adsabs/AstroCLIMB huggingface dataset:
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: Demonstration of the image characterization algorithm employed in Section 5. (Upper left) Sample 1.3 mm black hole image for a spin of a = 0.6, an observer inclination of 30°, and the analytic plasma model described in Section 3. (Upper right) Same image after a 15 G λ, n = 2 Butterworth filter has been applied to mimic the finite resolution of the EHT. The solid green curve identifies the location of maximum brightness along each radial cross section of the image. The dashed green curves identify the FWHM of the brightness distribution of the equivalent Gaussian representation of the image along each radial cross section. (Lower left) Horizontal cross section of the image. The green curve shows the brightness of the original image, the blue curve shows the brightness of the filtered image, and the red curve shows the equivalent Gaussian representation of the cross section. (Lower right) Two cross sections of the visibility amplitudes of the original and filtered images. The Butterworth filter only marginally affects the visibility amplitudes and not at the locations of the deep minima, on which the observational measurement of the image size is based.
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: (Left) Equatorial radial velocity, (middle) density, and (right) comoving 230 GHz synchrotron emissivity profiles of accretion flows around Kerr black holes with spins equal to (top) a = 0 and (bottom) a = 0.7. In all panels, the region inside the horizon is shown with a gray-filled area, and the coordinate radii of the photon obit (r ph) and of the ISCO (r ISCO) are shown with vertical dashed lines. Curves of different colors correspond to different radial profiles outside the ISCO, whereas curves of different line styles correspond to different magnitudes of the radial velocity at the ISCO. In the rightmost panels, the ion-to-electron temperature ratio is set to R = 10 and the magnetic field strength at the ISCO to B ISCO = 10 G. The density and emissivity have been normalized to their respective values at the ISCO. Even though the magnitude of the radial velocity increases rapidly inside the ISCO, conservation of mass and energy throughout the flow causes the 230 GHz emissivity to always increase inwards. There is no evidence of a sharp reduction in emissivity with decreasing radius inside the ISCO or anywhere else in the flow.
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: Brightness cross sections of images around a nonspinning black hole with the simple emissivity model but for profiles arbitrarily truncated at various radii r in. (a) Images where r in = 3M and r in = 4M show extremely little difference from those with the horizon boundary condition, even for small values of the disk thickness and observer’s inclination, and a sharp drop in the image brightness still occurs at the critical impact parameter. (b) Images with r in = 6M exhibit a disjoint feature associated with the truncation radius, in addition to the peak at the photon radius, but the intensity drops to zero between peaks only for extremely small values of the disk thickness.
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: Radial and azimuthal components of the velocity in the flow as a function of the polar angle θ. The top panels show the velocity components at constant cylindrical radii ϖ and the bottom panels at constant spherical radii r for a GRMHD simulation with a black hole spin a = 0.7. The shaded bands in the left panels show the rms range of the azimuthal velocities, for different azimuths and snapshots. The curves in the right show the mean values of the radial velocities, averaged over azimuth and time. The vertical arrows in all panels denote the polar angle that corresponds to one disk scale height θ = h/r. As expected from the self-similar analytic solutions, the radial velocity v  r  is constant along cylindrical surfaces, whereas the angular velocity u  ϕ  is constant on spherical surfaces.
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: Images of black holes at 1.3mm calculated using the analytic plasma model described in Section 3, for different black hole spins, observer inclinations, and parameters of the radial velocity profile. In all panels, we have set R = 5 and B 0 = 20 G. The outline of the black hole shadow on each image is shown as a dashed red line. The bright ring of emission closely traces the boundary of the shadow for a wide range of assumptions regarding the spacetime, the plasma properties, or the observer.
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: Comparison of the radial profiles of various flow properties in the analytic model to an example GRMHD simulation with a black hole spin a = 0.7. Top left shows the azimuthal velocity, top right the equatorial density, bottom left the ion temperature, and bottom right the magnetic field strength. GRMHD simulation results have been averaged over the azimuthal direction and over multiple snapshots. Analytic models derived from conservation laws show good agreement with the detailed GRMHD models, as expected.
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: Effect of (left) a radial infall velocity and (right) of a frequency-dependent emissivity on the image cross section in the simple analytic model. Both effects cause a reduction in the image brightness at small impact parameters, increasing the contrast between the bright emission ring and the black hole shadow.
