adsabs/AstroCLIMB huggingface dataset:
Paper: X-Ray Quasi-periodic Eruptions and Tidal Disruption Events Prefer Similar Host Galaxies
Authors: T. Wevers, K. D. French, A. I. Zabludoff, T. C. Fischer, K. Rowlands, M. Guolo, B. Dalla Barba, R. Arcodia, M. Berton, F. Bian, I. Linial, G. Miniutti, D. R. Pasham
Figure caption: Stellar velocity dispersion maps of GSN 069 (left), RX J1301 (middle), and eRO-QPE2 (right).
Paper: X-Ray Quasi-periodic Eruptions and Tidal Disruption Events Prefer Similar Host Galaxies
Authors: T. Wevers, K. D. French, A. I. Zabludoff, T. C. Fischer, K. Rowlands, M. Guolo, B. Dalla Barba, R. Arcodia, M. Berton, F. Bian, I. Linial, G. Miniutti, D. R. Pasham
Figure caption: BPT and WHAN diagrams for the source eRO-QPE3.
Paper: X-Ray Quasi-periodic Eruptions and Tidal Disruption Events Prefer Similar Host Galaxies
Authors: T. Wevers, K. D. French, A. I. Zabludoff, T. C. Fischer, K. Rowlands, M. Guolo, B. Dalla Barba, R. Arcodia, M. Berton, F. Bian, I. Linial, G. Miniutti, D. R. Pasham
Figure caption: Bagpipe fits and inferred SFH, assuming a double starburst as detailed in the text. From top to bottom: GSN 069, RX J1301, eRO-QPE1, eRO-QPE2, and eRO-QPE3.
Paper: Probing Velocity Dispersion Inside Coronal Mass Ejections: New Insights on Their Initiation
Authors: Satabdwa Majumdar, Elke D'Huys, Marilena Mierla, Nitin Vashishtha, Dana-Camelia Talpeanu, Dipankar Banerjee, Martin A. Reiss
Figure caption: (a) Height–time plot of the LE and core in blue and brown data points for the CME on 2014 November 5 as tracked in the K-Cor FOV and in black data points for the eruption front as tracked in the SWAP FOV. (b) Plot of the difference in height of the LE and core for the same CME in the K-Cor FOV and LASCO FOV (in blue) and the difference in height of the SWAP front and K-Cor core (in black). The corresponding height of the LE is plotted on the top axis.
Paper: Probing Velocity Dispersion Inside Coronal Mass Ejections: New Insights on Their Initiation
Authors: Satabdwa Majumdar, Elke D'Huys, Marilena Mierla, Nitin Vashishtha, Dana-Camelia Talpeanu, Dipankar Banerjee, Martin A. Reiss
Figure caption: A view of the eruption front for the CME that occurred on 2014 November 5 in (a) the SWAP FOV (up to 1.7 R ⊙) and in (b) the three-part-structured CME in the K-Cor FOV (1.05–3 R ⊙). A circle fitted to the cross section of the CME is shown in (b) with the corresponding minor radius. (c) Running difference image in the SWAP FOV (created using JHelioviewer) with blue lines tracing the eruption front and (d) running difference image in the K-Cor FOV (created using JHelioviewer) with blue lines corresponding to (c) overlaid on the K-Cor FOV.
Paper: Probing Velocity Dispersion Inside Coronal Mass Ejections: New Insights on Their Initiation
Authors: Satabdwa Majumdar, Elke D'Huys, Marilena Mierla, Nitin Vashishtha, Dana-Camelia Talpeanu, Dipankar Banerjee, Martin A. Reiss
Figure caption: A plot of the velocity profile of the LE and core in the combined K-Cor and LASCO FOV for the CME on 2014 November 5 in (a) and for the CME on 2022 May 24 in (b). The solid lines represent a smooth spline fitted to the data points, and the shaded regions indicate the uncertainty in the fitted spline.
