adsabs/AstroCLIMB huggingface dataset:
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption: Locations of our symbiotic star on the Hertzsprung–Russell diagram. Gray points represent background stars within 125 pc from Gaia. Light green points denote the 355 known symbiotic stars from the J. Merc et al. (2020) catalog (hereinafter referred to as the Merc catalog). The yellow rectangle marks the solar position. Purple diamonds indicate our newly identified candidates. Blue diamonds show known symbiotic stars from the Merc catalog identified in LAMOST. Star symbols represent symbiotic stars identified in this work but not previously listed in the Merc catalog. Notably, during the completion of this work, two star-symbol objects—V* V758 Cyg and LAMOST J072528.18+342530.4—were confirmed as symbiotic stars by J. Chen et al. (2025).
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption:  Comparison of the spectrum from the symbiotic star LAMOST J072528.17+342530.4 (fiberid 194) with that of its adjacent fiber LAMOST J072439.08+341202.7 (fiberid 193). Their spectra are clearly different in the key features diagnostic of symbiotic stars, confirming that our source is not contaminated by the adjacent fiber.
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption: Similar to the symbiotic stars KM Vel, V704 Cen, HD 149427, V471 Per, Wray 15–57, AS 201, and HD 330036, the low-resolution LAMOST spectrum of Cl* NGC 2244 PS 47 shows comparable features (U. Munari & T. Zwitter 2002). Detailed analysis is given in Section 4.3.2.
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption: Spectrum of the symbiotic star LAMOST J200310.90+360822.6 (fiberid 13) compared with its adjacent fiber LAMOST J200321.88+361111.2 (fiberid 12). The distinct differences in their symbiotic spectral features confirm that our target's spectrum is not contaminated.
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption: Similar to the symbiotic star V347 Nor, the low-resolution LAMOST spectrum of ZTF J205748.33+443130.0 shows comparable features (U. Munari & T. Zwitter 2002). Detailed analysis is presented in Section 4.3.1.
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption: Same as Figure 3 but for ATO J094.1375+07.5304. The details are discussed in Section 4.1.2.
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption: Same as Figure 4 but for V* V758 Cyg. The details are shown in Section 4.2.2.
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption: Same as Figure 3 but for LAMOST J200310.90+360822.6. The details are described in Section 4.1.3.
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption: Same as Figure 4 but for LAMOST J072528.18+342530.4. The details are presented in Section 4.2.1.
Paper: ORACLE: A Real-time, Hierarchical, Deep Learning Photometric Classifier for the LSST
Authors: Ved G. Shah, Alex Gagliano, Konstantin Malanchev, Gautham Narayan, Alex I. Malz
Figure caption: Macroaveraged precision (top), recall (middle), and F-1 score (bottom) as a function of the number of days since event trigger. Performance for the full model (trained using both time-dependent and time-independent features) is plotted using solid lines. Performance for ORACLE-lite (trained using only time-dependent features) is plotted using dotted lines.
Paper: ORACLE: A Real-time, Hierarchical, Deep Learning Photometric Classifier for the LSST
Authors: Ved G. Shah, Alex Gagliano, Konstantin Malanchev, Gautham Narayan, Alex I. Malz
Figure caption: Diagram for the taxonomy used in this work. The taxonomy is loosely inspired by the structure of the ELAsTiCC data set, where the leaf nodes are the astrophysical classes, detailed in Table 9.
Paper: ORACLE: A Real-time, Hierarchical, Deep Learning Photometric Classifier for the LSST
Authors: Ved G. Shah, Alex Gagliano, Konstantin Malanchev, Gautham Narayan, Alex I. Malz
Figure caption: Histograms of redshifts (spectroscopic if available, else photometric) for extragalactic classes in the test set used for this work. Histograms for events in the LSST DDFs (shown in orange) indicate a higher fraction of sources at higher redshifts compared to WFD (shown in teal). The combined distribution for both WFD and DDF is shown with a solid black line. The total number of sources in each class is labeled.
Paper: ORACLE: A Real-time, Hierarchical, Deep Learning Photometric Classifier for the LSST
Authors: Ved G. Shah, Alex Gagliano, Konstantin Malanchev, Gautham Narayan, Alex I. Malz
Figure caption: Architecture of the RNN model used for this work.
Paper: ORACLE: A Real-time, Hierarchical, Deep Learning Photometric Classifier for the LSST
Authors: Ved G. Shah, Alex Gagliano, Konstantin Malanchev, Gautham Narayan, Alex I. Malz
Figure caption: Per-class F-1 scores for the level_1 (top), level_2 (middle), and the leaf (bottom) as a function of the number of days since event trigger.
