adsabs/AstroCLIMB huggingface dataset:
Paper: Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu, Tze-En Chang
Figure caption: Same as Figure 4, but the analysis was performed with the best-fit Keplerian disk model with the inclination of 16° and M ⋆ of 2 M ☉.
Paper: Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu, Tze-En Chang
Figure caption: Same as Figure 1, but with C18O J = 3 − 2.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Plots of the power-law (PL) flux and index as functions of the shock velocity (proper motion velocity is substituted), emission measure (﹩\propto {n}_{{\rm{e}}}^{2}﹩), and electron temperature (kT). The PL flux is calculated for 0.5–7.0 keV. The EM is shown in the same units as in Table 4. The 95% upper limits of the EMs of the nonthermal-dominated filaments are shown with the blue arrows in panels (b). The best-fit power-law functions for the plots of the PL flux and index over the emission measure are also shown with red lines.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Flux profiles of the regions SW1–SW6. The black and red crosses represent the data taken in 2001 and 2013, respectively. The positive directions of positions correspond to the directions of the arrows shown in Figure 1. The displayed flux ranges are different for different panels. The vertical dashed lines represent the ranges used for proper motion measurement.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Plots of the cutoff energy of the ZA07 model (E 0) against the shock velocity (proper motion velocity is substituted). A distance of 2.8 kpc is assumed. The black solid, dashed, and dotted lines indicate the ZA07 model with different gyrofactors (η).
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Plots of the power-law flux and index against the shock obliquity. As a proxy for the shock obliquity, we assume two cases: we use the angle made by the Galactic plane and the vector connecting the filament position and geometric center of RCW 86 (case (a)), and the angle made by the Galactic plane and the direction of motion of the filament defined in Figure 1 (case (b)). For the shock obliquity, a typical error of 1° is assigned to all the regions.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Flux profiles of the regions SW7–SW12. The same convention for the plots is used as in Figure 17.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Magnetic field directions estimated at the stars around the RCW 86 region. Δl ∥, Δb ∥, and P indicate the Galactic longitude and latitude with respect to the coordinates (l, b) = (315.°4015, −2.°31664), and polarization degree, respectively. Left and right panels show the estimates for distances of 2–3 kpc and 3–4 kpc, respectively.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Plots of the filament width (w) against the shock velocity (v sh;  proper motion velocity is substituted). A distance of 2.8 kpc is assumed. The solid lines indicate two functions, ﹩w\propto {v}_{\mathrm{sh}}^{-3/2}﹩ (green) and ﹩w\propto {v}_{\mathrm{sh}}^{-9/4}﹩ (blue).
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Plots of the emission measure (﹩\propto {n}_{{\rm{e}}}^{2}﹩) as a function of the shock velocity (v sh;  proper motion velocity is substituted). A distance of 2.8 kpc is assumed. The EM is shown in the same units as in Table 4. The solid lines indicate two conditions, ﹩{n}_{{\rm{e}}}{v}_{\mathrm{sh}}=\mathrm{const}.﹩ (green) and ﹩{n}_{{\rm{e}}}{v}_{\mathrm{sh}}^{2}=\mathrm{const}.﹩ (blue).
