adsabs/AstroCLIMB huggingface dataset:
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: Comparison of the SN peak time and FXT properties of several FXT events with SN counterparts (SNe 1998bw, 2006aj, 2008D, 2010bh, 2024gsa, and 2025kg). EP 250108a/SN 2025kg is marked with a pink star in the first two rows. We caution that the different instruments’ bandpasses and slewing strategies impact both the X-ray peak luminosities and durations, making direct comparisons inadvisable. However, the span of several orders of magnitude in some parameters mitigate some of these biases.
Paper: Nonstandard Collapse of Strong Langmuir Turbulence: Constraints on Its Occurrence and Observation in the Solar Corona
Authors: Yaokun Li, Haomin Sun, Hao Ning, Sulan Ni, Xiangliang Kong, Jiansen He, Yao Chen
Figure caption: (a)–(b) Spatial distribution of the normalized energy density W and proton density fluctuation δnp in Case 1. (c)–(d) The corresponding distribution of W and δnp in Case 2. The rectangle outlines the locations of wave packets (#1–#3) shown in Figures 2–4.
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: Our spectroscopic sequence of SN 2025kg. We observe broad absorption features around ∼5000 Å and ∼6100 Å that we ascribe to Fe II λ5169 and Si λ6355. In the spectrum at δt = 42.5 days we observe broadened Hα emission. We mark the location of a telluric feature with a ⊕.
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: The JWST/NIRSpec spectrum of SN 2025kg (pink) and the near-IR spectrum of SN 1998bw (black; binned to mitigate telluric noise in the spectrum) in velocity space around the 1 μm (upper) and 2 μm (lower) features. We show our combined fit (gray dashed) and individual contributions to the 1 μm feature due to C I (1.0693 μm and 2.1259 μm; dotted turquoise) and He I (λ10830 and λ20587; dotted blue) absorption. We also mark the velocity derived from a single Gaussian fit to the 1 μm feature with a vertical gray line. In the top spectrum, the superposition of the C I and He I absorption provides a strong fit to the observed feature. Our analysis (Section 3.4) shows that a small (≲0.5 M⊙) amount of He is likely present in SN 2025kg.
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: Comparison of SN 2025kg spectra (pink) to SN 1998bw (black; F. Patat et al. 2001), and three SNe associated with FXTs (blue), SN 2006aj (E. Pian et al. 2006), SN 2008D (M. Modjaz et al. 2009, 2014), and SN 2010bh (F. Bufano et al. 2012) around their SNe peak. We also show a spectrum of the Type Ic-BL SN 2020bvc (D. Hiramatsu et al. 2020) taken ∼1.9 days postexplosion. We label the approximate locations of Fe II λ5169 and Si λ6355. Due to its broad-lined features and lack of He lines (labeled in SN 2008D) SN 2025kg is comparable to SN 1998bw and SN 2006aj.
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: Images of the 2D (top) and 1D (bottom) GMOS spectrum of SN 2025kg taken at δt = 42.5 days, centered around Hα λ6562.8. For comparison, we show our other GMOS spectra in gray, which show only the narrow Hα component. In addition to the narrow component, which is present in other epochs (Figure 2) and likely due to the underlying host galaxy, we observe broad, underlying emission, indicating an H-rich source is interacting with SN 2025kg at this epoch. We show an orange Gaussian superimposed on the continuum for visual purposes.
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: Optical–near-IR detections (circles) and upper limits (triangles) of the counterpart to EP 250108a. The data at δt > 6 days are well described by a one-zone radioactive decay model (lines; W. D. Arnett 1982; N. Sarin et al. 2024) with a 56Ni mass of 0.6 ± 0.1 M⊙ (Section 4). Observations during the fast-cooling phase prior to the emergence of SN 2025kg (δt < 6 days; open symbols and gray vertical band) are discussed in detail in R. A. J. Eyles-Ferris et al. (2025). We also show the times of the spectroscopic observations with black vertical lines at the bottom of the figure.
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: The JWST spectrum of SN 2025kg near maximum light. In the top and bottom panels we show the 1D spectrum and the S/N, respectively. In the top panel, we highlight the three features discussed in detail in Section 3.4 (the 1 μm and 2 μm features) and Section 3.5 (the 4–4.5 μm feature, shown in the inset panel).
