adsabs/AstroCLIMB huggingface dataset:
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: Final mosaics of all six bands in the MIRI1 pointing. The mosaics are astrometrically aligned to Gaia DR3, as described further in Section 2.2.3. See Figure 1 for an RGB version of a portion of this pointing.
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: The F560W − F770W color distribution. Here, for accuracy, we only adopt sources with S/N > 3 in both bands. The vertical black solid, dashed, and dotted lines indicate the colors of Arp 220 at z = 0.5, 1, and 2, respectively (Brown et al. 2014). The bulk (84%) of the sources have negative color values, as expected from starlight in higher-redshift galaxies (z ≳ 1).
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: Cumulative number counts of different MIRI bands. The error bars represent Poisson uncertainties calculated using ASTROPY.STATS.POISSON_CONF_INTERVAL. The dashed vertical line in each panel indicates the median 5σ depth of the CEERS pointings (Table 3). The red squares in the F560W/F770W panel indicate the IRAC Ch3/Ch4 number counts from Fazio et al. (2004). The blue solid and orange dashed curves represent the predictions of the Santa Cruz and Cowley et al. (2018) SAMs, respectively. The F560W and F770W numbers are based on SEXTRACTOR   photometry from the blue MIRI pointings (MIRI3, MIRI6, MIRI7, and MIRI9), while F1000W, F1280W, F1500W, F1800W, and F2100W are based on TPHOT photometry from the red MIRI pointings (MIRI1, MIRI2, MIRI5, and MIRI8). All of the MIRI number counts and their associated errors are publicly available with this figure.(The data used to create this figure are available.)
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: Left: MIRI SED of the Galactic stars covered by MIRI1. The blue dashed and red dotted lines represent the best fits of the Rayleigh–Jeans law (normalization as free parameter) and a power law (normalization and index as free parameters). The two fits are very similar, indicating that our MIRI colors are reliable. Right: corresponding 5″ × 5″ cutouts of HST/F160W and MIRI. Although the sources are sometimes truncated by the detector edge (e.g., F1800W of the second star, from top to bottom), the corresponding photometry is still acceptable. This shows that, for these sources, TPHOT can still robustly constrain the flux by fitting the pixels within the detector coverage.
Paper: AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
Authors: Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, Fabio D'Amico
Figure caption: Evolution of the hard X-ray and gamma-ray emission of GRB 221009A as detected by AGILE. From top to bottom: AC-Top (50–200 keV) RM in linear scale, MCAL (350 keV–100 MeV) data (black curve) and RM (blue curve) in logarithmic scale, “unvetoed” GRID RM in linear scale, GRID photon flux lightcurve (50 MeV–50 GeV) in logarithmic scale.
Paper: AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
Authors: Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, Fabio D'Amico
Figure caption: AGILE-GRID lightcurve of the first observation window. Top panel: AGILE RMs (magenta line: “unvetoed” GRID; green line: AC-Top). Bottom panel: AGILE-GRID lightcurve, obtained with ML (10 s time bins for the first OW), for a photon energy above 50 MeV. The gray bands represent the time intervals with low GRID exposure, not considered in this analysis (GRB off-axis angles greater than 60°), the green bands show the time intervals of the AC RM saturation, excluded from this analysis.
Paper: AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
Authors: Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, Fabio D'Amico
Figure caption: Spectral evolution of the GRB 221009A, as obtained from available data of the AGILE-MCAL and the AGILE-GRID. Panels (a)–(f) provide spectral information for the corresponding time intervals defined in Figure 1 and Table 1; the sequence is to be read from left to right, and from top to bottom. The GRID spectra are presented together with the corresponding best-fit curves with their uncertainties (see Table 3).
Paper: AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
Authors: Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, Fabio D'Amico
Figure caption: Spectral energy distribution of the external shock model with the set of parameters adopted in the text. Data from the GRID detector of the AGILE instrument for the c1 time interval are reported in green: [273, 303 s] after T 0, corresponding to [47, 77 s] after T* (the reference time adopted in Cao et al. 2023). Additionally, we include also data from the LHAASO observatory (Cao et al. 2023) for time interval [248, 326 s] after T 0, corresponding to [22, 100 s] after T*. LHAASO data points are reported in blue, both for the observed data and the EBL deabsorbed data (faded). More details are reported in the main text.
Paper: AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
Authors: Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, Fabio D'Amico
Figure caption: Energy flux evolution of the GRB 221009A: prompt phase and afterglow. Black points: AGILE-MCAL. Red points: AGILE-GRID. Blue points: Swift-XRT (Williams et al. 2023). Time power-law indices are indicated in the figure.
Paper: AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
Authors: Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, Fabio D'Amico
Figure caption: Spectral evolution of the GRB 221009A, as detected by AGILE-GRID during the afterglow phase detected in gamma-rays. Spectral energy distribution (from left to right) for the c1, c2, and d time intervals. The spectra are presented together with the corresponding best-fit curves with their uncertainties (see Table 4).
