adsabs/AstroCLIMB huggingface dataset:
Paper: A Comparative Study of Solar Active Region 12371 with Data-constrained and Data-driven Magnetohydrodynamic Simulations
Authors: Satoshi Inoue, Keiji Hayashi, Takahiro Miyoshi, Ju Jing, Haimin Wang
Figure caption: (a) The temporal evolution of the magnetic energy obtained from Run A (red) and Run B (blue). The vertical value is normalized by the initial value at t = 0 in the horizontal axis that corresponds to the NLFFF extrapolated at 16:36 UT. (b) The temporal evolution of the magnetic flux that satisfies T  w  ≤ −1.0. The format is the same as in (a). The vertical axis is normalized by the initial value that corresponds to 1.4 × 1021[Mx]. The dashed horizontal line sets the value at which the magnetic flux in Run B saturates. (c)−(d) The magnetic field lines projected in the x − z plane are plotted for Runs A and Run B where B 0 = 0.28(T) and L −1 = 1/(L 0) = 2.9 × 10−9[1/m], where L 0 = 345 (Mm).
Paper: A Comparative Study of Solar Active Region 12371 with Data-constrained and Data-driven Magnetohydrodynamic Simulations
Authors: Satoshi Inoue, Keiji Hayashi, Takahiro Miyoshi, Ju Jing, Haimin Wang
Figure caption: (a) Extreme ultraviolet 131 Å image obtained from AIA at 17:39 UT, which corresponds to the onset time of an M6.5 flare, is exhibited. The arrow indicates the location where the M6.5 flare occurred. The insert shows the photospheric magnetic field at 16:36 UT, which is used as the boundary condition of the simulations. The white and black colors represent the positive and negative polarities, respectively, where B 0 = 0.28(T). (b) The AIA image of AR 12371 observed at 16:36 UT. The field of view corresponds to the area enclosed by the red square in (a). (c) The 3D magnetic field lines that are plotted are extrapolated under a force-free assumption. The color of the field lines corresponds to the magnitude of the current density ﹩| {\boldsymbol{J}}| =\sqrt{{J}_{x}^{2}+{J}_{y}^{2}+{J}_{z}^{2}}﹩. These field lines are superimposed on the AIA image shown in (b). J 0 = B 0/(μ 0 L 0) = 6.5 × 10−4[A ﹩{m}^{-2}﹩                      ], where L 0 = 345 (Mm) and μ 0( = 4π × 10−7) is the magnetic permeability in free space. (d) Summary of Runs A–C. The light blue and dark blue circles correspond to the NLFFF and the magnetic field produced by the data-driven simulation, respectively. The light blue arrow means that the boundary is driven by the time-varying electric field (data-driven simulation), while the purple arrow means that the electric field is turned off (data-constrained simulation).
Paper: A Comparative Study of Solar Active Region 12371 with Data-constrained and Data-driven Magnetohydrodynamic Simulations
Authors: Satoshi Inoue, Keiji Hayashi, Takahiro Miyoshi, Ju Jing, Haimin Wang
Figure caption: (a)–(b) The magnetic fields (NLFFF) that are extrapolated from the photospheric magnetic fields obtained at 16:36 UT and 17:24 UT. (c) The top view of the NLFFF at 17:24 UT. (d)–(e) The temporal evolution of the magnetic field lines during the data-driven MHD simulation. The vertical cross section plots ∣ J ∣/∣ B ∣. (f) The top view of (e). B 0 = 0.28(T) and L −1 = 1/(L 0) = 2.9 × 10−9[1/m] where L 0 = 345 (Mm).
