adsabs/AstroCLIMB huggingface dataset:
Paper: Preperihelion Development of Interstellar Comet 3I/ATLAS
Authors: David Jewitt, Jane Luu
Figure caption: Heliocentric indices computed from equilibrium sublimation models for CO, CO2, and H2O ices as a function of heliocentric distance. Hemispherical sublimation is assumed, and the ices are taken to be perfectly absorbing and emissive. The measured index for 3I/ATLAS is shown. The vertical error on the 3I point denotes the ±0.3 uncertainty on the heliocentric index and shows consistency with free sublimation of CO and CO2 but not H2O. The horizontal bar marks the range of distances over which 3I was reliably observed (see Table 1).
Paper: Preperihelion Development of Interstellar Comet 3I/ATLAS
Authors: David Jewitt, Jane Luu
Figure caption: The heliocentric brightness indices of 2I and 3I, n = 1.9 ± 0.1 and 3.8 ± 0.3, respectively, compared with histograms of the same quantity for comets in three dynamical groups. Dynamically new (solid blue line), intermediate (orange dashed–dotted line), and old (red dashed line) are shown. The formal uncertainties on the indices for 2I and 3I are shown as shaded regions. Comet data are from P. Lacerda et al. (2025).
Paper: Preperihelion Development of Interstellar Comet 3I/ATLAS
Authors: David Jewitt, Jane Luu
Figure caption: The normalized surface brightness as a function of angular distance (positive toward the east) from the nucleus measured in a 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 wide strip along the projected antisolar direction. On August 7 (blue line) the profile is asymmetric with an extension toward the Sun, best seen in the inner few arcseconds. By September 26 (red line) the sense of the asymmetry has reversed, and the antisolar tail is dominant.
Paper: Preperihelion Development of Interstellar Comet 3I/ATLAS
Authors: David Jewitt, Jane Luu
Figure caption: Reduced photometry from NOT, assuming βR = 0.04 mag degree−1, as a function of heliocentric distance. The straight line is a least-squares fit of slope n = 3.8.
Paper: Preperihelion Development of Interstellar Comet 3I/ATLAS
Authors: David Jewitt, Jane Luu
Figure caption: Composite preperihelion lightcurves of 2I/Borisov and 3I/ATLAS compared, with error bars omitted for clarity. The best-fit heliocentric indices are marked for each object.
Paper: Preperihelion Development of Interstellar Comet 3I/ATLAS
Authors: David Jewitt, Jane Luu
Figure caption: Yellow filled circles show measurements of the position angles of asymmetries as a function of date, the latter being expressed as day of year in 2025. In the lower part of the plot the solid red and blue lines marked “–V” and “–S” show, respectively, the projected antivelocity vector and antisolar directions. The dashed red and blue lines in the upper part of the plot marked +V and +S are 180° from their solid counterparts. Note that the vertical axis is broken between 110° and 270° for clarity of presentation.
Paper: Preperihelion Development of Interstellar Comet 3I/ATLAS
Authors: David Jewitt, Jane Luu
Figure caption: Normalized surface brightness profile of the antisolar tail on UT 2025 September 26, with error bars computed from the standard deviation of nearby sky brightness measurements. Lines of logarithmic slope −1, −3/2, and −2 are marked for reference.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Left: X-ray lightcurve of GRB 250702B combining Swift and Chandra in the 0.3–10 keV energy range. The start time T0 is the GBM “D” burst. The red lines show the best-fit decay from the initial trigger time of GRB 250702D (Table 4). The dashed red line (t−1.9) includes the first XRT orbit in the fit, whereas the solid red line excludes the first XRT orbit and provides a better fit to the late-time data (t−1.8). The observation windows of our NuSTAR data are shown as the orange shaded regions. For reference, we show the expected slopes for a relativistic TDE, corresponding to both complete (t−5/3) and partial (t−9/4) disruption. The bottom panel shows the 0.3–10 keV lightcurve fit residuals relative to the solid red line. Right: histogram showing the posterior probability density of the best-fit T0 time for the X-ray afterglow emission. The gray histogram shows the T0 posterior obtained when fitting all XRT data, and the red histogram shows the T0 posterior when excluding the first XRT orbit. The trigger times reported by Fermi (red) and EP (blue) are shown as vertical lines (Table 4). The July 1 window in which EP reports an initial detection is to the left of the vertical blue line. We also show as vertical black lines the times of the Swift/BAT gamma-ray detections. All times are relative to the trigger of GRB 250702D at MJD 60858.548.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Left: Swift/BAT Survey mode (14–195 keV) emission from GRB 250702B from the start of 2025 July 1 to the end of 2025 July 4. The black points show the Swift/BAT detections (14–195 keV; Tables 2 and 3) from both the GUANO and survey data. The gray downward triangles represent the 5σ upper limits from Swift/BAT in the 14–195 keV energy range. The trigger times reported by Fermi (red) and EP (blue) are shown as vertical lines (Table 4). The 2025 July 1 window in which EP reported an initial detection is shown as the blue shaded region. The time window of our initial NuSTAR observation (starting 1.3 days after the initial Fermi trigger) is shown as the orange shaded region. Right: best-fit temporal power law to the NuSTAR lightcurve in 3–79 keV. The 1σ error on the fit is shown as the shaded orange region. The Swift/BAT upper limits are shown as the gray triangles and the detections as black circles. The start time T0 is taken as the trigger time of GRB 250702D. The vertical red lines show the Fermi trigger times of GRBs 250702B, 250702C, and 250702E (see Table 4).