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Power-law fluxes of the individual filaments (top) and their 2013-to-2001 ratios (bottom; only for the nonthermal-dominated filaments). The flux is calculated for the 0.5–7.0 keV energy range.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: (a) QS—Left: solar disk observed in the AIA 171 ﹩\dot{A}﹩ channel. The image was taken on 2014 February 25 at 12:56:11 UT by SDO. The green rectangle shows the QS area observed in this study. Right: graph of chromospheric height in terms of wavelength. The magenta lines indicate the height of the peaks h and k. (b) Limb filament loop—Left: Solar disk observed in the AIA 171 ﹩\dot{A}﹩ channel. The image was taken on 2014 August 16 at 22:59:47 UT by SDO. The green rectangle shows the limb filament loop observed in this study. Right: graph of chromospheric height in terms of wavelength. The magenta lines indicate the height of the peaks h and k. (c) Coronal hole—Left: solar disk observed in the AIA 171 ﹩\dot{A}﹩ channel. The image was taken on 2017 August 15 at 01:48:57 UT by SDO. The green rectangle shows the coronal hole area observed in this study. Right: graph of chromospheric height in terms of wavelength. The magenta lines indicate the height of the peaks h and k. (d) Active region—Left: solar disk observed in the AIA 171 ﹩\dot{A}﹩ channel. The image was taken on 2014 August 27 at 21:58:35 UT by SDO. The green rectangle shows the active region observed in this study. Right: graph of chromospheric height in terms of wavelength. The magenta lines indicate the height of the peaks h and k.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Point 1 (P1)—first row: Doppler velocity time slice diagram at k3 peak of Mg II spectral line core. In this diagram, the speeds are shown in blue, white, and red form, and from −40 to +40 km s−1. Second row—right: global wavelet spectrum of Doppler velocity of k 3 peak of Mg II spectral line core. Second row—left: Doppler velocity wavelet analysis at k 3 peak of Mg II spectral line core. Values normalized to mean value, with blueish color depicting lower values and yellowish color depicting higher ones. Third row: Doppler velocity time slice diagram at h 3 peak of Mg II spectral line core. In this diagram, the speeds are shown in blue, white, and red form, and from −40 to +40 km s−1. Fourth row—right: global wavelet spectrum of Doppler velocity of h 3 peak of Mg II spectral line core. Fourth row—left: Doppler velocity wavelet analysis at h 3 peak of Mg II spectral line core. Values normalized to mean value, with blueish color depicting lower values and yellowish color depicting higher ones. Fifth row: cross wavelet analysis of Doppler velocities of k 3 and h 3 peak of Mg II spectral line core.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: (a) Active region: Mg II distribution diagram of active region (2014 February 25 at 12:56:11 UT). Investigation of the Mg II spectrum reveals two index peaks, k and h, each peak highlighted by blue. (b) Coronal hole: Mg II frequency distribution diagram of active region (2014 August 16 at 22:59:47 UT). Investigation of the Mg II spectrum reveals two index peaks, k and h, each peak highlighted by blue. The valleys of this index peak are identified by the names k 3 and h 3, which correspond to the peaks k and h, respectively.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: SDO/HMI images in three wavelengths of 193, 171, and 304 ﹩\dot{A}﹩ and SDO/HMI magnetogram related to the photosphere, respectively. (a) SJI Si IV(1400 ﹩\dot{A}﹩), in which the network BPs are marked with black circles and the internetwork BPs are marked with red triangles. (b) SDO/HMI magnetograms, in which the network BPs are marked with black circles and the internetwork BPs are marked with red triangles.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: The maximum Doppler velocity diagram shows well the red and blueshifts of the spectrum based on the Doppler velocity. Upper left The maximum Doppler velocity diagram of AR Mg II k. Upper right: the maximum Doppler velocity diagram of AR Mg II h. Bottom left: the maximum Doppler velocity diagram of CH Mg II k. Bottom right: the maximum Doppler velocity diagram of CH Mg II h.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: (a) The positions of points P1 to P5 are shown on SJI 1403 ﹩\dot{A}﹩ (Si IV). This SJI is related to the AR, which was captured on 2016 August 2. In this figure, the intensity is inverted and negatived. (b) The positions of points P6 to P9 are shown on SJI 1403 ﹩\dot{A}﹩ (Si IV). This SJI is related to the coronal hole area, which was captured on 2016 October 14. In this figure, the intensity is inverted and negatived.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Upper: Mg II spectral data for a specific wavelength in terms of time. Bottom left: compressed spectral Mg II related to certain wavelength over time. Bottom middle: averaging spectral data over time and converting it to a column. Bottom right: intensity–height graphs for accurate readings of specified chromosphere height at each wavelength.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Point 3 (P3)—same as Figure 6 explanation but for P3.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Point 2 (P2)—same as Figure 6 explanation but for P2.
Paper: On the Mass Function of GWTC-2 Binary Black Hole Systems and Their Progenitors
Authors: Hye-Jin Park, Shin-Jeong Kim, Shinna Kim, Maurice H. P. M. van Putten
Figure caption: Overview of the primary (M 1) and secondary (M 2) mass estimates of the intermediate BBHs in GWTC-2. Grey crosses indicate uncertainties. A linear fit shows a slope 0.67 with a correlation coefficient of r = 0.93 ± 0.06 (Section 2).
