adsabs/AstroCLIMB huggingface dataset:
Paper: Fe Abundances of Early Galaxies at z = 9–12 Derived with Deep JWST Spectra
Authors: Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Ken'ichi Nomoto, Miho N. Ishigaki, Hiroto Yanagisawa, Daichi Kashino, Nozomu Tominaga, Koh Takahashi, Moka Nishigaki, Yui Takeda, Kuria Watanabe
Figure caption: Comparison of the observed abundance ratios with the PISN models. The top, middle, and bottom panels show [O/Fe] as a function of stellar age (left) with our PISN models constructed under the assumption of a constant star formation history (SFH), decreasing SFH (K. N. Hainline et al. 2024), and increasing SFH (S. Tacchella et al. 2023; right), respectively. The red and magenta star symbols represent measurements of GS-z11-0 and GN-z11, respectively. The purple, black, green, and orange lines indicate the PISN models with top-heavy, E. E. Salpeter (1955), P. Kroupa et al. (1993), and top-light IMFs, respectively. The solid and dashed lines denote the PISN models without and with failed SNe, respectively. The yellow-shaded regions present the PISNe yield models (K. Takahashi et al. 2018).
Paper: Fe Abundances of Early Galaxies at z = 9–12 Derived with Deep JWST Spectra
Authors: Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Ken'ichi Nomoto, Miho N. Ishigaki, Hiroto Yanagisawa, Daichi Kashino, Nozomu Tominaga, Koh Takahashi, Moka Nishigaki, Yui Takeda, Kuria Watanabe
Figure caption: Redshift evolution of [O/Fe]. The cyan, orange, red, magenta, and black symbols are the same as in Figure 10. The blue circles denote measurements for local EMPGs (Y. I. Izotov et al. 2018; T. Kojima et al. 2020; Y. Isobe et al. 2022). The gray, green, pink, yellow and blue shaded regions represent the CCSNe, HNe, BrHNe, PISNe, and SNe Ia yield models, respectively.
Paper: Fe Abundances of Early Galaxies at z = 9–12 Derived with Deep JWST Spectra
Authors: Minami Nakane, Masami Ouchi, Kimihiko Nakajima, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Ken'ichi Nomoto, Miho N. Ishigaki, Hiroto Yanagisawa, Daichi Kashino, Nozomu Tominaga, Koh Takahashi, Moka Nishigaki, Yui Takeda, Kuria Watanabe
Figure caption: O/H ratio as a function of absolute UV magnitude. The star symbols show the measurements of our sample galaxies (this work; A. Calabrò et al. 2024; K. N. Hainline et al. 2024; T. Y.-Y. Hsiao et al. 2024b; J. Álvarez-Márquez et al. 2025; M. Curti et al. 2025). The open circles indicate the measurements of galaxies at z ∼ 4–9 (K. Nakajima et al. 2023).
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: Top: early B − V color evolution of objects in the sample, with background red and blue data points from the objects in M. D. Stritzinger et al. (2018), colored according to their classification in Table 1 of that paper. Bottom: early U − V color evolution. Whereas most objects just show a blueward color evolution, the three objects with early excesses (SNe 2017cbv, 2017erp, and 2018yu) have an initial redward evolution from the rapid cooling of the shocked ejecta before becoming dominated by the usual blueward evolution.
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: Color evolution of the sample in a number of filter combinations. Note the logarithmic scale of the time axis, to emphasize early heterogeneity while showing evolution into the nebular phase. Observed color NUV-red and -blue regions are shown for UVW2 – V and UVW1 – V (see Figure 4 of P. A. Milne et al. 2013), where it can be seen that after extinction correction most objects in this sample are NUV-blue.
Paper: Confirming Near- to Mid-infrared Photometrically Identified Obscured AGNs in the JWST Era
Authors: George H. Rieke, Yang Sun, Jianwei Lyu, Christopher N. A. Willmer, Yongda Zhu, Pierluigi Rinaldi, Meredith A. Stone, Kevin N. Hainline, Pablo G. Pérez-González
Figure caption: Left: placement of our sample of galaxies on the BPT diagram with lines of demarcation between star-forming and active galaxies from L. J. Kewley et al. (2001) and G. Kauffmann et al. (2003). The non-AGN spectra are obtained from other galaxies targeted in the SMILES spectroscopy. Right: spectra of galaxies “A” (87191), “B” (209962), and “C” (196290) marked on the BPT diagram. “A” and “C” have lines broadened by outflows, as shown by the similar widths of the [O III] λ4959, 5007 lines to those of the hydrogen lines. “B” appears to be a combination of outflow and broad-line AGN.