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Left: FS and RS afterglow models fit to multiwavelength observations. The start time T0 is the GBM “E” burst. The Markov Chain Monte Carlo parameter posterior distributions are shown in Figure 20, which only considers the last five X-ray detections for the X-ray lightcurve. The lightcurves are obtained for the following model parameters that keep the X-ray afterglow emission below the flaring X-ray emission at early times: θj = 7.8 × 10−3 rad, Ek,iso = 6.2 × 1054 erg, Γ0 = 306, n0 = 0.6 at R0 = 1018 cm, p = 2.1, and ϵe = 0.2, ϵB = 10−3, k = 2. The same dynamical parameters are used for the RS emission with these shock microphysical parameters: pRS = 2.2, εe,RS = 0.1, εB,RS = 10−3, tgrb = 103 s, and gRS = 2.0. The start time T0 is taken as GRB 250702E (Table 4). Right: model spectra comparisons with observations at two different times, with the RS spectra shown with dashed lines.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: The 3–79 keV NuSTAR lightcurve (FPMA+FPMB) in 300 s bins (purple). The lightcurve is not background-subtracted, but the background lightcurve (gray) is also shown for comparison. The dashed black line shows the mean count rate. The Bayesian Blocks results are shown as the larger black circles. The bottom panel shows the residuals with respect to the mean count rate, to underscore the source’s short-timescale variability.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: K-corrected rest-frame (0.3–10 keV) X-ray lightcurves of Swift long-duration GRBs, ultralong GRBs (GRBs 111209A, 121027A, and 130925A; P. A. Evans et al. 2014a; A. J. Levan et al. 2014), and relativistic jetted TDEs (J. S. Bloom et al. 2011; S. B. Cenko et al. 2012; G. C. Brown et al. 2015; D. R. Pasham et al. 2023) compared to GRB 250702B for a few different T0. For the 2025 July 2 start time (purple), we have used the trigger time of GRB 250702D as T0 (Table 4). For the 2025 July 1 start time (blue), we use the beginning of the first EP detection window (H. Sun 2025, private communication).
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Rest-frame X-ray luminosity (0.3–10 keV) at 11 hr (in the rest frame) from discovery versus gamma-ray energy (1–10,000 keV). GRB 250702B is shown by a red star. We measure 11 hr from the start of the “D” burst (discovery trigger). We show Sw J1644+57 as a shaded region (see the text for details; D. N. Burrows et al. 2011). A sample of short (black squares) and long (gray circles) GRBs are compiled from M. Nysewander et al. (2009) and E. Berger (2014). We show GRB 221009A as a purple square (E. Burns et al. 2023; B. O’Connor et al. 2023; S. Lesage et al. 2023). A sample of ultralong GRBs is shown for comparison (GRBs 101225A, 111209A, 121027A, and 130925A; P. A. Evans et al. 2014a; A. J. Levan et al. 2014). The long-GRB correlation of LX,11 ≈ ﹩5.6\times 1{0}^{44}{({E}_{\gamma ,{\rm{iso}}}/1{0}^{51}\,{\rm{erg}})}^{0.72}﹩ erg s−1 is shown by the black dashed line (E. Berger 2014). Reproduced from B. O’Connor et al. (2025b).
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Left: X-ray lightcurve comparing NuSTAR (FPMA+FPMB) data to the XRT lightcurve and best-fit temporal power law as shown in Figure 1. The start time T0 is the GBM “D” burst. The solid red line is the best fit (t−1.7) when including only XRT at >2.5 days, and the red dashed line is the best fit (t−1.9) when including all XRT data. The NuSTAR data are in 150 s bins and the XRT data are in 100 s bins. The XRT count rate and power-law fit are rescaled to their expected NuSTAR 3–79 keV count rate. We emphasize that this scale factor is not arbitrary and is computed directly based on the best-fit spectral shape (Section 3.2). Right: the same as the left panel but zoomed in on the NuSTAR data in linear space. Note that the temporal axis is in units of kiloseconds in this panel.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Intrinsic ratio of hydrogen column density to visual extinction versus visual extinction inferred from long-GRB (black circles) afterglows (P. Schady et al. 2010; J. Greiner et al. 2011; T. Krühler et al. 2011b; D. A. Perley et al. 2011; T. Zafar et al. 2011). Sources with either upper limits on the column density (white) or upper limits on the extinction (gray) are shown as pentagons. GRB 250702B is shown as a red star, based on our near-infrared-to-X-ray modeling. A more conservative range of the allowed values (even breaking the assumption that both X-ray and near-infrared data originate from the external shock) is shown as a shaded red region. The ultralong GRBs 111209A (G. Stratta et al. 2013) and GRB 130925A (J. Greiner et al. 2014) are also shown. We display as a shaded region the range for the relativistic TDE Sw J1644 (J. S. Bloom et al. 2011; D. N. Burrows et al. 2011; A. J. Levan et al. 2011, 2016) and as a triangle that for AT2022cmc (based on an upper limit on reddening; see Y. Yao et al. 2024). The dashed and dotted lines refer to the median values for the Milky Way (T. Güver & F. Özel 2009) and SMC (P. Bouchet et al. 1985), respectively. This figure is reproduced from T. Krühler et al. (2011b).
