adsabs/AstroCLIMB huggingface dataset:
Paper: Angle-dependent in Situ Fast Flavor Transformations in Post-neutron-star-merger Disks
Authors: Kelsey A. Lund, Payel Mukhopadhyay, Jonah M. Miller, G. C. McLaughlin
Figure caption: Bolometric luminosity for neutrinos of each species as a function of time for the simulations with (pink) and without (teal) oscillations. From left to right, each panel shows the luminosity from νe, ﹩{\bar{\nu }}_{e}﹩, νX, and ﹩{\bar{\nu }}_{X}﹩as dashed lines, as well as the total neutrino luminosity as solid lines. Oscillations systematically suppress electron flavors and enhance heavy flavors. Furthermore, between ∼3 and ∼60 ms, the total luminosity with FFCs exceeds the luminosity without, suggesting that the disk is more efficiently cooled.
Paper: ADF22-WEB: Detection of a Molecular Gas Reservoir in a Massive Quiescent Galaxy Located in a z ≈ 3 Protocluster Core
Authors: Hideki Umehata, Mariko Kubo, Kouichiro Nakanishi
Figure caption: NIRCam color image (F200W/F356W/F444W) of the AzTEC14 dense galaxy group at z ≈ 3.09 in ADF22 (H. Umehata et al. 2014; M. Kubo et al. 2015). Cyan (white) contours indicate CO(3–2)(1.1 mm) emission at levels of 2σ, 3σ, ..., 5σ. Confirmed protocluster members, including DSFGs (ADF22.A4, ADF22.A10, ADF22.A11, ADF22.A16, and ADF22.A17, H. Umehata et al. 2017; H. Umehata et al. 2019), an LBG (MD48, C. C. Steidel et al. 1998), and QGs (ADF22-QG1, ADF22-QG2, and ADF22-QG3, M. Kubo et al. 2021, 2022) are labeled with their zspec values. ADF22-QG1 is detected in CO(3–2) but not in the dust continuum. Neither the dust continuum nor the CO(3–2) line is significantly detected in ADF22-QG2 or ADF22-QG3.
Paper: ADF22-WEB: Detection of a Molecular Gas Reservoir in a Massive Quiescent Galaxy Located in a z ≈ 3 Protocluster Core
Authors: Hideki Umehata, Mariko Kubo, Kouichiro Nakanishi
Figure caption: CO(3–2) spectra of the three QGs in the AzTEC14 group. ADF22-QG1 is detected in CO(3–2), with a redshift broadly consistent with that determined from Balmer absorption lines (M. Kubo et al. 2021). The best-fit Gaussian profile is shown as a red solid line. The yellow shaded region indicates the frequency range used to create the moment-zero map. No significant CO(3–2) detection is found for ADF22-QG2 or ADF22-QG3.
Paper: Dual Directional Expansion of Classical Cepheids in the Small Magellanic Cloud Revealed by Gaia Data Release 3
Authors: Satoya Nakano, 覚矢 中野, Kengo Tachihara, 研悟 立原
Figure caption: A comparison of the internal PMs of the clipped CC samples, considering only the 241 distant (>70 kpc) and 276 nearby (<55 kpc) populations, with the H I redshifted and blueshifted components. The magenta PM vectors represent the distant Cepheids, while the green PM vectors represent the nearby Cepheids. The background is a color multivelocity montage of the H I emission observed with ASKAP and Parkes (N. M. McClure-Griffiths et al. 2018), where red represents the integrated intensity for the 179–187 km s−1 range, and blue for the 105–113 km s−1 range, both displayed on a common logarithmic scale of 10–1000 K km s−1. Contours highlight the regions where the H I redshifted and blueshifted components are present, with yellow contours corresponding to the redshifted component and cyan contours to the blueshifted component. Note that these velocity components are consistent with those shown in Figure 2 of N. M. McClure-Griffiths et al. (2018). The white dotted arrow in the lower left of the figure indicates the direction in which the Dstar gradient of the clipped CC samples is the largest.
