adsabs/AstroCLIMB huggingface dataset:
Paper: Transient Gamma Rays from the 2021 Outburst of the Recurrent Nova RS Ophiuchi: The Effect of Gamma-Ray Absorption
Authors: Vo Hong Minh Phan, Pierre Cristofari, Enrico Peretti, Vincent Tatischeff, Andrea Ciardi
Figure caption: Schematic view of the system.
Paper: The Milky Way Is a Less Massive Galaxy—New Estimates of the Milky Way’s Local and Global Stellar Masses
Authors: Jianhui Lian, Tao Wang, Qikang Feng, Yang Huang, Helong Guo
Figure caption: Vertical mass density profiles of living stars and stellar remnants. Asymmetric and offset density models with exponential, sech2, and sech2/n profiles are applied to fit the vertical density profiles as shown in the right panel. In the left panel, only the best-fitted exponential model for the living stars is included as shown in the black line.
Paper: Simultaneous Optical and Radio Observations of a Large Stellar Flare on EV Lac
Authors: Hong-Peng Lu, Jia-Le Zhang, Hui Tian, Li-Yun Zhang, He-Chao Chen, Jie Zheng, Jun-Bo Zhang, Jian-Guo Wang, Shun Inoue, Hiroyuki Maehara, Kosuke Namekata
Figure caption: Results of simultaneous optical and radio observations of a full-phase stellar flare on EV Lac from 12:00 to 15:00 UT on 2022 October 25. (A) Normalized TESS light curve. (B) Normalized light curves in the U, B, and V bands observed with the 85 cm telescope. (C) Time evolution of the EW of Hα (6562.8 Å), Hβ (4861.3 Å), Hγ (4340.5 Å), and Hδ (4101.7 Å) lines, observed with the 2.16 m telescope, calculated after subtracting the reference spectrum. (D) Stokes V dynamic spectra from FAST radio observations. Positive values indicate LCP emission. The two vertical gray dashed lines in each panel mark the interval during which blue wing enhancement was detected in the Hα line profile.
Paper: Simultaneous Optical and Radio Observations of a Large Stellar Flare on EV Lac
Authors: Hong-Peng Lu, Jia-Le Zhang, Hui Tian, Li-Yun Zhang, He-Chao Chen, Jie Zheng, Jun-Bo Zhang, Jian-Guo Wang, Shun Inoue, Hiroyuki Maehara, Kosuke Namekata
Figure caption: Fitting results of the 20th Hα line profile using a double-Gaussian model and a two-cloud model. Panel (A) shows the double-Gaussian fitting result, with the reduced chi-square (﹩{\chi }_{\nu }^{2}﹩; H. Peter 2001; H. Tian et al. 2011) of 3.66 indicated in the upper left corner. Panel (B) presents the two-cloud model fitting result, performed using the Markov Chain Monte Carlo (MCMC; D. W. Hogg & D. Foreman-Mackey 2018) method. The posterior distributions of the model parameters are unimodal and well-converged, and the 1σ confidence interval is shown as the shaded region.
Paper: The Milky Way Is a Less Massive Galaxy—New Estimates of the Milky Way’s Local and Global Stellar Masses
Authors: Jianhui Lian, Tao Wang, Qikang Feng, Yang Huang, Helong Guo
Figure caption: Circular velocity decomposition based on our new stellar mass surface density profile. Observational results are taken from Y. Zhou et al. (2023). The disk component is calculated based on the mass profile presented in Figure 2. We separate the disk into low- and high-α parts based on a chemical definition. The bulge and gas disk components are calculated based on the density profiles taken from J. Binney & P. McMillan (2011). The sum of all baryon components are denoted as the longest dashed curve in brown. The contribution of DM is set free and fitted, assuming an NFW mass density profile with the best-fitted scaling radius (rs) and characteristic density (ρs) presented in the figure.