Paper: Confirming Near- to Mid-infrared Photometrically Identified Obscured AGNs in the JWST Era
Authors: George H. Rieke, Yang Sun, Jianwei Lyu, Christopher N. A. Willmer, Yongda Zhu, Pierluigi Rinaldi, Meredith A. Stone, Kevin N. Hainline, Pablo G. Pérez-González
Figure caption: H − KS vs. J − H for the subset of AIGs and Haro 11, NGC 5253, and II Zw 40. The standard colors for low-metallicity galaxies are shown as dashed lines. An AGN-like excess would lie above the vertical line and to the right of the vertical one. In this case, we use the 2MASS point source photometry to focus on the galaxy nuclei and also because it has higher signal to noise than the extended source photometry. The position of Haro 11 is shown as a blue diamond, with photometry from J. P. Vader et al. (1993); photometry for NGC 5253 is a red square, from the 2MASS extended objects catalog 14″ beam; and II Zw 40 is a green triangle from T. X. Thuan (1985). “1” is J123948.06-171753.9, “2” is J032224.64+401119.8, and “3” is J133245.62+263449.3, cases that are discussed in the text.
Paper: Confirming Near- to Mid-infrared Photometrically Identified Obscured AGNs in the JWST Era
Authors: George H. Rieke, Yang Sun, Jianwei Lyu, Christopher N. A. Willmer, Yongda Zhu, Pierluigi Rinaldi, Meredith A. Stone, Kevin N. Hainline, Pablo G. Pérez-González
Figure caption: Decomposition of photometry into stellar (green lines), AGN (purple lines), and stellar-powered infrared excess (orange lines). We present the galaxy ID and redshift in the top-left corner of each panel. To demonstrate the model degeneracy, we use the light lines to indicate a range of fits that would be acceptable to emphasize that they have little effect on the decision of whether an embedded AGN is present.
Paper: Confirming Near- to Mid-infrared Photometrically Identified Obscured AGNs in the JWST Era
Authors: George H. Rieke, Yang Sun, Jianwei Lyu, Christopher N. A. Willmer, Yongda Zhu, Pierluigi Rinaldi, Meredith A. Stone, Kevin N. Hainline, Pablo G. Pérez-González
Figure caption: IRAC color–color plot for the sample of A. Rémy-Ruyer et al. (2013). The dotted line outlines the AGN zone from T. H. Jarrett et al. (2011), and the dashed line is the W1 − W2 criterion proposed by D. Stern et al. (2012). The dotted line is the refined relation from J. L. Donley et al. (2012), and the broad red lines represent the maximum scatter around this relation for 5% errors, which are typical for the measurements plotted.
Paper: Confirming Near- to Mid-infrared Photometrically Identified Obscured AGNs in the JWST Era
Authors: George H. Rieke, Yang Sun, Jianwei Lyu, Christopher N. A. Willmer, Yongda Zhu, Pierluigi Rinaldi, Meredith A. Stone, Kevin N. Hainline, Pablo G. Pérez-González
Figure caption: Comparison of the SEDs of non-AGN galaxies with that of Haro 11, all normalized at W3. The range from 4 through 12 μm for the dwarf galaxies is matched well by the SED of Haro 11. (We do not show J160135.95+311353.7 because of the lack of JHK measurements and inconsistencies between the extended and point source photometry.)
Paper: Confirming Near- to Mid-infrared Photometrically Identified Obscured AGNs in the JWST Era
Authors: George H. Rieke, Yang Sun, Jianwei Lyu, Christopher N. A. Willmer, Yongda Zhu, Pierluigi Rinaldi, Meredith A. Stone, Kevin N. Hainline, Pablo G. Pérez-González
Figure caption: Similar to Figure 6 but for the dwarf galaxies with emission line spectra indicating the presence of AGNs. Although the SED of Haro 11 is a good match for some, as anticipated in Section 4.1, three have excesses in the 2–5 μm range suggestive of a contribution by their AGNs (J090613.75+561015.5, J133245.62+263449.3, and J173501.25+570308.8).