Paper: Dual Directional Expansion of Classical Cepheids in the Small Magellanic Cloud Revealed by Gaia Data Release 3
Authors: Satoya Nakano, 覚矢 中野, Kengo Tachihara, 研悟 立原
Figure caption: The (GBP − GRP, G) CMD of the CC samples. The colored circles and star symbols represent the CC samples, with their colors indicating the respective values of Dstar. The black dots represent massive star candidates (Mini ≥ 8M⊙, age ≲ 50.0 Myr; S. Nakano et al. 2025). The colored star symbols represent massive Cepheids, corresponding to 38 massive star candidates among the CC samples. The cyan crosses represent five objects that have counterparts in massive star candidates but are excluded from the CC samples due to the 3.5σ-clipping applied to ΔW(V,  Ks). The cyan dashed line represents an approximate main sequence constructed using PARSEC isochrones (version 1.2S; A. Bressan et al. 2012; Y. Chen et al. 2014, 2015; J. Tang et al. 2014; P. Marigo et al. 2017; G. Pastorelli et al. 2019, 2020). The metallicity of the main sequence is assumed to be Z = 0.1Z⊙, with Z⊙ = 0.0152. Additionally, a reddening correction of AV = 0.15 mag due to the Milky Way foreground is applied to the main sequence using dustapprox (M. Fouesneau et al. 2022).
Paper: Dual Directional Expansion of Classical Cepheids in the Small Magellanic Cloud Revealed by Gaia Data Release 3
Authors: Satoya Nakano, 覚矢 中野, Kengo Tachihara, 研悟 立原
Figure caption: The internal PMs of the clipped CC samples determined by subtracting the mean PM of the clipped CC samples. The legends indicate the magnitudes of PM vectors corresponding to 85 km s−1, representing the minimum escape velocity derived under the assumption of H I rotation (S. Stanimirović et al. 2004; N. M. McClure-Griffiths et al. 2018). The colors of the PM vectors represent the distances Dstar of the CCs, with more distant objects shown in magenta and nearer ones in green. The magenta and green star symbols indicate the mean positions of 241 distant (>70 kpc) and 276 nearby (<55 kpc) Cepheids, respectively. The thick vectors extending from the star symbols represent the mean PM vectors of the distant and nearby Cepheids, drawn at 10 times the length of the individual stellar vectors for better visibility. Note that the distance thresholds for distant and nearby Cepheids (70 and 55 kpc) are consistent with those used in F. Niederhofer et al. (2021). The white dotted arrow in the lower left of the figure indicates the direction in which the Dstar gradient of the clipped CC samples is the largest.
Paper: Exploring the Link between Fast Radio Burst and Binary Neutron Star Origins with Spaceborne Gravitational Wave Observations
Authors: Yu-xuan Yin, 宇轩 尹, En-kun Li, 恩坤 李, Bing Zhang, 冰 张, Yi-Ming Hu, 一鸣 胡
Figure caption: The TianQin/LISA horizon distance for BNS systems at various evolution stages of coalescence, as denoted by tc − t. TianQin/LISA could observe sources beneath the dark blue dashed curve/orange solid curve with ρ > 7. The cyan/green/red/blue lines indicate the distances to M81/M33/M31/opposite edge of the Milky Way, respectively.
Paper: Exploring the Link between Fast Radio Burst and Binary Neutron Star Origins with Spaceborne Gravitational Wave Observations
Authors: Yu-xuan Yin, 宇轩 尹, En-kun Li, 恩坤 李, Bing Zhang, 冰 张, Yi-Ming Hu, 一鸣 胡
Figure caption: Evolution of the SNR of a BNS in M81. The blue solid curve represents the SNR results that account for the antenna response effect, whereas the green dashed curve shows the results without considering the antenna response effect. The green dashed–dotted line and the blue solid line denote the SNR thresholds of 7 and 5, respectively.
