adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Observations of the Pleiades Cluster: A Nursery for δ Scuti Stars
Authors: Timothy R. Bedding, Simon J. Murphy, Courtney Crawford, Daniel R. Hey, Daniel Huber, Hans Kjeldsen, Yaguang Li, 亚光 李, Andrew W. Mann, Guillermo Torres, Timothy R. White, George Zhou
Figure caption: H–R diagram of the Pleiades, corrected for extinction and reddening, showing the location of the δ Scuti pulsators. Sloping lines indicate both the theoretical instability strip (solid blue lines; Dupret et al. 2005) and the observed strip from Kepler (dashed purple lines show the region in which at least 20% of Kepler stars pulsate; Murphy et al. 2019).
Paper: TESS Observations of the Pleiades Cluster: A Nursery for δ Scuti Stars
Authors: Timothy R. Bedding, Simon J. Murphy, Courtney Crawford, Daniel R. Hey, Daniel Huber, Hans Kjeldsen, Yaguang Li, 亚光 李, Andrew W. Mann, Guillermo Torres, Timothy R. White, George Zhou
Figure caption: The effect of reddening on the pulsation instability strip. The Kepler samples of δ Scuti stars (from Murphy et al. 2019) and γ Doradus stars (Li et al. 2020) are restricted to Galactic latitude b > 10°.
Paper: The Collimation of Relativistic Jets in Post–Neutron Star Binary Merger Simulations
Authors: Matteo Pais, Tsvi Piran, Yuri Lyubarsky, Kenta Kiuchi, Masaru Shibata
Figure caption: Escape energy, E j,esc, (blue lines) and collimation energy, E j,coll, (red and green lines) vs. θ for three different snapshots at: t = t 1 = 0.33 s (left), t = 2t 1 = 0.667 s (center), and t = 3t 1 = 1 s (right). The red (and green lines) are drawn varying the luminosity of the collimation contour and calculating, from the contour fit, the corresponding opening angle θ measured at z  s  = 1670 km (left), z  s  = 3300 km (center), and z  s  = 5000 km (right), which approximately represent the maximal heights of the low-density, low-pressure cavity at each snapshot, respectively. The jet energy is calculated from the luminosity assuming a jet engine working time of 1 s (red solid line) or 0.1 s (red dotted line). The red-shaded region represents the uncertainty on the estimate taking different values of the height at which the slope is measured. The blue lines indicate the energy required for a magnetic (solid) and hydrodynamic (dashed) jets to overrun the expanding ejecta and escape the external vacuum as expressed by Equation (1). Collimated jets that break out should be on red (green) lines and above the blue lines.
Paper: The Collimation of Relativistic Jets in Post–Neutron Star Binary Merger Simulations
Authors: Matteo Pais, Tsvi Piran, Yuri Lyubarsky, Kenta Kiuchi, Masaru Shibata
Figure caption: Left: density map in a logarithmic scale of a 2D slice (x–z plane) through the center of the simulation box at t = 1 s. We superposed the velocity streamlines (white color). Right: the jet parameter ﹩\tilde{L}﹩ calculated for the 2D slice of the ambient density for a jet luminosity of 1050 erg s−1. Note the almost empty cone along the axis.
Paper: The Collimation of Relativistic Jets in Post–Neutron Star Binary Merger Simulations
Authors: Matteo Pais, Tsvi Piran, Yuri Lyubarsky, Kenta Kiuchi, Masaru Shibata
Figure caption: Left: map of the thermal pressure superposed onto the collimation contours that satisfy Equation (13). The bottom color bar shows the values of the ambient pressure while the different colors of the contour lines represent different jet luminosities (vertical color bar in a log scale). We fixed the light cylinder radius at R L = 40 km. We chose a different scale ratio for the x- and z-axes to stretch the central underdense polar region of the jet where the contours crowd. Right: same as the left panel but superposed onto a power-law fit z = ax  b . The horizontal color bar at the bottom of the figure represents the local slope of the curve fit (in degrees). The curves with L j = 1049 erg s−1 and 1050 erg s−1 show an outer slope between 4° and 7°. Note that the horizontal axis covers x ∈ [ − 1500, 1500] km while the vertical axis covers z ∈ [ − 4500, 4500] km to better distinguish the curves closer to the central axis.
Paper: The Collimation of Relativistic Jets in Post–Neutron Star Binary Merger Simulations
Authors: Matteo Pais, Tsvi Piran, Yuri Lyubarsky, Kenta Kiuchi, Masaru Shibata
Figure caption: Evolution of the angle θ as a function of the time t and the collimation energy E j,coll (in units of erg) for t e = 1 s. The gray area at the left of the plot represents the premerger and early postmerger phase of the system, where the calculation of the collimation contour is still very noisy. The fainter area on the top of the map represents the region where the contour is no more calculated assuming γ = R/R L but using the curvature of the jet magnetic surface. The black curves represent the contour lines for fixed values of θ, from 1° to 10°. The color scale on the right indicates the value of θ in degrees.