Paper: Very-high-energy γ-Ray Emission from Young Massive Star Clusters in the Large Magellanic Cloud
Authors: F. Aharonian, F. Ait Benkhali, J. Aschersleben, H. Ashkar, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, K. Bernlöhr, M. Böttcher, J. Bolmont, M. de Bony de Lavergne, J. Borowska, R. Brose, A. Brown, F. Brun, B. Bruno, C. Burger-Scheidlin, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, P. Cristofari, J. Devin, A. Djannati-Ataï, J. Djuvsland, A. Dmytriiev, K. Egberts, S. Einecke, K. Feijen, M. Filipovic, G. Fontaine, S. Funk, S. Gabici, Y. A. Gallant, J. F. Glicenstein, J. Glombitza, G. Grolleron, L. Haerer, B. Heß, J. A. Hinton, W. Hofmann, T. L. Holch, D. Horns, Zhiqiu Huang, M. Jamrozy, F. Jankowsky, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, A. Kundu, R. G. Lang, S. Le Stum, A. Lemière, M. Lemoine-Goumard, J.-P. Lenain, F. Leuschner, J. Mackey, V. Marandon, G. Martí-Devesa, R. Marx, A. Mehta, A. Mitchell, R. Moderski, M. O. Moghadam, L. Mohrmann, A. Montanari, E. Moulin, M. de Naurois, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, M. Ostrowski, S. Panny, U. Pensec, G. Peron, G. Pühlhofer, A. Quirrenbach, S. Ravikularaman, M. Regeard, A. Reimer, O. Reimer, H. Ren, M. Renaud, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, K. Sabri, V. Sahakian, H. Salzmann, A. Santangelo, M. Sasaki, J. Schäfer, F. Schüssler, H. M. Schutte, H. Sol, S. Spencer, Ł. Stawarz, S. Steinmassl, C. Steppa, K. Streil, I. Sushch, A. M. Taylor, R. Terrier, M. Tsirou, N. Tsuji, C. van Eldik, M. Vecchi, C. Venter, J. Vink, S. J. Wagner, R. White, A. Wierzcholska, M. Zacharias, A. A. Zdziarski, A. Zech, N. Żywucka
Figure caption: Evaluation of systematic uncertainties of the PSF using PKS 2155−304 data. (a) Residual significance map obtained with the nominal PSF, in the energy range 0.27–1 TeV. (b) Same but with the PSF made narrower by 5%. In both maps, the green cross marks the position of PKS 2155−304, which is modeled as a pointlike source. (c) Distribution of θ 2, where θ is the angular offset between the reconstructed direction of each event and the position of PKS 2155−304. The black histogram and data points show the observed data, while the blue histogram displays the expected distribution based on the nominal PSF. The dashed gray and solid blue lines show fits of a Gaussian to the two distributions, respectively. These fits indicate that the predicted distribution is about 5% broader than the observed one (in terms of θ, not θ 2).
Paper: Probing Velocity Dispersion Inside Coronal Mass Ejections: New Insights on Their Initiation
Authors: Satabdwa Majumdar, Elke D'Huys, Marilena Mierla, Nitin Vashishtha, Dana-Camelia Talpeanu, Dipankar Banerjee, Martin A. Reiss
Figure caption: (a) and (b) A simulated breakout CME for two different time frames, with the two arrows denoting the LE and core of the flux rope. The referenced time is measured from the initiation of shearing. The color bar signifies the relative running difference density, denoted as ﹩{\rho }_{\mathrm{rel}}=\tfrac{\rho ({t}_{i})-\rho ({t}_{i-1})}{{\rho }_{0}}﹩, where ρ 0 represents the density of the equilibrium state before applying the shear and ρ(t  i ) represents the density in the ith time frame. (c) A plot of the difference in the height of the LE and flux-rope center for the breakout CME simulated in (a) and (b) vs. time, with the corresponding LE height plotted along the top axis.
Paper: Probing Velocity Dispersion Inside Coronal Mass Ejections: New Insights on Their Initiation
Authors: Satabdwa Majumdar, Elke D'Huys, Marilena Mierla, Nitin Vashishtha, Dana-Camelia Talpeanu, Dipankar Banerjee, Martin A. Reiss
Figure caption: A plot of the critical height (left-hand scale) and magnitude of velocity dispersion (right-hand scale) for all the CMEs vs. (a) flux-rope minor radius and (b) CME mass.