Paper: Simultaneous Optical and Radio Observations of a Large Stellar Flare on EV Lac
Authors: Hong-Peng Lu, Jia-Le Zhang, Hui Tian, Li-Yun Zhang, He-Chao Chen, Jie Zheng, Jun-Bo Zhang, Jian-Guo Wang, Shun Inoue, Hiroyuki Maehara, Kosuke Namekata
Figure caption: Analysis of red–blue wing asymmetry in the Hα, Hβ, Hγ, and Hδ Balmer line profiles during the flare. (A) Evolution of the time-sequenced Hα line profiles: the first four black profiles correspond to the preflare phase, the 5th to 16th red profiles correspond to the first flare peak, and the 17th to 32nd blue profiles correspond to the second flare peak. (B) Difference between the EWs of the red and blue wings for the four Balmer lines. (C) Doppler velocity evolution derived from Gaussian fitting of the time-sequenced Hα line profiles. (D) Comparison of the 20th Hα line profile with the reference profile, with vertical dashed lines indicating the rest wavelength of the Hα line and a blueshifted velocity of −200 km s−1.
Paper: The Milky Way Is a Less Massive Galaxy—New Estimates of the Milky Way’s Local and Global Stellar Masses
Authors: Jianhui Lian, Tao Wang, Qikang Feng, Yang Huang, Helong Guo
Figure caption: Radial surface mass density profile of various stellar objects. The thin dashed line in the left panel represents an exponential profile with scale length of 2.1 kpc. Each type of stellar object is separated into mono-age populations shown in colorful lines in the right four panels. Shade regions indicate 1σ uncertainties of the density measurements.
Paper: Simultaneous Optical and Radio Observations of a Large Stellar Flare on EV Lac
Authors: Hong-Peng Lu, Jia-Le Zhang, Hui Tian, Li-Yun Zhang, He-Chao Chen, Jie Zheng, Jun-Bo Zhang, Jian-Guo Wang, Shun Inoue, Hiroyuki Maehara, Kosuke Namekata
Figure caption: Evolution of stellar flare blackbody temperature estimated from UBV-band photometric data.
Paper: Simultaneous Optical and Radio Observations of a Large Stellar Flare on EV Lac
Authors: Hong-Peng Lu, Jia-Le Zhang, Hui Tian, Li-Yun Zhang, He-Chao Chen, Jie Zheng, Jun-Bo Zhang, Jian-Guo Wang, Shun Inoue, Hiroyuki Maehara, Kosuke Namekata
Figure caption: Flare emission enhancement ratio (﹩\frac{{\rm{\Delta }}{L}_{U}+{\rm{\Delta }}{L}_{V}}{{\rm{\Delta }}{L}_{U}+{\rm{\Delta }}{L}_{B}}﹩) as a function of the stellar flare blackbody temperature. The plot shows the variation in this ratio for stellar flare blackbody temperatures ranging from 1000 K to 31,000 K.
Paper: Simultaneous Optical and Radio Observations of a Large Stellar Flare on EV Lac
Authors: Hong-Peng Lu, Jia-Le Zhang, Hui Tian, Li-Yun Zhang, He-Chao Chen, Jie Zheng, Jun-Bo Zhang, Jian-Guo Wang, Shun Inoue, Hiroyuki Maehara, Kosuke Namekata
Figure caption: Circularly polarized radio bursts of EV Lac. (A) Stokes V dynamic spectrum of the entire 3 hr radio observation on 2022 October 25. Red dashed lines mark the positive frequency-drifting features. Orange bars indicate the time intervals shown in the zoom-in panels. (B–E) Detailed substructures of the positive frequency-drifting radio bursts. Measured frequency drift rates are annotated.
Paper: Further Evidence for a Direct-collapse Origin of the Supermassive Black Hole at the Center of the ∞ Galaxy
Authors: Pieter van Dokkum, Gabriel Brammer, Connor Jennings, Imad Pasha, Josephine F. W. Baggen
Figure caption: Emission line fits in the central pixel. Left: the [O III] λ5007 line. The line profile has a blue wing and is modeled as a combination of two Gaussians (red line). The average [O III] line profile of the Type 1 SDSS AGN is also shown (blue). Middle: the Hβ line is modeled with a combination of the [O III] profile and a broad component, with FWHM = 970 ± 123 km s−1. Right: residual of the Hβ line isolating the broad component, after subtracting the best-fitting scaled [O III] profile.