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Observed X-ray-to-near-infrared SED with Swift/XRT (black), NuSTAR FPMA (blue) and FPMB (red), VLT HAWK-I (HK bands; purple; A. J. Levan et al. 2025b), and optical upper limits (riJ bands; orange; J. Carney et al. 2025). The middle panel displays the fit residuals for an absorbed power-law model, and the bottom panel shows the fit residuals for an absorbed broken power law.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: A zoom-in on the early Swift/XRT lightcurve using 25 s bins. The start time T0 is the GBM “D” burst. The red lines are the same as in the temporal fit shown in Figure 1 (left). The HR between 2–10 and 0.3–2 keV is shown in the bottom panel. The dashed black line shows the mean HR of the full lightcurve.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Joint spectral fit including Swift/XRT (black) and NuSTAR FPMA (blue) and FPMB (red) in the 0.3–30 keV energy range. The middle panel displays the fit residuals for an absorbed power-law model, and the bottom panel shows the fit residuals for an absorbed broken power law. The data have been rebinned within XSPEC for visualization purposes.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: GRB 250702B’s 3–30 keV average power density spectrum from NuSTAR FPMA+FPMB data. The black step line shows the mean Leahy-normalized power spectrum, the gray shading indicates 1σ uncertainties, and the dashed line marks the expected Poisson noise level of 2. The inset shows the number of contributing values per frequency bin on log–log axes.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Corner plot showing the posterior parameter distributions of our FS afterglow modeling, as detailed in Section 3.3. We have used the GBM “E” burst as T0. The condition Γ0θj ≥ 1 is enforced, to prevent the jet from spreading laterally in the coasting phase.
Paper: Observed Joy’s Law of Bipolar Magnetic Region Tilts at Emergence Supports the Thin Flux Tube Model
Authors: Anu Sreedevi, Bidya Binay Karak, Bibhuti Kumar Jha, Rambahadur Gupta, Dipankar Banerjee
Figure caption: Timeline of the BMR evolution, illustrating two tracking phases: the backtracking and forward tracking. The backtracking phase traces BMRs from T0 (AutoTAB’s first detection) to the very initial emergence Te. Forward tracking follows a BMR’s growth from T0 through Tm, when the unsigned flux reaches its peak, to the end of tracking Tf (Te < T0 < Tm < Tf).
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: The same as Figure 16 but for multiple NuSTAR observations of GRB afterglows (see Appendix D for details).
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: HRs (background-subtracted) computed between 10–20 and 3–6 keV in 500 s bins for both FPMA and FPMB. The weighted mean HRs for both FPMs are shown as horizontal lines. The bottom panel shows the residuals from the weighted mean HR.
Paper: Comprehensive X-Ray Observations of the Exceptional Ultralong X-Ray and Gamma-Ray Transient GRB 250702B with Swift, NuSTAR, and Chandra: Insights from the X-Ray Afterglow Properties
Authors: Brendan O'Connor, Ramandeep Gill, James DeLaunay, Jeremy Hare, Dheeraj Pasham, Eric R. Coughlin, Ananya Bandopadhyay, Akash Anumarlapudi, Paz Beniamini, Jonathan Granot, Igor Andreoni, Jonathan Carney, Michael J. Moss, Ersin Göğüş, Jamie A. Kennea, Malte Busmann, Simone Dichiara, James Freeburn, Daniel Gruen, Xander J. Hall, Antonella Palmese, Tyler Parsotan, Samuele Ronchini, Aaron Tohuvavohu, Maia A. Williams
Figure caption: Left: Swift/XRT HR computed between 2–10 and 0.3–2 keV. The mean HR is shown as a horizontal line. The bottom panel shows the residuals from the mean HR. We also show the HR on a per-observation (red) and a per-snapshot (blue) basis for the first few days before multiple observations must be combined to achieve a detection. Right: hard (2–10 keV) versus soft (0.3–2 keV) count rates for the Swift/XRT lightcurve. The dashed line shows the expectation for a one-to-one HR. In both panels, the data are binned to a minimum of 20 counts per bin.