Paper: Very-high-energy γ-Ray Emission from Young Massive Star Clusters in the Large Magellanic Cloud
Authors: F. Aharonian, F. Ait Benkhali, J. Aschersleben, H. Ashkar, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, K. Bernlöhr, M. Böttcher, J. Bolmont, M. de Bony de Lavergne, J. Borowska, R. Brose, A. Brown, F. Brun, B. Bruno, C. Burger-Scheidlin, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, P. Cristofari, J. Devin, A. Djannati-Ataï, J. Djuvsland, A. Dmytriiev, K. Egberts, S. Einecke, K. Feijen, M. Filipovic, G. Fontaine, S. Funk, S. Gabici, Y. A. Gallant, J. F. Glicenstein, J. Glombitza, G. Grolleron, L. Haerer, B. Heß, J. A. Hinton, W. Hofmann, T. L. Holch, D. Horns, Zhiqiu Huang, M. Jamrozy, F. Jankowsky, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, A. Kundu, R. G. Lang, S. Le Stum, A. Lemière, M. Lemoine-Goumard, J.-P. Lenain, F. Leuschner, J. Mackey, V. Marandon, G. Martí-Devesa, R. Marx, A. Mehta, A. Mitchell, R. Moderski, M. O. Moghadam, L. Mohrmann, A. Montanari, E. Moulin, M. de Naurois, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, M. Ostrowski, S. Panny, U. Pensec, G. Peron, G. Pühlhofer, A. Quirrenbach, S. Ravikularaman, M. Regeard, A. Reimer, O. Reimer, H. Ren, M. Renaud, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, K. Sabri, V. Sahakian, H. Salzmann, A. Santangelo, M. Sasaki, J. Schäfer, F. Schüssler, H. M. Schutte, H. Sol, S. Spencer, Ł. Stawarz, S. Steinmassl, C. Steppa, K. Streil, I. Sushch, A. M. Taylor, R. Terrier, M. Tsirou, N. Tsuji, C. van Eldik, M. Vecchi, C. Venter, J. Vink, S. J. Wagner, R. White, A. Wierzcholska, M. Zacharias, A. A. Zdziarski, A. Zech, N. Żywucka
Figure caption: Count profiles for the slice across the target region indicated in Figure 5(b). The black data points, identical in all panels, show the observed number of events in 0.°03 wide bins along the slice. The dark gray histogram displays the predicted residual hadronic background, while the light gray histogram denotes the total model prediction including γ-ray source models. (a) After adding N157B to the ROI model. (b) After adding 30 Dor C to the ROI model. (c) After adding R136 to the ROI model. Indicated in the top right corner of each panel is the result of a χ 2 test between the total model prediction and the observed data.
Paper: Very-high-energy γ-Ray Emission from Young Massive Star Clusters in the Large Magellanic Cloud
Authors: F. Aharonian, F. Ait Benkhali, J. Aschersleben, H. Ashkar, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, K. Bernlöhr, M. Böttcher, J. Bolmont, M. de Bony de Lavergne, J. Borowska, R. Brose, A. Brown, F. Brun, B. Bruno, C. Burger-Scheidlin, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, P. Cristofari, J. Devin, A. Djannati-Ataï, J. Djuvsland, A. Dmytriiev, K. Egberts, S. Einecke, K. Feijen, M. Filipovic, G. Fontaine, S. Funk, S. Gabici, Y. A. Gallant, J. F. Glicenstein, J. Glombitza, G. Grolleron, L. Haerer, B. Heß, J. A. Hinton, W. Hofmann, T. L. Holch, D. Horns, Zhiqiu Huang, M. Jamrozy, F. Jankowsky, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, A. Kundu, R. G. Lang, S. Le Stum, A. Lemière, M. Lemoine-Goumard, J.-P. Lenain, F. Leuschner, J. Mackey, V. Marandon, G. Martí-Devesa, R. Marx, A. Mehta, A. Mitchell, R. Moderski, M. O. Moghadam, L. Mohrmann, A. Montanari, E. Moulin, M. de Naurois, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, M. Ostrowski, S. Panny, U. Pensec, G. Peron, G. Pühlhofer, A. Quirrenbach, S. Ravikularaman, M. Regeard, A. Reimer, O. Reimer, H. Ren, M. Renaud, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, K. Sabri, V. Sahakian, H. Salzmann, A. Santangelo, M. Sasaki, J. Schäfer, F. Schüssler, H. M. Schutte, H. Sol, S. Spencer, Ł. Stawarz, S. Steinmassl, C. Steppa, K. Streil, I. Sushch, A. M. Taylor, R. Terrier, M. Tsirou, N. Tsuji, C. van Eldik, M. Vecchi, C. Venter, J. Vink, S. J. Wagner, R. White, A. Wierzcholska, M. Zacharias, A. A. Zdziarski, A. Zech, N. Żywucka
