken with the Hubble Space Telescope. Interestingly, the drop in magnitude effect is larger in the UVM2 band than the u band, on top of this the drop in UVW1 is similar in magnitude to that of the u band. (Right): the synthetic light curves (bottom panel) of the spectrophotometric time series with a different velocity evolution. The upper panel shows the chosen velocity evolution for this analysis. These are velocity profiles between SN 2021aefx and SN 2011fe. The u-band light curves show significant changes in magnitudes and shape for various velocity profiles, whereas the B band remains relatively constant. At −17.3 days the u band changes by 0.96 mag between the high-velocity and low-velocity models. Conversely, the B band only changes by 0.03 mag at the same epoch.
Paper: A Speed Bump: SN 2021aefx Shows that Doppler Shift Alone Can Explain Early Excess Blue Flux in Some Type Ia Supernovae
Authors: C. Ashall, J. Lu, B. J. Shappee, C. R. Burns, E. Y. Hsiao, S. Kumar, N. Morrell, M. M. Phillips, M. Shahbandeh, E. Baron, K. Boutsia, P. J. Brown, J. M. DerKacy, L. Galbany, P. Hoeflich, K. Krisciunas, P. Mazzali, A. L. Piro, M. D. Stritzinger, N. B. Suntzeff
Figure caption: (Left): the six color-adjusted spectra chosen for this analysis, including three early spectra of SN 2021aefx and three spectra of SN 2009ig. The spectra are color matched to the observed photometry of SN 2021aefx. (Top right): an example of the merging process between SN 2021aefx and SN 2009ig. Before the merging process, the spectra of SN 2009ig are shifted in velocity to match the velocity of SN 2021aefx at the same phase. The gray shade marks the overlapping region used to match the flux scale. (Bottom right): Velocity profiles of the minimum of the Si II λ6355 feature in SN 2011fe, SN 2009ig, and SN 2021aefx.
Paper: The Large Superfast Rotators Discovered by the Zwicky Transient Facility
Authors: Chan-Kao Chang, 展誥 章, Ting-Shuo Yeh, 庭碩 葉, HanJie Tan, 瀚傑 譚, Wing-Huen Ip, 永烜 葉, Michael S. P. Kelley, Quanzhi Ye, 泉志 叶, Zhong-Yi Lin, 忠義 林, Chow-Choong Ngeow, 兆聰 饒, Bryce T. Bolin, Thomas. A. Prince, Eric C. Bellm, Richard Dekany, Dmitry A. Duev, Matthew Graham
Figure caption: The comparison between the lightcurves folded to the second and third or fourth harmonic rotation periods. Left panel: the five objects that have slightly better fittings in the third harmonics than the second harmonics. Right panel: the seven objects that have slightly better fittings in the fourth harmonics than the second harmonics. The designation is given at the upper-left corner of each plot on the left column of each panel. The rotation periods used in the folded lightcurves are shown at the upper-right corner of each plot. Different colors represent data points obtained from different nights. The gray lines are the fitting results of the second harmonics and the pink lines are that of the third or fourth harmonics.
Paper: The Large Superfast Rotators Discovered by the Zwicky Transient Facility
Authors: Chan-Kao Chang, 展誥 章, Ting-Shuo Yeh, 庭碩 葉, HanJie Tan, 瀚傑 譚, Wing-Huen Ip, 永烜 葉, Michael S. P. Kelley, Quanzhi Ye, 泉志 叶, Zhong-Yi Lin, 忠義 林, Chow-Choong Ngeow, 兆聰 饒, Bryce T. Bolin, Thomas. A. Prince, Eric C. Bellm, Richard Dekany, Dmitry A. Duev, Matthew Graham
Figure caption: Rotation period vs. diameter for the ZTF large SFRs (orange dots). The same is shown for previously measured MBAs and near-Earth objects (background gray dots). The dashed and dotted lines indicate the spin-rate limits of cohesion models (Holsapple 2007) with κ = 2.25 × 107 (i.e., a few hundreds of pascals) and 1.125 × 108 dynes cm−3/2 (i.e., a few thousands of pascals), respectively. Note that previously known MBA rotation periods were obtained from the LCDB.
Paper: The Large Superfast Rotators Discovered by the Zwicky Transient Facility
Authors: Chan-Kao Chang, 展誥 章, Ting-Shuo Yeh, 庭碩 葉, HanJie Tan, 瀚傑 譚, Wing-Huen Ip, 永烜 葉, Michael S. P. Kelley, Quanzhi Ye, 泉志 叶, Zhong-Yi Lin, 忠義 林, Chow-Choong Ngeow, 兆聰 饒, Bryce T. Bolin, Thomas. A. Prince, Eric C. Bellm, Richard Dekany, Dmitry A. Duev, Matthew Graham
Figure caption: 25 folded lightcurves of the ZTF large SFRs. The designation, derived rotation period, and lightcurve amplitude are indicated on each plot at the upper-left, upper-right, and lower-right corners. Different colors represent data points obtained from different nights. The gray lines are the fitting results.