Paper: Further Evidence for a Direct-collapse Origin of the Supermassive Black Hole at the Center of the ∞ Galaxy
Authors: Pieter van Dokkum, Gabriel Brammer, Connor Jennings, Imad Pasha, Josephine F. W. Baggen
Figure caption: Left: velocities in the ∞ galaxy, with respect to the redshift of the SMBH. Spaxels are ﹩0\mathop{.}\limits{^{\prime\prime} }05\times 0\mathop{.}\limits{^{\prime\prime} }05﹩ near the SMBH and ﹩0\mathop{.}\limits{^{\prime\prime} }1\times 0\mathop{.}\limits{^{\prime\prime} }1﹩ elsewhere. Right: line widths. The kinematics of the galaxy are complex, with strong local velocity gradients and several regions with very broad emission lines. The broadest lines are seen in the two nuclei and in the gas that connects them.
Paper: Further Evidence for a Direct-collapse Origin of the Supermassive Black Hole at the Center of the ∞ Galaxy
Authors: Pieter van Dokkum, Gabriel Brammer, Connor Jennings, Imad Pasha, Josephine F. W. Baggen
Figure caption: Velocity distribution in the ∞ system. The open histogram shows all spaxels in the ﹩0\mathop{.}\limits{^{\prime\prime} }1﹩ cube; the blue histogram shows spaxels in the ﹩0\mathop{.}\limits{^{\prime\prime} }05﹩ cube that are within a distance of ﹩0\mathop{.}\limits{^{\prime\prime} }15﹩ of the SMBH. The gray band indicates the uncertainty in the redshift of the SMBH of ±35 km s−1. The SMBH’s velocity is within ∼50 km s−1 of that of the surrounding gas.
Paper: Further Evidence for a Direct-collapse Origin of the Supermassive Black Hole at the Center of the ∞ Galaxy
Authors: Pieter van Dokkum, Gabriel Brammer, Connor Jennings, Imad Pasha, Josephine F. W. Baggen
Figure caption: Spectra of ﹩0\mathop{.}\limits{^{\prime\prime} }2\times 0\mathop{.}\limits{^{\prime\prime} }2﹩ regions centered on the two nuclei. Both nuclei show very broad Hα emission, in addition to a narrow Hα + [N II] component. The line widths of the broad components are FWHM = 2850 km s−1 and FWHM =2480 km s−1 for ∞ SE and ∞ NW, respectively. There are evidently three active SMBHs in the ∞ system.
Paper: Discovery of the Second Y+Y Dwarf Binary System: CWISEP J193518.59-154620.3
Authors: Matthew De Furio, Jacqueline Kelly Faherty, Daniella C. Bardalez Gagliuffi, Jonathan Gagné, Eileen C. Gonzales, Rocio Kiman, Marc Kuchner, Federico Marocco, Sherelyn Alejandro Merchan, Melanie Rowland, Adam C. Schneider, Genaro Suárez, Johanna M. Vos
Figure caption: Simultaneous single PSF fitting to F1000W and F1280W data of W1935. The left column shows a cutout of the data, the middle column shows the PSF model, and the right column shows the residual. The first row shows a single-PSF fit for the first dither in F1000W, the second row for the second dither in F1000W, the third row for the first dither in F1280W, and the fourth row for the second dither in F1280W. The single-PSF fit gives a ﹩{\chi }_{\nu }^{2}﹩ = 2.3. Residuals follow the expected pattern in the core for a single-PSF fit to the photocenter of a binary, i.e., negative residuals in the core (model overestimate of flux) and positive residuals immediately away from the core (model underestimate of flux). Units are in counts s−1. Each image has a size of 17 by 17 pixels.
