adsabs/AstroCLIMB huggingface dataset:
Paper: Volatile-rich Sub-Neptunes as Hydrothermal Worlds: The Case of K2-18 b
Authors: Cindy N. Luu, Xinting Yu, 馨婷 余, Christopher R. Glein, Hamish Innes, Artyom Aguichine, Joshua Krissansen-Totton, Julianne I. Moses, Shang-Min Tsai, Xi Zhang, Ngoc Truong, Jonathan J. Fortney
Figure caption: Logarithmically fitted Henry's law constants for CH4, CO2, and CO across temperatures between 444.15 K and 623.15 K represented by solid lines, with extrapolated values between 624.15 K and 647.15 K represented by dashed lines. Pressures correspond to water-saturated conditions as shown in Figure 2(a).
Paper: Volatile-rich Sub-Neptunes as Hydrothermal Worlds: The Case of K2-18 b
Authors: Cindy N. Luu, Xinting Yu, 馨婷 余, Christopher R. Glein, Hamish Innes, Artyom Aguichine, Joshua Krissansen-Totton, Julianne I. Moses, Shang-Min Tsai, Xi Zhang, Ngoc Truong, Jonathan J. Fortney
Figure caption: Possible conceptual structures for K2-18 b that were explored previously (R. Hu 2021; R. Hu et al. 2021; S.-M. Tsai et al. 2021; X. Yu et al. 2021; N. Madhusudhan et al. 2023b; G. J. Cooke & N. Madhusudhan 2024; F. E. Rigby et al. 2024; O. Shorttle et al. 2024; N. F. Wogan et al. 2024) and in this work.
Paper: Volatile-rich Sub-Neptunes as Hydrothermal Worlds: The Case of K2-18 b
Authors: Cindy N. Luu, Xinting Yu, 馨婷 余, Christopher R. Glein, Hamish Innes, Artyom Aguichine, Joshua Krissansen-Totton, Julianne I. Moses, Shang-Min Tsai, Xi Zhang, Ngoc Truong, Jonathan J. Fortney
Figure caption: (a)–(c) Aqueous and (d)–(f) gaseous CO/CO2 ratios. The symbols and colors are labeled the same way as in Figure 3. The region of uncertainty surrounding the curves is due to the one-offset error for the CH4/CO2 ratio.
Paper: Millinovae: A New Class of Transient Supersoft X-Ray Sources without a Classical Nova Eruption
Authors: Przemek Mróz, Krzysztof Król, Hélène Szegedi, Philip Charles, Kim L. Page, Andrzej Udalski, David A. H. Buckley, Gulab Dewangan, Pieter Meintjes, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Upper panels: on-sky view of the LMC (upper left) and SMC (upper right) with positions of millinovae marked. Middle panels: dereddened color–magnitude diagrams for stars in the LMC. Blue points mark (V − I)0 and MI of millinovae in quiescence (middle left) and in outburst (middle right). The prototype, ASASSN-16oh, is marked with a red asterisk, and OGLE-mNOVA-11 is marked with a green cross. Lower panels: histograms of MI of millinovae, classical novae, and dwarf novae in quiescence (lower left) and in outburst (lower right). Data were taken from H. Ritter & U. Kolb (2003), W. Pietsch (2010), and Gaia Collaboration et al. (2023). The background images of the LMC and SMC were generated with BSRENDER written by Kevin Loch, using the ESA/Gaia database.
Paper: Millinovae: A New Class of Transient Supersoft X-Ray Sources without a Classical Nova Eruption
Authors: Przemek Mróz, Krzysztof Król, Hélène Szegedi, Philip Charles, Kim L. Page, Andrzej Udalski, David A. H. Buckley, Gulab Dewangan, Pieter Meintjes, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Example light curves of millinovae. The upper panel shows the prototype, ASASSN-16oh. The y-axis ticks are every 0.5 mag. There is a gap in the data between 2020.4 and 2022.4.