Figure caption: Chandra X-ray image of N157B (Chen et al. 2006), with properties of the best-fit γ-ray source model overlaid. The green circle marker, thin solid line, thick solid line, and thick dotted line indicate the best-fit position, position uncertainty (95% confidence level), 1σ Gaussian radius, and 68% containment radius, respectively. In addition, the transparent band shows the statistical uncertainty on the 1σ radius, while the arrows denote the systematic uncertainty.
Paper: Observational Evidence for Magnetic Field Amplification in SN 1006
Authors: Moeri Tao, Jun Kataoka, Takaaki Tanaka
Figure caption: Top: double synchrotron and IC (CMB) model fit to the broadband SED of the entire SN 1006 (including both NE  SW shells). Radio (this study; blue open circles), Suzaku X-ray (Bamba et al. 2008; filled red circles), Fermi (Xing et al. 2019; cyan open circles) data, and H.E.S.S. (Acero et al. 2010; yellow region) data are shown with the first synchrotron (green dashes), second synchrotron, and its IC (CMB; magenta dashes) emissions, respectively. Black open circles represent the doubled values of the optical and UV fluxes obtained for the NE shell. Bottom: same as above, but the SED is fit to the NE shell of SN 1006. Blue open circles represent half the value of the radio fluxes obtained for the entire remnant. The red open circles represent the X-ray measurement for the NE shell reported in Kalemci et al. (2006). The optical (Winkler et al. 2003) and UV (Korreck et al. 2004) data are represented as black open circles.
Paper: Observational Evidence for Magnetic Field Amplification in SN 1006
Authors: Moeri Tao, Jun Kataoka, Takaaki Tanaka
Figure caption: Upper: comparison between the MeerKAT (1335 MHz) and Chandra (2.0−7.0 keV) images of SN 1006. (a) MeerKAT and (b) Chandra images of the NE shell. (c) MeerKAT and (d) Chandra images of the SW shell. Lower: comparison between the radial profiles of MeerKAT (1335 MHz; green line) and Chandra (2.0−7.0 keV; red line) images across the (e) NE and (f) SW shells along the white line. Note that the spike structure seen in (a), which is vertical to the shock front, is not related to SN 1006 but the background FR-I radio galaxy WISEA J150403.60-415550.9. Full details are given in p. 24 of Cotton et al. (2024). Also in (f)-1, the radio profile is normalized at the second peak, which is more likely the shock front.
Paper: Observational Evidence for Magnetic Field Amplification in SN 1006
Authors: Moeri Tao, Jun Kataoka, Takaaki Tanaka
Figure caption: Comparison of thickness of the X-ray shell (D X) and radio shell (D R) derived from Figure 2. The red lines represent a = 100 and 300, which correspond to D X/D R = 19.0 and 3.7, respectively.
Paper: Observational Evidence for Magnetic Field Amplification in SN 1006
Authors: Moeri Tao, Jun Kataoka, Takaaki Tanaka
Figure caption: The broadband radio spectrum of SN 1006. The filled circles are derived from Planck measurements in this study. The open circles represent the archival radio flux densities from Gardner & Milne (1965), Kundu (1970), Milne (1971), Milne & Dickel (1975), Rothenflug et al. (2004), Dyer et al. (2009), Petruk et al. (2009), and Arnaud et al. (2016).