Paper: Confirming Near- to Mid-infrared Photometrically Identified Obscured AGNs in the JWST Era
Authors: George H. Rieke, Yang Sun, Jianwei Lyu, Christopher N. A. Willmer, Yongda Zhu, Pierluigi Rinaldi, Meredith A. Stone, Kevin N. Hainline, Pablo G. Pérez-González
Figure caption: WISE color–color plot similar to those used in K. N. Hainline et al. (2016) but for the sample of A. Rémy-Ruyer et al. (2013). The dotted line outlines the AGN zone from T. H. Jarrett et al. (2011) and the dashed line is the W1 − W2 criterion proposed by D. Stern et al. (2012).
Paper: Dark Gaps and Resonances in Barred Galaxies
Authors: Taehyun Kim, Dimitri A. Gadotti, Myeong-gu Park, Yun Hee Lee, Francesca Fragkoudi, Minjin Kim, Woong-Tae Kim
Figure caption: Bar radius and dark gap radius, which is traced with (a): ﹩{R}_{{\rm{Max}}}(\mu )﹩ for all galaxies, (b): RDip for galaxies exhibiting a single dip along the bar minor axis, (c): the first dip position, ﹩{R}_{{1}^{{\rm{st}}},2{\rm{Dip}}}﹩, for galaxies with two dips, and (d): the second dip, ﹩{R}_{{2}^{{\rm{nd}}},2{\rm{Dip}}}﹩, for galaxies with two dips. Pearson correlation coefficients and corresponding linear fits are shown in the lower right corner of each panel.
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: Differential-abundance pattern of the r-I star HD 107752 with respect to the r-II star CS 31082-0001. The circles and boxes represent neutral and ionized species, respectively. For easy identification, we have also marked each symbol with the respective atomic symbols. Elements up to Zn exhibit approximately zero differential abundance. The first r-process peak elements show higher differential abundances than the main r-process peak elements.
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: Top row: the evolution of first-peak r-process abundance ratios ([Sr/Fe], [Y/Fe], and [Zr/Fe]), as a function of [Eu/Fe]. Bottom row: the same elements are shown relative to the level of europium ([Sr/Eu], [Y/Eu], and [Zr/Eu]), as a function of [Eu/Fe]. The gray, yellow, cyan, and magenta colors represent non-RPE stars, limited-r stars, r-I stars, and r-II stars, respectively. The black-solid lines are linear fits to the data, and the gray-shaded regions are the 1σ dispersions. The fitted equations are shown on the top of each respective panel. The gray-dashed horizontal lines represent solar values. For reference, see P. Saraf et al. (2023) and P. Saraf & T. Sivarani (2024).
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: Top panel: the mean abundance patterns of r-I (cyan) and r-II (magenta) stars compiled from the literature with [Fe/H] < −2.0. The mean of r-I and r-II are calculated after scaling the Eu of the stars to the solar Eu. For comparison, the black curve shows the solar r-process pattern. Bottom panel: the mean differential-abundance pattern of r-I stars with respect to r-II stars in blue colored symbols; the blue-shaded region shows the 1σ error range. For comparison, we have overplotted the differential-abundance pattern of HD 107752 with respect to CS 31082-0001 using yellow colored symbols. We note a decreasing differential-abundance pattern with increasing atomic number.
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: Stellar-parameter estimation of HD 107752 using a differential-abundance analysis with respect to CS 31082-0001. The top panel shows the differential abundances of iron, as a function of LEP, while the bottom panel shows these abundances as a function of reduced equivalent width. Blue and magenta colored circles represent Fe I and Fe II features, respectively. In each panel, the gold horizontal line represents the best fit to the data. The figure legend displays the fitting parameters.
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: A comparison of the stellar spectra for the r-I star HD 107752 (magenta spectrum) and the r-II star CS 31082-0001 (cyan spectrum) in the Eu region. We have also marked spectral features of various elements. The enhancement of neutron-capture elements in CS 31082-0001 relative to HD 107752 is clearly evident. For reference, our analysis (see Section 3) yields Teff = 4826 K, ξ = 1.80 km s−1, ﹩\mathrm{log}g=1.55﹩ (cgs), and [Fe/H] = −2.81 for CS 31082-0001, and Teff = 4926 K, ξ = 1.83 km s−1, ﹩\mathrm{log}g=1.46﹩ (cgs), and [Fe/H] = −2.77 for HD 107752.