Paper: Discovery of the Second Y+Y Dwarf Binary System: CWISEP J193518.59-154620.3
Authors: Matthew De Furio, Jacqueline Kelly Faherty, Daniella C. Bardalez Gagliuffi, Jonathan Gagné, Eileen C. Gonzales, Rocio Kiman, Marc Kuchner, Federico Marocco, Sherelyn Alejandro Merchan, Melanie Rowland, Adam C. Schneider, Genaro Suárez, Johanna M. Vos
Figure caption: Simultaneous double-PSF fitting to F1000W and F1280W data of W1935, arranged as in Figure 1. Double-PSF fit gives a ﹩{\chi }_{\nu }^{2}﹩ = 1.4. Residuals follow the expected pattern for a good model fit to the data, i.e., random noise. The red x marks the location of W1935A, and the blue circle marks the location of W1935B.
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Left: absolute B-band light curve of SN 2024uwq in comparison with SNe IIb in the literature, with a zoom-in on the earliest phases shown in the inset. Right: extinction-corrected U − B, B − V, g − r, and r − i color evolution of SN 2024uwq in comparison to the color evolution of typical SNe IIb. We use the relationships prescribed in K. Jordi et al. (2006) for converting V − R, R − I to g − r, r − i, respectively (for SN 1993J, SN 2011dh, SN 2011ei, SN 2011fu, and SN 2013df). Data used in this figure are from M. W. Richmond et al. (1994; SN 1993J), A. Pastorello et al. (2008; SN 2008ax), I. Arcavi et al. (2011; SN 2011dh), A. Morales-Garoffolo et al. (2015; SN 2011fu), A. Morales-Garoffolo et al. (2014; SN 2013df), and L. Tartaglia et al. (2017) and C. D. Kilpatrick et al. (2022; SN 2016gkg).
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Multiwavelength observations of SN 2024uwq with early phases of the light curve showing characteristic SCE from the progenitor. The offsets for each bands are marked in the legend. The time of explosion is marked in the left panel, which zooms in on the early light-curve evolution. The observations provided in this figure are not corrected for extinction. The gray vertical lines mark the phases where optical spectra were obtained. The photometric data used to generate this figure are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq
Authors: Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell, Curtis McCully
Figure caption: Top: composite gri image of SN 2024uwq obtained using Las Cumbres Observatory observations on 2024 September 28. SN 2024uwq is marked with white cross hairs in the composite image. Bottom: normalized spectrum of SN 2024uwq showing Na I D absorption from the MW (blue) and host galaxy (pink), used to estimate line-of-sight extinction.
Paper: Tidal Suppression of Fuzzy Dark Matter Heating in Milky Way Satellite Galaxies
Authors: Yu-Ming Yang, Zhao-Chen Zhang, Xiao-Jun Bi, Peng-Fei Yin
Figure caption: Tidal suppression of FDM-induced dynamical heating in Fornax. Vertical dashed lines indicate the 2D half-light radius. Solid and dotted lines represent the line-of-sight velocity dispersion profiles obtained from simulations and by solving the Jeans equation, respectively. Cyan lines denote the initial state (t = −10 Gyr), while red, green, and blue lines represent the final states (t = 0 Gyr) under conditions of no, weak, and strong tidal effects, respectively. The pink shaded area between the green and blue solid lines reflects the uncertainties arising from the Galactic halo density parameter ρ0,h and the Fornax’s orbital parameters. The vertical light blue band indicates the 1σ uncertainty range of the 2D half-light radius derived in M. Y. Wang et al. (2019), due to the uncertainty in Fornax’s distance. Gray and black points with error bars represent velocity dispersion data from M. G. Walker et al. (2009) and M. A. Breddels & A. Helmi (2013), respectively.
Paper: Tidal Suppression of Fuzzy Dark Matter Heating in Milky Way Satellite Galaxies
Authors: Yu-Ming Yang, Zhao-Chen Zhang, Xiao-Jun Bi, Peng-Fei Yin
Figure caption: Left: 3D FDM density field. These panels show the 3D FDM density distribution, ρFDM(t, x) = ma∣ψ(t, x)∣2, on a plane centered on the solitonic core. The upper-left panel depicts the initial state at t = −10 Gyr, while the remaining panels show the final states under no, weak, and strong tidal conditions, respectively. Right: 2D stellar density field. The panels display stellar density maps obtained via the particle-mesh method after projecting stellar particle positions onto the z = 0 plane. The first two columns correspond to the four states shown on the left side, while the last column displays the stellar distributions near pericenter at t = −7 Gyr for the weak and strong tidal cases.