Paper: Millinovae: A New Class of Transient Supersoft X-Ray Sources without a Classical Nova Eruption
Authors: Przemek Mróz, Krzysztof Król, Hélène Szegedi, Philip Charles, Kim L. Page, Andrzej Udalski, David A. H. Buckley, Gulab Dewangan, Pieter Meintjes, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Photometric and X-ray observations of the 2023/2024 outburst of OGLE-mNOVA-11. Dotted lines mark times of SALT spectroscopic observations.
Paper: Millinovae: A New Class of Transient Supersoft X-Ray Sources without a Classical Nova Eruption
Authors: Przemek Mróz, Krzysztof Król, Hélène Szegedi, Philip Charles, Kim L. Page, Andrzej Udalski, David A. H. Buckley, Gulab Dewangan, Pieter Meintjes, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Orbital period (Porb)–decline rate (τd) relation for dwarf nova outbursts, using data from V. Simon (2021), and extended to include the range of decline rates (gray area) observed in millinovae (20 ≲ τd ≲ 70 day mag−1). The red asterisk and green diamond mark the locations of ASASN-16oh (A. Rajoelimanana et al. 2017) and OGLE-mNOVA-08, respectively.
Paper: Millinovae: A New Class of Transient Supersoft X-Ray Sources without a Classical Nova Eruption
Authors: Przemek Mróz, Krzysztof Król, Hélène Szegedi, Philip Charles, Kim L. Page, Andrzej Udalski, David A. H. Buckley, Gulab Dewangan, Pieter Meintjes, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: SALT spectroscopic observations of the 2023/2024 outburst of OGLE-mNOVA-11 reveal narrow emission lines, including He II (4686 Å) and Bowen blend.
Paper: Millinovae: A New Class of Transient Supersoft X-Ray Sources without a Classical Nova Eruption
Authors: Przemek Mróz, Krzysztof Król, Hélène Szegedi, Philip Charles, Kim L. Page, Andrzej Udalski, David A. H. Buckley, Gulab Dewangan, Pieter Meintjes, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Example light curves of millinovae (continuation of Figure 1).
Paper: Millinovae: A New Class of Transient Supersoft X-Ray Sources without a Classical Nova Eruption
Authors: Przemek Mróz, Krzysztof Król, Hélène Szegedi, Philip Charles, Kim L. Page, Andrzej Udalski, David A. H. Buckley, Gulab Dewangan, Pieter Meintjes, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Quiescent light curve of OGLE-mNOVA-08 folded with the orbital period Porb = 4.830893 days.
Paper: Silicon Isotopic Composition of Mainstream Presolar SiC Grains Revisited: The Impact of Nuclear Reaction Rate Uncertainties
Authors: Hung Kwan Fok, Marco Pignatari, Benoît Côté, Reto Trappitsch
Figure caption: Silicon isotope integrated stellar yield variations for the 12 M⊙ and 25 M⊙ stars at Z = 0.01 and Z = 0.02. The dotted horizontal line indicates the unmodified stellar yields. The variations in the integrated yields are shown as boxes and bars for the 50% and 95% confidence interval, respectively. The top panel shows the yield variation factors using the Si (n, γ) rates by K. H. Guber et al. (2003), and the bottom panel uses the rates by Z. Y. Bao et al. (2000). Note that the dashed line at unity represents in both cases the original stellar models, which used the Si (n, γ) rates by K. H. Guber et al. (2003). Clearly, the largest effects due to nuclear reaction rate uncertainties are seen in 29Si.
Paper: Silicon Isotopic Composition of Mainstream Presolar SiC Grains Revisited: The Impact of Nuclear Reaction Rate Uncertainties
Authors: Hung Kwan Fok, Marco Pignatari, Benoît Côté, Reto Trappitsch
Figure caption: Schematic overview of the GCE pipeline that we employ in this work to study the effects of nuclear reaction rate uncertainties on the evolution of silicon isotopes in the Milky Way. The gray scale shows schematically how uncertainties propagate through the model and how small initial uncertainties can have a large effect on predicting isotopic compositions.
