adsabs/AstroCLIMB huggingface dataset:
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: Observed (dereddened) SEDs (black) of AT 2018cow at six sample epochs including the three HST epochs (bottom panels). The HST measurements are marked as stars. The best-fit models (solid lines) are also shown, derived using the BLACKBODY + POWER LAW model. Photometry excluded from the fit is shown in gray (see text for reasoning). The UV–optical continuum of AT 2018cow at t ≃ 50–60 days is consistent with a blackbody curve peaking at λ ∼ 3000 Å.
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: Analog of the Branch diagram for the very-early-phase spectra we used (left). Circles represent the NV type, inverse triangles indicate the HV type, and stars correspond to the 1999aa-like type. The same figure but marked with Δm 15 is shown in the middle panel; the colors of the symbols indicate the values of Δm 15 following the color bar on the right side. The same but marking the photospheric temperature is shown in the right panel.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: Blackbody luminosity and power-law luminosity (L BB and L PL) derived from the BLACKBODY + POWER LAW model, as well as the Swift 0.3–10 keV luminosity from Margutti et al. (2019; similar X-ray light curves were also derived in Rivera Sandoval et al. 2018, Kuin et al. 2019, and Ho et al. 2019). Blackbody luminosities derived using HST photometry are shown as stars. Best-fit broken power laws to the luminosities are shown in dashed lines. A dotted line is shown to illustrate the expected decline of the blackbody luminosity if the rate of decline remained t −2.40.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: Example cutout images of the field of AT 2018cow taken by Swope (left) and HST (right). The filter and observation date are shown at the top, and a circular aperture is placed at the position of AT 2018cow. The high-resolution HST image shows AT 2018cow as an isolated point source not affected by any significant contamination from the diffuse background or nearby sources.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: Properties derived from fitting the BLACKBODY + POWER LAW model. Properties derived using HST photometry are shown as stars. The blackbody luminosity was calculated through the Stefan–Boltzmann law while the power-law luminosity was calculated by integrating between 2000 Å ≤ λ ≤ 1 mm.
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: Relation between the time since the explosion and luminosity. The symbols represent the results of the TARDIS modeling. This is overlapped with the R- or r-band light curve for each object. Different colors are used for different subclasses (see the caption of Figure 8). Note that SN 2011fe is hidden behind SN 2018gv.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: Blackbody luminosity of AT 2018cow (L BB) and best-fit radioactive decay models (56Ni) for the light curve after 25 days. The model without γ-ray leakage cannot fit the light curve at all while the model with γ-ray leakage can fully describe the light curve after t ∼ 25 days.
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: Major axis one-dimensional surface brightness profiles of the source-plane reconstruction for each filter. The large inferred inclination, clear asymmetry, and lack of an obvious center for all filters make this a more robust approach than a radial profile, as tested by Devour & Bell (2017, 2019). Left: filter-by-filter surface brightness profiles along the major axis (as determined by the median position angle from GALFIT models for all filters). Each bin along the profile, which shows the sum of pixels above a 2σ clipped threshold, is extracted from a 1.″5 wide box perpendicular to the major axis. The profile for each filter (each convolved to match the F444W PSF) is normalized between 0 and 1 and has arbitrary flux units, and they are shifted vertically for the purpose of legibility. Bins are spaced at intervals of ≈0.″045 along the 2″ long slit, comparable to the pixel size. The thickness of the curve indicates signal-to-noise, which is determined from the signal-to-noise ratio of the 95th percentile value of pixels in each bin. Differing pixel scales and depths likely play a role in discrepancies between adjacent filters. Vertical dashed lines show the smallest effective radius (for F606W). Center: an RGB image showing all 8 NIRCam filters (red, F356W + F410M + F444W; green, F200W + F277W; blue, F090W + F115W + F150W). The white box shows the slit used to compute the surface brightness profiles, with the middle line showing the major axis orientation. The beams in the lower left show the FWHM and orientation of representative source-plane PSFs for F115W (cyan) and F444W (red). These are created by ray-tracing a model PSF placed at the location of the galaxy centroid in the less-magnified counter-image (1a) into the source plane, which has the least spatial variation in PSF. While the more magnified images can offer better resolution on their own, this source-plane reconstruction combines all images together, effectively smearing the structure to the resolution of the counter-image. Right: inferred surface brightness profiles in the same manner as the left panel, but applied to our GALFIT-modeled light profiles. Dashed curves for the three reddest NIRCAM filters show the 2-component models, which shift the profiles slightly.
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: Variation in the reconstructed source-plane light profile for the HST/ACS and JWST/NIRCam filters. Top: best-fit Sérsic index n determined with GALFIT for each filter. For the three longest-wavelength filters, excess model residuals near the galaxy nucleus suggest the need for a 2-component (bulge and disk) model. Here, an effective Sérsic index is shown, as discussed in Section 3.2. Filters are denoted by color as in Figure 8. As the uncertainties reported by GALFIT are likely underestimations, we scale them up to match the fractional uncertainties in magnification for each filter (Table 3). Bottom: as above, but showing effective radii for the Sérsic profiles for each filter, in angular and physical units (at the redshift of the source, z = 2.291).
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: Derived magnification μ total is shown for each HST and JWST filter available for El Anzuelo. Corresponding filter throughput curves are shown at the bottom. A dramatic rise in magnification with wavelength is due to a steepening in the light profile, as shown also with the RGB inset images showing rest-frame UV, optical, and near-IR images of the source-plane reconstruction. There is a notable discontinuity in magnification around 1 μm, which is due primarily to the lack of signal in the central core, where magnification is greatest. This is likely due to some combination of a dust attenuation and an age gradient, especially given the location of the 4000 Å break, redshifted to 1.3 μm for z = 2.291.