Paper: Fundamentalization of Periods for First- and Second-overtone Classical Cepheids
Authors: Bogumił Pilecki
Figure caption: Period ratios for double-mode (1O + 2O) Cepheids from the OGLE-4 catalog for MW, LMC, and SMC. Black lines are the best parabolic fit for the data. The green dashed line represents the relation from A95. For MW, the data are generally highly scattered except around P 1O = 1 day. The ranges of the X- and Y-axes are the same in all panels.
Paper: Fundamentalization of Periods for First- and Second-overtone Classical Cepheids
Authors: Bogumił Pilecki
Figure caption: Period ratios for double-mode (F + 1O) Cepheids from the OGLE-4 catalog for three considered galaxies. Black lines are the best linear fit for the data. Green dashed lines represent relations from A95. Blue dotted relations were taken from Sz18 for adopted average [Fe/H] of 0.0, −0.35, and −0.75 dex for MW, LMC, and SMC, respectively. Red dashed relations (P24) are not based on double-mode Cepheids (see the main text) but are shown here for comparison. The ranges of the X- and Y-axes are the same in all panels.
Paper: Fundamentalization of Periods for First- and Second-overtone Classical Cepheids
Authors: Bogumił Pilecki
Figure caption: Comparison of the fitted relations for all considered galaxies. Shaded areas mark the 2σ range around them. The relations of A95 and Sz18 are plotted here only in their validity range, ﹩\mathrm{log}{P}_{0}=﹩ 0.1–0.7 for the A95 LMC relation and 0.3–0.80 for the rest. The position of known beat Cepheids in the M31 and M33 galaxies is also shown.
Paper: Fundamentalization of Periods for First- and Second-overtone Classical Cepheids
Authors: Bogumił Pilecki
Figure caption: Similar to Figure 2 but for Cepheids pulsating in 1O and 2O modes. The fitted relations cross at around P 1O = 0.9 days. The relation of A95 is plotted here only in its validity range, ﹩\mathrm{log}{P}_{0}=﹩ −0.2–0.1. The position of one M31 beat (1O + 2O) Cepheid is shown.
Paper: Cosmology from One Galaxy in a Void?
Authors: Bonny Y. Wang, 玥 汪, Alice Pisani
Figure caption: Ωm predictions using only one galaxy with fully connected layers. Blue dots and error bars represent the predicted posterior mean and standard deviation of Ωm from the networks. The orange line in the diagonal indicates the perfect match between predicted and true values. The left, middle, and right columns show the results when using nonvoid galaxies, randomly selected galaxies, and void galaxies, respectively; therefore moving from left to right shows the change when considering the large-scale environment. For the right column, the top row shows the results after selecting void galaxies with a cutoff value of Voronoi cell volume at 100 (Mpc/h)3, while the bottom row shows a more restrictive Voronoi cell volume cut at 150 (Mpc/h)3, corresponding to more isolated galaxies and accounting for the local environment. These results correspond to the void catalog considering the purity cut on core density. For better visual comparison, in the case of nonvoid and randomly selected galaxies we subsample the number of points to the same number of data points shown in the plot for void galaxies. The R 2 and RMSE values improve for void galaxies (from left to right) and further improve if we consider more isolated galaxies among the void galaxies (from top to bottom, right column).
Paper: Cosmology from One Galaxy in a Void?
Authors: Bonny Y. Wang, 玥 汪, Alice Pisani
Figure caption: Similar to Figure 2 with the additional radius cut applied for purity to the void catalog. Here, R 2, RMSE, and ϵ values all improve for void galaxies (from left to right, accounting for the large-scale environment) and further improve when considering more isolated galaxies among void galaxies, that is, considering the local environment (right column, from top to bottom). The strongest improvement is obtained when accounting for selections on both the large-scale and local environments (right column, bottom plot).
Paper: Cosmology from One Galaxy in a Void?
