adsabs/AstroCLIMB huggingface dataset:
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: Top left: the 2022 EPIC pn lightcurve folded at the peak spin period, demonstrating the phase bins the spectra were cut into. The dotted red line denotes the mean counts, while the blue lines mark the five phase intervals (ϕ = 0.0–0.2, 0.2–0.4, 0.4–0.6, 0.6–0.8, and 0.8–1.0) where the XMM-Newton spectra were separately fitted. Top right: the soft X-ray (0.3–2 keV) flux plotted against the fitted n H across the phase bins with all temperatures fit freely. It can be observed that fitted absorption decreases in the brightest bins. Bottom: the flux normalization variation and plasma temperature variation for each APEC component across the five phase intervals. For comparison, the phase-averaged values are shown as dotted lines. The phase-resolved spectroscopy demonstrated a change in normalization that similarly affects all three single-temperature components of the model. The fourth phase bin at ϕ = 0.6–0.8 shows a substantial, but poorly constrained, spectral hardening that is pronounced across all temperature components.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: Left: XMM-Newton/NICER spectra and residuals of CJ2056 fit with a tbabs∗(APEC+APEC+APEC + Gauss) model, which yielded a ﹩{\chi }_{\nu }^{2}=1.01﹩ for 2324 dof. The 2019 XMM-Newton observation (obsID = 0842570101) is presented in the 0.3–10 keV band with MOS1 in cyan, MOS2 in yellow, and pn in black. Similarly, the 2022 XMM-Newton observation (obsID = 0902500101) is presented in the 0.3–10 keV band with MOS1 in magenta, MOS2 in orange, and pn in red. The NICER observations are presented in the 0.5–1.5 keV band, with obsID = 459201020* in green and obsID = 459201030* in blue. Right: NuSTAR spectrum and residuals fit with a tbabs∗APEC model, which yielded a ﹩{\chi }_{\nu }^{2}=0.99﹩ for 254 dof. The NuSTAR observation is presented in the 3–30 keV band, with FPMA in black and FPMB in red.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: XMM-Newton and NuSTAR spectra and residuals of CJ2056 fit with the tbabs∗(mcvspec+Gauss) model. The cases are presented as follows: Case 1 (upper left), Case 2 (upper right), Case 3 (lower left), and Case 4 (lower right). The 2019 XMM-Newton observation (obsID = 0842570101) is presented in the 0.3–10 keV band with MOS1 in blue, MOS2 in yellow, and pn in black. Similarly, the 2022 XMM-Newton observation (obsID = 0902500101) is presented in the 0.3–10 keV band with MOS1 in cyan, MOS2 in orange, and pn in red. The NuSTAR (obsID = 30801006002) observation is presented in the 3–30 keV band, with FPMA in green and FPMB in magenta.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: The XMM-Newton and NuSTAR spectra and residuals of CJ2056 fit with tbabs∗(mkcflow+Gauss) with ﹩{\chi }_{\nu }^{2}=0.98﹩ for 628 dof. The 2019 XMM-Newton observation (obsID = 0842570101) is presented in the 0.3–10 keV band with MOS1 in blue, MOS2 in yellow, and pn in black. Similarly, the 2022 XMM-Newton observation (obsID = 0902500101) is presented in the 0.3–10 keV band with MOS1 in cyan, MOS2 in orange, and pn in red. The NuSTAR observation is presented in the 3–30 keV band, with FPMA in black and FPMB in red.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: The variation of shock temperature for an IP with M = 0.8 M ⊙ as a function of R m/R and ﹩\dot{m}﹩. For low-﹩\dot{m}﹩ IPs (bottom left), which may be representative of LLIPs and CJ2056, kT s is substantially lower than it is in high-﹩\dot{m}﹩ systems (top right).
Paper: Constraints on Interacting Dark Energy Models from the DESI Baryon Acoustic Oscillation and DES Supernovae Data
Authors: Tian-Nuo Li, Peng-Ju Wu, Guo-Hong Du, Shang-Jie Jin, Hai-Li Li, Jing-Fei Zhang, Xin Zhang
Figure caption: Two-dimensional marginalized contours (68.3% and 95.4% confidence level) in the β–H 0 and β–Ω m  planes by using the CMB+DESI+DESY5 data in the IΛCDM1, IΛCDM2, IΛCDM3, and IΛCDM4 models.
Paper: Constraints on Interacting Dark Energy Models from the DESI Baryon Acoustic Oscillation and DES Supernovae Data
Authors: Tian-Nuo Li, Peng-Ju Wu, Guo-Hong Du, Shang-Jie Jin, Hai-Li Li, Jing-Fei Zhang, Xin Zhang
Figure caption: Two-dimensional marginalized contours (68.3% and 95.4% confidence level) in the β–H 0 and β–Ω m  planes by using the CMB data in the IΛCDM1, IΛCDM2, IΛCDM3, and IΛCDM4 models.
