adsabs/AstroCLIMB huggingface dataset:
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Interpolation results from using Cryo-coefficient splines (solid lines), GPs (filled circles), and splines directly to the gains in spherical coordinate pixels (crosses) for all antenna cases. Each color denotes a different hyperparameter grid resolution, from low (black) to medium (cyan) to high (red). The left column shows the relative beam error (Equation (6)) between the interpolated Cryo-beam from MEDEA and the true CST beam. Note that the rms over all beam pixels is computed for the relative error. The right column shows the difference in antenna temperatures between the interpolated Cryo-beam and the true CST beam when both weight the same intrinsic foreground map (Equation (7)). The light-gray-dashed line indicates the zero-point for each antenna case.
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Results from truncating the Cryofunk basis to the number of terms shown on the x-axis for each antenna case. Each color denotes a different antenna at a healpy resolution of N side = 32: the ROLSES dipole (purple), the patch antenna (cyan), and the analytical dipole (gold). The y-axis represents the amount of gain removed by each Cryo-mode, normalized to the rms of the full gain of the CST beam. Therefore, the y-axis is unity and the fractional gain removed is zero when no Cryo-modes are included in the Cryo-beam; in contrast, the fractional gain approaches zero when all modes are included in the Cryo-beam, as the Cryo-basis is a complete basis. As can be seen from the inset, 20–40 modes remove approximately 90% of the gain for all cases, and most of the gain is removed by ∼100 modes. While the remaining modes above l = 100 remove several orders of magnitude of power, all of them are well below <10−5, so they contribute comparatively little to the overall beam pattern.
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Triangle plot showing the galactic foreground spectral index parameters (β  i ) and beam hyperparameter h for the analytical dipole fit. The mock beam-weighted foreground spectra were made using a beam hyperparameter of h = 2.0 m. The contours here correspond to the thermal noise case, where the mock radio spectrometer data is well described by the beam-weighted foreground model of Equation (13). The black dotted line indicates the input beam hyperparameter value used to generate the mock radio spectrometer data.
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Rendering of the ROLSES-inspired Stacer antennas simulation setup in CST using the same FIT solver and PML boundary conditions as the patch antenna. Depicted are the side view (left) and top view (right) of the simplified ROLSES lander above the lunar regolith on landing struts.
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Rendering of the patch antenna simulation setup in CST using the FIT solver and contained within a bounding box with PML boundary conditions. The top panel shows the cross section and interior construction of the patch antenna. The bottom panel shows the location of the patch antenna situated on top of a simplified generic lander resting on a lunar regolith slab.
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Polar plots showing the E- and H-plane cuts for the relative beam errors (Equation (6) without calculating the rms over pixels) for all three antennas at mid-band frequencies. Note that these are the beams generated at the missing hyperparameter value ζ  T  for each case.
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Orthographic projection of the direct decomposition of all antenna cases. Each antenna case is shown at a representative beam hyperparameter and mid-band frequency. We note that these beams exhibit significant topographical complexity, but that Cryofunk has little difficulty in describing these complex beam patterns up to numerical precision in floating-point operations.
Paper: Detection of a Transient Quasiperiodic Oscillation in γ-Rays from Blazar PKS 2255-282
Authors: Ajay Sharma, Anuvab Banerjee, Avik Kumar Das, Avijit Mandal, Debanjan Bose
Figure caption: A transient QPO examined with LSP and WWZ methods. (Top panel): the LSP is depicted by the solid black line with a 99.73% significance line in red. Notably, the LSP exhibits a peak at ∼0.0107 day−1 with a confidence level surpassing 3σ. In addition, a false alarm probability (FAP) has been computed, and the value is 0.000406, and 95% confidence is visually represented with a horizontal dashed orange line, indicating a 5% FAP level. Furthermore, the Poisson noise level is calculated to be approximately 0.0183, represented in a horizontal gray line. (Bottom right): a WWZ map with the cone of influence (dark-shaded region) is depicted. (Bottom left): the solid black line represents the average wavelet power across time, while the red line denotes the 99.73% level of significance.
Paper: Detection of a Transient Quasiperiodic Oscillation in γ-Rays from Blazar PKS 2255-282
Authors: Ajay Sharma, Anuvab Banerjee, Avik Kumar Das, Avijit Mandal, Debanjan Bose
Figure caption: Weekly binned Fermi-LAT light curve of PKS 2255-282 (MJD 57783.5–59358.5). Bayesian block representation of the light curve is shown by a black solid line.
Paper: Detection of a Transient Quasiperiodic Oscillation in γ-Rays from Blazar PKS 2255-282
Authors: Ajay Sharma, Anuvab Banerjee, Avik Kumar Das, Avijit Mandal, Debanjan Bose
Figure caption: In the left panel, we present the AIC distribution map of ARIMA models for the source PKS 2255-282. The optimal model, ARIMA(2, 0, 0), is highlighted in red, with an AIC of −2815.80. On the right, the AIC map for SARIMA models shows that SARIMA(1, 0, 5) × (0, 0, 1) s=91 is identified as the best model, with an AIC value of -2802.03. In the bottom panel, the AIC values for this SARIMA model were explored for different periods, and the model achieved its global minimum AIC at s = 91 days. The blue dots represent AIC values at various seasonal positions.