Paper: Exploring the Link between Fast Radio Burst and Binary Neutron Star Origins with Spaceborne Gravitational Wave Observations
Authors: Yu-xuan Yin, 宇轩 尹, En-kun Li, 恩坤 李, Bing Zhang, 冰 张, Yi-Ming Hu, 一鸣 胡
Figure caption: SNR distribution for BNS systems assuming a double Gaussian mass distribution. Considering a BNS at M81 that will merge in 80 yr, there is a 1.5% probability it will be detectable, while a GW190425-like BNS system with a total mass of 3.4M⊙ will definitely be detectable.
Paper: Formation of Chromospheric Fan-shaped Jets through Magnetic Reconnection
Authors: Annu Bura, Tanmoy Samanta, Avijeet Prasad, Ronald L. Moore, Alphonse C. Sterling, Vasyl Yurchyshyn, Arun Surya
Figure caption: Panels of (A) show the temporal evolution around the fan-shaped jets. The black contours outline the jet area, plotted in panel (D). Panels of (B) show the corresponding magnetic field evolution. The blue and red contours represent the flux above +20 and −20 G, respectively. The white arrows highlight the base of dark recurrent fan-shaped jets. Panel (C) is the same as the leftmost subpanel of (B). The blue and red square boxes that cover the positive and negative polarities of the dipole are used to compute the magnetic flux of the two opposite polarities. (D) Variation of measured positive (blue line) and negative flux (red line) over time. The golden curve shows the variation in the area of the fan-shaped jet over time within the rectangular box marked in panel (A). The timestamps in panel (A) show the time in minutes elapsed from 16:46:10 UT.
Paper: Formation of Chromospheric Fan-shaped Jets through Magnetic Reconnection
Authors: Annu Bura, Tanmoy Samanta, Avijeet Prasad, Ronald L. Moore, Alphonse C. Sterling, Vasyl Yurchyshyn, Arun Surya
Figure caption: The top and bottom panels show snapshots of the fan-shaped jets at two different time instances as seen in different AIA filters. The top panels reveal the presence of strong brightening in the AIA 304 Å channel and faint but less distinct brightening in the AIA 171 and AIA 193 Å channels at 17:02:17 UT. The later phase images of different AIA filters (for example, in the bottom subpanels) do not show any noticeable brightening at the canceling neutral line in any of the AIA images at 17:15:55 UT.
Paper: Formation of Chromospheric Fan-shaped Jets through Magnetic Reconnection
Authors: Annu Bura, Tanmoy Samanta, Avijeet Prasad, Ronald L. Moore, Alphonse C. Sterling, Vasyl Yurchyshyn, Arun Surya
Figure caption: A cartoon illustrating the proposed mechanism for fan-shaped jets between a pair of same-polarity sunspots, based on the minifilament eruption model. The magenta lines represent the overarching magnetic field, while the magenta loop lines indicate the preexisting bipole. The orange line depicts a sheared and twisted field containing a minifilament flux rope, likely containing trapped chromospheric (minifilament) material. The crosses mark the reconnection sites, where opposite-polarity field lines interact. The small blue loop in panels (B) and (C) represents the newly reconnected field from the internal reconnection, which we suggest makes the AIA 304, 171, and 193 Å brightenings at the canceling neutral line in the top panels of Figure 3. In panel (C), the large blue loop (labeled “Newly formed loop”) results from external reconnection (upper cross), with the upper blue reconnected line facilitating plasma ejection, including the formation of the fan-shaped jets, shown as an inverted orange triangle regions.
