adsabs/AstroCLIMB huggingface dataset:
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: Optical image (credit: ESO; https://www.eso.org/public/images/eso1816a) showing the LH 90 association of star clusters. The yellow circles mark the positions of the compact clusters α–ζ found by Lortet & Testor (1984). The pink contour line outlines the SB 30 Dor C as visible in X-rays (1–2 keV) with XMM-Newton; the red circle denotes MCSNR J0536−6913, a putative SNR (Kavanagh et al. 2015). 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 30 Dor C, respectively. The transparent band shows the statistical uncertainty on the 1σ radius, while the arrows denote the systematic uncertainty. The turquoise diamond marks the position reported in H.E.S.S. Collaboration (2015). The green contour lines denote bright spots of 12CO(1–0) emission measured with the Atacama Large Millimeter/submillimeter Array (Yamane et al. 2021).
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: (a) Significance map for the entire ROI, above an energy of 0.5 TeV, after adjustment of the hadronic background model. The map has been smoothed with a top-hat kernel of 0.°07 radius, as indicated in the bottom right corner. The dark gray lines enclose regions that have been excluded in the fit of the background, and the white dashed line indicates the target region of the analysis, shown in more detail on the right. The inset shows the distribution of significance values outside the exclusion regions (purple histogram) as compared to a normal distribution with unity width (green line). (b) Cutout of the significance map, showing the target region. The white rectangle denotes a slice along which γ-ray excess profiles have been computed (see Figure 9).
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:  γ-ray flux maps of the target region of the analysis. The maps show the γ-ray flux F in units of 10−8 cm−2 s−1 sr−1, integrated above an energy of 0.5 TeV, assuming a power-law spectrum with index −2.5. Smoothing with a top-hat kernel of 0.°07 radius has been applied. (a) Entire emission. (b) Residual emission after subtraction of the emission from N157B predicted by the best-fit ROI model. Dashed blue lines show flux contours at (2.5/7.5/12.5) × 10−8 cm−2 s−1 sr−1 in panel (a) and (1.5/3) × 10−8 cm−2 s−1 sr−1 in panel (b). Pixels with a negative excess after background subtraction are clipped at zero. The light green contour lines denote Hα emission as inferred by SHASSA (Gaustad et al. 2001).
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: Spectral energy distribution for N157B (a), 30 Dor C (b), and R136 (c). The blue line and band show the best-fit spectral model with its statistical uncertainty. The flux points have been obtained by refitting the flux normalization ϕ 0 in the corresponding energy range, keeping the other parameters of the spectral model of the respective source fixed. The published spectra are taken from H.E.S.S. Collaboration (2015).
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:  γ-ray luminosity of 30 Dor C and R136. Shown on the vertical axis is the power output per logarithmic energy interval, that is, ﹩{E}^{2}\cdot ({dN}/{dE})\cdot \,4\pi {d}^{2}﹩, with d the distance to the source. For comparison, the γ-ray luminosity of the YMC Westerlund 1 is also shown (H.E.S.S. Collaboration et al. 2022). The solid and dashed lines display a leptonic and a hadronic model, respectively, which we have fitted to both sources using the NAIMA package (Zabalza 2015).
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: Maps of residual significance of the analysis target region. (a) After the background model adjustment (see Appendix A). (b) After adding N157B to the ROI model. (c) After adding 30 Dor C to the ROI model. (d) After adding R136 to the ROI model. The blue crosses denote the best-fit position of the respective source models, while the blue circles indicate the best-fit Gaussian width.
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: Images of the host galaxies. Top row: RGB color composites. The continuum is shown in red, while green hues denote Hα (QPE2) or N II (RX J1301 and GSN 069). O III is shown in blue. Zoomed-in panels can be found in Figure B1. Second row: grayscale continuum images overlaid with a contour map of the emission line. The red plus sign indicates the continuum nucleus position. Kiloparsec-scale EELRs of ionized gas are discernible in three out of five QPE hosts. This ionized gas is decoupled from the continuum emission. Third row: BPT diagram of the line ratios using the regions indicated in the panel above, after correcting for the stellar continuum component. Bottom row: WHAN diagram of the same regions.