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: Top panel: a schematic diagram illustrating the expected differential-abundance pattern of HD 107752 relative to CS 31082-0001, if the neutron-capture elements are formed in the same kind of progenitor r-process sites. Bottom panel: a schematic diagram explaining the expected differential-abundance pattern of HD 107752 with respect to CS 31082-0001 if the lighter and main r-process elements originate from different types of progenitor sites. This is similar to the observed differential abundance.
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: A comparison of the stellar spectra in the Hβ (left panel) and Hα (right panel) regions for HD 107752 (solid magenta) and CS 31082-0001 (dotted black). The very similar profiles indicate similar temperatures for both stars.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: The evolution of the torque for the case with α1 = 0°, α2 = 45°, ΔΦ = 0°, and λ = −1 (↑ ↙) in the regular (solid line) and higher resolution (dashed line).
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Profile of the surface brightness ﹩{ \mathcal I }﹩ (top plot), autocorrelation function ﹩{C}_{\delta { \mathcal I }}﹩ (middle), and power spectrum ﹩{ \mathcal F }{\left\{{ \mathcal I }(r)\right\}}^{2}(k)﹩ (bottom) for the 330°–345° sector (measured counterclockwise from north). The left column is for the X-ray and the right column is for the radio images. Brightness is averaged over the azimuth by taking 45 individual radial profiles within the sector. The autocorrelation function and the power spectrum are calculated individually from each of these 45 brightness profiles and then averaged. The errors shown are at the 1σ level. The horizontal line on the plot for ﹩{ \mathcal I }﹩ shows the average brightness. The red horizontal line on the plot for ﹩{C}_{\delta { \mathcal I }}﹩ corresponds to a correlation of 0.1. The red dashed line on the power spectrum is a power law with an index of 5/3. Vertical lines on the power spectrum plot mark the 1/R, 1/3″, and Nyquist wavenumbers. Spatial scales are normalized to the average radius ﹩R={4}^{{\prime} }﹩. The black dashed lines in the middle row represent the autocorrelation function calculated from the average brightness profile. The same lines in the bottom plots are the power spectra from the average brightness profiles, with a Wiener filter (with a window size of 4 pixels) applied to reduce the noise in the spectrum.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Top: the radial power spectrum of the X-ray and radio brightness derived from a FFT of the autocorrelation function. It is calculated from Figure 3 by averaging over the azimuth in the Fourier space. Bottom: the radial power spectrum calculated as azimuth-averaged squares of the FFT amplitudes of the SNR images from Figure 1. The amplitudes on the bottom plot are divided by ﹩{\sigma }_{{ \mathcal I }}^{2}N﹩ to match the normalization of the top plot. Orange lines correspond to the X-ray image, and blue lines correspond to the radio image of the Tycho SNR. Dashed black lines show the power spectrum for the X-ray image corrected for the geometrical factor, which reflects the integration along the line of sight. The red dashed line shows a power law with an index of 8/3 with the same normalization in both plots. Vertical lines mark the wavenumbers corresponding to the average radius ﹩R={4}^{{\prime} }﹩ (left), a distance of 3″ (middle), and the Nyquist wavenumber (right).
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Azimuthal average of the radial component of Fourier amplitudes from a 2D Fourier transform of the X-ray image of the Tycho SNR (orange and green lines) and its radio image (blue lines). Solid lines represent the FFT of the image, while dashed lines represent the FFT of the background noise. The vertical lines correspond to the average radius ﹩R={4}^{{\prime} }﹩ (left), to the wavenumber k = 1/3″ (middle), and the Nyquist wavenumber (right). Green lines correspond to the X-ray data before and the orange lines after Gaussian smoothing with a 1 pixel kernel was applied to the X-ray image. The green lines coincide with the orange lines at wavenumbers R/ℓ ≲ 30. Shaded areas show 1σ errors for the log Gaussian; the errors are statistical, due to averaging between the radial profiles in 2D Fourier space at azimuths from 0 to 2π.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Two-dimensional autocorrelation functions for the X-ray image of the Tycho SNR (left) and for the radio image (right) with the background noise removed. Numbers on axes are in units of the average radius of the SNR ﹩R={4}^{{\prime} }﹩, while lines correspond to directions of density (left) and magnetic field (right) gradients found by O. Petruk et al. (2024).
