adsabs/AstroCLIMB huggingface dataset:
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: Linear instability analysis results for the parallel-propagating right-helicity waves at 0 < ω  r  < Ω p  (left column) and ω  r  ≥ Ω p  (right column) at a wide range of T  p  and different pickup angles, as labeled. The growth rate is indicated by the color scale, while the black contours represent the real frequency.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: Linear instability analysis results for the parallel- and antiparallel-propagating left-helicity waves at a wide range of T  p  and different pickup angles, as labeled. The growth rate is indicated by the color scale, while the black contours represent the real frequency.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The pickup ion temperature range of the unstable parallel-propagating right-helicity waves at frequencies below (blue region) and above (orange) the proton cyclotron frequency as a function of the pickup angle. The hatched area indicates where γ/Ω p  > 10−5.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The pickup ion velocity distributions at tΩ p  = 0, 3000, and 30,000 in the one-dimensional simulations of different pickup angles and pickup ion temperatures, as labeled on the top of each panel.
Paper: Unstable Phenomena in Stable Magnetospheres: Searching for Radio Flares from Magnetic OBA Stars Using VCSS
Authors: Emil Polisensky, Barnali Das, Wendy Peters, Matt E. Shultz, Eugene Semenko, Tracy E. Clarke
Figure caption: Fraction of 50,000 simulated catalogs having N match matches to the VCSS catalog. A Poisson distribution with an expected value equal to the average number of matches (0.34) is a good fit to the simulations (dashed line). The simulations agree with the calculations for the stellar catalog (solid line) that the probability of three VCSS matches is <1%.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The growth rates and real frequencies of the mirror waves for α = 80°, 70°, and 45° and at different pickup ion temperatures. Each column corresponds to a different pickup angle and each row corresponds to a different pickup ion temperature, as labeled.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: Temporal evolution of the wave magnetic field energy densities normalized to the background magnetic field energy density in several one-dimensional hybrid simulations corresponding to different pickup angles and pickup ion temperatures.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: Magnetic power spectra of the enhanced waves in frequency and wavenumber space in two different intervals in the one-dimensional simulations of different pickup angles and pickup ion temperatures.
Paper: Cannonball or Bowling Ball: Proper Motion and Parallax for PSR J0002+6216
Authors: S. Bruzewski, F. K. Schinzel, G. B. Taylor, P. Demorest, D. A. Frail, M. Kerr, P. Kumar
Figure caption: Constraints in the density–energy space derived from the observed outer and inner radii of CTB 1, assuming a distance of 3 kpc (near that found in Hailey & Craig 1994). The red region represents outer radii which are within ﹩1^{\prime} ﹩ of ﹩17\buildrel{\,\prime}\over{.} 5﹩, while the blue region represents inner/shell radii which are within ﹩2^{\prime} ﹩ of ﹩13^{\prime} ﹩. The space where both regions overlap is shown for 3 kpc as well as a few other distances.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: Fits to the 7300 Å region containing [Fe II] and [Ni II] features are consistent with a low Ni II abundance. The observed spectra are shown in gray. The colored lines correspond to the models of [Fe II] (orange) and [Ni II] (purple) features. For the model parameters we adopt the mean values of their posterior distributions. The black solid lines are the overall models.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: Prominent C II λλ6580, 7234 absorption lines at maximum luminosity. No evident C II λ6580 lines are found in the earliest spectrum (−12 days; though there is one absorption feature that might be associated with C II λ7234 at ∼14,000 km s−1) or in the post-maximum spectrum (+3 days). All spectra are binned with a bin size of 5 Å, except for the low-resolution SEDM spectrum (+3 days). The dashed lines correspond to the wavelengths of the C II lines assuming a range of velocities.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: The solid-black profile is the measured VSWR of the prototype CLPDA. The dashed-gray profile, the measured VSWR of the 50–500 MHz prototype LPDA (the same as the solid-black profile of Figure 6), is overplotted for the sake of comparison.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Top to bottom: VSWR profiles of the prototype CLPDAs having OB ratios 1:3 (200–600 MHz), 1:11 (40–440 MHz), 1:20 (30–600 MHz), and 1:25 (30–750 MHz).