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: Observed argon emission-line profiles for SN 2021aefx at +255 days (black) compared to model line emission from a Gaussian emission distribution for [Ar II] 6.985 μm (top); a thick uniform shell or hollow uniform sphere emission distribution for [Ar III] 8.991 μm with an inner radius corresponding to ﹩{v}_{\min }=8700\pm 200﹩ km s−1, and an outer radius corresponding to ﹩{v}_{\max }={\rm{13,500}}\pm 300﹩ km s−1 (bottom); and a thick shell distribution for [Ar II] 6.985 μm, which has been forced to have the same inner and outer radius as the [Ar III] fit (middle). The model profile for the central line is shown in dotted red, with contributions from other lines shown in dotted blue and the full modeled superposition of lines shown in solid blue.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: MIR line identifications for our JWST/MIRI spectrum of SN 2021aefx (black) at +255 days. We compare to scaled Spitzer/IRS MIR spectra of SN 2005df (red) at +117 days and SN 2003hv (green) at +359 days (Gerardy et al. 2007), SN 2006ce (blue) +127 days, and a MIR spectrum from GTC/CanariCam of SN 2014J (orange) at +121 days (Telesco et al. 2015). All phases are given in rest-frame days relative to B                      ﹩{}_{\max }﹩. The JWST/MIRI spectrum shows impressive improvement in S/N, allowing for additional identification of weaker lines. The dominant emission lines are marked in gray, with uncertain line identifications marked in light gray. Details of the MIR lines can be found in Table 2.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: Cobalt emission-line profiles of SN 2021aefx at +255 days (black) across the optical, NIR, and MIR compared with model line emission from Gaussian distributions of emission. The model profile for the central line is shown in dashed red, with contributions from other lines shown in dashed blue and the full modeled superposition of lines shown in solid blue.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: Observed NIR and MIR nickel emission-line profiles for SN 2021aefx at +255 days (black) compared to model line emission from Gaussian distributions, except for [Ni IV] 8.405 μm, which is better fit by emission from a uniform spherical emission distribution. The model profile for the central line is shown in dashed red, with contributions from other lines shown in dashed blue and the full modeled superposition of lines shown in solid blue.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: Optical + NIR emission-line profiles of SN 2021aefx at +255 days (black) for complex spectral features dominated by iron. The model profile for the central line is shown in dashed red, with contributions from other lines shown in dashed light red and dashed light blue, and the full modeled superposition of lines shown in solid blue.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: FWHM vs. kinematic offset for species with fitted line profiles in Section 4. MIR lines (red) are compared against NIR lines (blue) and optical lines (gray). Error bars show fit uncertainties, in combination with wavelength calibration uncertainties for the MIR lines, and take into account instrument resolution. Low opacity points represent uncertain line identifications. Values and errors for these measurements are given in Table 2.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: NIR emission-line profiles of SN 2021aefx at +255 days (black) for the 3 μm region features. The model profile for the central line is shown in dashed red, with contributions from other lines shown in dashed blue and the full modeled superposition of lines shown in solid blue.
Paper: A JWST Near- and Mid-infrared Nebular Spectrum of the Type Ia Supernova 2021aefx
Authors: Lindsey A. Kwok, Saurabh W. Jha, Tea Temim, Ori D. Fox, Conor Larison, Yssavo Camacho-Neves, Max J. Brenner Newman, Justin D. R. Pierel, Ryan J. Foley, Jennifer E. Andrews, Carles Badenes, Barnabas Barna, K. Azalee Bostroem, Maxime Deckers, Andreas Flörs, Peter Garnavich, Melissa L. Graham, Or Graur, Griffin Hosseinzadeh, D. Andrew Howell, John P. Hughes, Joel Johansson, Sarah Kendrew, Wolfgang E. Kerzendorf, Keiichi Maeda, Kate Maguire, Curtis McCully, John T. O'Brien, Armin Rest, David J. Sand, Melissa Shahbandeh, Louis-Gregory Strolger, Tamás Szalai, Chris Ashall, E. Baron, Chris R. Burns, James M. DerKacy, Tyco Mera Evans, Alec Fisher, Lluís Galbany, Peter Hoeflich, Eric Hsiao, Thomas de Jaeger, Emir Karamehmetoglu, Kevin Krisciunas, Sahana Kumar, Jing Lu, Justyn Maund, Paolo A. Mazzali, Kyle Medler, Nidia Morrell, Mark. M. Phillips, Benjamin J. Shappee, Maximilian Stritzinger, Nicholas Suntzeff, Charles Telesco, Michael Tucker, Lifan Wang
Figure caption: JWST/NIRSpec line identifications in the 3 μm region, previously unobserved for SN Ia. The main line features arise from [Fe III] 2.874 and 2.905 μm, and [Ni I] 3.120 μm and [Fe III] 3.229 μm emission (gray). Several possible weaker lines that may be blended with the dominant lines are shown in light gray. Details of the dominant lines can be found in Table 2.