Paper: ORACLE: A Real-time, Hierarchical, Deep Learning Photometric Classifier for the LSST
Authors: Ved G. Shah, Alex Gagliano, Konstantin Malanchev, Gautham Narayan, Alex I. Malz
Figure caption: Mean train (top) and validation (bottom) losses for every epoch in the model’s training history. A window size of 10 was used for computing the rolling mean. The large fluctuations in the training loss (and to a lesser extent, the validation loss) are likely due to large variations in the training set, as a result of the augmentations made at the start of every epoch.
Paper: New Symbiotic Stars or Candidates in LAMOST Low-resolution Spectra
Authors: Yabing Zhao, Sufen Guo, Guoliang Lü, Chunhua Zhu, Jiao Li, Jianrong Shi
Figure caption: The Galactic coordinates of the symbiotic stars and candidates.
Paper: ORACLE: A Real-time, Hierarchical, Deep Learning Photometric Classifier for the LSST
Authors: Ved G. Shah, Alex Gagliano, Konstantin Malanchev, Gautham Narayan, Alex I. Malz
Figure caption: Confusion matrices for classification at level 1, as a function of the number of days since event trigger.
Paper: 3D Modeling of Moist Convective Inhibition in Idealized Sub-Neptune Atmospheres
Authors: Namrah Habib, Raymond T. Pierrehumbert
Figure caption: Overview of the atmospheric state from the initially isothermal simulations. In each row, the panels show from left to right, profiles of temperature (K), virtual potential temperature (K), vapor mixing ratio (kg kg−1), relative humidity, and condensate mixing ratio (g kg−1). In the temperature panels, the gray dashed and solid lines plot dry and moist adiabats, and the gray dotted–dashed line plots the temperature profile assuming gray gas pure radiative equilibrium. The dashed gray line in the vapor mixing ratio panels plots the critical vapor mixing ratio of the final state. Blue lines show the initial state, while black lines show the final state. In the third row, the final state in the temperature profile lies perfectly on top of the gray moist adiabat curve throughout the domain. The ratio qv,init/qv,crit is calculated using the surface values of the initial state of the respective simulation. No initial state is shown in the ql panels, as this was set to be zero everywhere in all of the simulations.
Paper: Bridging the Atmospheric Circulations of Hot and Warm Giant Exoplanets
Authors: J. W. Skinner, S. Wei
Figure caption: (A) ﹩\mathrm{log}(| q(\lambda ,\phi ,p)| )﹩, where q is the potential vorticity in units of 10−6 K m2 kg−1 s−1, and (B) temperature T(λ, ϕ, p) fields in units of kelvin at time t = 200τp for T341L50 simulations of tidally synchronized hot and warm gas giant exoplanets (HP and WP, respectively). Fields are shown for p ∈ {0.15,  0.95,  4.95} bar. These p-levels are near the top, middle, and bottom of the simulation domains. Fields are shown in Mollweide projection, centered on the substellar point (λ, ϕ) = (0∘, 0∘), where λ is the longitude and ϕ is the latitude. White horizontal dashed lines indicate the latitudes ϕ ∈ {0∘, ±30∘, ±60∘}, and the white dashed circle indicates the dayside–nightside boundary.
Paper: Bridging the Atmospheric Circulations of Hot and Warm Giant Exoplanets
Authors: J. W. Skinner, S. Wei
Figure caption: Left: maximum and minimum equilibrium temperature profiles (yellow and blue lines, respectively) for the giant hot planet and warm planet (HP and WP, respectively). Profiles at several different longitudes are shown: substellar point (SS), antistellar point (AS), and terminators (TS). Right: thermal relaxation timescale τr(p) for HP and WP.
Paper: Bridging the Atmospheric Circulations of Hot and Warm Giant Exoplanets
Authors: J. W. Skinner, S. Wei
Figure caption: Hovmöller plots showing the time evolution of meridional wind velocity v as a function of pressure for the simulated hot planet (HP) and warm planet (WP) at the substellar point (λ, ϕ) = (0∘, 0∘) (left) and midlatitudes (λ, ϕ) = (0∘, 45∘) (right) with red and blue colors corresponding to northward and southward flow, respectively. Both planets exhibit oscillations in their equatorial regions with a period of ≲3τp and a downward propagation in time, as illustrated by red arrows. The HP has higher amplitude and more clear oscillations in v compared to the WP. Rossby waves appear as oscillations in the deep regions of both planets at (λ, ϕ) = (0∘, 45∘).