Paper: Silicon Isotopic Composition of Mainstream Presolar SiC Grains Revisited: The Impact of Nuclear Reaction Rate Uncertainties
Authors: Hung Kwan Fok, Marco Pignatari, Benoît Côté, Reto Trappitsch
Figure caption: Comparison of GCE model predictions of silicon isotope evolution using different stellar yield sets with presolar SiC mainstream grains (SiC M). The simulated time range is between 4.2 Ga prior to solar system formation (left-hand side of the model lines) up to solar system formation (right-hand side of model lines). Citation key: N13—K. Nomoto et al. (2013), LC18—M. Limongi & A. Chieffi (2018), R18—C. Ritter et al. (2018b). Presolar grain measurements are taken from the presolar grain database (T. Stephan et al. 2024).
Paper: Silicon Isotopic Composition of Mainstream Presolar SiC Grains Revisited: The Impact of Nuclear Reaction Rate Uncertainties
Authors: Hung Kwan Fok, Marco Pignatari, Benoît Côté, Reto Trappitsch
Figure caption: Slope distribution of the silicon isotope correlation line based on varying the nuclear reaction rates within the described uncertainties. Each histogram was calculated at a given time in GCE history prior to solar system formation. Dotted lines represent the 95% confidence intervals, while the dashed line shows the measured slope by analyzing presolar SiC mainstream grains (T. Stephan et al. 2024). The top histograms (blue) show the slope distribution when using the 28,29,30Si(n, γ) rates by K. H. Guber et al. (2003), and the bottom histograms (orange) use the rates by Z. Y. Bao et al. (2000).
Paper: Silicon Isotopic Composition of Mainstream Presolar SiC Grains Revisited: The Impact of Nuclear Reaction Rate Uncertainties
Authors: Hung Kwan Fok, Marco Pignatari, Benoît Côté, Reto Trappitsch
Figure caption: Silicon abundance at the end of the CCSN explosion within the explosive silicon production zone of the 12 M⊙ (top) and 25 M⊙ (bottom) stars for Z = 0.01 (left) and Z = 0.02 (right). Lines represent the unmodified abundance, as in C. Ritter et al. (2018b). Shaded areas show the overall range for 10,000 MC simulations while varying the nuclear reactions rates, while the dotted lines show the 95% confidence interval of our MC simulations.
Paper: Silicon Isotopic Composition of Mainstream Presolar SiC Grains Revisited: The Impact of Nuclear Reaction Rate Uncertainties
Authors: Hung Kwan Fok, Marco Pignatari, Benoît Côté, Reto Trappitsch
Figure caption: Convergence test of our MC model. Clearly, the mean silicon isotope correlation lines have converged well at our chosen value after several thousand MC runs, showing that our results will not change when running more than 10,000 simulations.
Paper: Silicon Isotopic Composition of Mainstream Presolar SiC Grains Revisited: The Impact of Nuclear Reaction Rate Uncertainties
Authors: Hung Kwan Fok, Marco Pignatari, Benoît Côté, Reto Trappitsch
Figure caption: Isotopic abundances of silicon isotopes at a given mass coordinate for representative 1D trajectories taken for the 12 M⊙ (top) and 25 M⊙ (bottom) stars for Z = 0.01 (left) and Z = 0.02 (right).
Paper: Quantitative Constraint on the Contribution of Resolved Gamma-Ray Sources to the Sub-PeV Galactic Diffuse Gamma-Ray Flux Measured by the Tibet ASγ Experiment
Authors: S. Kato, M. Anzorena, D. Chen, K. Fujita, R. Garcia, J. Huang, G. Imaizumi, T. Kawashima, K. Kawata, A. Mizuno, M. Ohnishi, T. Sako, T. K. Sako, F. Sugimoto, M. Takita, Y. Yokoe
Figure caption: Tibet diffuse flux (orange points) compared with the total gamma-ray flux of the sub-PeV LHAASO sources plus the Cygnus Cocoon that is not masked in the Tibet diffuse analysis (source flux, blue solid curve). The comparison is made for regions A (left panel) and B (right panel). The statistical error of the Tibet diffuse flux is shown with the orange vertical bars, while the yellow vertical bars show the quadrature sum of the statistical and systematic errors. The blue shaded band shows the error of the source flux; see the text for detailed descriptions of the error calculation. The downward arrows at 100 TeV and 1 PeV indicate that the calculated source flux should be regarded as the upper limit in the sub-PeV energy range; see the text. The gray lines show the best-fit energy spectra of some sources that largely contribute to the source flux in the sub-PeV energy range; see the text and Appendix B.
