adsabs/AstroCLIMB huggingface dataset:
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: The skill scores for selected diagnostic ratios, varying with the time cutoff between a prediction and the flux rope eruption. Axial rope current and flux are denoted I  a  and Φ a  respectively, poloidal rope flux is denoted Φ p , and the reference-based quantities are as defined in Section 2.4. The particular diagnostic ratios in black are selected as they perform well in at least one of the simulation sets.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Top panel: BC B  values for SNe IIb vs. the intrinsic B − V color, where blue (red) symbols correspond to epochs before (after) the maximum of the B − V color. Middle panel: BC B  values shifted by δ BC, where solid lines are polynomial fits. Bottom panel: inverse CDF for the δ BC estimates, where the solid line indicates the mean value. Dashed lines are the ﹩\pm 1\,\hat{\sigma }﹩ limits.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Top panel: UV corrections against the intrinsic B − V color for t − t expl < 40 days. Bottom-left panel: UVC values shifted by δ α UVC, where the solid line is a straight line fit corresponding to Ψ0,UVC. Bottom-right panel: inverse CDF for the δ UVC values, where the solid line is the mean value. Dashed lines are ﹩\pm 1\,\hat{\sigma }﹩ limits, and error bars are 1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Top panel: bolometric light curve of SN 2009jf computed with different band-color combinations (empty symbols). The dotted line is the ALR fit to the weighted-average light curve (black circles). Bottom panel: residuals around the ALR fit. Error bars are 1σ errors due to uncertainties on photometry, while the blue vertical bar depicts the 1σ error at peak due to the error on μ, reddening, and BC. Dashed lines are the ﹩\pm 1\,\hat{\sigma }﹩ limits.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: BC calibrations along with the residuals with respect to the Lyman et al. (2014) and Lyman et al. (2016) calibrations (black lines). Colored solid (dashed) lines are our BC calibrations for times before (after) the epoch of maximum color. The number of SNe used to calibrate the BC is indicated in parentheses. Error bars indicates the 1σ error around our calibrations, while dotted lines indicate the ﹩\pm 1\,\hat{\sigma }﹩ limits of the Lyman et al. (2014) and Lyman et al. (2016) calibrations.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Spectra of SN 2011dh at −14 (top panel) and 15 days (bottom panel) since ﹩{t}_{V}^{\mathrm{peak}}﹩. Colored symbols are monochromatic fluxes computed from observed photometry.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Power-law indices for the JHK (left panel) and YJH (right panel) photometry against the intrinsic V − H. Filled symbols are k values with relative errors lower than 10%. Solid lines are straight line fits to the filled symbols, dashed lines are ﹩\pm 1\,\hat{\sigma }﹩ limits. Error bars are omitted for clarity.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Bolometric SN light curves interpolated with the ALR code (top panels) and normalized to the peak (bottom panels).
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: UV corrections against the intrinsic B − V color for t − t expl > 40 days.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Fractional flux in a given wavelength range as a function of the time since the V-band maximum light.
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: Left: on-sky distribution of stars with >20% probability (gray points) for being Ret II members from Jensen (2023) over the one (solid), two, and three (both dashed lines) half-light-radius ellipses (light gray lines), and highlighting GDR3 0928 (red diamond) and GDR3 1760 (blue square). Positions are given relative to Ret II's R.A. (03:35:42.1) and decl. (–54:02:57.0). Middle: Gaia DR3 G BP − G RP vs. G color–magnitude diagram of the probability >20% stars, with GDR3 0928 and GDR3 1760 highlighted as before. Right: radial velocities and metallicities of Ret II stars from Ji et al. (2023) and the two stars from this paper. The stars from Ji et al. (2023) are shown as points (black), other than their values for GDR3 0928 and GDR3 1760, which have been color coded the same as for our measurements for ease of comparison. The literature value (McConnachie 2012) for the systemic radial velocity of Ret II is also marked (dashed gray line).
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: LTE [X/Fe] abundances for a selection of elements as a function of metallicity. Symbols are for HD 122563 (gray circle), GDR3 1760 (blue square), and GDR3 0928 (red diamond), compared to other Reticulum 2 stars (black points) from Ji et al. (2016b; large points) and Ji et al. (2016b; small points), preferring the abundances from Ji et al. (2016b) for stars in common, except for GDR3 1760 and GDR3 0928, whose measurements are shown when possible. Our NLTE abundances for HD 122563, GDR3 1760, and GDR3 0928 are also shown (open symbols).
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: [X/Fe] abundances in LTE (filled points) and with NLTE corrections applied (open points) as a function of atomic number for HD 122563, GDR3 1760, and GDR3 0928. As seen in other Ret II stars, GDR3 1760 and GDR3 0928 both exhibit neutron-capture element abundances that are enhanced over field stars with a typical r-process-dominated abundance pattern. GDR3 0928 also has enhanced light-element abundances that are not seen in other Ret II stars to date.
