adsabs/AstroCLIMB huggingface dataset:
Paper: Implications from the Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating Black Hole Magnetosphere
Authors: Motoki Kino, Masaaki Takahashi, Tomohisa Kawashima, Jongho Park, Kazuhiro Hada, Hyunwook Ro, Yuzhu Cui, 玉竹 崔
Figure caption: We show the ﹩{ \mathcal E }﹩ dependence of u  p .
Paper: Implications from the Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating Black Hole Magnetosphere
Authors: Motoki Kino, Masaaki Takahashi, Tomohisa Kawashima, Jongho Park, Kazuhiro Hada, Hyunwook Ro, Yuzhu Cui, 玉竹 崔
Figure caption: We show the Ω dependence of u  p .
Paper: Implications from the Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating Black Hole Magnetosphere
Authors: Motoki Kino, Masaaki Takahashi, Tomohisa Kawashima, Jongho Park, Kazuhiro Hada, Hyunwook Ro, Yuzhu Cui, 玉竹 崔
Figure caption: Same as Figure 2 but with q = 1.7.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: Overview of event (5), which occurred on 2016 November 5. (a) A full-disk solar image at the Hα-center wavelength observed by SMART/SDDI. Celestial north is up, and west is to the right. The orange dashed−dotted region corresponds to the images in Figure 9(b), and the blue solid region is a QR. The direction of the solar north is shown by the white arrow labeled SN. (b) The time evolution of the filament eruption on 2016 November 5. The field of view in each panel corresponds to the orange dashed−dotted region in Figure 9(a). In each row, images at the times t = 9, 54, and 90 minutes measured from 02:41 UT on 2016 November 5 are shown from top to bottom. In each column, the images AIA 304 Å, Hα − 1.0 Å, Hα center, and Hα + 1.0 Å are shown from left to right. The red dashed region indicated in the Hα center image at t = 9 minutes is a TR. The red arrow in the Hα − 1.0 Å image at t = 54 minutes indicates the upward motion of the filament eruption. The red arrow in the Hα + 1.0 Å image at t = 54 minutes indicates the plasma downflow associated with the filament eruption.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: Overview of event (6), which occurred on 2017 February 19. (a) A full-disk solar image at the Hα-center wavelength observed by SMART/SDDI. Celestial north is up, and west is to the right. The red dashed region is a TR, and the blue solid region is a QR. The direction of the solar north is shown by the white arrow labeled SN. (b) The time evolution of the filament eruption on 2017 February 19. The field of view in each panel corresponds to the TR in Figure 12(a). In each row, images at the times t = 1, 9, and 39 minutes measured from 05:11 UT on 2017 February 19 are shown from top to bottom. In each column, the images AIA 304 Å, Hα − 1.0 Å, Hα center, and Hα + 1.0 Å are shown from left to right. The pink arrows indicate plasma downflows associated with the filament eruption.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: Overview of event (8), which occurred on 2017 June 19. (a)A full-disk solar image at the Hα-center wavelength observed by SMART/SDDI. Celestial north is up, and west is to the right. The orange dashed−dotted region corresponds to the images in Figure 16(b). The direction of the solar north is shown by the white arrow labeled SN. (b) The time evolution of the filament eruption on 2017 June 19. The field of view in each panel corresponds to the orange dashed−dotted region in Figure 16(a). In each row, images at the times t = 2, 15, and 20 minutes measured from 04:30 UT 2017 June 19 are shown from top to bottom. In each column, the images Hα − 1.0 Å, Hα center, and Hα + 1.0 Å are shown from left to right. The red dashed region in the Hα center image at t = 2 minutes is a TR, and the blue solid region is a QR.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: The same as Figure 2, but for event (6), the filament eruption and the two-ribbon flare on 2017 February 19. In addition to the differenced equivalent widths of Hα ± 3.0 Å, the differenced equivalent widths of Hα ± 0.5 Å are also plotted as gray triangles in panel (b), as in Figure 10(b).