Paper: Quantitative Constraint on the Contribution of Resolved Gamma-Ray Sources to the Sub-PeV Galactic Diffuse Gamma-Ray Flux Measured by the Tibet ASγ Experiment
Authors: S. Kato, M. Anzorena, D. Chen, K. Fujita, R. Garcia, J. Huang, G. Imaizumi, T. Kawashima, K. Kawata, A. Mizuno, M. Ohnishi, T. Sako, T. K. Sako, F. Sugimoto, M. Takita, Y. Yokoe
Figure caption: Same as the left panel of Figure 2 but additionally shows the source flux of unresolved leptonic sources estimated by K. Samy et al. (2024; green points). This leptonic source flux is estimated for the inner Galactic plane region observed by LHAASO when no masking scheme is adopted. Therefore, the flux should be regarded as a stringent upper limit on the contribution of unresolved leptonic sources to the Tibet diffuse flux in region A. The vertical error bars of the green point indicate the standard deviation obtained for the 100 simulations performed by K. Samy et al. (2024).
Paper: Quantitative Constraint on the Contribution of Resolved Gamma-Ray Sources to the Sub-PeV Galactic Diffuse Gamma-Ray Flux Measured by the Tibet ASγ Experiment
Authors: S. Kato, M. Anzorena, D. Chen, K. Fujita, R. Garcia, J. Huang, G. Imaizumi, T. Kawashima, K. Kawata, A. Mizuno, M. Ohnishi, T. Sako, T. K. Sako, F. Sugimoto, M. Takita, Y. Yokoe
Figure caption: Positions and extensions of the sub-PeV LHAASO sources and the Cygnus Cocoon (blue circles) shown in the Galactic coordinates. The extensions have 95% containment radii. The point-like sources with only upper limits on the extensions are plotted with the blue dots. The large circle with a radius of ≃5° centered at (l, b) ≃ (﹩79\mathop{.}\limits^{^\circ }6﹩, ﹩1\mathop{.}\limits^{^\circ }2﹩) shows the extension of LHAASO J2027+4119 to represent that of the Cygnus Cocoon; see the text. The gray circles with a fixed radius of ﹩0\mathop{.}\limits^{^\circ }5﹩ enclose the sky regions masked in the Tibet diffuse analysis (M. Amenomori et al. 2021).
Paper: Quantitative Constraint on the Contribution of Resolved Gamma-Ray Sources to the Sub-PeV Galactic Diffuse Gamma-Ray Flux Measured by the Tibet ASγ Experiment
Authors: S. Kato, M. Anzorena, D. Chen, K. Fujita, R. Garcia, J. Huang, G. Imaizumi, T. Kawashima, K. Kawata, A. Mizuno, M. Ohnishi, T. Sako, T. K. Sako, F. Sugimoto, M. Takita, Y. Yokoe
Figure caption: Same as Figure 2 but additionally shows the source flux including the contribution from all the 1LHAASO catalog sources detected above 25 TeV plus the Cygnus Cocoon (green solid curves and shaded bands).