Paper: AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
Authors: Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, Fabio D'Amico
Figure caption: Time evolution of the AGILE scientific RMs during the GRB 221009A. Top panel: AC-Top RM. Bottom panel: MCAL RM.
Paper: AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
Authors: Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, Fabio D'Amico
Figure caption: Observational parameters of the GRB 221009A, as detected by AGILE-GRID. From top to bottom: (1) off-axis angle with respect to the AGILE boresight axis; (2) GRID lightcurve (E ≥ 50 MeV), the gray bands are related to off-axis angles greater than 60°, and the green bands show the time intervals of the AC RM saturation; (3) GRID exposure.
Paper: AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
Authors: Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, Fabio D'Amico
Figure caption: Sky count map above 100 MeV in Galactic coordinates of the AGILE-GRID gamma-ray detector during the time interval [T 0, T 0 + 48 hr]. The gamma-ray source associated with GRB 221009A is shown inside the green circle. The darkened sky regions are due to seasonal lack of exposure of the GRID detector, due to solar panel constraints.
Paper: Fleeting Small-scale Surface Magnetic Fields Build the Quiet-Sun Corona
Authors: L. P. Chitta, S. K. Solanki, J. C. del Toro Iniesta, J. Woch, D. Calchetti, A. Gandorfer, J. Hirzberger, F. Kahil, G. Valori, D. Orozco Suárez, H. Strecker, T. Appourchaux, R. Volkmer, H. Peter, S. Mandal, R. Aznar Cuadrado, L. Teriaca, U. Schühle, D. Berghmans, C. Verbeeck, A. N. Zhukov, E. R. Priest
Figure caption: Coronal dynamics emerging from weaker-field regions. Panels (a), (c), (e), and (g) display examples of four jet-like events from the weak-field sections of loops, L1, L4, L5, and L6. The green and purple colored boxes are positioned along the parts of this jet-like activity. The magnetic flux density contours have the same meaning as in Figure 1. The green and purple light curves in panels (b), (d), (f), and (h) show the average HRIEUV intensities from the corresponding boxes overlaid on the left-side panels, as functions of time, normalized to their respective minima and maxima within the plotted time period. These light curves are derived from the images at their native cadence. See Section 2 and Appendix A for details.
Paper: Fleeting Small-scale Surface Magnetic Fields Build the Quiet-Sun Corona
Authors: L. P. Chitta, S. K. Solanki, J. C. del Toro Iniesta, J. Woch, D. Calchetti, A. Gandorfer, J. Hirzberger, F. Kahil, G. Valori, D. Orozco Suárez, H. Strecker, T. Appourchaux, R. Volkmer, H. Peter, S. Mandal, R. Aznar Cuadrado, L. Teriaca, U. Schühle, D. Berghmans, C. Verbeeck, A. N. Zhukov, E. R. Priest
Figure caption: Persistent surface magnetic and coronal loop features. Time-averaged SO/PHI magnetic flux density (panel (a)) and the HRIEUV coronal (panel (b)) maps are displayed. Green ellipse and boxes L1–L8 have the same meaning as in Figure 1. The red (positive) and blue (negative) contours outline magnetic concentrations with flux densities above 6 Mx cm−2 (i.e., 3σ avg), while the yellow (positive) and cyan (negative) contours mark regions with flux densities between 2σ avg and 3σ avg level, based on the time-averaged SO/PHI magnetic flux density map. See Appendices A and B for details.
Paper: Fleeting Small-scale Surface Magnetic Fields Build the Quiet-Sun Corona
Authors: L. P. Chitta, S. K. Solanki, J. C. del Toro Iniesta, J. Woch, D. Calchetti, A. Gandorfer, J. Hirzberger, F. Kahil, G. Valori, D. Orozco Suárez, H. Strecker, T. Appourchaux, R. Volkmer, H. Peter, S. Mandal, R. Aznar Cuadrado, L. Teriaca, U. Schühle, D. Berghmans, C. Verbeeck, A. N. Zhukov, E. R. Priest
Figure caption: Small-scale and weaker magnetic footpoints of QS coronal loops. Same as Figure 2, but plotted for sections of loops L5–L8. Ellipses in panels (f) and (g) outline regions of footpoints of coronal loop bundle L6 without clear underlying magnetic field structures.
Paper: Fleeting Small-scale Surface Magnetic Fields Build the Quiet-Sun Corona
Authors: L. P. Chitta, S. K. Solanki, J. C. del Toro Iniesta, J. Woch, D. Calchetti, A. Gandorfer, J. Hirzberger, F. Kahil, G. Valori, D. Orozco Suárez, H. Strecker, T. Appourchaux, R. Volkmer, H. Peter, S. Mandal, R. Aznar Cuadrado, L. Teriaca, U. Schühle, D. Berghmans, C. Verbeeck, A. N. Zhukov, E. R. Priest
Figure caption: Small-scale and weaker magnetic footpoints of QS coronal loops. HRIEUV sequences of sections of loops L1–L4, marked in Figure 1, and contours of the line-of-sight component of the corresponding magnetic field concentrations at their footpoints, as seen with SO/PHI are displayed. The magnetic contours have the same meaning as in Figure 1. Time runs from left to right. See Section 2 and Appendix A for details.