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: Overview of event (7), which occurred on 2017 April 23. (a) A full-disk solar image at the Hα-center wavelength observed by SMART/SDDI. Celestial north is up, and west is to the right. The red dashed region is a TR, and the blue solid region is a QR. The direction of the solar north is shown by the white arrow labeled SN. (b) The time evolution of the filament eruption on 2017 April 23. The field of view in each panel corresponds to the TR in Figure 14(a). In each row, images at the times t = 5, 38, and 44 minutes measured from 05:00 UT on 2017 April 23 are shown from top to bottom. In each column, the images AIA 304 Å, Hα − 1.0 Å, Hα center, and Hα + 1.0 Å are shown from left to right.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: The same as Figure 2, but for event (7), the filament eruption and the two-ribbon flare on 2017 April 23. In addition to the differenced equivalent widths of Hα ± 3.0 Å, the differenced equivalent widths of Hα ± 0.5 Å are also plotted as gray triangles in panel (b), as in Figure 10(b) and Figure 13(b). We note that only Hα ± 3.0 Å data were available for performing the Sun-as-a-star analysis in this event.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: The same as Figure 2, but for the event (5), the filament eruption on 2016 November 5. In addition to the differenced equivalent widths of Hα ± 3.0 Å, the differenced equivalent widths of Hα ± 0.5 Å are also plotted as gray triangles in panel (b).
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: The same as Figure 2, but for event (8), the prominence eruption on 2017 June 19. We note that the peak time of GOES soft X-ray (1−8 Å) is before 2017 June 19 04:30 UT.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: The contributions to the differenced equivalent widths from the filament eruption and the two-ribbon flare. The differenced equivalent widths of Hα ± 0.5 Å for the filament eruption are plotted as gray triangles and for the two-ribbon flare as light gray circles. The GOES X-ray (1−8 Å) flux is also plotted as a blue dashed line.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: HCN and HNC column density (left axis) and column density ratio (right axis) as a function of CRIR ζ and mechanical heating rate Γmech from the PDR models presented by Meijerink et al. (2011). Volume density ﹩{n}_{{{\rm{H}}}_{2}}﹩ and far-UV radiation field intensity G0 are fixed at 105.5 cm−3 and 105 Habing, respectively, in these models.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: HCN integrated intensity (moment-0) images toward NGC 253. For each image, the green circle in the lower-left corner shows the final imaged beam size (1.″6). White-bordered numbers indicate the locations of the dense molecular emission regions identified by Leroy et al. (2015, Table 4). The yellow black-bordered square locates the position of the strongest radio continuum emission peak identified by Turner & Ho (1985b, TH2: R.A.(J2000) = 00h47m33s.18, Decl. (J2000) = ﹩-25^\circ 17^{\prime} 16\buildrel{\prime\prime}\over{.} 93﹩). A scale bar in the lower right of each panel provides the physical scale in parsecs for each image. The lower integrated intensity limit for each transition is set to 3σ (see Table 1). Overlaid in contours is the associated continuum emission distribution for each transition. Continuum contours are in steps of 3, 6, 9, 12, 30, 120, 240, and 900 times the respective continuum rms, where the peak continuum intensity dictates the number of these levels actually used for a given panel. The respective continuum rms values for the transitions shown are 0.07, 1.5, 0.3, and 1.0 mJy beam−1.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Location of radio continuum sources (Ulvestad & Antonucci 1997) and super hot cores (Rico-Villas et al. 2020) within the NGC 253 CMZ plotted over the 212 GHz ALCHEMI dust continuum emission. Numbered white circles indicate GMCs identified in Leroy et al. (2015). The beam size of 1.″6 is shown by the green circle in the bottom left corner.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: HCN/HNC integrated intensity (moment-0) ratio images toward NGC 253. Contour levels are (0.2, 0.5, 1.0, 3.0, 7.0), (1.0, 2.0, 4.0, 10.0, 20.0), (1.0, 5.0, 10.0, 20.0, 50.0), and (1.0, 5.0, 20.0, 50.0) Jy beam−1 km s−1 for the 1–0, 2–1, 3–2, and 4–3 HCN integrated intensities, respectively. Markings in each panel are the same as in Figure 3.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Flowchart describing our nested sampling + chemical and radiative transfer modeling process.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Spectral interloper diagnostic spectrum associated with HNC 4–3. Individual (blue lines) and cumulative (red lines) Gaussian fits are shown.