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: Spatially resolved kinematics. Shown are stellar velocity (top), gas velocity (middle), and gas velocity dispersion (bottom) maps. The contours indicate the EELR to guide the eye. The left column shows GSN 069, the middle column shows RX J1301, and the right column shows eRO-QPE2. The sky area is identical for every source across the panels to highlight the differences in EELR kinematics compared to the stellar continuum.
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: Continuum grayscale image and Hα contours overlaid for sources eRO-QPE1 (left) and eRO-QPE3 (right), which do not show an EELR. The faintest contours represent Hα flux levels of 35 × 10−20 erg cm−2 s−1 Å  and 15 × 10−20 erg cm−2 s−1 Å  for eRO-QPE1 and eRO-QPE3, respectively.
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: Aperture spectra of GSN 069, for the regions indicated in Figure 1, with the same color-coding.
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: Same as the top row of Figure 1, but zoomed in to improve the detailed view of the nuclear regions of the galaxies. Note the presence of a ringlike structure surrounding the nucleus of GSN 069, which may be a star-forming ring.
Paper: Observations of the Formation and Disappearance of a Funnel Prominence
Authors: Bo Yang, Jiayan Yang, Yi Bi, Junchao Hong
Figure caption: AIA 304 Å (panels (a)–(d)) and the negative 171 Å (panels (e)–(h)) images exhibiting the disappearance of the funnel prominence and the associated hornlike structure by the drainage of prominence material along well-defined curved coronal loops.
Paper: Discovery of a Barium Blue Straggler Star in M67 and “Sighting” of Its White Dwarf Companion 
Authors: Harshit Pal, Annapurni Subramaniam, Arumalla B. S. Reddy, Vikrant V. Jadhav
Figure caption: (a) Barium and (b) yttrium abundances of single members (SM) and binary members (BM) of M67 (from Geller et al. 2021) as estimated by GALAH (Buder et al. 2021) are shown. Panel (c) shows the color–magnitude diagram of M67 using the Gaia DR3 data.
Paper: Discovery of a Barium Blue Straggler Star in M67 and “Sighting” of Its White Dwarf Companion 
Authors: Harshit Pal, Annapurni Subramaniam, Arumalla B. S. Reddy, Vikrant V. Jadhav
Figure caption: Binary SEDs of WOCS 9005. The left panel shows the binary fit using Kurucz and Koester models. The middle panel shows the binary fit using Kurucz_UVBLUE and Koester models. The fitted SEDs for A component (orange), B component (blue for Kurucz and purple for Kurucz_UVBLUE), and total (green). The bottom subpanel shows the fractional residual flux for the A component and total binary SED. The observed points are shown as black error bars and data removed during fitting is shown as black circles. The right panel shows the H–R diagram of the components based on SED fit parameters, with the same colors as the SEDs. The contours represent the top 1 percentile fits of the corresponding model. The PARSEC isochrone of log(age) 9.6 (gray curve) and WD cooling curves for WD masses of 0.176 (Althaus et al. 2013), 0.3, 0.5, and 0.9 (Holberg & Bergeron 2006) are shown for reference.
Paper: Discovery of a Barium Blue Straggler Star in M67 and “Sighting” of Its White Dwarf Companion 
Authors: Harshit Pal, Annapurni Subramaniam, Arumalla B. S. Reddy, Vikrant V. Jadhav
Figure caption: Observed spectra of WOCS 9005 (red) and WOCS 1020 (blue) covering the wavelength regions containing Na and the s-process elements Y, Ba, and La. The spectral lines due to other species are also shown.
Paper: Investigation of the Gamma-Ray Bursts Prompt Emission Under the Relativistically Expanding Fireball Scenario
Authors: Soumya Gupta, Sunder Sahayanathan
Figure caption: The plot represents the spectrum (α = 0.6) for the time-averaged case (﹩\nu \,{{\mathscr{F}}}_{\nu }﹩) in a red solid line, the instantaneous case (ν F  ν ) in a teal dashed line, and the blackbody in a black dotted line.