Paper: Formation of Chromospheric Fan-shaped Jets through Magnetic Reconnection
Authors: Annu Bura, Tanmoy Samanta, Avijeet Prasad, Ronald L. Moore, Alphonse C. Sterling, Vasyl Yurchyshyn, Arun Surya
Figure caption: (A)–(B) shows the NFFF extrapolated magnetic field lines of a large region at 17:00:46 UT plotted over an HMI continuum image and an HMI line-of-sight magnetogram, respectively. Panel (C) highlights the 3D magnetic null point structure near the location of the fan-shaped jets. Panel (D) shows the magnetic field strength and direction (indicated by the blue arrows) at a height of ∼1.25 Mm.
Paper: It’s Not Just a Phase: Oblique Pulsations in Magnetic Red Giants and Other Stochastic Oscillators
Authors: Nicholas Z. Rui, Jim Fuller, J. M. Joel Ong
Figure caption: Linear g-mode frequency shifts δν = δω/2π relative to the power-weighted average shift of the triplet ﹩\delta \bar{\nu }﹩ (defined in Section 2.3), plotted against the strength of the magnetic perturbation δνmag = δωmag/2π. The magnetic field strengths corresponding to δνmag are also shown for the M = 1.5 M⊙, R = 5.2 R⊙ red giant model described in Section 2.3. For illustrative purposes, here we have fixed 2πσ0 = 180 μHz, δωrot ≈ 1.2 μHz, i = 60°, and β = 70°. Line colors indicate the underlying mode, and line thicknesses are proportional to the spectral power. Low field strengths leave the rotational triplet symmetrically split, moderate field strengths introduce asymmetry in the triplet, and higher field strengths induce oblique pulsations in which each mode individually appears as a triplet.
Paper: It’s Not Just a Phase: Oblique Pulsations in Magnetic Red Giants and Other Stochastic Oscillators
Authors: Nicholas Z. Rui, Jim Fuller, J. M. Joel Ong
Figure caption: “Phase diagram” of pulsation regimes in the space of magnetic field vs. rotation rate, where data points indicate known magnetic red giants with observed rotational triplets. Regions of rotational alignment (δωmag < δωrot) and magnetic obliquity (δωmag > δωrot) are shown for the case of pure g modes, assuming the stellar model described in Section 2.3 and the stellar parameters described in Section 2.4. The condition for magnetic g-mode suppression (B > Bcrit; Equation (24)) is also shown for the same model. These shaded regions show approximate, model-dependent estimates for these regimes, and the precise boundaries between the regimes depend on stellar parameters and therefore vary from star to star.
Paper: It’s Not Just a Phase: Oblique Pulsations in Magnetic Red Giants and Other Stochastic Oscillators
Authors: Nicholas Z. Rui, Jim Fuller, J. M. Joel Ong
Figure caption: Synthetic data of a magnetically oblique g-mode triplet in a red giant (described further in Section 2.3). Background shading indicates the location of a periodicity, where the color represents the physical mode from which a periodicity originates. Top: the observed PSD ﹩| \delta \tilde{I}{| }^{2}﹩, normalized to the expectation value of the simulated white noise floor. Bottom: the absolute value of the windowed normalized cross-correlation (∣NCC∣) with respect to the three windows indicated by the black bars. ∣NCC∣ measures whether segments of the Fourier transform are spectrally correlated to the chosen window. As discussed in Section 2.3, ∣NCC∣ peaks at secondary periodicities whose corresponding mode matches the periodicity in the window while mostly ignoring periodicities corresponding to different modes.