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: Spectra of HD 122563, GDR3 1760, and GDR3 0928 around the [O I] λλ6300 and 6363 Å lines, where the stellar O and Fe features have been highlighted with black lines and the telluric lines in each spectrum are identified by the ⊕ symbol. Despite being relatively weak lines intrinsically, these two [O I] features can be seen in GDR3 0928 due to the high abundance of O in this star and are sufficiently unblended with telluric features to provide reliable abundances.
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: Spectra of HD 122563, GDR3 1760, and GDR3 0928, all with similar stellar parameters and metallicities (T eff = 4500–5000 K and [Fe/H] = −2.8 to −2.5) around the Mg b triplet. Notable is the 5165 Å C2 Swan band head and strong Mg b triplet lines in GDR3 0928, while the Fe and Ti lines in this region are relatively comparable to HD 122563 and GDR3 1760.
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: Spectrum of GDR3 0928 compared to synthetic spectra with with our best-fit abundances for lines of different elements, 0.3 dex around the best fit for that line, and without that element. All other elements in the syntheses are held fixed to the final abundance measured for that element.
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: Spectrum of GDR3 0928 around the 5165 Å C2 Swan band head compared to synthetic spectra with no carbon, our best-fit carbon abundance ﹩\mathrm{log}\epsilon =7.95﹩, and 0.1 dex around our best-fit carbon abundance.
Paper: High-energy Electromagnetic, Neutrino, and Cosmic-Ray Emission by Stellar-mass Black Holes in Disks of Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman
Figure caption: The contribution to the background intensity (panel (a)) and the flux from NGC 1068 (panel (b)) for a single neutrino flavor by internal shocks for models M1 (solid black), M2 (black dashed line), and M3 (black dotted line). The observed neutrino intensity (Aartsen et al. 2020a) is presented by red points (panel (a)), and the blue shaded region represents the 1σ, 2σ, and 3σ uncertainty on the spectrum measured by Aartsen et al. (2020b) (panel (b)).
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The EB-correlation phase for models with zero inclination and fluid speed (top row) models with i = 17° while no fluid speed (middle row) and models with i = 17° and nonzero fluid speed (bottom row), respectively. In each row, from left, to right we study different magnetic field morphologies including a radial, toroidal, and mixed magnetic field, respectively. In each panel, we overlay the ring image, on the top right corner, to build a sense of the geometry of the ring. The phase is zero for cases with zero inclination, while it is nonzero for models with nonzero inclination. It is also degenerate between models with different B- and v-field geometries.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: Time-averaged images of MAD simulations with different BH spins. From top to bottom, we present the total intensity (I), fractional linear polarization (P/I), and the Stokes Q parameter. As expected, the images show a clear handedness in their EVPAs.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: A family of different Gaussian models. For a single Gaussian model (top panel), the phase of the EB correlation is either zero or 180°. In a double Gaussian model (middle panel), with the same EVPA ticks, the phase remains the same despite the brightness asymmetry. Finally, for a double Gaussian model with different EVPA ticks, the bottom panel, the phase gets non-vanished owing to the polarization anisotropies.
Paper: High-energy Electromagnetic, Neutrino, and Cosmic-Ray Emission by Stellar-mass Black Holes in Disks of Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman
Figure caption: The parameter range for efficient particle acceleration on the Γj–L j,iso plane for Γ12 = 4 and T vari = 10−3 s. The parameters adopted for models M1–M3 are represented by orange, cyan, and red circles, respectively.
Paper: High-energy Electromagnetic, Neutrino, and Cosmic-Ray Emission by Stellar-mass Black Holes in Disks of Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman
Figure caption: Same as Figure 4, but with parameters varied from the fiducial model (model M1) as indicated in the legend.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The polarized image of M87* from EHT 2017 data on April 6 and April 11 as well as the EB-correlation phase in the visibility space (bottom).
Paper: High-energy Electromagnetic, Neutrino, and Cosmic-Ray Emission by Stellar-mass Black Holes in Disks of Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman
Figure caption: Same as Figure 5, but with parameters varied from model M2 as indicated in the legend.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The comparison between the imaginary part of the EB correlation in SANE simulations from the full numeric as well as with different m-order cuts. From top to bottom, we present the full numeric, the case with m cut = 2, m cut = 3, and m cut = 4, respectively.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The real, imaginary, and the phase of the gridded EB-correlation function for the EHT 2017 data for 3598 (first row) and 3601 (second row) and the time-averaged GRMHD MAD simulations with a = 0.0 and a = +0.5 spins, respectively. The phase map in the EHT data contains both dark and bright regions, which is similar to the MAD with a = 0.0 in the dark regions while similar to MADs with a = +0.5 for the bright regions.