Paper: Tracing Interstellar Heating: An ALCHEMI Measurement of the HCN Isomers in NGC 253
Authors: Erica Behrens, Jeffrey G. Mangum, Jonathan Holdship, Serena Viti, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Ko-Yun Huang, P. K. Humire, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: HNC integrated intensity (moment-0) images toward NGC 253. Markings, intensity scaling, and contours in each panel are the same as in Figure 3.
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: Action space (J  r  vs. J  z ) of stellar streams present in m12f for all the models (labeled on the top left) at two time steps, 13.8 and 8 Gyr, respectively. The complete time-evolving action-space videos are posted for all the models and simulations. The action clusters are completely incoherent (lose clustering and change positions) at 13.8 Gyr compared to 8 Gyr due to a potential varying merger at 10.8 Gyr.
Paper: Comparison of Electron Capture Rates in the N = 50 Region using 1D Simulations of Core-collapse Supernovae
Authors: Zac Johnston, Sheldon Wasik, Rachel Titus, MacKenzie L. Warren, Evan P. O'Connor, Remco Zegers, Sean M. Couch
Figure caption: Core bounce properties vs. progenitor iron core mass, M Fe, for all simulations (Section 3.2). From top to bottom: electron fraction at bounce in the M = 0.1 M ⊙ mass shell (Y  e ); inner core mass at bounce (﹩{M}_{\mathrm{core}}﹩); gravitational potential at the shock at bounce (V  b ); and convergence time of the shock with the ν  e  sphere, relative to bounce (﹩{t}_{{\nu }_{e}}-{t}_{b}﹩). The 0.01× and 10× rate-scaled models are marked by downward and upward-pointing triangles, respectively (appearing from left to right: 12, 20, and 40 M ⊙). In most cases, the differences between EC rates are larger than the dependence on stellar progenitor.
Paper: Comparison of Electron Capture Rates in the N = 50 Region using 1D Simulations of Core-collapse Supernovae
Authors: Zac Johnston, Sheldon Wasik, Rachel Titus, MacKenzie L. Warren, Evan P. O'Connor, Remco Zegers, Sean M. Couch
Figure caption: Radial matter profiles at core bounce vs. enclosed mass for the 20 M ⊙ progenitor (left), and all 200 progenitors between 9 and 120 M ⊙ (right). From top to bottom: electron fraction (Y  e ); specific entropy (S); density (ρ); and radial velocity (v  r ). Differences between the EC rate are typically larger than differences between the progenitors. For the 20 M ⊙ progenitor, the IPA and 0.01× models fail to explode, whereas the LMP, LMP+N50, and 10× models successfully explode (Figure 1).
Paper: Comparison of Electron Capture Rates in the N = 50 Region using 1D Simulations of Core-collapse Supernovae
Authors: Zac Johnston, Sheldon Wasik, Rachel Titus, MacKenzie L. Warren, Evan P. O'Connor, Remco Zegers, Sean M. Couch
Figure caption: Post-bounce evolution of shock radius (r sh) and neutrino heating efficiency in the gain region (η heat) for three reference progenitors (Section 3.1). The 0.01× and 10× models consist of the LMP and LMP+N50 rates systematically scaled by factors of 0.01 and 10 (Section 2.1). Note the different η heat ranges.