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: SED-fitting results for image 1a, as with Figure 7, but fluxes from Table 4 are demagnified using the median magnification μ 1a = 2.7 ± 0.2 (see Table 5). The SED is spatially decomposed into the total disk (top), inner ∼1 kpc (middle), and outer disk (bottom) according to the method described in Section 3.4.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Galaxy properties–stellar mass relations for (from top to bottom) size, SFR, color, and morphology. The blue/red points in each panel represent clumpy/nonclumpy SFGs, with their median values given by the diamonds of the same color. The orange diamonds indicate the median of the two combined populations. The corresponding error bars are shown, although most are smaller than the median symbol. The vertical black lines represent mass bin boundaries for low-, intermediate- and high-mass SFGs as defined in the text. The statistical difference between the respective medians is listed at the top of each bin.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Clump luminosity (expressed in UV absolute magnitude) vs. host galactic properties for our UVCANDELS clump distribution. The galactic properties (x-axis) shown in panels 1−3 are the host galaxy’s specific star formation rate, absolute magnitude in the rest-frame 1600 Å, and size. Panel 4 shows the clump’s galactocentric distance normalized by the host galaxy’s size. The clumps (blue points) are fitted linearly (red line) to show the robustness of each of the gradients. The blue shaded region and the dashed black lines indicate the 95% confidence and prediction intervals, respectively. At the top of each plot we show the Spearman’s rank coefficient (ρ- and r-values) statistics of each relation.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Relations of host-galaxy properties vs. stellar mass for clumpy and nonclumpy galaxies with magnitude F275W ≤ 25 AB (left) and whose clumps contribute at least 8% of the total UV luminosity. From top to bottom, we show host-galaxy size, SFR, color, and morphology. Symbols, colors, and lines are the same as in Figure 5.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Clumpy fraction for (from left to right) low-, intermediate-, and high-mass galaxies. Our UVCANDELS results (outlined red diamonds) show good agreement with the UV-selected samples (colored lines) for all mass bins.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Fiducial surface brightness distribution before our F275W magnitude restriction (left panel) and after (right panel). The blue/red points represent clumpy/nonclumpy galaxies with the dashed lines and corresponding shaded regions representing their respective medians and errors. The right panel shows the same distribution as the left with the medians now representing the subsample of data points with F275W mag ≤ 25. The gray shaded region represents the data points that were excluded in the new median calculations. With the magnitude restriction the difference between clumpy and nonclumpy surface brightness is below 0.3 dex, indicating a sufficient level of sample completeness.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: The top panel shows the apparent F275W–size distribution for our sample, while the middle and lower plots show apparent F275W–mass relations. The middle plot represents our fiducial SFG sample with individual clump luminosity M UV ≤ −16 AB, while the bottom plot represents a sample of flux ratio ≥8%. The structure of each panel is the same as in Figure 5.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Frequency of detected clumps per galaxy for our UVCANDELS (blue) and HDUV (orange) SFG samples. The dashed bars represent all detections, while the solid bars represent those clumps that pass the selection criterion for our fiducial sample.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Clump luminosity vs. host galactic SFR density. The format is the same as in Figure 9.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Histograms for Sérsic index and SFR to be compared to Shibuya et al. (2016). The figure shows (from top to bottom) the low-, intermediate-, and high-mass bins for Sérsic index (left) and SFR (right). The red (outline) histograms represent clumpy (nonclumpy) distributions, respectively, and the two-sample Kolmogorov–Smirnov test p-value is shown within each panel.
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: BdHNe I: GRB 190114C. Luminosity light curves obtained from Fermi-GBM, in 10 keV–10 MeV, Fermi-LAT in 0.1 GeV–10 GeV, Swift-BAT in 15 keV–50 keV, Swift-XRT in 3 keV–10 keV and optical R band. The late X-ray afterglow luminosity of BdHN I GRB 190114C observed by Swift-XRT is best fit by a temporal decaying power law of L X = (2.5 ± 0.4) × 1053 t 1.44±0.01 erg s−1. The light curve of Fermi-LAT in is fitted by temporal decaying power law of L GeV = (4.6 ± 2.9) × 1053 t −1.94±0.04 erg. The prediction of the associated SN by Ruffini et al. (2019b) has been successfully observed by Melandri et al. (2019) and has made GRB 190114C as a prototype of BdHN I (Moradi et al. 2021c) to study the properties of GRB-SN sources. The rest-frame visual absolute magnitude of the SN associated with GRB 190114C is ∼ − 18 mag Melandri et al. (2019), which is ∼1 mag less than the famous SN 1998bw (Patat et al. 2001). This fainter brightness could be due to the extinction of this event (Kann et al. 2019). The energies of the episodes are given in Section 7 and Table 4.
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: BdHN III: GRB 171205A. Luminosity light curves obtained from Swift-BAT in 15–50 keV, Swift-XRT in 3–10 keV and Swift-UVOT in the V and B bands. After t rf ∼ 105 s, it follows a decaying power law with index α  X  = 1.12 ± 0.08 and amplitude of A X = (1.1 ± 0.8) × 1048 erg s−1. The optical and radio data were taken from D’Elia et al. (2018) and Maity & Chandra (2021), and the X-ray data were retrieved from the Swift-XRT repository. The blue color indicates an SN bump.
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: BdHN II: GRB 190829A. Luminosity light curves obtained from H.E.S.S. in 200 GeV–4 TeV, Fermi-GBM in 10 keV–10 MeV, Swift-BAT in 15–50 keV, Swift-XRT in 3–10 keV and i band and radio band. An SN component at ∼106 is indicated as the blue color. The power-law fitting of the X-ray, shown as a green dotted line, gives a power-law index of −1.1. The T 0 is taken from the trigger of Fermi-GBM to which the initial time of other telescopes is aligned.