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: (Left) Different path lengths that contribute to the observed image brightness at four impact parameters through an accretion flow. (Right) Contribution of different impact parameters to the various features in the image cross section.
Paper: Searching for Extremely Blue UV Continuum Slopes at z = 7–11 in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies
Authors: Michael W. Topping, Daniel P. Stark, Ryan Endsley, Adele Plat, Lily Whitler, Zuyi Chen, Stéphane Charlot
Figure caption: Comparison of our two high-f esc,H II  candidates with low-redshift samples. (a) SFR vs. effective radius for the two objects in our sample (yellow stars), the KLCS sample (red circles; Steidel et al. 2018; Pahl et al. 2022), and the LzLCS (blue circles; Flury et al. 2022a). Lines of constant SFR surface density are shown for reference. (b) Distribution of sSFR surface density (ΣsSFR) for the LzLCS sample. The values for the two objects in our sample are indicated by the vertical yellow lines. (c) f esc as a function of β. We note that the f esc of the LzLCS represents a direct measure of the global escape fraction, while the f esc,H II  for our objects is a measure local to the H II regions. Furthermore, β for these two samples is measured over a different wavelength range; however, the two measures of the UV slope can be compared in a relative sense, such that objects would be “blue” using both measures.
Paper: Searching for Extremely Blue UV Continuum Slopes at z = 7–11 in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies
Authors: Michael W. Topping, Daniel P. Stark, Ryan Endsley, Adele Plat, Lily Whitler, Zuyi Chen, Stéphane Charlot
Figure caption: (a) Regions of the β–EW parameter space probed by SED models with varying amounts of f esc,H II . These regions were derived by constructing grids of SED models spanning a broad range of ages and metallicities (i.e., ﹩\mathrm{log}(\mathrm{Age}/\mathrm{yr})=6\,\mathrm{to}\,9)﹩; ﹩\mathrm{log}(Z/{Z}_{\odot })=-2\,{to}\ 0.3﹩). Models with an f esc,H II   = 1 will trend toward bluer β, down to a minimum of −3.2 (see Figure 2) but do not produce any line emission (i.e., EW). As such, they are not displayed in this figure. (b) Same as left panel, except calculated from BEAGLE models with a modest attenuation from dust, corresponding to τ  V,eff = 0.1. The addition of dust in these models results in reddened UV slopes and decreased EWs.
Paper: Searching for Extremely Blue UV Continuum Slopes at z = 7–11 in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies
Authors: Michael W. Topping, Daniel P. Stark, Ryan Endsley, Adele Plat, Lily Whitler, Zuyi Chen, Stéphane Charlot
Figure caption: Best-fit SEDs for the two extremely blue objects in our sample. The best-fit SED calculated from BEAGLE using models that allow for the escape of ionizing radiation is displayed in the left panel, while the model with fixed f esc,H II   = 0 is given on the right. In both panels, the observed photometry is displayed as the cyan diamonds, while the predicted photometry from the models is displayed as colored squares. The minimum χ 2 found for each set of models, as well as the best-fit f esc,H II  , are given in the lower right of each panel.
Paper: Searching for Extremely Blue UV Continuum Slopes at z = 7–11 in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies
Authors: Michael W. Topping, Daniel P. Stark, Ryan Endsley, Adele Plat, Lily Whitler, Zuyi Chen, Stéphane Charlot
Figure caption: Image cutouts in all NIRCam filters and combined color image of the two extremely blue objects in the sample. Postage stamps are all 1″ on a side centered at the location of the object. All of the objects present clear detections in multiple filters, indicating they are not artifacts.
Paper: Searching for Extremely Blue UV Continuum Slopes at z = 7–11 in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies
Authors: Michael W. Topping, Daniel P. Stark, Ryan Endsley, Adele Plat, Lily Whitler, Zuyi Chen, Stéphane Charlot
Figure caption: UV slopes as a function of M UV for the full sample of z ∼ 7 (blue circles; Endsley et al. 2022) and z ∼ 8.5–11 (red diamonds; Whitler et al. 2022b) galaxies. The two objects identified with extremely blue UV slopes and described in Tables 1 and 3 are shown as the yellow stars.