Paper: Discovery of a Dusty, Chemically Mature Companion to a z ∼ 4 Starburst Galaxy in JWST ERS Data
Authors: Bo Peng, Amit Vishwas, Gordon Stacey, Thomas Nikola, Cody Lamarche, Christopher Rooney, Catie Ball, Carl Ferkinhoff, Henrik Spoon
Figure caption: Left: Hα pseudo-narrowband image of the SPT0418 system, averaged over the channels including the Hα emission in the original spectral cube. The strongly lensed ring and the two newly discovered sources (SE-1 and SE-2) are highlighted by a red annulus and gray and black ellipses, marked as “A,” “B,” and “C,” respectively. The lensing galaxy is shown as the central bright source. The 835 μm continuum is plotted as the thin black contours, with the levels 2, 4, 8, 16, 32 × σ where σ = 56.7 μJy beam −1. Right: the spectra of the three sources integrated over the regions highlighted in the left panel, using the same color scheme. The spectrum for the ring is scaled by a factor of 0.1 for clarity. The small black bar below the Hα line marks the wavelength coverage of the pseudo-narrowband image. The potentially detected lines are marked by vertical dotted lines.
Paper: Discovery of a Dusty, Chemically Mature Companion to a z ∼ 4 Starburst Galaxy in JWST ERS Data
Authors: Bo Peng, Amit Vishwas, Gordon Stacey, Thomas Nikola, Cody Lamarche, Christopher Rooney, Catie Ball, Carl Ferkinhoff, Henrik Spoon
Figure caption: The moment 0 map and spectrum snippets of the strong emission lines. For each strong line(s), the lens-subtracted, continuum-subtracted moment 0 map is displayed in the first row, with the same marked regions as in Figure 1. The spectrum snippets are shown in the second row, integrated over the three regions. The spectra are offset vertically to aid vision, with the zero baseline indicated by a thin black line. The green dashed line indicates the Gaussian fit to the line or line associations plus the linear fit to the local continuum. The labeling style and color of the spectrum are the same as Figure 1.
Paper: Discovery of a Dusty, Chemically Mature Companion to a z ∼ 4 Starburst Galaxy in JWST ERS Data
Authors: Bo Peng, Amit Vishwas, Gordon Stacey, Thomas Nikola, Cody Lamarche, Christopher Rooney, Catie Ball, Carl Ferkinhoff, Henrik Spoon
Figure caption: Atlas of lens-subtracted NIRCam and MIRI images in the wavelength range λ obs = 1.15–10 μm, corresponding to λ rest = 0.22–1.9 μm. The filter is shown as the title of each stamp. The images are oriented and cropped to fit the image stamps in the previous images, as are the highlighted regions and color scheme. The color map is adjusted manually to increase the contrasts of the weak sources.
Paper: PHANGS–JWST First Results: Duration of the Early Phase of Massive Star Formation in NGC 628
Authors: Jaeyeon Kim, Mélanie Chevance, J. M. Diederik Kruijssen, Ashley. T. Barnes, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Enrico Congiu, Daniel A. Dale, Oleg V. Egorov, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Annie Hughes, Ralf S. Klessen, Kathryn Kreckel, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daizhong Liu, Steven N. Longmore, Sharon E. Meidt, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Erik Rosolowsky, Toshiki Saito, Karin Sandstrom, Eva Schinnerer, Rowan J. Smith, Antonio Usero, Elizabeth J. Watkins, Thomas G. Williams
Figure caption: The left panel shows the measured deviation of gas-to-SFR tracer (CO-to-21 μm) flux ratios compared to the galactic average as a function of the size of apertures centered on CO and 21 μm emission peaks. The data underlying this figure can be found in Appendix B. The error bars show the 1σ uncertainty of each measurement whereas the shaded region within the error bar indicates the effective 1σ error, considering the covariance between data points. Our best-fitting model (dashed line), as well as the galactic average (horizontal line) are also shown. The constrained λ is indicated with a downward arrow and other best-fitting parameters (t 21 μm and t fb,21 μm) are listed in Table 1. The right panel illustrates the evolutionary sequence from inert molecular clouds to embedded star formation, partially exposed star formation, and finally to fully revealed young stellar regions. The duration of the CO emitting phase (t CO) is shown in orange while the time during which 21 μm and Hα emission are detected without associated CO emission are shown in dark blue and dark purple, respectively. The feedback timescale, which is the time for which both CO and an SFR tracer are found coincident, is shown in light blue (for 21 μm) and light purple (for Hα). The error bars indicate the 1σ uncertainty for each measurement.