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Discrete Fourier transform of the 2D autocorrelation maps from Figure 2, for the X-ray (left) and radio (right) images. The color scale corresponds to the decimal logarithm of the Fourier amplitudes; the scale is the same for both images because they are derived from the autocorrelation functions, which are normalized to unity for the zero shift. The inner red circle has a radius that corresponds to the wavenumber k = 1/3″. The radius of the outer circle equals the Nyquist wavenumber k = 1/1″.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Function Sδn(ℓ) calculated for the X-ray (top) and the radio (bottom) images of Tycho SNR from a few contours consisting of pixels at distances ﹩r/{ \mathcal R }﹩ (numbers in the legend), where ﹩{ \mathcal R }(\varphi )﹩ is the radius from the explosion center that varies with azimuth. The plots are approximately representative of the plasma density fluctuations (upper) and the magnetic disturbances (lower). The dashed lines show the power law ℓ2/3. The vertical lines mark the wavenumbers k = 1/1″ (left), k = 1/3″ (middle), and corresponding to the average radius ﹩R={4}^{{\prime} }﹩ (right). The horizontal axis is in units of ﹩R={4}^{{\prime} }﹩. The maximum shift along the contour corresponds to the total length of that contour. The 1σ statistical errors for the structure function are also shown (by lighter colors around solid lines).
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Two-dimensional autocorrelation functions for X-ray images of the Tycho SNR in the 1.6–2.1 keV (upper left), 2.3–2.6 keV (upper right), and 4.1–6.0 keV (bottom left) energy ranges. The bottom-right plot shows the radial power spectra calculated as the angle average of ﹩{ \mathcal F }{\{{I}_{x}\}}^{2}﹩, for the SNR images Ix in different photon energy ranges indicated in the legend. The dashed red line on this plot shows the k−8/3 dependence. The images were convolved before the analysis with kernels of 1, 1, 1.5, and 2.5 pixels, as described in Appendix A.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Power spectrum nearly representative of the density (top) and magnetic field (bottom) fluctuations in the Tycho SNR calculated as a square of the Fourier transform of ﹩{{ \mathcal I }}_{x}^{1/2}﹩ and ﹩{{ \mathcal I }}_{r}^{1/1.6}﹩, respectively, across the same contours as used for Figure 7. To reduce the noise while preserving the main dependence, we applied a Wiener filter (J. S. Lim 1990, Section 9.2.4) with a window size of 9 pixels to the spectra. The dashed lines show the decreasing power law with index 5/3. The vertical lines mark the wavenumbers 1/R (left), 1/3″ (middle), and 1/1″ (right).
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Top: the correlation length ℓc (the distance where the correlation is 0.1) for each direction as a fraction of R. Bottom: the autocorrelation value for a shift ﹩1\mathop{.}\limits^{{\rm{^{\prime} }}}5﹩ (0.375R) as a function of the azimuthal direction. The orange lines correspond to the X-ray image and the blue lines to the radio image of the Tycho SNR.
Paper: A Novel Test for MOND: Gravitational Lensing by Disk Galaxies
Authors: Christopher Harvey-Hawes, Marco Galoppo
Figure caption: Example image configurations, caustic curves, and critical curves for spiral galaxy MOND lenses with varying inclination and point source objects placed at a constant position relative to the lens center. The solid black line, dotted red line, and dashed–dotted red line indicate the critical curve, radial caustic curve, and tangential caustic curves, respectively. The blue star represents the source image, and black dots show the corresponding lensed images. The parameters of the lens galaxy are fixed to be Md = 1011 M⊙, Rd = 3.5 kpc, zd = 0.35 kpc, Mb = 109 M⊙, and rb = 0.7 kpc. The interpolating function employed was the standard function of Equation (21). The lens and source are placed at redshift zL = 0.5 and zS = 2.0, respectively.