Paper: The Collimation of Relativistic Jets in Post–Neutron Star Binary Merger Simulations
Authors: Matteo Pais, Tsvi Piran, Yuri Lyubarsky, Kenta Kiuchi, Masaru Shibata
Figure caption: The Lorentz factor as a function of the height, z, for different jet luminosities. The jet luminosity values are the same as shown in Figure 2.
Paper: Imbalanced Turbulence Modified by Large-scale Velocity Shears in the Solar Wind
Authors: Juska E. Soljento, Simon W. Good, Adnane Osmane, Emilia K. J. Kilpua
Figure caption: 2D distributions of ﹩{\sigma }_{{\rm{c}}}^{* }﹩ (top row) and ﹩{r}_{{\rm{E}}}^{* }﹩ (bottom row) against ∣Δv∣/v A in the upstream solar wind, the sheath, and the ejecta, binned across all 74 events, with adjoining 1D histograms of ∣Δv∣/v A (top panels), and ﹩{\sigma }_{{\rm{c}}}^{* }﹩ and ﹩{r}_{{\rm{E}}}^{* }﹩ (right-hand panels). The 2D histograms have been normalized to the maximum bin count. The black lines indicate mean ﹩{\sigma }_{{\rm{c}}}^{* }﹩ or ﹩{r}_{{\rm{E}}}^{* }﹩ within the vertical ∣Δv∣/v A bins (calculated as an arithmetic mean). In the bottom row panels the red lines indicate mean ﹩{r}_{{\rm{E}}}^{* }﹩, but calculated as a geometric mean. The shaded error regions have been calculated as a standard error of the mean.
Paper: Imbalanced Turbulence Modified by Large-scale Velocity Shears in the Solar Wind
Authors: Juska E. Soljento, Simon W. Good, Adnane Osmane, Emilia K. J. Kilpua
Figure caption: Distributions of key turbulence parameters upstream of the shock (purple), inside the sheath (blue), and in the ICME ejecta (green), summed across all 74 events. The residual energy, σ r, and Alfvén ratio, r A, are on the top row, the rectified cross helicity, ﹩{\sigma }_{{\rm{c}}}^{* }﹩, and Elsasser ratio, ﹩{r}_{{\rm{E}}}^{* }﹩, in the middle row, and the rectified PSDs, ﹩{E}_{\pm }^{* }﹩, of  z  ± are on the bottom row.
Paper: Imbalanced Turbulence Modified by Large-scale Velocity Shears in the Solar Wind
Authors: Juska E. Soljento, Simon W. Good, Adnane Osmane, Emilia K. J. Kilpua
Figure caption: An example ICME. From top to bottom, the panels show the following: the magnetic field components in GSE coordinates and the magnetic field magnitude; proton velocity components in GSE coordinates; normalized residual energy; normalized cross helicity; the Alfvén ratio and the Elsasser ratio; the magnetic field longitude angle in GSE coordinates; the magnitude of the difference in the nonradial velocity components normalized by the local Alfvén speed; and magnetic compressibility along with a 10 minute running average (black curve) to show its overall evolution. In the longitude panel the horizontal dashed lines denote the boundaries between the sunward and antisunward sectors of the interplanetary magnetic field. The dashed vertical lines across all panels denote the shock and the ICME leading edge, respectively.
Paper: Extremely Relativistic Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran
Figure caption: Illustration of the evolution and shape of debris in an extremely relativistic event with r p ∼ 4.02r g (upper panels) and an ordinary TDE with r p ∼ 110r g (lower panels). Four phases are shown for each. For the eTDE: crescent (note that the star has already been fully disrupted at this stage and a significant fraction of its mass has been captured); spiral; ring; and ring with inflow. For evolution of an ordinary TDE: beginning of the disruption; highly stretched star; and two stages of the stream’s return to the vicinity of the SMBH. In all cases, the color scale represents the logarithmic density in the orbital plane. Insets show the matter near the SMBH.
Paper: Extremely Relativistic Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran
Figure caption: (Upper panel) The orbital energy distribution of the debris from a 1M ⊙ star disrupted after following an orbit with r p ≃ 4.03r g around an SMBH with M BH = 106 M ⊙. Energy is in units of Δϵ. The black dashed line shows the energy distribution in the gas remaining immediately after half the stellar mass plunges directly into the SMBH; the four colored curves show its evolution at later times. Here, E = −(1 + u t) and ﹩{\rm{\Delta }}\epsilon ={{GM}}_{\mathrm{BH}}{R}_{\star }/{r}_{{\rm{t}}}^{2}﹩ where ﹩{r}_{{\rm{t}}}={({M}_{\mathrm{BH}}/{M}_{\star })}^{1/3}{R}_{\star }﹩. The time (in seconds) is measured since the initial pericenter passage. (Bottom panel) The thick black curve shows the mass fallback rate predicted from the energy distribution as of t = 40,000 s. The thin gray lines indicate the Eddington accretion rate assuming radiation efficiencies of η = 0.01 or 0.1.