Paper: On the Mass Function of GWTC-2 Binary Black Hole Systems and Their Progenitors
Authors: Hye-Jin Park, Shin-Jeong Kim, Shinna Kim, Maurice H. P. M. van Putten
Figure caption: (Top panel) Histogram of normalized mass differences in the BBHs of GWTC-2, ﹩\left|\delta M/\mu \right|﹩. (Bottom panel) Symmetric histogram of signed normalized mass difference (over all individual BH masses) in three bins with standard deviation 22%.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Point 5 (P5)—same as Figure 6 explanation but for P5.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Point 6 (P6)—same as Figure 6 explanation but for P6.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Point 8 (P8)—same as Figure 6 explanation but for P8.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Point 7 (P7)—same as Figure 6 explanation but for P7.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Point 9 (P9)—same as Figure 6 explanation but for P9.
Paper: A New Approach to Kinetic Energy Flux at the Different Frequencies above the IRIS Bright Points 
Authors: Rayhane Sadeghi, Ehsan Tavabi
Figure caption: Point 4 (P4)—same as Figure 6 explanation but for P4.
Paper: On the Mass Function of GWTC-2 Binary Black Hole Systems and Their Progenitors
Authors: Hye-Jin Park, Shin-Jeong Kim, Shinna Kim, Maurice H. P. M. van Putten
Figure caption: (Top panel) The true and observed BBH mass functions of GWTC-2 modeled by a broken power-law distribution (Abbott et al. 2021b), shown in a log-log plot rescaled to μ according to Equation (8) in units of Gpc−3yr﹩{}^{-1}{M}_{\odot }^{-1}﹩ and ﹩{M}_{\odot }^{-1}﹩, respectively. The breaks shown are at μ  b1 = 4.64 M ⊙ and μ  b2 = 31.4 M ⊙ (solid black dots). (From Equation (8), the equivalent values of M 1 = 5.56 M ⊙ and M 1 = 37.6 M ⊙ are obtained; the latter is consistent with ﹩{m}_{\mathrm{break}}={39.7}_{-9.1}^{20.3}{M}_{\odot }﹩ in Abbott et al. 2021b). Section A refers to a model extension, below the observed BBH mass range 6.9 M ⊙ ≤ μ ≤ 79.1 M ⊙. (Lower panel) The tail of the distribution corresponds (Section C) to a power-law index of −4.98 of the true distribution, which is steeper by about 17% than the index of −4.26 of the observed distribution.
Paper: On the Mass Function of GWTC-2 Binary Black Hole Systems and Their Progenitors
Authors: Hye-Jin Park, Shin-Jeong Kim, Shinna Kim, Maurice H. P. M. van Putten
Figure caption: (Left panel) The binned PDF of the BBH mass function by the mean mass μ of BBH systems in GWTC-2. The tail of the μ distribution beyond the peak at ≳  31.4 M ⊙ (solid green) is fitted to derive a power-law index α  B  indicated by the straight line (red with black uncertainties by counting statistics) in the bins with 13, 5, 1, and 1 element(s). (Right panel) μ-redshift relation (circles) with elements in the tail highlighted (filled). The mean values ﹩(\bar{\mu },\bar{z})=(41.9\,{M}_{\odot },0.51)﹩ of the mass and redshift in the tail (+) are indicated with 1σ uncertainty (ellipse).
Paper: On the Mass Function of GWTC-2 Binary Black Hole Systems and Their Progenitors
Authors: Hye-Jin Park, Shin-Jeong Kim, Shinna Kim, Maurice H. P. M. van Putten
Figure caption: Steepening in the power-law index Δα  B  reaches about 8% of Equation (9) in the progenitor redshift ﹩{z}^{{\prime} }﹩ by the cosmic-time-dilation factor J  z  in the ansatz in Equation (16) over the index range 0.5 ≤ γ ≤ 1 on a three-flat ΛCDM background for f = 0.03, 0.049, 0.068. The results for a fiducial uniform distribution (U) and the BBH data in the tail of the GWTC-2 catalog (D) are rather similar.
Paper: On the Mass Function of GWTC-2 Binary Black Hole Systems and Their Progenitors
Authors: Hye-Jin Park, Shin-Jeong Kim, Shinna Kim, Maurice H. P. M. van Putten
Figure caption: Progenitor redshifts ﹩{z}^{{\prime} }﹩ for γ = 0.30 (blue), γ = 0.75 (orange), and γ = 1.00 (green) in Equation (16) on a three-flat ΛCDM cosmological background. Horizontal dashed lines highlight ﹩{z}^{{\prime} }=2﹩ and 10. The associated mean of ﹩{z}^{{\prime} }﹩ vs. model parameter γ increases above the mean redshift z = 0.51 in the tail of the BBHs of GWTC-2 for γ > 0.75. ﹩{\alpha }_{B}^{{\prime} }﹩ of their PDFs is summarized in Table 1, showing steepening when μ − t  c  satisfies a positive correlation (γ > 0.75).