Paper: Investigation of the Gamma-Ray Bursts Prompt Emission Under the Relativistically Expanding Fireball Scenario
Authors: Soumya Gupta, Sunder Sahayanathan
Figure caption: The plot depicts the equal-time surface via the red dashed line, photospheric radius R ph(θ) via the teal solid line, and emission cone of angle 1/Γ via the black dotted line for the Γ of 800. The R ph0 is scaled to unity, and the gray dotted–dashed line is the axis for θ = 0.
Paper: New Insights into the Internal Structure of GJ 1214 b Informed by JWST
Authors: Matthew C. Nixon, Anjali A. A. Piette, Eliza M.-R. Kempton, Peter Gao, Jacob L. Bean, Maria E. Steinrueck, Alexandra S. Mahajan, Jason D. Eastman, Michael Zhang, Leslie A. Rogers
Figure caption: Interior P–T (left) and P–ρ (right) profiles for best-fit models with a 300× solar composition envelope. Since the maximally reflective hazes lead to a hotter envelope, the envelope density is lower, leading to smaller envelope mass fractions that are required to match the mass and radius of GJ 1214 b. Note that we do not calculate a temperature gradient for the core, since our EOS for iron is not temperature-dependent.
Paper: New Insights into the Internal Structure of GJ 1214 b Informed by JWST
Authors: Matthew C. Nixon, Anjali A. A. Piette, Eliza M.-R. Kempton, Peter Gao, Jacob L. Bean, Maria E. Steinrueck, Alexandra S. Mahajan, Jason D. Eastman, Michael Zhang, Leslie A. Rogers
Figure caption: H2O mass fractions consistent with the observed mass and radius of GJ 1214 b to within 1σ, in the case of a pure water envelope, for different haze production rates. Across all cases, the H2O mass fraction must be at least 79%. For a maximal haze production rate (10−11g cm−2 s−1) of tholin hazes, even a 100% H2O mass fraction is not sufficient to match the planet’s mass and radius.
Paper: Investigation of the Gamma-Ray Bursts Prompt Emission Under the Relativistically Expanding Fireball Scenario
Authors: Soumya Gupta, Sunder Sahayanathan
Figure caption: The plot represents the variation of ﹩{ \mathcal W }﹩ of time-averaged spectra (﹩\nu \,{{\mathscr{F}}}_{\nu }﹩) with α for a different parameter space. The variation with T ph0, Γ, R ph0, and Δt is plotted in the top-left, top-right, bottom-left, and bottom-right panels, respectively, and color mapped on the right axis of each panel. The black dotted–dashed line corresponds to ﹩{ \mathcal W }﹩ of the blackbody spectrum. In the first panel, the red dashed line corresponds to ﹩{ \mathcal W }﹩ of the instantaneous (ν F  ν ) spectrum.
Paper: Investigation of the Gamma-Ray Bursts Prompt Emission Under the Relativistically Expanding Fireball Scenario
Authors: Soumya Gupta, Sunder Sahayanathan
Figure caption: The plot exhibits the evolution of the time-integrated spectrum with a different parameter space. The variation with T ph0, Γ, R ph0, and Δt is plotted in the top-left, top-right, bottom-left, and bottom-right panels, respectively, and color mapped on the right axis of each panel. The gray dashed line is the spectral width. The spectrum is scaled with the value at peak energy to illustrate the shift in peak energy (direction of the arrow) with an increase in model parameters.
Paper: Investigation of the Gamma-Ray Bursts Prompt Emission Under the Relativistically Expanding Fireball Scenario
Authors: Soumya Gupta, Sunder Sahayanathan
Figure caption: The plot represents the change in the time-integrated spectrum for the α ranging from 0 to 2/3, color mapped on the right axis. The vertical gray dashed line represents the energy range of the NaI detector of the Gamma-ray Burst Monitor (GBM) on board Fermi.