Paper: Extremely Relativistic Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran
Figure caption: (Top) Regions in parameter space for five kinds of disruption events: partial TDE (orange), common full TDE (blue), circularized TDE (red), and direct capture (gray, r p < 4g). We define partial TDEs as events where the star loses more than 10% of its mass at the first pericenter passage. This plot is an extended version of Figure 3 in Krolik et al. (2020). (Bottom) The cross section as a function of M BH for each class of observable full disruption events, i.e., common (dashed black), circularized (dotted black), extreme (solid red), in units of the total disruption cross section for a 1 M ⊙ main-sequence star.
Paper: Extremely Relativistic Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran
Figure caption: The solid white curve depicts the geodesic of an orbit with r p ≃ 4.03r g around an SMBH (red disk at the center); the arrow indicates the direction of the orbit. The color scale shows the density distribution of stellar debris 241 s before a star whose center of mass follows this geodesic passes through pericenter.
Paper: Extremely Relativistic Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran
Figure caption: The distribution of the density (top) and the ratio of the cooling time to the evolution time (bottom) in the r−z plane at ϕ = 0 at t ≃ 10,000, 20,000, 30,000, 40,000 s. The location of the thermalization photosphere as seen by a distant observer is plotted using a white line. We define the thermalization optical depth as ﹩\sqrt{{\tau }_{{\rm{t}}}{\tau }_{\mathrm{ff}}}﹩, for τ T (τ ff) the Thomson (absorption) optical depths integrated radially inwards from the outer boundary. The prominent break in structure roughly halfway out in the debris corresponds to the density peak of the expanding ring.
Paper: Extremely Relativistic Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran
Figure caption: The luminosity estimated using Equation (B2) as a function of time (left) and the distribution of the temperature dL/dT at a few different times (right). The horizontal dashed line in the left panel indicates the Eddington limit for M BH = 106 M ⊙.
Paper: The IXPE View of GRB 221009A
Authors: Michela Negro, Niccolò Di Lalla, Nicola Omodei, Péter Veres, Stefano Silvestri, Alberto Manfreda, Eric Burns, Luca Baldini, Enrico Costa, Steven R. Ehlert, Jamie A. Kennea, Ioannis Liodakis, Herman L. Marshall, Sandro Mereghetti, Riccardo Middei, Fabio Muleri, Stephen L. O'Dell, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Masanobu Terashima, Andrea Tiengo, Domenico Viscolo, Alessandro Di Marco, Fabio La Monaca, Luca Latronico, Giorgio Matt, Matteo Perri, Simonetta Puccetti, Juri Poutanen, Ajay Ratheesh, Daniele Rogantini, Patrick Slane, Paolo Soffitta, Elina Lindfors, Kari Nilsson, Anni Kasikov, Alan P. Marscher, Fabrizio Tavecchio, Nicoló Cibrario, Shuichi Gunji, Christian Malacaria, Alessandro Paggi, Yi-Jung Yang, Silvia Zane, Martin C. Weisskopf, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovc̆iak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Simone Maldera, Frédéric Marin, Andrea Marinucci, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption: Polarization PCUBE analysis results for  r  1 (top row) and  r  2 (middle row), for one energy bin 2–8 keV (left column) and two logarithmic energy bins 2–4 and 4–8 keV (right column). Table 4 provides the values and 1σ errors on the PD and PA for the energy-resolved PCUBE analysis. Note that the PCUBE analysis of the rings’ emission is performed without a proper background subtraction (we refer to the caption of Table 4 for further discussion on the caveats of this point). The PAs of the two rings seem to be significantly different, however: as mentioned in the main text, the uncertainties are underestimated. Polarization measurements with significance below the 99% C.L. are not considered as a detection, and the PAs are to be considered unconstrained. Furthermore, under the assumption that the two rings originate from the same prompt emission, there is no (known) reason to expect the polarization of the two rings to be intrinsically rotated. This fact is symptomatic of fluctuations due to the low photon statistics of the signal, and further justifies our approach of combining the two rings for a more accurate spectropolarimetric analysis.