Paper: The Impact of Shear on Disk Galaxy Star Formation Rates
Authors: Xena Fortune-Bashee, Jiayi Sun, 嘉懿 孙, Jonathan C. Tan
Figure caption: (a) Top left: similar to Figure 2(a), total SFE per orbit, ϵorb, vs. rotation curve gradient, β, for 32 PHANGS-ALMA galaxies with molecular and atomic gas data. Barred/nonbarred annuli are shown in blue/red, respectively. Median values of ϵorb of the combined sample in bins of Δβ = 0.05 with ≥10 data points are shown by black points. In this range of β, we also show medians of barred/nonbarred annuli with dark blue/red points, respectively. Best-fitting functions to the medians of form ϵorb = ϵorb,0(1 − αCCβ) are shown by the black, blue, and red lines for total, barred, and nonbarred samples, respectively. (b) Top right: as (b), but now for SFE from molecular gas per orbit, ϵorb,mol, vs. β, for 49 PHANGS-ALMA galaxies. (c) Bottom left: as (a), but now showing “galaxy-normalized efficiency”, ﹩{\epsilon }_{\mathrm{orb}}^{* }﹩. (d) Bottom right: as (b), but now showing ﹩{\epsilon }_{\mathrm{orb},\mathrm{mol}}^{* }﹩.
Paper: The Impact of Shear on Disk Galaxy Star Formation Rates
Authors: Xena Fortune-Bashee, Jiayi Sun, 嘉懿 孙, Jonathan C. Tan
Figure caption: (a) Top left: total SFE per orbit, ϵorb, vs. rotation curve gradient, β, for 321 annuli located in 32 PHANGS-ALMA galaxies with observations probing molecular and atomic gas (gray points). Black points show the median values of ϵorb in bins of Δβ = 0.05 that have at least 10 data points, with associated error bars showing the uncertainties in the median. The solid black line shows the best-fit function of the form ϵorb = ϵorb,0(1 − αCCβ) to the binned medians with β ≤ 0.5, with αCC reported in the upper right corner of each panel. The red dotted line shows the equivalent fit with a fixed αCC = 0.7, i.e., the prediction of the shear-driven GMC collision model. (b) Top right: as (a), but now excluding annuli within r = 1 kpc. (c) Bottom left: as (a), but with ϵorb normalized by the median value of each galaxy (i.e., “galaxy-normalized” ﹩{\epsilon }_{\mathrm{orb}}^{* }﹩). (d) Bottom right: as (c), but now excluding annuli within r = 1 kpc. A trend of declining efficiency with increasing β is seen in all cases.
Paper: The Impact of Shear on Disk Galaxy Star Formation Rates
Authors: Xena Fortune-Bashee, Jiayi Sun, 嘉懿 孙, Jonathan C. Tan
Figure caption: (a) Top left: SFE from molecular gas per orbit, ϵorb,mol, vs. rotation curve gradient, β, for 489 annuli located in 49 PHANGS-ALMA galaxies (gray points). Median values of ϵorb,mol in bins of Δβ = 0.05 that have ≥10 data points are shown by black points, with uncertainties shown by the error bars. The best-fitting function of the form ϵorb,mol = ϵorb,mol,0(1 − αCC,molβ) to median values with β ≤ 0.5 is shown by the solid black line, with αCC,mol reported in the upper right. The red dotted line shows the equivalent fit when αCC,mol = 0.7. (b) Top right: as (a), but now excluding annuli within r = 1 kpc. (c) Bottom left: as (a), but now showing the “galaxy-normalized efficiency,” ﹩{\epsilon }_{\mathrm{orb},\mathrm{mol}}^{* }﹩. (d) Bottom right: as (c), but now excluding annuli within r = 1 kpc.
Paper: The Impact of Shear on Disk Galaxy Star Formation Rates
Authors: Xena Fortune-Bashee, Jiayi Sun, 嘉懿 孙, Jonathan C. Tan
Figure caption: Example data set for NGC 4321. The top panel shows the radial profile of mass surface density of total (black solid), molecular (blue dotted), and atomic gas (orange dotted). The second and third panels show orbital velocity and its logarithmic derivative, β. The fourth panel shows the observed SFR surface density profile (solid) and theoretical predictions of the J. C. Tan (2000) shear-driven GMC collision model, ΣSFR = BΩΣgasΩ(1–0.7β) (dashed), and the dynamical KS model (B. G. Elmegreen 1997; J. Silk 1997) with a fixed SFE per orbit, i.e., ΣSFR = BΩΣgasΩ with BΩ = 8 × 10−3 (dotted). The fifth panel shows observed SFE per orbit with reference to the total gas as well as theoretically predicted values (the same models as in the fourth panel). The sixth panel is the same as the fifth, but now showing SFE per orbit with reference to the molecular gas.
