adsabs/AstroCLIMB huggingface dataset:
Paper: Eccentric Dust Ring in the IRS 48 Transition Disk
Authors: Haifeng Yang, 海峰 杨, Manuel Fernández-López, Zhi-Yun Li, Ian W. Stephens, Leslie W. Looney, Zhe-Yu Daniel Lin, Rachel Harrison
Figure caption: Left: the synthesized dust continuum image of IRS 48 at 870 μm or 345 GHz. Both the color map and the contours represent the flux density in mJy beam−1. The contours are plotted at the levels of (−3, 3, 8, 16, 64, 128, 256, 512, 1024, 1200) × σ, where σ = 14 μJy beam−1 is the rms noise. The synthesized beam is 0.″11 × 0.″072. The inset shows a 0.″15 wide zoom, with contours representing the flux density at the levels of (3, 6, 10, 14) × σ. The star location is labeled as a gray cross. Right: the same image but with a different color map with a maximum value 0.14 mJy beam−1, 10σ, to saturate the crescent-shaped structure and display the dim long tail better. The white and gray contours correspond to flux densities of 3σ and 2σ, respectively.
Paper: Eccentric Dust Ring in the IRS 48 Transition Disk
Authors: Haifeng Yang, 海峰 杨, Manuel Fernández-López, Zhi-Yun Li, Ian W. Stephens, Leslie W. Looney, Zhe-Yu Daniel Lin, Rachel Harrison
Figure caption: Left: the fitted elliptical ring in the deprojected view. The image shares the color bar with the bottom right panel. The central star (gray cross; derived from Gaia DR3) is assumed to be one of the foci. The contours are plotted at the same levels as in Figure 1. The colored ellipse shows the best-fitted ring, with colors representing the ratio of the orbital velocity to the local Keplerian velocity, v/v  K  on the color bar. The yellow ellipse at the lower left corner shows the synthetic beam deprojected to the disk plane. Bottom right: the deprojected image in (r, θ) coordinates, where θ = 0 corresponds to the aphelion of the best-fitted elliptical ring. Note that a circular orbit is a straight horizontal line in this view. Top right: the flux density along the best-fitted elliptical ring in logarithmic scale. It shares the x-axis with the panel below. The gray contours are plotted at the same levels as in Figure 1.
Paper: Eccentric Dust Ring in the IRS 48 Transition Disk
Authors: Haifeng Yang, 海峰 杨, Manuel Fernández-López, Zhi-Yun Li, Ian W. Stephens, Leslie W. Looney, Zhe-Yu Daniel Lin, Rachel Harrison
Figure caption: The R.A. (a) and decl. (c) of the crescent peak from archival ALMA data and the star assuming Gaia proper motion in units of arcseconds. The relative displacement from the assumed stellar location at each epoch is plotted in units of arcseconds in (b) and (d). The dashed lines are linear fits to each data sets. The up (down) triangles represent data points observed at ALMA Band 9 (Band 7). Panel (e): the intensity image overlaid with the predicted proper motion. The smaller and larger ellipses represent the circular and the best-fit eccentric orbit, respectively. The colorful crosses represent the fitted peak location at each epochs with errors.
Paper: JWST and ALMA Imaging of Dust-obscured, Massive Substructures in a Typical z ∼ 3 Star-forming Disk Galaxy
Authors: Wiphu Rujopakarn, Christina C. Williams, Emanuele Daddi, Malte Schramm, Fengwu Sun, Stacey Alberts, George H. Rieke, Qing-Hua Tan, 清华 谈, Sandro Tacchella, Mauro Giavalisco, John D. Silverman
Figure caption: To search for substructures in the stellar-mass distribution, we first model all components of the F430M emission (a), whose subtraction from the original image affords a flat residual (b), then only subtract the primary Sérsic model of the stellar-mass disk (c). The residuals in (d) indicate the presence of stellar-mass substructures northeast and southwest of the galaxy center. Cutouts in panels (a)–(d) are 3″ × 3″ and with a log scaling. Panel (e) shows the central 1″ × 1″ of the residuals in panel (d) with a linear scaling; the tapered ALMA residuals overplotted as orange contours start from 3σ in 1σ increments. The gray contours show the presubtraction ALMA continuum, tapered to the same scale, starting from 3σ in 5σ increments. The substructure in the northeast harboring SF and significant stellar-mass buildup, dubbed the “northern ridge,” is clearly visible.
Paper: JWST and ALMA Imaging of Dust-obscured, Massive Substructures in a Typical z ∼ 3 Star-forming Disk Galaxy
Authors: Wiphu Rujopakarn, Christina C. Williams, Emanuele Daddi, Malte Schramm, Fengwu Sun, Stacey Alberts, George H. Rieke, Qing-Hua Tan, 清华 谈, Sandro Tacchella, Mauro Giavalisco, John D. Silverman
Figure caption: To search for substructures in UDF2's star-forming regions, we subtract from the ALMA rest-frame 240 μm continuum visibilities a Spergel profile (an approximation of the Sérsic profile with analytical Fourier transform). From left to right is the dirty ALMA image, the residual map with the main dust disk modeled by a single Spergel profile subtracted, and the residual after all components are subtracted, respectively. The top row is the native resolution image, whereas the bottom row is tapered at 1000 m to enhance the sensitivity to extended features. Each cutout is 1″ × 1″; north is up, and east is to the left; contours are [−1.5, 1.5, 1.51.5, 1.52,...] × σ.