Paper: Tidal Suppression of Fuzzy Dark Matter Heating in Milky Way Satellite Galaxies
Authors: Yu-Ming Yang, Zhao-Chen Zhang, Xiao-Jun Bi, Peng-Fei Yin
Figure caption: Left: density profiles of FDM and stars. The solid, dotted, and dashed curves represent the spherically averaged FDM density profiles, the corresponding soliton profiles, and the spherically averaged stellar density profiles, respectively. Right: stellar velocity dispersion and anisotropy profiles. In the top three panels, the solid, dashed, and dotted lines represent the velocity dispersion profiles along the r, θ, and ϕ directions, respectively. The bottom panel displays the anisotropy parameter as a function of radial distance from the center. The color scheme follows that used in Figure 4.
Paper: Tidal Suppression of Fuzzy Dark Matter Heating in Milky Way Satellite Galaxies
Authors: Yu-Ming Yang, Zhao-Chen Zhang, Xiao-Jun Bi, Peng-Fei Yin
Figure caption: Orbital evolution of Fornax. Top and bottom panels show Fornax’s distance to the centers of the MW and the LMC over time, respectively. Green and blue lines represent the weak and strong tidal cases, respectively. In the top panel, dotted lines illustrate the scenario excluding the influence of the LMC.
Paper: Hubble Space Telescope Observations of the Interstellar Interloper 3I/ATLAS
Authors: David Jewitt, Man-To Hui, Max Mutchler, Yoonyoung Kim, Jessica Agarwal
Figure caption: Surface brightness plot computed using concentric circular annuli 1 pixel (0﹩\mathop{.}\limits{^{\prime\prime} }﹩04) in width and centered on the photocenter. The point-spread function of HST is shown for comparison.
Paper: Hubble Space Telescope Observations of the Interstellar Interloper 3I/ATLAS
Authors: David Jewitt, Man-To Hui, Max Mutchler, Yoonyoung Kim, Jessica Agarwal
Figure caption: FWHM measured perpendicular to the tail axis, as a function of ℓ, the angular distance from the nucleus. Horizontal bars indicate the widths over which the tail signal was binned. The vertical bars indicate uncertainties, crudely estimated at ±10% of the FWHM. The solid black line shows FWHM ∝∣ℓ∣1/2, expected from the effects of radiation-pressure acceleration on the tail particles.
Paper: Hubble Space Telescope Observations of the Interstellar Interloper 3I/ATLAS
Authors: David Jewitt, Man-To Hui, Max Mutchler, Yoonyoung Kim, Jessica Agarwal
Figure caption: Normalized surface brightness plotted as a function of ℓ, the angular distance from the nucleus. The brightness was averaged over a 0﹩\mathop{.}\limits{^{\prime\prime} }﹩8 wide strip along position angle 100°.
Paper: Li Enrichment in Red Clump Giants: Clues for Past Binary Interaction or Merger Events
Authors: Raghubar Singh, Bacham E. Reddy, Anohita Mallick, Gang Zhao
Figure caption: In the left panel, mass vs. metallicity for the entire sample of 5227 stars is shown. Gray and orange symbols represent RC giants with no detectable Li line. The RC giants with A(Li) measured are shown as large colored symbols. The dashed and solid red lines denote the minimum mass of RC giants without and with mass loss (∼0.2 M⊙), respectively. The orange symbols left of the dashed red line represent RCs with extremely low mass attributed to the past binary interactions (Y. Li et al. 2022; M. Matteuzzi et al. 2024). Note, of the 89 extremely low-mass RC giants, 13 are Li-rich, which is about 15%, a high occurrence of 7 times more than Li-rich giants among the RC sample. The encircled squares represent those with anomalous [C/N] (see right panel), and the red dotted squares are fast-spinning RC giants. On the right, plots of [C/N] and mass are shown for two metallicities: (a) metal-rich (Fe/H] ≥ −0.1 dex) and (b) metal-poor [Fe/H] < −0.1 dex. The bulk of the RC giants follow the main trend, which is the average of [C/N] values in mass bins of 0.1 M⊙. Red clump giants with [C/N] ratio 1.5σ away from the average trend on either side are outliers (E. Bufanda et al. 2023). A total of 77 Li-rich RC giants have [C/N] ratio available. We found 43 Li-rich RC giants among the 351 outliers with anomalous [C/N], which is about 10 times more Li-rich RC giants than we found among the total sample.