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Measured polarization crosstalk of the CLPDA as a function of azimuthal angle when the transmitter was kept in horizontal orientation. The values at 50, 250, and 500 MHz are shown with open circle, square, and diamond symbols, respectively. A custom fit (﹩-{\rm{a}}\,{\cos }^{b}\theta -{\rm{c}}﹩) to the average crosstalk values is shown with dashed marks. The best fit (χ 2 ≈ 0.93 and rms error ≈2.5) was obtained when the coefficients a, c, and power index b were equal to ≈30, 0.3, and 0.65, respectively. The latter gives ≈−30, −29, −27, −24, −19, −13, and 0 dB as the average crosstalk values at position angles 0°, 15°, 30°, 45°, 60°, 75°, and 90°, respectively.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Photograph of the prototype CLPDA.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Same as Figure 16 but when the transmitter was kept in the vertical orientation. The best fit (χ 2 ≈ 0.82 and rms error ≈2.0) was obtained when the coefficients a, c, and power index b were equal to ≈9.3, 17.8, and 0.85, respectively. The average crosstalk values are ≈−27, −27, −26, −25, −23, −21, and −18 dB at 0°, 15°, 30°, 45°, 60°, 75°, and 90°, respectively.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Polarization crosstalk or isolation pattern of the CLPDA at 50 (solid-gray), 250 (solid-black), and 500 MHz (dashed-black). Left: transmitter kept in horizontal orientation. Right: transmitter kept in vertical orientation.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Measured E-plane (left panel) and H-plane (right panel) radiation patterns at 50, 250, and 500 MHz.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Isolation/crosstalk of the CLPDA at 0° azimuthal angle vs. frequency. The “filled circle” symbols correspond to the measured crosstalk level at different frequencies, and the “solid-black” line represents the mean value.
Paper: Chemical Evolution of Some Selected Complex Organic Molecules in Low-mass Star-forming Regions
Authors: Bratati Bhat, Rumela Kar, Suman Kumar Mondal, Rana Ghosh, Prasanta Gorai, Takashi Shimonishi, Kei E. I. Tanaka, Kenji Furuya, Ankan Das
Figure caption: Abundances of the COMs at the different evolutionary stages of low-mass star-forming regions.
Paper: ALMA 400 pc Imaging of a z = 6.5 Massive Warped Disk Galaxy
Authors: Marcel Neeleman, Fabian Walter, Roberto Decarli, Alyssa B. Drake, Anna-Christina Eilers, Romain A. Meyer, Bram P. Venemans
Figure caption: Rest-frame 1900 GHz continuum (top left), integrated [C II] flux density (top right), mean [C II] velocity field (bottom left), and [C II] velocity dispersion field (bottom right) of the quasar P036+03. In the top two panels, the contours start at 2σ and increase by powers of ﹩\sqrt{2};﹩ negative contours at similar levels are dashed. The integrated [C II] flux shows the emission over a velocity range between −180 km s−1 and +180 km s−1, relative to z = 6.5406. The mean velocity field and velocity dispersion field were generated by fitting Gaussian profiles to the spectra at each pixel (for further details, see Neeleman et al. 2021). In all panels, the synthesized beam is shown in the bottom left corner.
Paper: ALMA 400 pc Imaging of a z = 6.5 Massive Warped Disk Galaxy
Authors: Marcel Neeleman, Fabian Walter, Roberto Decarli, Alyssa B. Drake, Anna-Christina Eilers, Romain A. Meyer, Bram P. Venemans
Figure caption: Kinematic modeling of the [C II] emission line for P036+03. The top row shows the results from a simple thin disk model, whereas the bottom row shows the results of a thin disk model that has a warp. The left panel of each row shows the data, the middle panel the model, and the right panel the residual. In all cases, the raster image is the velocity field whereas the contours show the integrated [C II] emission line. The plotted range in the velocity field has been truncated to ± 30 km s−1 in order to highlight the distortion in the velocity field and the residuals in the rightmost panels. Contours start at 2σ and increase by powers of ﹩\sqrt{2};﹩ negative contours at similar levels are dashed. The bottom left inset in the left panels shows the synthesized beam of the observations.