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Velocity (top panel), opacity (middle panel), and mass flux (bottom panel) profiles for the 1.2 + 3 × 10−5 M ⊙ C/O-enriched envelope calculation. The location of the τ = 2/3 photosphere is shown as a circle for each profile, and the location of the Roche radius assuming a 0.3 M ⊙, 0.3 R ⊙ Roche-lobe-filling donor is shown as a dotted line. Times are given with respect to the time of maximum effective temperature.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Same as Figure 2, but showing radial profiles of the density (top panel), temperature (middle panel), and mass above the location of maximum energy generation (bottom panel). Comparison of Figures 2 and 3 shows that most of the envelope is lost between days 2 and 11 when the outflow velocities at the Roche radius are low. In reality, binary interactions thus dominate the properties of the ejected mass.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Time evolution of the velocity at the Roche radius for a 1.2 M ⊙ WD with a C/O-enriched 3 × 10−5 M ⊙ outbursting envelope. The thin line represents the evolution after the photosphere recedes to the location of the iron opacity bump and is only shown for completeness, as our models are not quantitatively accurate during this phase. The Roche radius is calculated assuming a 0.3 M ⊙, 0.3 R ⊙ Roche-lobe-filling donor, and the dotted line is the WD’s orbital velocity in such a CV system.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Same as Figure 2, but showing radial profiles of the ratio of the velocity to the isothermal gas sound speed (middle panel) and the ratio of the velocity to the radiation sound speed (bottom panel). The velocity profile is shown again in the top panel for clarity.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Photospheric luminosity vs. effective temperature for a simulation of a 1.2 M ⊙ WD with a 10−5 M ⊙ C/O-enriched outbursting nova envelope. The model is evolved with MESA and does not include any effects of a companion star. See Sections 2 and 3 for more details.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Same as Figure 6, but vs. the remaining envelope mass, defined as the mass contained between the maximum in the energy generation rate and the τ = 2/3 photosphere. Most of the mass is lost at low speeds for which binary interaction cannot be neglected.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Fraction of the ejected mass that is ejected with v Roche < v orb vs. initial envelope mass for the solar composition envelope models. The WD masses are as labeled.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Radial profiles of various luminosities, as labeled, for the 1.2 + 3 × 10−5 M ⊙ C/O-enriched envelope model.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: Left): the simulated number of LGRB afterglows serendipitously detected by ZTF as intranight transients in two years of observations (2020 and 2021) based on the all-sky Swift/BAT rate, the sample of Swift/BAT afterglows from Cenko et al. (2009), and 1000 Monte Carlo trials. The distribution is well described by a Poisson function with λ = 1.04. The vertical dotted line shows the observed number, including one LGRB-associated and two orphan events. (Right): the simulated number of dirty fireballs serendipitously detected by ZTF for four different hypothetical relative rates. The vertical dotted line shows the number of observed orphan afterglows. If both are dirty fireballs, their rate does not exceed 6× the LGRB rate (95% confidence). If neither are dirty fireballs, then the upper limit is 3× the LGRB rate (95% confidence). Note that the true number of ZTF-detected afterglows is higher; we consider a restricted sample for the rate estimate to ensure completeness.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: Evolution of the radio SED of AT 2021any (circles) and AT 2021lfa (squares), afterglows with no associated detected GRB. The lines show power-law fits to the data for each epoch with >2 data points. The SEDs of AT 2021any appear optically thin throughout. The SEDs of AT 2021lfa appear self-absorbed up to 21.71 days and then become optically thin, suggesting that the self-absorption frequency has passed through the VLA observing bands. Note that the light curve of AT 2021lfa shows evidence for scintillation at ν ≲ 10 GHz.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: The UVOIR SED of AT 2021lfa, an afterglow with no associated detected GRB. The SED was obtained at Δt = 1.7 days by LT in the ugriz bands and shows a dropoff before the u band, likely due to extinction. We show a fit to an SMC dust extinction law.