Paper: Searching for Extremely Blue UV Continuum Slopes at z = 7–11 in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies
Authors: Michael W. Topping, Daniel P. Stark, Ryan Endsley, Adele Plat, Lily Whitler, Zuyi Chen, Stéphane Charlot
Figure caption: Rest-frame coverage of available NIRCam filters throughout the rest-UV continuum. Bands are shown at three different redshifts spanning the different photometric selections described in Section 3.1. The positions of Lyα and the Balmer break are displayed as the vertical lines. Filters that extend past these boundaries, and thus are less sensitive to the UV continuum, are displayed at a reduced opacity.
Paper: Searching for Extremely Blue UV Continuum Slopes at z = 7–11 in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies
Authors: Michael W. Topping, Daniel P. Stark, Ryan Endsley, Adele Plat, Lily Whitler, Zuyi Chen, Stéphane Charlot
Figure caption: Posterior probability distributions for the parameters inferred for EGS-9466 using the BEAGLE model setup described in Section 4.
Paper: Searching for Extremely Blue UV Continuum Slopes at z = 7–11 in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies
Authors: Michael W. Topping, Daniel P. Stark, Ryan Endsley, Adele Plat, Lily Whitler, Zuyi Chen, Stéphane Charlot
Figure caption: Same as Figure 9 but for EGS-16168.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Schematic diagram of magnetic acceleration. Panel (1) shows the phase before the cloudlet collision. Panel (2) displays the cloudlet collision, corresponding to panel (a) of Figure 6. The yellow arrows correspond to the vector arrows in panel (c) of Figure 6. Panel (3) shows magnetic acceleration, corresponding to panel (b) of Figure 6.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Time evolution of the ratio of the mass of the gravitationally unbound gas to the initial cloudlet mass for all models.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Our model setup. Panel (a) shows the 3D structures of the protoplanetary disk, cloudlet, and magnetic field lines. The magnetic field is imposed only on the cloudlet. Panel (b) shows the midplane (z = 3.5 au) slice. The orange dashed arrow indicates the parabolic orbit of the cloudlet. Panel (c) displays the cutout at y = 3.5 au. Color in panels (b) and (c) denotes the density.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Same as Figure 2, but for model S150_B116.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: The ratio of Keplerian orbital period τ Kep to acceleration timescale by magnetic tension force τ mag at the midplane for model S150_B116; τ Kep/τ mag is larger than two in the spiral and super-Keplerian regions where τ Kep=7.4  ×  103 yr and 1.6  ×  104 yr at r = 300 au and 500 au, respectively. It means that the acceleration timescale is τ mag ≤ 3.7 × 103 and 8.0 × 103 yr at r = 300 au and 500 au, respectively. The acceleration can be explained by magnetic tension force.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Evolution of the density (left) and the rotational velocity (right) distributions at the midplane z = 3.5 au for the hydrodynamic model, S60_NB. The rotational velocity is normalized by the local Keplerian orbital velocity, v Kep.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Same as Figure 2, but for model S60_B116. Black arrows indicate a local reduction in the rotational velocity.
Paper: EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension
Authors: Akinori Matsumoto, Masami Ouchi, Kimihiko Nakajima, Masahiro Kawasaki, Kai Murai, Kentaro Motohara, Yuichi Harikane, Yoshiaki Ono, Kosuke Kushibiki, Shuhei Koyama, Shohei Aoyama, Masahiro Konishi, Hidenori Takahashi, Yuki Isobe, Hiroya Umeda, Yuma Sugahara, Masato Onodera, Kentaro Nagamine, Haruka Kusakabe, Yutaka Hirai, Takashi J. Moriya, Takatoshi Shibuya, Yutaka Komiyama, Keita Fukushima, Seiji Fujimoto, Takashi Hattori, Kohei Hayashi, Akio K. Inoue, Shotaro Kikuchihara, Takashi Kojima, Yusei Koyama, Chien-Hsiu Lee, Ken Mawatari, Takashi Miyata, Tohru Nagao, Shinobu Ozaki, Michael Rauch, Tomoki Saito, Akihiro Suzuki, Tsutomu T. Takeuchi, Masayuki Umemura, Yi Xu, Kiyoto Yabe, Yechi Zhang, Yuzuru Yoshii
Figure caption: Comparison of our Y P values with those reported in recent literature. The blue circles with errors show the 1σ confidence regions derived from He emission line analyses (Izotov et al. 2014; Aver et al. 2015; Peimbert et al. 2016; Fernández et al. 2019; Valerdi et al. 2019; Hsyu et al. 2020; Kurichin et al. 2021) and an analysis of a quasar absorption system (Cooke & Fumagalli 2018). The gray region shows the constraint from CMB observations at a 2σ confidence limit (Planck Collaboration et al. 2020). The red circle represents our result at a 1σ limit. The result with the sample from Hsyu et al. (2020) using our likelihood function given by Equation (9) is denoted with the black circle.