Paper: Eccentric Dust Ring in the IRS 48 Transition Disk
Authors: Haifeng Yang, 海峰 杨, Manuel Fernández-López, Zhi-Yun Li, Ian W. Stephens, Leslie W. Looney, Zhe-Yu Daniel Lin, Rachel Harrison
Figure caption: The velocity map of the disk, assuming an elliptical orbit with e = 0.27, as fitted from Section 3.1. The color bar is similar to van der Marel et al. (2021b) with v source = 4.55 km s−1. The solid contours represent the same velocity map as the color map at the levels of (−4, −2.67, −1.33, 0, 1.33, 2.67, 4) km s−1  +  v source. The dashed contours are plotted at the same velocity levels but assumes circular (Keplerian) orbit. A gray 3σ contour of the nonpolarized flux from our observation is also plotted as a background.
Paper: Eccentric Dust Ring in the IRS 48 Transition Disk
Authors: Haifeng Yang, 海峰 杨, Manuel Fernández-López, Zhi-Yun Li, Ian W. Stephens, Leslie W. Looney, Zhe-Yu Daniel Lin, Rachel Harrison
Figure caption: Orbital fits shown in the deprojected plane without using the assumption of the star at one of the foci. We plot 1000 gray ellipses with a reasonable fit. The worst of these orbits has a loss function that is only 1% larger than the best. The foci (near the star) of these ellipses are also plotted as gray crosses. The yellow star at the center marks the primary star location.
Paper: The Luminosity Function of Tidal Disruption Events from Fallback-powered Emission: Implications for the Black Hole Mass Function
Authors: Eric R. Coughlin, Matt Nicholl
Figure caption: The luminosity function as calculated in Equation (6) with the break luminosity equal to 1043.5 erg s−1.
Paper: A New Definition of Exoplanet Habitability: Introducing the Photosynthetic Habitable Zone
Authors: C. Hall, P. C. Stancil, J. P. Terry, C. K. Ellison
Figure caption: The photosynthetic habitable zone. Region where positive net photosynthesis is possible shown in pink, and habitable zone shown in blue. The overlapping region is where photosynthesis can actually occur, and is named “the photosynthetic habitable zone,” since it is possible that oxygenic photosynthesis, and therefore biosignatures, could exist on planets in this location. Overplotted in yellow markers are planets of interest, i.e., planets in the habitable zone expected to have a solid surface (R ≲ 1.8 R E). Blue markers indicate water world candidates. Earth is shown by the white Earth symbol. The tidal lock radius with upper and lower limits is also shown.
Paper: A New Definition of Exoplanet Habitability: Introducing the Photosynthetic Habitable Zone
Authors: C. Hall, P. C. Stancil, J. P. Terry, C. K. Ellison
Figure caption: Mass–period relationship. Day lengths of planets either measured directly (blue points) or estimated through empirically determined relationship in Equation (16) (green and yellow points). Yellow points indicate that mass was also estimated using Equation (17). Gray solid lines are plots of Equation (18) for a plausible range of planet densities. Horizontal dashed lines mark the range of Earth’s day length predicted for the GOE (Klatt et al. 2021).
Paper: A New Definition of Exoplanet Habitability: Introducing the Photosynthetic Habitable Zone
Authors: C. Hall, P. C. Stancil, J. P. Terry, C. K. Ellison
Figure caption: Net photosynthetic rate vs. irradiance intensity. Dotted green line indicates where rate of photosynthetic production of O2 is equal to consumption of O2 during respiration, such that net photosynthetic production of O2 is zero. Rate of respiration is R rate = 20 μmol O2 mg−1 hr−1. Orange vertical line is intensity of PAR at Earth.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: Bayesian inference presented in Section 3.4.2. Shown are the predicted light curves for the two classes of parameters reported in Figure 10 and found using a top-hat model with a fixed observing angle θ obs = 0° and assuming only synchrotron radiation. Observing frequencies or energies are shown on top of each panel, and the fitted observational data are displayed in gray. Blue curves show the model with a low ﹩{\theta }_{\mathrm{core}}﹩ and p ∼ 2. Orange curves show the model with a high ﹩{\theta }_{\mathrm{core}}﹩.
Paper: First Detection of the Powerful Gamma-Ray Burst GRB 221009A by the THEMIS ESA and SST Particle Detectors on 2022 October 9
Authors: O. V. Agapitov, M. Balikhin, A. J. Hull, Y. Hobara, V. Angelopoulos, F. S. Mozer
Figure caption: (a)—the light curve of the combined THB and THC ESA proton flux counts in the energy range from 8 eV to 20 keV. (b)—zoomed-in plot of the two main bursts from (a) with curve shown at 1 s resolution. (c)—the light curve of the combined THB and THC SST proton flux counts in the energy range from 30 keV to 1 MeV. (d)—zoomed-in plot of the two main bursts from (c) with solid curve shown at 1 s resolution.