Paper: Comparison of Electron Capture Rates in the N = 50 Region using 1D Simulations of Core-collapse Supernovae
Authors: Zac Johnston, Sheldon Wasik, Rachel Titus, MacKenzie L. Warren, Evan P. O'Connor, Remco Zegers, Sean M. Couch
Figure caption: Lepton fraction (Y  l ) vs. density (ρ) at core bounce for the 20 M ⊙ progenitor. Of the baseline EC rate sets, IPA has the weakest deleptonization at densities ≳1012g cm3, but the strongest at lower densities.
Paper: X-Ray and GeV-γ-Ray Emission Property of TeV Compact Symmetric Object PKS 1413+135 and Implication for Episodic Jet Activity
Authors: Ying-Ying Gan, Jin Zhang, Su Yao, Hai-Ming Zhang, Yun-Feng Liang, En-Wei Liang
Figure caption: Light curves of PKS 1413+135 in the X-ray and γ-ray bands. Panel (a): the X-ray light curve obtained by the observations of Swift-XRT (black squares), Chandra (red circles), and XMM-Newton (blue stars), where the horizontal red dashed line represents the mean flux of all the data points derived with Equation (2). Panel (b): the ∼13.5 yr γ-ray light curve derived with an adaptive-binning method based on a criterion of TS ≥ 9 for each time bin, where the minimum time-bin step is 7 days. The horizontal blue solid line indicates the 13.5 yr average flux of 2.28 × 10−11 erg cm−2 s−1. The horizontal green short-dashed line is the sensitivity of Fermi-LAT, which is obtained and derived from the data at https://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm. Panel (c): the γ-ray light curve after MJD 58500 also obtained with the adaptive-binning method and the criterion of TS ≥ 9 for each time bin, where the minimum time-bin step is 1 day. The horizontal red dashed line indicates the average flux of 7.74 × 10−11 erg cm−2 s−1 while the horizontal blue solid line represents the same value as that in panel (b).
Paper: X-Ray and GeV-γ-Ray Emission Property of TeV Compact Symmetric Object PKS 1413+135 and Implication for Episodic Jet Activity
Authors: Ying-Ying Gan, Jin Zhang, Su Yao, Hai-Ming Zhang, Yun-Feng Liang, En-Wei Liang
Figure caption: Observed SEDs with model fitting for PKS 1413+135 in the low-flux (panel (a)) and high-flux (panel (b)) states of γ-rays. The γ-ray spectra in the two panels are the time-integrated spectrum before MJD 58500 (panel (a)) and the time-resolved spectrum during MJD 59589–59591 (panel (b)), respectively. The data in radio-optical bands, the gray solid and opened squares, are taken from NED. The green solid and magenta opened stars indicate the data of the radio core and knot-D, which are taken from Perlman et al. (1996). In the X-ray band, the red inverted triangle represents the highest flux point as shown in Figure 1(a) observed by Swift-XRT on 2020 March 26 (MJD 58934), which is the integral flux value of F 2–10 keV. The cyan bowtie is obtained with the lowest flux point as shown in Figure 1(a) observed by Chandra on 2019 December 20 (MJD 58837), which indicates the flux at 6 keV with Γ X  = 1.83 ± 0.32. The sensitivity curves of the MAGIC telescopes (pink dotted–dashed line, 50 hr) and CTA-N (blue dotted–dashed line, 50 hr) are also presented. Panel (a): the black solid line is the sum of each component emission for the source located at z = 0.247, synchrotron radiation (red lines), SSC process (magenta lines), and external Compton (EC) process (cyan lines), where the solid and dashed lines, respectively, represent the radiations from the sub-parsec-/parsec-scale jet component and the large-scale jet extended region. An insert in the upper left of panel (a) shows the fitting results for the spectra from 0.08–2.7 GHz and from 4.8−375 GHz with the power-law function of F  ν  ∝ ν −α , and α ∼ 0.66 (orange solid line) and α ∼ 0.09 (yellow solid line) are obtained, respectively. Panel (b): the dark-yellow dashed line is the same line as the black solid line in panel (a). The colored solid lines represent the different radiation components of the compact γ-ray emission region, synchrotron radiation (red line), SSC process (magenta line), and EC process (cyan line), where the cyan line at the VHE band indicates the intrinsic flux of the source without considering the extragalactic background light (EBL) absorption. The black solid line is the sum of the dark-yellow dashed line and three colored solid lines after considering the EBL absorption for the source located at z = 0.247. The green dotted–dashed line represents the fitting result when the source is located at z = 0.5.