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: Light-curve comparison of SN 2025kg (pink circles) and SNe associated with FXTs (blue), GRB-SNe (gray diamonds), Type Ic-BL SNe observed without GRB counterparts (dark gray diamonds), and Type Ib/c SNe (light gray diamonds). Observations are corrected for Milky Way extinction (E. F. Schlafly & D. P. Finkbeiner 2011) and presented in the nearest rest-frame band using the event’s known redshift. The light curve of SN 2025kg strongly resembles those of SN 1998bw, SN 2006aj, and SN 2024gsa in its peak luminosity and temporal evolution.
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: Si λ6355 velocities of SN 2025kg (pink circles) along with literature values for GRB-SNe, FXT-SNe, and Type Ic-BL SN 2002ap (R. Chornock et al. 2010). SN 2025kg is comparable in absorption velocity to SNe 1998bw and 2006aj.
Paper: EP 250108a/SN 2025kg: Observations of the Most Nearby Broad-line Type Ic Supernova Following an Einstein Probe Fast X-Ray Transient
Authors: Jillian C. Rastinejad, Andrew J. Levan, Peter G. Jonker, Charles D. Kilpatrick, Christopher L. Fryer, Nikhil Sarin, Benjamin P. Gompertz, Chang Liu, Rob A. J. Eyles-Ferris, Wen-fai Fong, Eric Burns, James H. Gillanders, Ilya Mandel, Daniele Bjørn Malesani, Paul T. O'Brien, Nial R. Tanvir, Kendall Ackley, Amar Aryan, Franz E. Bauer, Steven Bloemen, Thomas de Boer, Clécio R. Bom, Jennifer A. Chacón, Ken Chambers, Ting-Wan Chen, Ashley A. Chrimes, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Michael D. Fulton, Paul J. Groot, Rahul Gupta, Dieter H. Hartmann, Agnes P. C. van Hoof, Mark E. Huber, Luca Izzo, Wynn Jacobson-Galan, Páll Jakobsson, Albert Kong, Tanmoy Laskar, Thomas B. Lowe, Eugene A. Magnier, Elisabetta Maiorano, Antonio Martin-Carrillo, Lluis Mas-Ribas, Daniel Mata Sánchez, Matt Nicholl, Christopher J. Nixon, Samantha R. Oates, Gregory Paek, Jesse Palmerio, Diego Paris, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan A. Quirola Vasquez, Jan van Roestel, Andrea Rossi, Alicia Rouco Escorial, Ruben Salvaterra, Benjamin Schneider, Stephen J. Smartt, Ken Smith, Ian A. Smith, Shubham Srivastav, Manuel A. P. Torres, Chiara Ventura, Paul Vreeswijk, Richard Wainscoat, Yi-Jung Yang, Sheng Yang
Figure caption: Spectra of SN 2025kg centered around Hα at δt = 42.5 and 47.7 days binned at 40 Å (pink) in which regions affected by the telluric and narrow Hα have been removed. We observe a broadened Hα emission feature in the SN 2025kg Gemini-South/GMOS spectrum at δt = 42.5 days. We observe broadened Hα in the ESO/NTT spectrum of AT 2018cow (green) but not in the Danish/DFOSC spectrum of SN 1998bw (black) at similar epochs.
Paper: Understanding the Magnetic Field and Plasma-β along Umbral Fan Loops Traced Using 3 Minute Slow Waves
Authors: Ananya Rawat, Girjesh Gupta, Tom Van Doorsselaere, S. Krishna Prasad, Robertus Erdélyi
Figure caption: Images of sunspot and fan loops belonging to AR 12470 obtained from different AIA, IRIS, and HMI passbands as labeled. The red lines on the AIA 171 Å image represent the manual tracing of coronal fan loops 1 and 2, and asterisk symbols (*) represent their coronal footpoints. The yellow dashed lines represent the background regions for those loops. The sample slits across coronal Loop 2 are marked with solid red lines and numbered. The box enclosing the coronal footpoint of Loop 2 indicates the region chosen to identify loop locations at the lower atmospheric heights. Small open circles over different panels represent the loop locations identified at that atmospheric height (see details in Section 3.3). Contours over different panels indicate the umbra–penumbra boundary as obtained from the IRIS 2832 Å image.