Paper: ALMA 400 pc Imaging of a z = 6.5 Massive Warped Disk Galaxy
Authors: Marcel Neeleman, Fabian Walter, Roberto Decarli, Alyssa B. Drake, Anna-Christina Eilers, Romain A. Meyer, Bram P. Venemans
Figure caption: Left panel: integrated [C II] emission of P036+03. The black ellipses are elliptical fits to the contours in the integrated [C II] emission image, starting at 3σ and increasing by 1σ. The solid black circles mark the position of the apexes of the ellipses along the major axes. The dashed line is a simple parametric fit to these circles. Middle panel: mean velocity field of the [C II] emission line for P036+03 with the parametric fit overlaid. Also shown is the perpendicular curve to this fit (red dashed line). Right panel: position–velocity diagram along the parametric fitted line (black dashed line in left and middle panels). Positive x-values correspond to the southern “arm” of the parametric fit.
Paper: ALMA 400 pc Imaging of a z = 6.5 Massive Warped Disk Galaxy
Authors: Marcel Neeleman, Fabian Walter, Roberto Decarli, Alyssa B. Drake, Anna-Christina Eilers, Romain A. Meyer, Bram P. Venemans
Figure caption: Velocity field for the interstellar medium and circumgalactic medium of P036+03 as traced by [C II] and Lyα, respectively. The velocity field of the [C II] emission line is the same as in Figure 1, albeit at a different velocity scale. The velocity field of the Lyα line is described in detail in Drake et al. (2022) and is shown here at the native pixel scale of the VLT/MUSE observations (0.″2). For the MUSE observations, only Lyα emission belonging to the halo is shown (see Farina et al. 2019). Unlike the [C II] velocity field, the Lyα velocity field is the flux-weighted mean velocity, which is the first moment of the data cube along the spectral direction. However, this different approach does not affect the conclusions in this paper.
Paper: ALMA 400 pc Imaging of a z = 6.5 Massive Warped Disk Galaxy
Authors: Marcel Neeleman, Fabian Walter, Roberto Decarli, Alyssa B. Drake, Anna-Christina Eilers, Romain A. Meyer, Bram P. Venemans
Figure caption: Spatially resolved [C II] deficit for P036+03. Only pixels are shown for which both the 1900 GHz dust continuum emission and the [C II] emission line are detected at >2σ. The color bar shows the ratio of these two measurements, both expressed as an equivalent width and as a luminosity ratio. However, we caution the reader about the conversion factors used in obtaining this latter expression (see Walter et al. 2022). The average synthesized beam is shown in the bottom left inset.
Paper: ALMA 400 pc Imaging of a z = 6.5 Massive Warped Disk Galaxy
Authors: Marcel Neeleman, Fabian Walter, Roberto Decarli, Alyssa B. Drake, Anna-Christina Eilers, Romain A. Meyer, Bram P. Venemans
Figure caption: Channel maps of the [C II] emission line for P036+03. The redshift reference for the relative velocities is z = 6.5406 (252.040 GHz). Contours start at 2σ and increase in powers of ﹩\sqrt{2}﹩, where σ = 96 μ Jy bm−1. Negative contours at similar levels are shown in the figure with a dashed line. In the bottom left panel, we show the size of the synthesized beam for the observations.
Paper: ALMA 400 pc Imaging of a z = 6.5 Massive Warped Disk Galaxy
Authors: Marcel Neeleman, Fabian Walter, Roberto Decarli, Alyssa B. Drake, Anna-Christina Eilers, Romain A. Meyer, Bram P. Venemans
Figure caption: Channel maps of the residual after subtracting the best-fit warped disk model. The figure has the same scale, and contours are drawn at the same levels as in Figure 6.