Paper: Li Enrichment in Red Clump Giants: Clues for Past Binary Interaction or Merger Events
Authors: Raghubar Singh, Bacham E. Reddy, Anohita Mallick, Gang Zhao
Figure caption: Distribution of stars’ surface rotation with Li abundance for 16 red clump giants (top panel). The bottom panel is the plot of surface rotation against Li abundance. The color bar indicates the mass of the stars. The dotted vertical line separates SLR giants (A(Li) ≥ 3.2 dex) from Li-rich giants (1.0 < A(Li) < 3.2). We find a moderate positive correlation (Pearson coefficient, r = 0.36) between A(Li) and VS. In the SLR group, surface velocity is scattered with a standard deviation of 8.2 km s−1, and in the LR group, stars are clustered with a standard deviation of 1.9 km s−1.
Paper: Li Enrichment in Red Clump Giants: Clues for Past Binary Interaction or Merger Events
Authors: Raghubar Singh, Bacham E. Reddy, Anohita Mallick, Gang Zhao
Figure caption: Rotational period estimation from Kepler data. Left panel: long-cadence Kepler light curves of four stars. Right panel: corresponding Lomb–Scargle (LS) periodogram of stars. The estimated rotation period, which is the tallest peak in the periodogram, is marked with the red dotted vertical line.
Paper: Li Enrichment in Red Clump Giants: Clues for Past Binary Interaction or Merger Events
Authors: Raghubar Singh, Bacham E. Reddy, Anohita Mallick, Gang Zhao
Figure caption: Comparison of computed spectra (red solid line) with the observed spectra (empty circle) around the Li doublet line at 6707.7 Å for a few representative stars for LAMOST spectra of R = 1800 and 7500.
Paper: Transient Gamma Rays from the 2021 Outburst of the Recurrent Nova RS Ophiuchi: The Effect of Gamma-Ray Absorption
Authors: Vo Hong Minh Phan, Pierre Cristofari, Enrico Peretti, Vincent Tatischeff, Andrea Ciardi
Figure caption: Gamma-ray spectra compared to data from F. Aharonian et al. (2022) and V. A. Acciari et al. (2022). Solid and dashed lines are for the case with and without gamma-ray absorption, respectively.
Paper: Transient Gamma Rays from the 2021 Outburst of the Recurrent Nova RS Ophiuchi: The Effect of Gamma-Ray Absorption
Authors: Vo Hong Minh Phan, Pierre Cristofari, Enrico Peretti, Vincent Tatischeff, Andrea Ciardi
Figure caption: Shock speed evolution in time (dashed line) compared to data inferred from Hα and Hβ emission lines (red and green filled circles) by R. Pandey et al. (2022) and from X-ray data (yellow filled circles) by M. Orio et al. (2023).
Paper: Milky Way’s Metal-poor Stars Display Chemical Transition near the Solar Radius
Authors: Khyati Malhan
Figure caption: Same as Figure 3, but now additionally showing the distributions corresponding to the GSE sample (in green).
Paper: Milky Way’s Metal-poor Stars Display Chemical Transition near the Solar Radius
Authors: Khyati Malhan
Figure caption: Same as Figure 3, but now additionally showing the distributions corresponding to the thick-disk sample (in red) and the thick-disk-to-halo sample (in gold).