Paper: Bridging the Atmospheric Circulations of Hot and Warm Giant Exoplanets
Authors: J. W. Skinner, S. Wei
Figure caption: Relative vorticity ζ(λ, ϕ, p) fields in units ﹩{\tau }_{p}^{-1}﹩, in north polar stereographic projection at time t = 170τp. The plot boundaries are at ϕ = −10∘, and radial lines indicate the latitudes ϕ ∈ {0∘, 30∘, 60∘, 80∘}. Both planets exhibit anticyclonic vortices at their poles surrounded by cyclonic flows near ϕ ∼ 30∘. The HP’s cyclonic flows are more distorted and elongated than those on the WP. The WP’s anticyclonic vortices are centered on the pole, whereas the HP’s are offset from the pole and precess around it (see p = 0.95 bar) with a period of ∼4τp.
Paper: Bridging the Atmospheric Circulations of Hot and Warm Giant Exoplanets
Authors: J. W. Skinner, S. Wei
Figure caption: Normalized disk-averaged thermal flux ﹩{ \mathcal F }(t)/{ \mathcal F }(t=0)﹩ at p = 0.95  bar, computed using the Stefan–Boltzmann law and weighted by a cosine function. The disk average is centered on four key locations: the substellar point (SS), antistellar point (AS), eastern terminator (ET), and western terminator (WT). These represent the emergent flux observed by JWST and Ariel (see J. Kafle et al. 2025). The lines are offset in the y-axis by 0.03, and HP and WP are the hot and warm gas giant planets, respectively. The HP has larger amplitude and shorter period oscillations than the WP.
Paper: Bridging the Atmospheric Circulations of Hot and Warm Giant Exoplanets
Authors: J. W. Skinner, S. Wei
Figure caption: One-sided zonal wavenumber spectra for the meridional velocity field at p = 5 bar and t = 200τp for the WP (left) and HP (right). Both planets exhibit a dominant zonal mode of m = 2 (labeled).
Paper: First Eccentric Inspiral–Merger–Ringdown Analysis of Neutron Star–Black Hole Mergers
Authors: Maria de Lluc Planas, Sascha Husa, Antoni Ramos-Buades, Jorge Valencia
Figure caption: Posterior density distributions for the eccentricity at 20 Hz, e20 Hz, using the IMRPHENOMTEHM (TEHM, or TE when restricting to the (2, 2)-mode) model under different prior choices and starting frequencies. Solid lines correspond to a starting frequency of 17 Hz (default runs; see Table 1), dashed lines to 20 Hz, dotted lines to 13.3 Hz, and dotted–dashed lines also to 17 Hz, but with the likelihood integration starting at 25 Hz.
Paper: First Eccentric Inspiral–Merger–Ringdown Analysis of Neutron Star–Black Hole Mergers
Authors: Maria de Lluc Planas, Sascha Husa, Antoni Ramos-Buades, Jorge Valencia
Figure caption: Marginalized one- and two-dimensional posterior distributions for GW200105, recovered using the IMRPHENOMTEHM model with two different eccentricity priors: uniform (Uni, pink) and log-uniform (LogUni, purple). The figure shows the joint distribution of the primary aligned-spin component χ1 (top panel), the primary mass m1/M⊙ (middle panel), and the log-likelihood ﹩\mathrm{log}{ \mathcal L }﹩ (bottom panel), as a function of the eccentricity measured at 20 Hz (e20,Hz). The pink star marks the maximum-likelihood sample from the uniform prior run, while the pink square indicates the second peak in the posterior distribution also present in the uniform prior run.
Paper: First Eccentric Inspiral–Merger–Ringdown Analysis of Neutron Star–Black Hole Mergers
Authors: Maria de Lluc Planas, Sascha Husa, Antoni Ramos-Buades, Jorge Valencia
Figure caption: Marginalized one- and two-dimensional posterior distributions for GW200105. We show results from the QC models IMRPHENOMTHM (green) and IMRPHENOMNSBH (cyan, taken from the official LVK public release; R. Abbott et al. 2021a), as well as the eccentric model IMRPHENOMTEHM using a uniform prior in eccentricity (pink) and a log-uniform prior (purple). Parameters shown include the chirp mass ﹩{ \mathcal M }﹩, effective spin χeff, mass ratio q, and eccentricity at 20 Hz (e20 Hz).