Paper: Detection of a Transient Quasiperiodic Oscillation in γ-Rays from Blazar PKS 2255-282
Authors: Ajay Sharma, Anuvab Banerjee, Avik Kumar Das, Avijit Mandal, Debanjan Bose
Figure caption: The celerite modeling was performed utilizing a 7 day binned γ-ray light curve of PKS 2255-282, spanning from MJD 57783.5 to 60114.5, using the SHO × 2 model. The top left panel shows the flux points and their uncertainties in blue, along with the best-fit profile from the celerite modeling in orange, including the 1σ confidence interval. The bottom left panel presents the standardized residuals as blue dots, with the horizontal orange dotted line indicating the mean of the standardized residuals. The middle panel features a histogram of the scaled standardized residuals in blue, accompanied by a solid orange line representing the expected scaled normal distribution. The right top and right bottom panels display the autocorrelation functions (ACFs) of the standardized residuals and the squared standardized residuals, respectively, with 95% confidence intervals of the white noise.
Paper: Detection of a Transient Quasiperiodic Oscillation in γ-Rays from Blazar PKS 2255-282
Authors: Ajay Sharma, Anuvab Banerjee, Avik Kumar Das, Avijit Mandal, Debanjan Bose
Figure caption: The autocorrelation function and partial autocorrelation function of standardized residuals are depicted in the top two panels, and the bottom panel represents a histogram of standardized residuals fitted with normal distribution.
Paper: Detection of a Transient Quasiperiodic Oscillation in γ-Rays from Blazar PKS 2255-282
Authors: Ajay Sharma, Anuvab Banerjee, Avik Kumar Das, Avijit Mandal, Debanjan Bose
Figure caption: The uncertainty in the observed period from LSP and WWZ analysis was estimated by fitting the dominant peaks with a Gaussian function. Left panel: the LSP peak with a period of 92 ± 2.5 days. Right panel: the 〈WWZ 〉 power plot reveals a peak with a period of 92 ± 2.7 days. A green vertical line represents the peak position of best fit.
Paper: Detection of a Transient Quasiperiodic Oscillation in γ-Rays from Blazar PKS 2255-282
Authors: Ajay Sharma, Anuvab Banerjee, Avik Kumar Das, Avijit Mandal, Debanjan Bose
Figure caption: A PSD constructed from the celerite modeling results with SHO × 2 model for the 7 day binned γ-ray light curve of PKS 2255-282 during MJD 57783.5 to 60114.5. The figure displays a plausible QPO feature with a period of ∼93 days with the 68% confidence band.
Paper: Detection of a Transient Quasiperiodic Oscillation in γ-Rays from Blazar PKS 2255-282
Authors: Ajay Sharma, Anuvab Banerjee, Avik Kumar Das, Avijit Mandal, Debanjan Bose
Figure caption: The figure displays the posterior probability densities of parameters obtained from the celerite modeling with the SHO × 2 model. The left panel (red color) corresponds to the SHO1 model, while the right panel corresponds to the SHO2 model.
Paper: Detection of a Transient Quasiperiodic Oscillation in γ-Rays from Blazar PKS 2255-282
Authors: Ajay Sharma, Anuvab Banerjee, Avik Kumar Das, Avijit Mandal, Debanjan Bose
Figure caption: The folded Fermi-LAT light curve of PKS 2255-282 in the time domain from MJD 57783.5–59358.5 above 100 MeV with a period of 93 days. The dashed red line represents the mean value. We present two-period cycles here for better clarity.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The dynamic spectrum of an example sidelobe event, FRB 20190210D. The panels from left to right represent the de-dispersed dynamic spectra of each beam from E–W in the same N–S row. Each dynamic spectrum has a frequency resolution of 3.125 MHz with the range from 400 to 800 MHz and timing resolution of 0.98304 ms with a total range of 30 ms. The frequency channels dominated by RFI are masked. The color scale is linear with intensity.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The beam response averaged over 400–725 MHz for the three calibrators shown in Figure 18 as a function of ρ(f). At the top of the figure, the vertical lines mark the modeled positions of the 10 far sidelobe events in the ρ coordinate that we define in Equation (2) and list in Table 1, with the TNS names and the HA labeled. Note that the peaks appear slightly offset from 0 deg, which is a virtual effect due to a resolution of 0.15 deg.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: Spectra (solid black) and fitted model (solid red) for the intensity localization of an example sidelobe event, FRB 20190210D. The panels represent each E–W beam as in Figure 1. The model of CHIME/FRB’s synthesized beam (arbitrarily scaled) is plotted as gray dotted lines and the underlying fitted power-law FRB spectrum is plotted as gray dashed lines. Note that residual spike-to-spike amplitude variations are likely due to either (i) deviations of the underlying spectrum from a power-law and/or (ii) frequency-dependent structure of the unmodeled primary beam.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The apparent decl. of PSRs B0531+21 and B0329+54. The dashed and dotted lines represent the apparent positions of the two pulsars. PSR B0531+21 is below the horizon at CHIME when the apparent decl. is higher than 83.5 deg. The horizontal line marks the true decl. of the pulsar, when the detected LST is equal to the R.A. of the pulsar. The source is in a lower transit when the decl. of the apparent curve is higher than 90 deg, which is marked in gray.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: MCMC output samples for the intensity localization of an example sidelobe event, FRB 20190210D. Left: prior to filtering out suboptimal modes in parameter space. Right: filtered to include only the mode with the highest likelihood.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: Plot of the function W(f, θ).We assume a flat power-law index of zero and plot the W(f, θ) of the second beam column (i.e., ϕ 1 = 0 deg at θ of 5 and 20 deg, respectively.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The localization offsets of the far sidelobe events from PSR B0329+54 and B0531+21 in terms of the range of HAs using Method 1.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The S/N vs. HA for the sidelobe events of PSR B0531+21, PSR B0329+54, and 10 FRB events.