Paper: The IXPE View of GRB 221009A
Authors: Michela Negro, Niccolò Di Lalla, Nicola Omodei, Péter Veres, Stefano Silvestri, Alberto Manfreda, Eric Burns, Luca Baldini, Enrico Costa, Steven R. Ehlert, Jamie A. Kennea, Ioannis Liodakis, Herman L. Marshall, Sandro Mereghetti, Riccardo Middei, Fabio Muleri, Stephen L. O'Dell, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Masanobu Terashima, Andrea Tiengo, Domenico Viscolo, Alessandro Di Marco, Fabio La Monaca, Luca Latronico, Giorgio Matt, Matteo Perri, Simonetta Puccetti, Juri Poutanen, Ajay Ratheesh, Daniele Rogantini, Patrick Slane, Paolo Soffitta, Elina Lindfors, Kari Nilsson, Anni Kasikov, Alan P. Marscher, Fabrizio Tavecchio, Nicoló Cibrario, Shuichi Gunji, Christian Malacaria, Alessandro Paggi, Yi-Jung Yang, Silvia Zane, Martin C. Weisskopf, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovc̆iak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Simone Maldera, Frédéric Marin, Andrea Marinucci, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption:  Q/I vs. U/I plots resulting from the spectropolarimetric analysis for the combined analysis of  r  1 +  r  2 (top row) and for  r  1 and  r  2 individual analyses (middle and bottom row, respectively), shown for completeness. The three columns refer to different background assumptions: BKG1 (extracted from IXPE observations of 1ES 1959+65) on the left column, BKG2 (from BL Lacertae observation) on the central column, and BKG3 (from 3C 279 observation) on the right column. This shows that the result of the combined analysis is mostly driven by  r  1, while  r  2 seems more unpolarized. However, within the 50% contours,  r  1 and  r  2 are compatible.
Paper: The IXPE View of GRB 221009A
Authors: Michela Negro, Niccolò Di Lalla, Nicola Omodei, Péter Veres, Stefano Silvestri, Alberto Manfreda, Eric Burns, Luca Baldini, Enrico Costa, Steven R. Ehlert, Jamie A. Kennea, Ioannis Liodakis, Herman L. Marshall, Sandro Mereghetti, Riccardo Middei, Fabio Muleri, Stephen L. O'Dell, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Masanobu Terashima, Andrea Tiengo, Domenico Viscolo, Alessandro Di Marco, Fabio La Monaca, Luca Latronico, Giorgio Matt, Matteo Perri, Simonetta Puccetti, Juri Poutanen, Ajay Ratheesh, Daniele Rogantini, Patrick Slane, Paolo Soffitta, Elina Lindfors, Kari Nilsson, Anni Kasikov, Alan P. Marscher, Fabrizio Tavecchio, Nicoló Cibrario, Shuichi Gunji, Christian Malacaria, Alessandro Paggi, Yi-Jung Yang, Silvia Zane, Martin C. Weisskopf, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovc̆iak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Simone Maldera, Frédéric Marin, Andrea Marinucci, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption: Corner plots resulting from the Bayesian spectropolarimetric fit performed with 3ML of the core region (top) and the combined fit of  r  1 and  r  2 (bottom). This shows how the Bayesian approach yields results consistent with the frequentist approach adopted in this work. It also shows the nice convergence of the fit for all the parameters of interest. In both plots, we show the case of BKG2 assumed as background model for the background subtraction (the cases of BKG1 and BKG3 yield analogous results).
Paper: The IXPE View of GRB 221009A
Authors: Michela Negro, Niccolò Di Lalla, Nicola Omodei, Péter Veres, Stefano Silvestri, Alberto Manfreda, Eric Burns, Luca Baldini, Enrico Costa, Steven R. Ehlert, Jamie A. Kennea, Ioannis Liodakis, Herman L. Marshall, Sandro Mereghetti, Riccardo Middei, Fabio Muleri, Stephen L. O'Dell, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Masanobu Terashima, Andrea Tiengo, Domenico Viscolo, Alessandro Di Marco, Fabio La Monaca, Luca Latronico, Giorgio Matt, Matteo Perri, Simonetta Puccetti, Juri Poutanen, Ajay Ratheesh, Daniele Rogantini, Patrick Slane, Paolo Soffitta, Elina Lindfors, Kari Nilsson, Anni Kasikov, Alan P. Marscher, Fabrizio Tavecchio, Nicoló Cibrario, Shuichi Gunji, Christian Malacaria, Alessandro Paggi, Yi-Jung Yang, Silvia Zane, Martin C. Weisskopf, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovc̆iak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Simone Maldera, Frédéric Marin, Andrea Marinucci, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Brian D. Ramsey, John Rankin, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption: Time evolution of the dust-scattering halos. The counts maps are generated in three time bins combining the data of the 3 DUs. The core region has been removed to better show the rings. The images have been smoothed with a Gaussian beam for visualization purposes. To guide the eye, we added a thin circle in the first and last images of the sequence to mark the minimum of the counts gap between the two evolving rings.