Paper: First Eccentric Inspiral–Merger–Ringdown Analysis of Neutron Star–Black Hole Mergers
Authors: Maria de Lluc Planas, Sascha Husa, Antoni Ramos-Buades, Jorge Valencia
Figure caption: One-dimensional posterior distributions for the orbital eccentricity measured at a reference frequency of 20 Hz for the NSBH events GW200105 (solid green), GW200115 (dashed blue), and GW230529 (dotted–dashed pink) obtained using the IMRPHENOMTEHM model with a uniform eccentricity prior. Vertical lines indicate the 90% credible intervals.
Paper: An Alternative Explanation for the Helium Star Pulsar Binary J1928+1815: The Most Heavyweight Black Widow System to Date
Authors: Hang Gong, 航 巩, Alexey Bobrick, Francisco Garzón, Deven Bhakta, Thomas Maccarone, Sangita Kumari, Nieves Castro Rodríguez, Antonio Cabrera-Lavers, Arash Bahramian, Jifeng Liu, 继峰 刘
Figure caption: The distribution of pulsars in Table 1 on the ﹩\dot{E}-{P}_{\,\rm{b}\,}﹩ plane. The color map shows the ratio of heating timescale, Thaze,form, and the longest possible cooling timescale, Thaze,cool,max (which is the largest value for Thaze,cool in Table 2), on a log scale. One may see that J1928+1815 is unique in having its pulsar spindown power and orbital separation prevent it from cooling efficiently. We highlight the region facilitating the process, assuming a system with a 1 M⊙ WD and a 1.4 M⊙ NS, and show the boundary of the region with a black dashed line. For comparison, we show the same boundary for the case of 0.6 M⊙ WD with a gray dashed line. Newly discovered pulsars in the highlighted region are likely to also exhibit similar phenomena.
Paper: Reconstructing PSP/ISOIS Pitch-angle-resolved Intensities Using Unsupervised Learning
Authors: Spiridon Kasapis, Manuel E. Cuesta, Leng Ying Khoo, Hameedullah A. Farooki, Sungmin Pak, Jamey R. Szalay, Mitchell M. Shen, Jamie Rankin, Dionysios Christopoulos, George Livadiotis, David J. McComas
Figure caption: Original (top) and reconstructed (bottom) PAD spectrograms for the 2024 March 25 SEP event (Table 2, Event #206). The blue rectangle is the part featured in Figure 7. The reconstruction metrics for this event are as follows: Blob Test—RMSE = 28.54%, MAE = 2.66%, r = 0.36, ρ = 0.42; Random Test—RMSE = 28.51%, MAE = 0.05%, r = 0.40, ρ = 0.44.
Paper: Reconstructing PSP/ISOIS Pitch-angle-resolved Intensities Using Unsupervised Learning
Authors: Spiridon Kasapis, Manuel E. Cuesta, Leng Ying Khoo, Hameedullah A. Farooki, Sungmin Pak, Jamey R. Szalay, Mitchell M. Shen, Jamie Rankin, Dionysios Christopoulos, George Livadiotis, David J. McComas
Figure caption: Original (top) and reconstructed (bottom) PAD spectrograms for the 2024 January 21 SEP event (Table 2, Event #196). The reconstruction metrics for this event are as follows: Blob Test—RMSE = 209.90%, MAE = 28.06%, r = 0.10, ρ = 0.10; Random Test—RMSE = 148.62%, MAE = 7.34%, r = 0.30, ρ = 0.28.
Paper: Reconstructing PSP/ISOIS Pitch-angle-resolved Intensities Using Unsupervised Learning
Authors: Spiridon Kasapis, Manuel E. Cuesta, Leng Ying Khoo, Hameedullah A. Farooki, Sungmin Pak, Jamey R. Szalay, Mitchell M. Shen, Jamie Rankin, Dionysios Christopoulos, George Livadiotis, David J. McComas
Figure caption: Original (top) and reconstructed (bottom) PAD spectrograms for the 2023 September 23 SEP event (Table 2, Event #180). The reconstruction metrics for this event are as follows: Blob Test—RMSE = 18.9%, MAE = 0.43%, r = 0.29, ρ = 0.32; Random Test—RMSE = 32.03%, MAE = 1.51%, r = 0.28, ρ = 0.41.