Paper: ADF22-WEB: Detection of a Molecular Gas Reservoir in a Massive Quiescent Galaxy Located in a z ≈ 3 Protocluster Core
Authors: Hideki Umehata, Mariko Kubo, Kouichiro Nakanishi
Figure caption: Gas mass fraction (﹩{f}_{{\rm{gas}}}={M}_{{{\rm{H}}}_{2}}/{M}_{* }﹩) as a function of redshift for ADF22 QGs and other QGs at z ≳ 1 (J. Spilker et al. 2018; S. Belli et al. 2021; C. C. Williams et al. 2021; C. Woodrum et al. 2022 for z ∼ 1; J. Scholtz et al. 2024 for z ∼ 3). For QGs at z ∼ 3, filled symbols represent cases with αCO = 4.4, while empty symbols indicate αCO = 0.8. For comparison, DSFGs at z ∼ 4–6 (D. A. Riechers et al. 2020, 2021; H. Umehata et al. 2020; J. E. Birkin et al. 2021; C.-L. Liao et al. 2024; F. Sun et al. 2024) are also plotted. The black solid and dashed lines show the scaling relation suggested by L. J. Tacconi et al. (2020) for z = 1–3 star-forming galaxies and its extrapolation. The red dashed (dotted) curves represent models with constant tdep = 0.45 Gyr (tdep = 0.25 Gyr), assuming external gas accretion halts at z = 5. The red solid and dotted–dashed lines indicate the evolution of gas fraction based on the star formation history from M. Kubo et al. (2021), assuming no gas inflows, for αCO = 4.4 and 0.8, respectively. The gas fractions of QGs at z ∼ 3 can be explained if gas accretion onto DSFGs at z = 4–6 is halted for some reason and the majority of the gas reservoirs is consumed afterward.
Paper: ADF22-WEB: Detection of a Molecular Gas Reservoir in a Massive Quiescent Galaxy Located in a z ≈ 3 Protocluster Core
Authors: Hideki Umehata, Mariko Kubo, Kouichiro Nakanishi
Figure caption: (a) The relation between stellar mass and SFR for the three ADF22 QGs at z = 3.09. Their SEDs indicate that they are nearly completely quenched, in sharp contrast to the star-forming main sequence (J. S. Speagle et al. 2014). The nondetections in the ALMA 1 mm map provide independent constraints. For comparison, GS-10578, a quiescent system at z = 3.064, is also shown (J. Scholtz et al. 2024). (b) The relation between CO(3–2) luminosity and SFR. The SED-based SFR suggests that star formation is significantly lower than expected based on the molecular gas mass, assuming the typical scaling for star-forming galaxies (L. J. Tacconi et al. 2013). (c) The relation between molecular gas mass and dust mass for ADF22 QGs, shown for two assumptions of αCO. For comparison, dusty star-forming galaxies (DSFGs) at z = 4–6 from the literature (D. A. Riechers et al. 2020, 2021; H. Umehata et al. 2020; J. E. Birkin et al. 2021; C.-L. Liao et al. 2024; F. Sun et al. 2024) and the stacked value for the normal SFGs at z = 2 (G. Popping et al. 2023) are plotted. The current depth of the dust continuum emission may not be sufficient to put a tight constraint on δgdr.
Paper: Dual Directional Expansion of Classical Cepheids in the Small Magellanic Cloud Revealed by Gaia Data Release 3
Authors: Satoya Nakano, 覚矢 中野, Kengo Tachihara, 研悟 立原
Figure caption: The relationship between Dstar and RV for the 91 objects in the clipped CC samples with available RV measurements. The blue star symbols represent the 37 massive Cepheids that match the massive star candidates identified by S. Nakano et al. (2025; see Figure 1), while the black circles indicate the remaining 54 CCs. The magenta dashed line represents the result of a linear fit, with a correlation coefficient of −0.095 for the plotted data. The uncertainties in Dstar are uniformly assumed to be 1.6 kpc (V. Ripepi et al. 2017).
Paper: Dual Directional Expansion of Classical Cepheids in the Small Magellanic Cloud Revealed by Gaia Data Release 3
Authors: Satoya Nakano, 覚矢 中野, Kengo Tachihara, 研悟 立原
Figure caption: The internal PMs of the clipped CC samples, obtained by subtracting the mean PM of the massive star candidates (S. Nakano et al. 2025). The color of the PM vectors represents their direction, with the angle defined counterclockwise from north (0∘) in the (x, y) coordinates based on the orthographic projection centered on the H I dynamical center (S. Stanimirović et al. 2004). The magenta and green star symbols represent the mean positions of the distant (>70 kpc) and nearby (<55 kpc) Cepheids, respectively. The thick vectors extending from the star symbols indicate the mean PM vectors of the distant and nearby Cepheids, drawn at 10 times the length of individual stellar vectors for better visibility.