Paper: Understanding the Magnetic Field and Plasma-β along Umbral Fan Loops Traced Using 3 Minute Slow Waves
Authors: Ananya Rawat, Girjesh Gupta, Tom Van Doorsselaere, S. Krishna Prasad, Robertus Erdélyi
Figure caption: Left: DEM profiles at the coronal footpoint of Loop 2 shown by the asterisk in Figure 1. The green and blue curves are obtained with and without background-subtracted intensities, respectively. Right: temperature (left y-axis) and total number density (right y-axis) as a function of loop length shown by asterisks (*) and diamonds (⋄), respectively. Temperatures and densities from the photosphere to the corona are obtained from the sunspot model of J. Fontenla et al. (1999) and shown by blue lines, whereas those in the corona are obtained using DEM analysis and shown by red symbols. The green lines overplotted over coronal temperature and density represent average loop temperature and a fitted exponentially decaying function, respectively.
Paper: Understanding the Magnetic Field and Plasma-β along Umbral Fan Loops Traced Using 3 Minute Slow Waves
Authors: Ananya Rawat, Girjesh Gupta, Tom Van Doorsselaere, S. Krishna Prasad, Robertus Erdélyi
Figure caption: Left: variation of plasma-β along the fan loops belonging to AR 12470, where the light and dark blue shaded regions are for loops 1 and 2, respectively. Right: variation of plasma-β along the fan loops belonging to AR 12553 where the light blue, dark blue, and pink shaded regions are for loops 3, 5, and 6, respectively. The black solid lines represent data points extracted from G. A. Gary (2001) for the umbral region. The vertical green dashed lines indicate the plasma-β = 1 layer. The orange dashed lines are the linear extrapolation of data points to determine the plasma-β = 1 layer. The small boxes in the lower-left corners show the height at which loops 2 and 5 cross the plasma-β ≈ 1 layer as representative examples.
Paper: Understanding the Magnetic Field and Plasma-β along Umbral Fan Loops Traced Using 3 Minute Slow Waves
Authors: Ananya Rawat, Girjesh Gupta, Tom Van Doorsselaere, S. Krishna Prasad, Robertus Erdélyi
Figure caption: Left: cross-sectional area of the loop along its length. The area of the loop in the lower solar atmosphere is fitted with an exponentially rising function, shown by a blue solid line. The area along the coronal loop is also fitted with an exponentially rising function with a constant background, shown by the red solid line. Obtained area scale heights (λA) are printed in their respective color code at the top-left corner. The green line represents the equivalent diameter (w) of the loop along its length (right axis). Right: variation of magnetic field strength (left axis) and Alfvén wave speed (right axis) along the loop. The green open circle represents the rms magnetic field strength obtained from the HMI magnetogram.
Paper: Understanding the Magnetic Field and Plasma-β along Umbral Fan Loops Traced Using 3 Minute Slow Waves
Authors: Ananya Rawat, Girjesh Gupta, Tom Van Doorsselaere, S. Krishna Prasad, Robertus Erdélyi
Figure caption: Correlation images obtained between various atmospheric heights, as labeled. In each panel, the red asterisk symbol (*) in the center refers to the coronal footpoint of Loop 2, and the red circle in first panel represents the cross section of the loop obtained from the AIA 171 Å image using the FWHM method. Overplotted black contours are obtained at ≈94 ± 2% of maximum correlation values. The green open diamond symbols represent the locations of the maximum correlated pixel and the loop location at that height.
Paper: Understanding the Magnetic Field and Plasma-β along Umbral Fan Loops Traced Using 3 Minute Slow Waves
Authors: Ananya Rawat, Girjesh Gupta, Tom Van Doorsselaere, S. Krishna Prasad, Robertus Erdélyi
Figure caption: Intensity profiles along several slits across the coronal Loop 2 marked in Figure 1, as observed in the AIA 171 Å passband. All intensity profiles are fitted with the Gaussian function with a linear background. The obtained FWHM of the Gaussian function represents the diameter of the coronal loop along its length.