Paper: First Detection of the Powerful Gamma-Ray Burst GRB 221009A by the THEMIS ESA and SST Particle Detectors on 2022 October 9
Authors: O. V. Agapitov, M. Balikhin, A. J. Hull, Y. Hobara, V. Angelopoulos, F. S. Mozer
Figure caption: The apparent electron and proton fluxes recorded on board THB and THC probes with electrostatic analyzers (ESAs): (a)—the omnidirectional proton flux from the THB ESA detector; (b)—the energy integrated proton flux on the azimuthal angle phi; (c)—the energy integrated proton flux on the polar angle theta; (d)—the omnidirectional electron flux from the THB SST detector; (e)—the integrated proton (red) and electron (blue) fluxes. Panels (f)–(j) present the same characteristics from THC.
Paper: First Detection of the Powerful Gamma-Ray Burst GRB 221009A by the THEMIS ESA and SST Particle Detectors on 2022 October 9
Authors: O. V. Agapitov, M. Balikhin, A. J. Hull, Y. Hobara, V. Angelopoulos, F. S. Mozer
Figure caption: The electron and proton flux recorded by the SST detectors on board the THA and THE probes: (a)—the proton flux from the THA SST detector; (b)—the electron flux from the THA SST detector; (c)—the proton density in the SST energy range. Panels (d)–(f) present the same characteristics recorded on board THC, panels (g)–(i)—on board THB, and panels ((j)–(l))—on board THC.
Paper: First Detection of the Powerful Gamma-Ray Burst GRB 221009A by the THEMIS ESA and SST Particle Detectors on 2022 October 9
Authors: O. V. Agapitov, M. Balikhin, A. J. Hull, Y. Hobara, V. Angelopoulos, F. S. Mozer
Figure caption: (a)—the light curve of composite THB and THC ESA proton flux counts showing the fine structure of the two main bursts of GRB 221009A. (b)—wavelet decomposition of the light curve (b). The dashed line indicates the spacecraft spin frequency. (c)—time-averaged wavelet spectra collected during the interval indicated by the corresponding color in panel (a).
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: Top panel: 60 s exposure I C of GRB 221009A taken on the 0.61 m Dall–Kirkham458 telescope of the Burke–Gaffney Observatory ∼0.5 day after the Fermi GBM trigger time. Bottom panel: corresponding difference image using a PS1 template image downloaded from the CDS HIPS2FITS service. The optical afterglow is well detected in the residual image and cleaned of any nearby star contribution. The aperture radii (the flux aperture in green and the background flux annulus in red) used to compute the photometric measurement are also shown in both images.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: Unabsorbed X-ray light curve of GRB 221009A detected by the Swift/XRT (given at 10 keV in blue and 1 keV in red) and HXMT/LE (orange) instruments. The light curves were corrected for Galactic and intrinsic NH I column density absorption estimated from the late-time Swift/XRT spectrum analysis (https://www.swift.ac.uk/xrt_spectra/01126853/). In dark blue and red, we show the synthetic Swift/XRT light curve that we finally used in our afterglow modeling analysis; see Sections 3.4.2 and 3.4.1.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: Bayesian inference presented in Section 3.4.2. Shown is a marginalized posterior distribution of the free parameters best fitting the extended data with an on-axis observation of a top-hat jet radiating via synchrotron only, as presented in Section 3.4.2. In blue, we show marginalized distributions for the model that features a low ﹩{\theta }_{\mathrm{core}}﹩ and p ∼ 2, not found with NMMA. In orange, we show marginalized distributions for the model with a high ﹩{\theta }_{\mathrm{core}}﹩, similar to what is found with NMMA. The median values and 90% confidence intervals can be found in Table 4.
Paper: First Detection of the Powerful Gamma-Ray Burst GRB 221009A by the THEMIS ESA and SST Particle Detectors on 2022 October 9
Authors: O. V. Agapitov, M. Balikhin, A. J. Hull, Y. Hobara, V. Angelopoulos, F. S. Mozer
Figure caption: The configuration of THEMIS and ARTEMIS spacecraft during the GRB 211211A event is shown in panel (a) with the traces during the interval of 1200-1400 UT shown in the ecliptic plane. The modeled locations of Earth’s magnetopause and bow shock are indicated by the dashed and dotted curves respectively. (b)—the inner THEMIS spacecraft configuration. (c)—the ARTEMIS spacecraft THB and THC in the selenocentric system (the ecliptic plane projection).
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: The NMMA observational data (Extended data) and best-fit light curves of selected filters for the NMMA analysis using the SF11 extinction and the four employed jet structures. The X-ray bands are shown in microjanskys, and the rest of the bands are shown in AB magnitude. In the optical band, the GRANDMA data points are shown in orange.
Paper: GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann
Authors: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao
Figure caption: The NMMA posterior distribution (90% confidence intervals) for our selected data sets when using different jet models of afterglowpy analyzing the Extended data.