Paper: Reconstructing PSP/ISOIS Pitch-angle-resolved Intensities Using Unsupervised Learning
Authors: Spiridon Kasapis, Manuel E. Cuesta, Leng Ying Khoo, Hameedullah A. Farooki, Sungmin Pak, Jamey R. Szalay, Mitchell M. Shen, Jamie Rankin, Dionysios Christopoulos, George Livadiotis, David J. McComas
Figure caption: Original (top) and reconstructed (bottom) PAD spectrograms for the 2023 March 13 SEP event (Table 2, Event #137). The reconstruction metrics for this event are as follows: Blob Test—RMSE = 30.09%, MAE = 1.97%, r = 0.23, ρ = 0.53; Random Test—RMSE = 23.46%, MAE = 0.27%, r = 0.68, ρ = 0.75.
Paper: An Alternative Explanation for the Helium Star Pulsar Binary J1928+1815: The Most Heavyweight Black Widow System to Date
Authors: Hang Gong, 航 巩, Alexey Bobrick, Francisco Garzón, Deven Bhakta, Thomas Maccarone, Sangita Kumari, Nieves Castro Rodríguez, Antonio Cabrera-Lavers, Arash Bahramian, Jifeng Liu, 继峰 刘
Figure caption: Zoom in the J, left, and H, right, final frames around the position of J1928+1815, which is in the center of the blue circle. The annulus in white surrounding the aperture sets the area to measure local background. To illustrate the astrometric accuracy of the analysis, the open and filled red circles and the green point in the bright source on the lower left represent the positions of that object in Gaia, EMIR frame WCS, and the centroid measured by SExtractor, respectively.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Polarization of stars in the same field as V658 Car. Top left: polarization level for each field star. The dots corresponds to the observation at each band while the dashed lines represent the fits to the Serkowski function. Top right: ﹩{P}_{{\rm{\max }}}﹩ for each field star. The diagonal dashed line indicate the best fit for the interstellar polarization. The vertical lines indicate the distance for the measured GDR3 parallax of V658 Car (dashed) and the 3σ region (dotted). The purple line is the weighted average ﹩\left\langle {P}_{\max }\right\rangle ﹩, and the light purple shades represents its weighted standard deviation. Bottom: polarization map in equatorial coordinates for the field of V658 Car. The vectors indicate the direction of the average polarization in all observed filters. The length of the vector is proportional to Pmax.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: The luminosity and temperature of 15 known Be+sdO binaries (D. R. Gies et al. 1998; G. J. Peters et al. 2008, 2013, 2016; D. Mourard et al. 2015; L. Wang et al. 2017, 2021; S. D. Chojnowski et al. 2018; R. Klement et al. 2022, 2024) are plotted as open (Be) and filled (sdO) circles, with a line connecting the two components of each binary system. The Regulus system is plotted in a similar fashion with black squares, and κ Draconis is plotted with red stars. This figure was updated from R. Klement et al. (2022) to contain the solution (Table 2) of V658 Car in blue.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Same as panels (F) and (G) of Figure 2. Here, however, we add observed and modeled polarization for the other bands as indicated by the different colors.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Reproduction of Figure 2, where top left is panel (C), top right is panel (D), and bottom is panel (E). Here, however, the orange points represent measurements using the Be star’s motion as the line center, while the blue points use the Hα wings. The colored solid lines are the respective best fits.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Same as Figure 3 for additional lines, as labeled.
Paper: Shooting for the Stars: Jet-mode Feedback and AGN Jet Deceleration from Stellar Mass Loading
Authors: Talia M. O'Shea, Sebastian Heinz, Melinda Soares-Furtado, Zsofi Igo, Andrea Merloni
Figure caption: X-ray flux through the stellar surface as a function of stellar age. The black points show young open cluster data from A. Núñez & M. A. Agüeros (2016), and the purple points show stars measured by R. S. Booth et al. (2017). Thin teal lines display the bootstraps as described in the text. The dark blue line and shaded region show median and 1σ distribution of the bootstrapped data. The Sun is shown in yellow, at an age of 4.5 billion years, and the pink points show data from J. Sanz-Forcada et al. (2010) for reference.
Paper: Shooting for the Stars: Jet-mode Feedback and AGN Jet Deceleration from Stellar Mass Loading
Authors: Talia M. O'Shea, Sebastian Heinz, Melinda Soares-Furtado, Zsofi Igo, Andrea Merloni
Figure caption: Mass-loss rate (scaled by galaxy stellar mass) as a function of stellar population age for a variety of stellar types. Low-mass main-sequence stars (blue line) account for G-, K-, and M-type stars, while the cyan line shows mass loss from main-sequence O- and B-type stars. The contributions of evolved stars are shown, including red giants (pink dotted), and AGB stars (purple dashed). Finally, the black curve shows mass loss leaving the IMF.