Paper: Discovery of an Isolated Dark Dwarf Galaxy in the Nearby Universe
Authors: Jin-Long Xu, Ming Zhu, Naiping Yu, Chuan-Peng Zhang, Xiao-Lan Liu, Mei Ai, Peng Jiang
Figure caption: Morphology of dark galaxy FAST J0139+4328. (a) H I  column-density map from the FAST observation shown in white contours overlaid on the Pan-STARRS1 g-band image in color scale. The white contours begin at 3.0 × 1018 cm−2 (3σ) in steps of 1.9 × 1018 cm−2. The red dashed circle represents three times the expected D 25. (b) the global H I  profile of FAST J0139+4328. The blue dashed line indicates the BusyFit fitting result. The red and blue vertical lines mark the positions of the double peak. (c) position–velocity (PV) diagram in color scale overlaid with the cyan contours. The cyan contours begin at 2σ (1.8 mJy beam−1) in steps of 1σ. The blue dashed contours represent the PV diagram from the TiRiFiC fitting.
Paper: Discovery of an Isolated Dark Dwarf Galaxy in the Nearby Universe
Authors: Jin-Long Xu, Ming Zhu, Naiping Yu, Chuan-Peng Zhang, Xiao-Lan Liu, Mei Ai, Peng Jiang
Figure caption: (a) Baryonic Tully–Fisher relation (BTFR). The black dashed line represents a best-fit relation ﹩{M}_{\mathrm{bar}}={{AV}}_{\mathrm{rot}}^{4}﹩ with A = 47 ± 6 M ⊙km−4s4, and gas-dominated galaxies are marked by black points (McGaugh 2012). The red point represents the discovered dark galaxy FAST J0139+4328. (b) Relation between the H I  mass-to-light ratio and absolute B-band magnitude. The low surface brightness galaxies are obtained from Honey et al. (2018), while almost dark galaxies from Cannon et al. (2015), Janowiecki et al. (2015), Brunker et al. (2019), and Leisman et al. (2017), Leisman et al. (2021).
Paper: Discovery of an Isolated Dark Dwarf Galaxy in the Nearby Universe
Authors: Jin-Long Xu, Ming Zhu, Naiping Yu, Chuan-Peng Zhang, Xiao-Lan Liu, Mei Ai, Peng Jiang
Figure caption: Images of dark galaxy FAST J0139+4328 in different bands. (a) Optical emission from the Pan-STARRS1 g-band data. (b) Near-infrared K-band emission from the 2MASS data. (c) Near-ultraviolet (NUV) emission from the GALEX data. (d) Mid-infrared emission (W4, 22 μm) from the WISE data. Fluxes in each band are on an arbitrary unit. The red solid and dashed circles represent the expected D 25 and the three times D 25 in each panel, respectively. The black ellipses mark optical stars in the Galaxy identified from the Gaia star catalog.
Paper: Density Profiles of Collapsed Rotating Massive Stars Favor Long Gamma-Ray Bursts
Authors: Goni Halevi, Belinda Wu, Philipp Mösta, Ore Gottlieb, Alexander Tchekhovskoy, David R. Aguilera-Dena
Figure caption: Evolutions of several key quantities (from top to bottom: the central density, shock radius, and mass of the inner core) with time after the core bounce for all seven models. The shock radius r shock is defined as the place where the radial velocity exceeds the sound speed and the inner core is the region within this radius, so ﹩{M}_{\mathrm{core}}\equiv M(r\lt {r}_{\mathrm{shock}})﹩. Models that form BHs in our simulations are represented by solid lines, while models that do not are shown by dashed–dotted lines. The inset in the middle panel zooms in on the shock radius evolutions for the three models that do not form BHs, two of which experience a brief shock revival stage.
Paper: Density Profiles of Collapsed Rotating Massive Stars Favor Long Gamma-Ray Bursts
Authors: Goni Halevi, Belinda Wu, Philipp Mösta, Ore Gottlieb, Alexander Tchekhovskoy, David R. Aguilera-Dena
Figure caption: Initial (pre-core-collapse) and final density profiles for all seven stellar models. The initial profiles are shown by the dashed lines. For the final profiles, we use solid lines for the models that collapse to form BHs in our simulations and we use dashed–dotted lines for those that do not. Representative power-law scalings are shown by dotted black lines, for comparison. While all pre-collapse stellar models have steep density profiles (α ≈ 2.5), all post-collapse profiles are shallow (α ≈ 1.45). Stellar models that are initially inconsistent with lGRB observables evolve robustly to the post-collapse state that is necessary for jet properties that are consistent with observations, showing that massive stars that have undergone CHE are likely lGRB progenitors under the collapsar model.