Paper: Statistics of Solar White-light Flares. I. Optimization and Application of Identification Methods
Authors: Yingjie Cai, Yijun Hou, Ting Li, Jifeng Liu
Figure caption: Spatial and temporal distributions of WL emission enhancement signals produced by three WLFs with different GOES energy levels. (a1): Spatial distribution of the pixels with WL emission enhancement larger than 4% during the X9.3 WLF. The appearance time of these enhancement signals is marked by different colors. The blue contour approximates the flare ribbon region based on the AIA 1600 Å images with a cadence of 24 s and the red rectangle encompasses the surrounding quiet flare region of the flare ribbon region. (a2): Spatial distribution of the pixels where WL emission enhancement larger than 4% appears three times or more in total during the X9.3 WLF. The number of occurrences is marked by different colors. (a3): Spatial distribution of the pixels where WL emission enhancement larger than 4% successively appears three times or more during the X9.3 WLF. The number of occurrences is marked by different colors. (b1)–(c3): Similar to (a1)–(a3), but for the M6.6 and C8.6 WLFs, respectively.
Paper: Statistics of Solar White-light Flares. I. Optimization and Application of Identification Methods
Authors: Yingjie Cai, Yijun Hou, Ting Li, Jifeng Liu
Figure caption: Background WL emission with inherent fluctuation caused by constant convective motion in different regions around the X9.3 flare ribbon region. (a): Spatial distribution of the pixels with WL emission enhancement larger than 5% during one hour with no occurrence of flare (2017 September 6 02:00–03:00 UT) in two different regions. The red rectangle and blue contour denote the quiet Sun region and sunspot region, respectively. (b1): Temporal variation of the maximum fluctuation value among all the pixels in quiet Sun region and sunspot region at each moment (﹩{\delta }_{\max 1}﹩). (b2): Similar to (b1), but for the mean fluctuation value of all the pixels in each region (δ mean1). (c1): The proportion histogram of the maximum fluctuation value of every pixel during one hour in quiet Sun region and sunspot region (﹩{\delta }_{\max 2}﹩). (c2): Similar to (c1), but for the mean fluctuation value of the pixels during one hour (δ mean2).
Paper: Statistics of Solar White-light Flares. I. Optimization and Application of Identification Methods
Authors: Yingjie Cai, Yijun Hou, Ting Li, Jifeng Liu
Figure caption: Background WL emission with inherent fluctuation caused by constant convective motion in different regions around the C6.8 flare ribbon region. (a): Spatial distribution of the pixels with WL enhancement larger than 5% during one hour with no occurrence of flare (2015 December 29 08:00–09:00 UT) in two different regions. The red rectangle and blue contour denote the quiet Sun region and sunspot region, respectively. (b1): Temporal variation of the maximum fluctuation value among all the pixels in quiet Sun region and sunspot region at each moment (﹩{\delta }_{\max 1}﹩). (b2): Similar to (b1), but for the mean fluctuation value of all the pixels in each region (δ mean1). (c1): The proportion histogram of the maximum fluctuation value of every pixel during one hour in quiet Sun region and sunspot region (﹩{\delta }_{\max 2}﹩). (c2): Similar to (c1), but for the mean fluctuation value of the pixels during one hour (δ mean2).
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: Left: Comparison of the STIS and UVIT/FUV-G1 flux spectrum. Right: STIS spectrum: Best-fit is shown in blue, reddened and absorbed continuum is shown in black dotted line, emission lines are shown in red, and Fe II emission is shown in green. The (data-model)/error is shown in the bottom panel.