Paper: Fleeting Small-scale Surface Magnetic Fields Build the Quiet-Sun Corona
Authors: L. P. Chitta, S. K. Solanki, J. C. del Toro Iniesta, J. Woch, D. Calchetti, A. Gandorfer, J. Hirzberger, F. Kahil, G. Valori, D. Orozco Suárez, H. Strecker, T. Appourchaux, R. Volkmer, H. Peter, S. Mandal, R. Aznar Cuadrado, L. Teriaca, U. Schühle, D. Berghmans, C. Verbeeck, A. N. Zhukov, E. R. Priest
Figure caption: Quiet-Sun corona and plasma loops. The snapshot shows the full FOV of HRIEUV. The white box marks a partial FOV that we presented in Figure 1. See Section 2 and Appendix A for details.
Paper: Unprecedented Early Flux Excess in the Hybrid 02es-like Type Ia Supernova 2022ywc Indicates Interaction with Circumstellar Material
Authors: Shubham Srivastav, T. Moore, M. Nicholl, M. R. Magee, S. J. Smartt, M. D. Fulton, S. A. Sim, J. M. Pollin, L. Galbany, C. Inserra, A. Kozyreva, Takashi J. Moriya, F. P. Callan, X. Sheng, K. W. Smith, J. S. Sommer, J. P. Anderson, M. Deckers, M. Gromadzki, T. E. Müller-Bravo, G. Pignata, A. Rest, D. R. Young
Figure caption: Top and middle panels: Sequence of stacked difference and input images for SN 2022ywc during the early excess. The SN position is marked with a red circle. The image stamps cover a field of view of approximately ﹩6^{\prime} \times 6^{\prime} ﹩. Bottom panel: Absolute AB magnitude light curve of SN 2022ywc in the ATLAS c, o bands, corrected for MW extinction. Also shown for comparison are the MW extinction-corrected light curves of 02es-like events SN 2002es (Ganeshalingam et al. 2012), SN 2006bt (Foley et al. 2010), SN 2007cq (Ganeshalingam et al. 2010), iPTF14atg (Cao et al. 2015), SN 2016jhr (Jiang et al. 2017), and SN 2019yvq (Miller et al. 2020), and also the normal Ia SN 2011fe (Zhang et al. 2016). The inset highlights the strikingly luminous early excess for SN 2022ywc. The observed ATLAS photometry of SN 2022ywc shown in the lower panel of this figure is available as the data behind the figure. (The data used to create this figure are available.)
Paper: Electromagnetic Precursors to Black Hole–Neutron Star Gravitational Wave Events: Flares and Reconnection-powered Fast Radio Transients from the Late Inspiral
Authors: Elias R. Most, Alexander A. Philippov
Figure caption: Three-dimensional magnetic field line visualization of a flaring event for a GW200115-like binary for a magnetic dipole with θ NS = 30° inclination at a time t ≃ t orbit, where t orbit is the orbital period. Shown are selected field line bundles that highlight the presence of the equatorial current sheet. Unlike larger magnetic dipole inclinations, efficient reconnection in this current sheet self-limits the twist imposed on the flux tubes. The configuration shown here is in a quasi steady state, and no flaring is observed.
Paper: Electromagnetic Precursors to Black Hole–Neutron Star Gravitational Wave Events: Flares and Reconnection-powered Fast Radio Transients from the Late Inspiral
Authors: Elias R. Most, Alexander A. Philippov
Figure caption: Bulk EM luminosity of the flares, ﹩{{ \mathcal L }}_{\mathrm{EM}}﹩. Top: scaling with BH spin, χ BH, relative to the luminosity, ﹩{{ \mathcal L }}_{\mathrm{EM}}^{0}﹩, of the aligned system. Bottom: dependence on orbital separation, a, with absolute magnitudes scaled to a surface field strength B * = 1012 G.
Paper: Electromagnetic Precursors to Black Hole–Neutron Star Gravitational Wave Events: Flares and Reconnection-powered Fast Radio Transients from the Late Inspiral
Authors: Elias R. Most, Alexander A. Philippov
Figure caption: Spherical projection of the average outgoing EM energy flux density of the flares for various inclinations, θ NS, of the NS’s dipole magnetic field extracted at a radius r = 500 km. The background flux has been subtracted. From top left to bottom right, we show cases for θ NS = 30° (top left), 45° (top right), 60° (bottom left), and 90° (bottom right).