Paper: X-Ray and GeV-γ-Ray Emission Property of TeV Compact Symmetric Object PKS 1413+135 and Implication for Episodic Jet Activity
Authors: Ying-Ying Gan, Jin Zhang, Su Yao, Hai-Ming Zhang, Yun-Feng Liang, En-Wei Liang
Figure caption: Panel (a): the spectra observed by Fermi-LAT for PKS 1413+135, including the time-integrated spectrum of the whole light curve (magenta symbols) shown in Figure 1 together with the time-integrated spectra before (MJD 54682–58500, cyan symbols) and after (MJD 58500–59660, orange symbols) MJD 58500, the time-resolved spectra of MJD 58724–58726 (green symbols), MJD 58796–58798 (blue symbols), and MJD 59589–59591 (red symbols). The corresponding colored solid lines represent the fitting results. The sensitivity curves of the MAGIC telescopes (pink dotted–dashed line, 50 hr) and CTA-N (blue dotted–dashed line, 50 hr) are also given in the figure. Panel (b): ΓX against F 2–10 keV, where ΓX and F 2–10 keV are the photon spectral index and flux in the 2–10 keV band. They are obtained with the observations of Chandra (red circles) and XMM-Newton (blue stars).
Paper: Implications from the Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating Black Hole Magnetosphere
Authors: Motoki Kino, Masaaki Takahashi, Tomohisa Kawashima, Jongho Park, Kazuhiro Hada, Hyunwook Ro, Yuzhu Cui, 玉竹 崔
Figure caption: Map of the magnetic field strength of a GRMHD simulation in logarithmic scale in the poloidal plane. As GRMHD simulations are scale free, we normalized the mass accretion rate by carrying out GRRT calculations with RAIKOU code (Kawashima et al. 2019, 2021) using the parameters of M87* (M • = 6.5 × 109 M ⊙ and distance D = 16.9 Mpc) in such a way that the resulting image reproduces the ring-like image with a radiative flux ∼0.5 Jy at 230 GHz observed by EHT (Event Horizon Telescope Collaboration 2019a). Here we demonstrate the case of B  H  = 91 G in the GRMHD-simulation model. This is roughly consistent with the B  H  ≳ 200 G estimated from our analytical jet model. Although the GRMHD-simulation model shown here is in a semi-MAD state, we also confirmed that the MAD state achieved B  H  ≳ 200 G with the same procedure (T. Kawashima et al. 2022, in preparation) Although a detailed comparison with the EHT images is beyond the scope of this paper, it is clear that a reproduction of the photon-ring with the synchrotron flux density about 0.5 Jy at 230 GHz is feasible.
Paper: Implications from the Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating Black Hole Magnetosphere
Authors: Motoki Kino, Masaaki Takahashi, Tomohisa Kawashima, Jongho Park, Kazuhiro Hada, Hyunwook Ro, Yuzhu Cui, 玉竹 崔
Figure caption: Comparison of the obtained σ profile for each magnetic field line and estimation of the magnetization degree constrained in previous literature for the M87 jet. For comparison, a region indicating typical values for the location and the magnetization degree of blazars is also shown by a light blue filled square. Unfortunately, the estimates made by Kino et al. (2014, 2015b) are in a region beyond the applicability of the TT03 model (i.e., inside the light cylinder), which means that they cannot be directly compared with the obtained σ curves presented here. The result reported by MAGIC Collaboration et al. (2020) indicates an apparently much smaller magnetization degree than the values found in other reports.