Paper: The Large Superfast Rotators Discovered by the Zwicky Transient Facility
Authors: Chan-Kao Chang, 展誥 章, Ting-Shuo Yeh, 庭碩 葉, HanJie Tan, 瀚傑 譚, Wing-Huen Ip, 永烜 葉, Michael S. P. Kelley, Quanzhi Ye, 泉志 叶, Zhong-Yi Lin, 忠義 林, Chow-Choong Ngeow, 兆聰 饒, Bryce T. Bolin, Thomas. A. Prince, Eric C. Bellm, Richard Dekany, Dmitry A. Duev, Matthew Graham
Figure caption: Spin rate vs. amplitude for the ZTF large SFRs (orange dots) and MBAs and near-Earth objects (gray dots) found in the LCDB. The blue, orange, green, red, and purple dashed lines are the spin-rate limits for rubble-pile asteroids with bulk densities of 1, 2, 3, 5, and 10 g cm−3, respectively.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: 2D histogram of the peak and the pixel significance calculated for 2000 mock observations. The white dots indicate the individual significance values, the thick white line indicates the trend. The horizontal dashed line indicates the peak value of σ pixel found in Figure 15, and the vertical dashed line presents the projection again consistent with the respective σ peak in Figure 15.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Difference between significance using the pixel and peak significance used in Bartko et al. (2009) and Yelda et al. (2014) for the radial slice ranging from 3.″2 to 6.″5. The data used are taken from Yelda et al. (2014), and we use the uniform acceleration prior.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: KLF of all young stars with projected radii ranging from 1″ to 12″ (black), compared to previously published KLFs by Bartko et al. (2010) and Do et al. (2013). In order to compare the KLFs, we have normalized the distributions so that the area under the respective curves up to K mag = 13 is 1.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Similar to Figure 11, but including the combined KLF of the S star and the CW disk. As in Figure 11 and Figure 19, the KLFs have been normalized to make them comparable; see text for details.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Comparison of the eccentricity distributions, the semimajor axis distributions, and K mag distributions of the different kinematic features. The top row includes both the distributions of the 5D-constrained stars (dark green) and the stars with determined orbital solutions (light green) of CW1. CW2 is shown in light blue, CCW/F1 in purple, F2 in pink, and F3 in orange.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Distribution of orbital elements of different prior clusters, drawn from the stellar cusp prior, the uniform acceleration prior, the isotropic cluster prior, and the input isotropic cluster. The top panel shows the z vs. x distribution of the different prior clusters. See Appendix B.3 for details.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Comparison of the PDF of the z values for the star E29: The orange line shows the PDF of the stellar cusp prior (Equation (B1)), the blue line shows the histogram of z values sampled according to the uniform acceleration prior (Equation (B2)), and the dark red line shows the isotropic cluster prior (Equation (5)). For better comparison, we have normalized the mode of the respective distributions to 1.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Histograms of the highest value of the significance calculated for each mock observation. The black histogram shows the pixel significances σ pixel (Bartko et al. 2009), and the blue histogram shows the peak significance σ peak (Yelda et al. 2014), respectively.
Paper: The Young Stars in the Galactic Center
Authors: Sebastiano D. von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young
Figure caption: Comparison of the histogram of orbital nodes calculated in this work and presented in Figure 10 of Yelda et al. (2014). We have normalized the histogram to the same minimum and maximum values; see text for details.
Paper: Kink Oscillation of a Flux Rope During a Failed Solar Eruption
Authors: Pankaj Kumar, Valery M. Nakariakov, Judith T. Karpen, C. Richard DeVore, Kyung-Suk Cho
Figure caption: STEREO/EUVI-A composite image (171 and 195 Å) on 2014 April 2, 1 day before the eruption, demonstrating bright overlying loops (marked by an arrow) above an erupting structure from the same filament channel.
Paper: Triggering Mechanism for Eruption of Two Filaments Observed by the Solar Dynamics Observatory, Nobeyama Radioheliograph, and RHESSI
Authors: Sujin Kim, Vasyl Yurchyshyn
Figure caption: Time sequence of AIA 304 Å (top) and 94 Å (bottom) images. Panels (a) and (e) show the onset of Phase 1, panels (b) and (f) capture the peak of Phase 1, while panels (c), (g), and (d), (h) represent Phase 2 and Phase 3, respectively. The blue and red contours are NoRH 17 GHz and RHESSI 20–40 keV measurements, respectively. The contour levels are plotted at 70% and 90% of their maximum intensity. The line segments in panel (g) indicate directions of the eruption of filaments F1 and F2 and they also represent slits used to produce time-space plots shown in Figure 3. A color version of this figure is available in the online journal.