Paper: EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension
Authors: Akinori Matsumoto, Masami Ouchi, Kimihiko Nakajima, Masahiro Kawasaki, Kai Murai, Kentaro Motohara, Yuichi Harikane, Yoshiaki Ono, Kosuke Kushibiki, Shuhei Koyama, Shohei Aoyama, Masahiro Konishi, Hidenori Takahashi, Yuki Isobe, Hiroya Umeda, Yuma Sugahara, Masato Onodera, Kentaro Nagamine, Haruka Kusakabe, Yutaka Hirai, Takashi J. Moriya, Takatoshi Shibuya, Yutaka Komiyama, Keita Fukushima, Seiji Fujimoto, Takashi Hattori, Kohei Hayashi, Akio K. Inoue, Shotaro Kikuchihara, Takashi Kojima, Yusei Koyama, Chien-Hsiu Lee, Ken Mawatari, Takashi Miyata, Tohru Nagao, Shinobu Ozaki, Michael Rauch, Tomoki Saito, Akihiro Suzuki, Tsutomu T. Takeuchi, Masayuki Umemura, Yi Xu, Kiyoto Yabe, Yechi Zhang, Yuzuru Yoshii
Figure caption: Constraints on N eff, η, and ξ e. The solid gray contours show the constraint from our Y P value and the D P measurement (Cooke et al. 2018). The vertical dotted lines represent the Planck Collaboration et al. (2020) constraint on η. The constraint combining with the Y P, D P, and η measurements is shown with blue contours. These contours show the 1σ, 2σ and 3σ confidence limits. The Standard Model values of N eff = 3.046 and ξ  e  = 0 are represented with black dashed lines.
Paper: EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension
Authors: Akinori Matsumoto, Masami Ouchi, Kimihiko Nakajima, Masahiro Kawasaki, Kai Murai, Kentaro Motohara, Yuichi Harikane, Yoshiaki Ono, Kosuke Kushibiki, Shuhei Koyama, Shohei Aoyama, Masahiro Konishi, Hidenori Takahashi, Yuki Isobe, Hiroya Umeda, Yuma Sugahara, Masato Onodera, Kentaro Nagamine, Haruka Kusakabe, Yutaka Hirai, Takashi J. Moriya, Takatoshi Shibuya, Yutaka Komiyama, Keita Fukushima, Seiji Fujimoto, Takashi Hattori, Kohei Hayashi, Akio K. Inoue, Shotaro Kikuchihara, Takashi Kojima, Yusei Koyama, Chien-Hsiu Lee, Ken Mawatari, Takashi Miyata, Tohru Nagao, Shinobu Ozaki, Michael Rauch, Tomoki Saito, Akihiro Suzuki, Tsutomu T. Takeuchi, Masayuki Umemura, Yi Xu, Kiyoto Yabe, Yechi Zhang, Yuzuru Yoshii
Figure caption: Fifty nine galaxies (filled blue and gray circles) of our sample and the five EMPGs (open blue circles) that are excluded from the sample (Section 4.2.2) on the y − O/H plane. The blue (gray) circles represent the Subaru galaxies (the literature galaxies), which are described in Section 2.1 (2.2). The red solid line shows the linear regression for the 59 galaxies, and the red square denotes the y p value determined by the linear regression.