Paper: Dual Directional Expansion of Classical Cepheids in the Small Magellanic Cloud Revealed by Gaia Data Release 3
Authors: Satoya Nakano, 覚矢 中野, Kengo Tachihara, 研悟 立原
Figure caption: A comparison of the RVs of the 91 clipped CC samples with available RV data and the spatial distribution of the H I redshifted and blueshifted components. The star symbols represent 37 massive Cepheids that match the massive star candidates identified by S. Nakano et al. (2025; see Figure 1). The circles indicate the remaining 54 CCs. The colors of the star symbols and circles correspond to the RV values of the CCs. In this figure, the RVs are shown in reference to the LSRK, consistent with the line-of-sight velocities of the H I. The white dotted arrow in the lower left of the figure indicates the direction in which the RV gradient is the largest.
Paper: Dual Directional Expansion of Classical Cepheids in the Small Magellanic Cloud Revealed by Gaia Data Release 3
Authors: Satoya Nakano, 覚矢 中野, Kengo Tachihara, 研悟 立原
Figure caption: The median PMs of the clipped CC samples at locations corresponding to each Superstructure (S. Nakano et al. 2025). The median PMs are derived from the clipped CC samples located within the 2σ elliptical regions, defined using the half-number radius of each Superstructure, as listed in Table 2 of S. Nakano et al. (2025). Since the ellipses of Superstructure 1 and 2 contain only zero and three CCs, respectively, their median values are not statistically significant and are therefore omitted from this figure. The background displays Hα emission from SHASSA in the range of 0–600 deciRayleighs (dR; J. E. Gaustad et al. 2001).
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Individual transits of BD+05 4868 Ab from the TESS light curve. Transits are numbered based on the cycle count from the first transit at t0,#1 =  2459798.2587 (BJD), taking into account the presence of gaps in the light curve. Transits 1–18 are from TESS Sector 55, while Transits 580–598 are from TESS Sector 82. The mean transit depth across these transits is 1.2%. Also indicated are the minimum (0.8%, dashed line) and maximum (2.0%, dotted line) transit depths across these observations. The red curve in each panel represents the model transit profile ﹩{ \mathcal T }(\phi )﹩ (Equation (1)) that is fit to each transit individually.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: The fit to the mean transit profile of BD+05 4868 A using the transit model ﹩{ \mathcal T }(\phi )﹩, which convolves the dust extinction profile ﹩{ \mathcal Y }(d)﹩ (Equation (1)) with the stellar disk. (a) Decomposition of ﹩{ \mathcal Y }(d)﹩ as a superposition of two generalized-Gaussian distributions representing the trailing and leading tails of the dust cloud. The areas beneath the extinction profiles described by these distributions are indicated by Ab and Af, respectively. (b) Comparison of the model fit with the observed mean transit profile from TESS data (red). The blue vertical line at ϕ = −0.024 indicates when the planet crosses the central longitude of the host star, with the hatched region indicating the star’s diameter.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: (a) Radiation pressure cross sections calculated using Mie theory. The cross sections are normalized by the geometric cross section of the dust grain and are displayed as a function of the grain size (radius) r. Solid curves show cross sections for illustrative materials with a real part of the index of refraction nr = 1.65 across a range of kr, the imaginary part of the index of refraction. Cross sections for representative astronomical minerals are displayed as nonsolid curves. (b) Calculated values of β from Equation (12), as a function of grain size for the same materials presented in (a). The purple band corresponds to a plausible range of 0.0025 < β < 0.07 for grains in the trailing tail, as inferred from BD+05 4868 Ab’s transits.