Paper: Triggering Mechanism for Eruption of Two Filaments Observed by the Solar Dynamics Observatory, Nobeyama Radioheliograph, and RHESSI
Authors: Sujin Kim, Vasyl Yurchyshyn
Figure caption: Upper and middle panels: time-space plots made along the slits shown in Figure 2(g). The y-axis is along the direction of the eruption and the leading edge of the eruptions is marked with white cross symbols. The vertical dotted lines separate periods of nonthermal emission, as well as Phase 1, Phase 2, and Phase 3 of the flare. In both panels the solid curve represents NoRH 17 GHz emission. Bottom panel: velocity profiles during Phase 3 for F1 (thin) and F2 (thick solid line).
Paper: Triggering Mechanism for Eruption of Two Filaments Observed by the Solar Dynamics Observatory, Nobeyama Radioheliograph, and RHESSI
Authors: Sujin Kim, Vasyl Yurchyshyn
Figure caption: Left panel: background is an HMI magnetogram with outlines of filaments F1 (left) and F2 (right) and contours of the microwave source plotted at the 90% level of the maximum intensity (blue). The FOV is the same as that outlined by the white box in Figure 3(a). Right panel: HMI magnetograms acquired about 30 minutes before the event (left) and during Phase 1 (right). Black contours outline positive magnetic fields of 50, 100, 200, 300, and 400 G and white contours outline negative magnetic field of −250 and −300 G. Arrows in the white box indicate regions where the magnetic flux decreased and a green solid curve is a polarity inversion line.
Paper: Triggering Mechanism for Eruption of Two Filaments Observed by the Solar Dynamics Observatory, Nobeyama Radioheliograph, and RHESSI
Authors: Sujin Kim, Vasyl Yurchyshyn
Figure caption: Possible scenario of the eruption of the two filaments. Solid lines represent the filaments and their magnetic connectivity. The green line is the polarity inversion line (see Figure 4) and the blue circle marks the position of the microwave source.
Paper: Triggering Mechanism for Eruption of Two Filaments Observed by the Solar Dynamics Observatory, Nobeyama Radioheliograph, and RHESSI
Authors: Sujin Kim, Vasyl Yurchyshyn
Figure caption: M9.3 flare flux time profiles from top to bottom: GOES low 1–8 Å and high 0.5–4 Å energy bands, microwave NoRH 17 GHz (black line) and 34 GHz (gray line) flux, and RHESSI X-ray counts rate in 12–25 keV, 25–50 keV, and 50–100 keV bands. The vertical dotted lines in the middle panel mark the flare phases.
Paper: A Speed Bump: SN 2021aefx Shows that Doppler Shift Alone Can Explain Early Excess Blue Flux in Some Type Ia Supernovae
Authors: C. Ashall, J. Lu, B. J. Shappee, C. R. Burns, E. Y. Hsiao, S. Kumar, N. Morrell, M. M. Phillips, M. Shahbandeh, E. Baron, K. Boutsia, P. J. Brown, J. M. DerKacy, L. Galbany, P. Hoeflich, K. Krisciunas, P. Mazzali, A. L. Piro, M. D. Stritzinger, N. B. Suntzeff
Figure caption: (Top): multiband photometric observations of SN 2021aefx. The ASAS-SN last nondetection and DLT40 discovery are indicated with open triangle and filled star, respectively. The dotted lines show the interpolation of the early-time light curves that are used for color correcting the spectra. The diamonds represent the synthetic magnitudes of integrating the mangled spectra described in Section 3. The vertical blue lines on the bottom mark the epochs of the observed spectra of SN 2021aefx. (Middle): power-law fits to the rising u-band light. The dashed–dotted line is the f ∝ t 2 fit, the dashed line allows for the power-law index to vary, and the solid line is the two-component fit. (Bottom): the early-time B − V color curves of SN 2021aefx and SN 2018aoz. Both SNe have an initial period where they turn red before becoming blue. The error bars are plotted but are smaller than the points. The plotted light- and color curves are corrected for Milky Way extinction.
Paper: A Speed Bump: SN 2021aefx Shows that Doppler Shift Alone Can Explain Early Excess Blue Flux in Some Type Ia Supernovae
Authors: C. Ashall, J. Lu, B. J. Shappee, C. R. Burns, E. Y. Hsiao, S. Kumar, N. Morrell, M. M. Phillips, M. Shahbandeh, E. Baron, K. Boutsia, P. J. Brown, J. M. DerKacy, L. Galbany, P. Hoeflich, K. Krisciunas, P. Mazzali, A. L. Piro, M. D. Stritzinger, N. B. Suntzeff
Figure caption: Spectra comparison of SN 2021aefx and a variety of other SNe Ia. SN 2021aefx is most similar to SNe 2009ig and 2012fr. Interestingly, the comparison also shows that 2021aefx is not the same as SN 2012cg or SN 2017cbv despite them having an early excess blue flux. Throughout this work, we use the spectra of SN 2009ig to fill in gaps in wavelength and phase.