Paper: EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension
Authors: Akinori Matsumoto, Masami Ouchi, Kimihiko Nakajima, Masahiro Kawasaki, Kai Murai, Kentaro Motohara, Yuichi Harikane, Yoshiaki Ono, Kosuke Kushibiki, Shuhei Koyama, Shohei Aoyama, Masahiro Konishi, Hidenori Takahashi, Yuki Isobe, Hiroya Umeda, Yuma Sugahara, Masato Onodera, Kentaro Nagamine, Haruka Kusakabe, Yutaka Hirai, Takashi J. Moriya, Takatoshi Shibuya, Yutaka Komiyama, Keita Fukushima, Seiji Fujimoto, Takashi Hattori, Kohei Hayashi, Akio K. Inoue, Shotaro Kikuchihara, Takashi Kojima, Yusei Koyama, Chien-Hsiu Lee, Ken Mawatari, Takashi Miyata, Tohru Nagao, Shinobu Ozaki, Michael Rauch, Tomoki Saito, Akihiro Suzuki, Tsutomu T. Takeuchi, Masayuki Umemura, Yi Xu, Kiyoto Yabe, Yechi Zhang, Yuzuru Yoshii
Figure caption: Observational constraints on η and N eff. The blue contours show the 1σ, 2σ, and 3σ levels determined by this work. The black dashed line shows the Standard Model value of N eff = 3.046. The magenta and light magenta bands represent the Planck constraint on η at the 1σ and 2σ levels, respectively (Planck Collaboration et al. 2020).
Paper: EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension
Authors: Akinori Matsumoto, Masami Ouchi, Kimihiko Nakajima, Masahiro Kawasaki, Kai Murai, Kentaro Motohara, Yuichi Harikane, Yoshiaki Ono, Kosuke Kushibiki, Shuhei Koyama, Shohei Aoyama, Masahiro Konishi, Hidenori Takahashi, Yuki Isobe, Hiroya Umeda, Yuma Sugahara, Masato Onodera, Kentaro Nagamine, Haruka Kusakabe, Yutaka Hirai, Takashi J. Moriya, Takatoshi Shibuya, Yutaka Komiyama, Keita Fukushima, Seiji Fujimoto, Takashi Hattori, Kohei Hayashi, Akio K. Inoue, Shotaro Kikuchihara, Takashi Kojima, Yusei Koyama, Chien-Hsiu Lee, Ken Mawatari, Takashi Miyata, Tohru Nagao, Shinobu Ozaki, Michael Rauch, Tomoki Saito, Akihiro Suzuki, Tsutomu T. Takeuchi, Masayuki Umemura, Yi Xu, Kiyoto Yabe, Yechi Zhang, Yuzuru Yoshii
Figure caption: Comparison of the distributions of the emission line flux ratios of J1016+3754 derived at each step of the MCMC analysis with optical fluxes of the Gaussian fitting method (left) and the integration method (right). The black solid lines show the flux ratios with the best-recovered parameters. The red solid and dashed lines show the measured line flux ratios and their ±1σ values.
Paper: EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension
Authors: Akinori Matsumoto, Masami Ouchi, Kimihiko Nakajima, Masahiro Kawasaki, Kai Murai, Kentaro Motohara, Yuichi Harikane, Yoshiaki Ono, Kosuke Kushibiki, Shuhei Koyama, Shohei Aoyama, Masahiro Konishi, Hidenori Takahashi, Yuki Isobe, Hiroya Umeda, Yuma Sugahara, Masato Onodera, Kentaro Nagamine, Haruka Kusakabe, Yutaka Hirai, Takashi J. Moriya, Takatoshi Shibuya, Yutaka Komiyama, Keita Fukushima, Seiji Fujimoto, Takashi Hattori, Kohei Hayashi, Akio K. Inoue, Shotaro Kikuchihara, Takashi Kojima, Yusei Koyama, Chien-Hsiu Lee, Ken Mawatari, Takashi Miyata, Tohru Nagao, Shinobu Ozaki, Michael Rauch, Tomoki Saito, Akihiro Suzuki, Tsutomu T. Takeuchi, Masayuki Umemura, Yi Xu, Kiyoto Yabe, Yechi Zhang, Yuzuru Yoshii
Figure caption: Comparison of our constraints on N eff and η (blue contours) with those of Hsyu et al. (2020; gray contours). These contours show the 1σ, 2σ, and 3σ confidence regions.