Authors: Bonny Y. Wang, 玥 汪, Alice Pisani
Figure caption: The relationship between the size of error bars from the predictions and the Voronoi cell volume of the galaxies inside voids. We bin the galaxies in each range of error bars and calculate the average Voronoi cell volume of the galaxies in each bin. The error bars are calculated as the standard errors, which consider both the standard deviation and the sample size. The slope of the curve shows that the error bars of the predictions (on the x-axis) are smaller for galaxies with a larger Voronoi cell volume (on the y-axis), that is, showing that more isolated void galaxies provide more stringent constraints.
Paper: Cosmology from One Galaxy in a Void?
Authors: Bonny Y. Wang, 玥 汪, Alice Pisani
Figure caption: The top row shows the average prediction of Ωm using galaxies in the same simulation. The bottom row shows a zoom in on the lower values of Ωm. The figure shows an improvement especially on the lower values of Ωm when using void galaxies that have smaller error bars (the values of ϵ highlight the improvement).
Paper: Cosmology from One Galaxy in a Void?
Authors: Bonny Y. Wang, 玥 汪, Alice Pisani
Figure caption: Histogram of Voronoi cell volume in voids for galaxies in the data set. Galaxies with a larger Voronoi cell volume are more isolated.
Paper: Very-high-energy γ-Ray Emission from Young Massive Star Clusters in the Large Magellanic Cloud
Authors: F. Aharonian, F. Ait Benkhali, J. Aschersleben, H. Ashkar, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, K. Bernlöhr, M. Böttcher, J. Bolmont, M. de Bony de Lavergne, J. Borowska, R. Brose, A. Brown, F. Brun, B. Bruno, C. Burger-Scheidlin, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, P. Cristofari, J. Devin, A. Djannati-Ataï, J. Djuvsland, A. Dmytriiev, K. Egberts, S. Einecke, K. Feijen, M. Filipovic, G. Fontaine, S. Funk, S. Gabici, Y. A. Gallant, J. F. Glicenstein, J. Glombitza, G. Grolleron, L. Haerer, B. Heß, J. A. Hinton, W. Hofmann, T. L. Holch, D. Horns, Zhiqiu Huang, M. Jamrozy, F. Jankowsky, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, A. Kundu, R. G. Lang, S. Le Stum, A. Lemière, M. Lemoine-Goumard, J.-P. Lenain, F. Leuschner, J. Mackey, V. Marandon, G. Martí-Devesa, R. Marx, A. Mehta, A. Mitchell, R. Moderski, M. O. Moghadam, L. Mohrmann, A. Montanari, E. Moulin, M. de Naurois, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, M. Ostrowski, S. Panny, U. Pensec, G. Peron, G. Pühlhofer, A. Quirrenbach, S. Ravikularaman, M. Regeard, A. Reimer, O. Reimer, H. Ren, M. Renaud, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, K. Sabri, V. Sahakian, H. Salzmann, A. Santangelo, M. Sasaki, J. Schäfer, F. Schüssler, H. M. Schutte, H. Sol, S. Spencer, Ł. Stawarz, S. Steinmassl, C. Steppa, K. Streil, I. Sushch, A. M. Taylor, R. Terrier, M. Tsirou, N. Tsuji, C. van Eldik, M. Vecchi, C. Venter, J. Vink, S. J. Wagner, R. White, A. Wierzcholska, M. Zacharias, A. A. Zdziarski, A. Zech, N. Żywucka
Figure caption: Composite infrared image from Spitzer (credit: NASA/JPL-Caltech; https://www.spitzer.caltech.edu/image/ssc2020-06b-tarantula-nebula-spitzer-3-color-image) of the region around the star cluster R136. The nominal position of R136 (Høg et al. 2000) is marked with a gray cross. The white circle marker, solid line, and dotted line indicate the best-fit position, 1σ Gaussian radius, and 68% containment radius of the best-fit γ-ray model for R136, respectively. The transparent band shows the statistical uncertainty on the 1σ radius, while the arrows denote the systematic uncertainty. The green contour lines denote 12CO(1–0) emission (Johansson et al. 1998), while the light red contours indicate the positions of dense “knots” of molecular gas identified through 12CO(2–1) emission (Kalari et al. 2018).