Paper: Discovery of a Low-redshift Hot Dust-obscured Galaxy
Authors: Guodong Li, Chao-Wei Tsai, Daniel Stern, Jingwen Wu, Roberto J. Assef, Andrew W. Blain, Tanio Díaz-Santos, Peter R. M. Eisenhardt, Roger L. Griffith, Thomas H. Jarrett, Hyunsung D. Jun, Sean E. Lake, M. Lynne Saade
Figure caption: Best-fit SED template model (heavy gray line) of W1904+4853. The photometric data points are extinction corrected and emission line subtracted. The black open circles represent the photometry before the emission-line corrections. See Section 2.2 for details. The magenta open circle with an error bar is the line-subtracted GALEX NUV flux, assuming it is also affected by strong emission lines. See Section 3.1 for details. The SED modeling uses templates of irregular galaxies with ﹩{Av}={7.5}_{-1.0}^{+1.1}﹩ (brown) and starburst components (blue) from Assef et al. (2010), and the single power-law (SPL) dust distribution model (red) from C.-W. Tsai et al. (2023, in preparation) with p = −0.82 ± 0.02, ﹩{T}_{{\rm{h}}}={539}_{-6}^{+6}﹩ K, and ﹩{T}_{{\rm{c}}}\,=\,{37}_{-3}^{+3}﹩ K. The parameters of SPL (p, T h, and T c) represent the power-law index for dust grain number density with radius, and the upper and lower limits of the dust temperature (see Section 3.2).
Paper: Discovery of a Low-redshift Hot Dust-obscured Galaxy
Authors: Guodong Li, Chao-Wei Tsai, Daniel Stern, Jingwen Wu, Roberto J. Assef, Andrew W. Blain, Tanio Díaz-Santos, Peter R. M. Eisenhardt, Roger L. Griffith, Thomas H. Jarrett, Hyunsung D. Jun, Sean E. Lake, M. Lynne Saade
Figure caption: Optical spectrum of W1904+4853 obtained at Palomar Observatory. The spectrum covers wavelengths 3200–10,500 Å in the observed frame, with a gap from 5500–5700 Å due to the dichroic mirror. The emission lines labeled on the plot are for the spectroscopic redshift of z = 0.415, corresponding to rest-frame wavelength coverage of 2260–7420 Å.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The wave magnetic field wavenumber-frequency power spectra given by the Fourier decomposition analysis in two different intervals in the three two-dimensional simulations of α = 45° and different pickup ion temperatures, as labeled.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: Temporal evolution of the wave magnetic field energy densities normalized to the background magnetic field energy density in the two-dimensional hybrid simulations corresponding to different pickup angles and pickup ion temperatures, as labeled.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The wave magnetic field power spectra in k ∥ − k ⊥ space at three different times in the three two-dimensional simulations for α = 45° and different pickup ion temperatures, as labeled.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The evolution of the standard deviations of the pickup ion pitch angles in the one-dimensional hybrid simulations of different pickup angles and pickup ion temperatures.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The pickup ion velocity distributions at tΩ p  = 0 and tΩ p  = 2400 from the two-dimensional hybrid simulations of various pickup angles and pickup ion temperatures, as labeled.
Paper: The Impact of Pickup Ion Thermal Spread on Pickup Ion Ring-beam-driven Instabilities and Scattering in the Outer Heliosheath
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The evolution of the standard deviations of the pickup ion pitch angles in the two-dimensional hybrid simulations of different pickup angles and pickup ion temperatures.
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: Flux vs. the model light curve X(t) for all wave bands. The best-fitting flux–flux relations are shown as solid lines. X  g  indicates the value of X(t) where the error envelope of the fit to the shortest-wavelength band (1180 Å; purple) intercepts f  ν  = 0. The flux–flux relations at X(t) = X  g  gives the value of the constant flux in each band, while the slope of the relations gives the strength of the variable component. X  F  and X  B  indicate the faint and bright values of X(t), respectively.
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: Lags as a function of rest wavelength with respect to the UVW2 band (vertical dotted line) for the Swift (green) and HST (blue) wave bands for the three different lag determination methods. The left-hand panels (filled symbols) indicate lags calculated from the original light curves, while the right-hand panels (open symbols) are lags determined from the detrended light curves. The solid lines show the best-fitting τ ∝ λ 4/3 relation to the lags using the original and detrended light curves. The dashed line in panel (c) shows the best-fitting lag relation from the “bowl” model.