Paper: Comprehensive Study of Near-Earth Asteroid 2024 MK: Testing Planetary Encounters as a Source for Surface Refreshing
Authors: Lauren E. McGraw, Cristina A. Thomas, Tim A. Lister, Becky J. Williams, Andy S. Rivkin, Bryan Holler, Leslie A. Young
Figure caption: (A) NIR spectra of 2024 MK taken before (orange) and after (blue) its close Earth approach. Spectra are normalized to 1 at 2.25 μm. (B) Ratio of postapproach reflectance spectrum to preapproach spectrum. Red dashed line represents unity, i.e., where pre- and postapproach data are equal. The two spectra are nominally identical, except the preapproach spectrum exhibits a slightly deeper Band I than the postapproach spectrum. (C) The average 2024 MK NIR spectrum compared to the archetypal average Q-, Sq-, and S-type spectra used for classification (F. E. DeMeo et al. 2009), normalized to 1 at 1.2 μm. Dashed lines represent the slope for each spectrum. S-complex spectral types are more difficult to distinguish using NIR data alone. (D) The average 2024 MK VNIR spectrum compared to the archetypal average Q-, Sq-, and S-type spectra used for classification (F. E. DeMeo et al. 2009), normalized to 1 at 0.55 μm. Dashed lines represent the slope for each spectrum. Addition of visible data enables more robust spectral-type determination. (E) S-subtype (M. J. Gaffey et al. 1993) plot zoomed in to the “ordinary chondrite boot” with ordinary chondrite subtype lines from (T. L. Dunn et al. 2010). 2024 MK plots as an L-type ordinary chondrite, as shown by the purple star. (F) Ferrosilite mole percent vs. fayalite mole percent plot from M. P. Lucas et al. (2018) that confirms 2024 MK is an L-type ordinary chondrite analog.
Paper: Comprehensive Study of Near-Earth Asteroid 2024 MK: Testing Planetary Encounters as a Source for Surface Refreshing
Authors: Lauren E. McGraw, Cristina A. Thomas, Tim A. Lister, Becky J. Williams, Andy S. Rivkin, Bryan Holler, Leslie A. Young
Figure caption: NIR LXD spectrum of 2024 MK taken after its close Earth approach. Blue points represent thermally corrected reflectance data. Red dashed line represents reflected continuum. Spectra are normalized to 1 at 2.25 μm. (A) Thermally corrected spectrum when fitting thermal model to 3.5–4.0 μm. (B) Thermally corrected spectrum when fitting thermal model to 3.3–3.5 μm. Both methods yield no hydration band and show the poor overall fit of the thermal model.
Paper: Constraining the Progenitor of the Nearby Type II-P SN 2024ggi with Environmental Analysis
Authors: Xinyi Hong, Ning-Chen Sun, Zexi Niu, Junjie Wu, Qiang Xi, Jifeng Liu
Figure caption: CMDs of all stellar sources in the environment of SN 2024ggi. In all panels, the blue, green, and red isochrones correspond to stellar populations with ages of log(t/yr) = 7.41, 7.75, and 8.09, respectively. The arrows in the upper-left corner are reddening vectors for RV = 3.1 and total extinctions ﹩{A}_{V}^{{\rm{total}}}﹩ = 0.52, which correspond to a best-fitting host extinction ﹩{A}_{V}^{{\rm{host}}}﹩ = 0.30 and a Milky Way reddening of E(B − V)MW = 0.072 mag.
Paper: Constraining the Progenitor of the Nearby Type II-P SN 2024ggi with Environmental Analysis
Authors: Xinyi Hong, Ning-Chen Sun, Zexi Niu, Junjie Wu, Qiang Xi, Jifeng Liu
Figure caption: F435W/F555W/F814W three-color composite image of the environment of SN 2024ggi by HST observations. The white circle in panel (b) has a radius of 100 pc, within which we studied the star formation history in the local environment.