Paper: Constraints on Interacting Dark Energy Models from the DESI Baryon Acoustic Oscillation and DES Supernovae Data
Authors: Tian-Nuo Li, Peng-Ju Wu, Guo-Hong Du, Shang-Jie Jin, Hai-Li Li, Jing-Fei Zhang, Xin Zhang
Figure caption: Two-dimensional marginalized contours (68.3% and 95.4% confidence level) in the β–H 0 and β–Ω m  planes by using the CMB+DESI data in the IΛCDM1, IΛCDM2, IΛCDM3, and IΛCDM4 models.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Comparisons of the M BH–M ⋆ scaling relations under different seeding choices. The black straight lines are our input seeding relations at the corresponding redshifts, and the colored curves are our recovered scaling relations. The dotted black line overlaps with the solid black line at z = 0 and is thus invisible. The solid curves are our original ones following the AGN-based scaling relation in A. E. Reines & M. Volonteri (2015), the dashed curves represent the high-seed case, and the dotted curves represent the zevo-seed case.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The average number of wandering SMBHs per galaxy vs. M ⋆. The solid and dashed curves correspond to the p merge in M. Tremmel et al. (2018b) and p merge = 0, respectively. The gray shaded region is the relation in A. Ricarte et al. (2021b) at z = 0, where we convert the halo mass to M ⋆ using the scaling relation in Section 3 of B. P. Moster et al. (2013). We underestimate the number of wandering MBHs because MBHs from dwarf galaxies are not considered in our analyzes.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Differences in ﹩\mathrm{log}{M}_{\mathrm{BH}}﹩, denoted as ﹩{\rm{\Delta }}\mathrm{log}{M}_{\mathrm{BH}}﹩, when changing p merge to 1 and 0. At each redshift, the upper and lower curves represent the running medians of ﹩\mathrm{log}[{M}_{\mathrm{BH}}({p}_{\mathrm{merge}}=1)/{M}_{\mathrm{BH}}]﹩ and ﹩\mathrm{log}[{M}_{\mathrm{BH}}({p}_{\mathrm{merge}}=0)/{M}_{\mathrm{BH}}]﹩, respectively.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The BHMFs corresponding to different p merge choices. At each redshift, the solid curve is the original BHMF, while the upper and lower dashed curves represent p merge = 1 and 0, respectively.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The mass fraction of wandering SMBHs among all the SMBHs vs. ﹩\mathrm{log}{M}_{\star }﹩ at different redshifts. The solid and dashed curves correspond to the p merge in M. Tremmel et al. (2018b) and p merge = 0, respectively. The dashed curves represent the upper limits.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The difference between the median TNG100 and TNG300 ﹩\mathrm{log}{M}_{\mathrm{BH}}﹩ vs. M ⋆ at different redshifts. The difference is generally small, indicating that TNG100 and TNG300 M BH–M ⋆ scaling relations are similar.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The expected additional uncertainties of M BH in dex from the statistical uncertainties of ﹩{\dot{M}}_{a}﹩, color coded by the redshift.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The local BHMFs under different seeding cases, as labeled in the legend. The shaded region is from F. Shankar et al. (2020a) for comparison, as explained in Figure 6.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Similar to Figure 13, but for different seeding choices. The dashed and dotted curves are for the high-seed and zevo-seed cases, respectively.
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: The impact of the position of an X-ray source. The color bar shows Δζ X/ζ Xo. The result is for E ph = 20 keV at the peak of flare with ﹩{E}_{\mathrm{flare}}={10}^{35}﹩ erg.
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: The observationally constrained total water ice initially accreted into CI chondrite parent bodies (dashed black lines; ﹩{n}_{{{\rm{O}}}_{\mathrm{ex}}}﹩), including new constraints from the Ryugu and Bennu samples, compared to the predicted range (colored lines) of water abundances in CI chondrites and Ryugu (gray band) for the revised solar abundances proposed in this work. Due to space weathering (Appendix C), the lower bound of the constrained water ice initially accreted into Ryugu may be lower than that of CI. An upper limit for the equivalent O initially accreted as water ice per silicon atom in Ryugu is estimated to be ∼2.9 based on the upper-end value for the total porosity, ∼50% (E. Nakamura et al. 2022; A. Tsuchiyama et al. 2024), and Equation (5). The predicted water content for Ryugu (gray band) falls within the observationally constrained total water ice initially accreted into CI chondrite parent bodies (dashed black lines), making it consistent with Ryugu’s equivalent constraints. Note that the abundance of organic carbon in CI is about 10 times smaller than that from comet 67P/C-G (which is a compositional model for KBOs). This organic carbon abundance in Ryugu is similar to CI.
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: Mass ratio of heavy elements to hydrogen in this study (Z/X = 0.0251 ± 0.0013; TNT+24) compared to previous works (AG89, E. Anders & N. Grevesse 1989; GS98, N. Grevesse & A. J. Sauval 1998; AGS05, M. Asplund et al. 2005; AAG21, M. Asplund et al. 2021; EM+22, E. Magg et al. 2022). The classical models here refer to the 1D LTE radiative transfer models (E. Anders & N. Grevesse 1989, AG89; N. Grevesse & A. J. Sauval 1998, GS98). Despite their simplicity, these agreed well with constraints inferred from helioseismology such as the base of the convective zone (R CZ), the sound speed and density profiles, and the He abundance in the top surface (Y  S ; S. Basu & H. M. Antia 2008). Subsequent 3D models (AGS05; AGSS09; AGS21) have decreased the abundances of several heavy elements, which led to disagreements with observations from helioseismology. AGSS09 reported a Z/X of 0.0181, and in K. Lodders (2003), this value is 0.0177. Both are within the range of values in the low-metallicity models by AGS05 and AGS21; therefore, they are not shown here.
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: Estimates of the present-day photospheric oxygen abundance from solar wind data (B07, P. Bochsler 2007; vSZ16, R. von Steiger & T. H. Zurbuchen 2016; JML+2017, J. M. Laming et al. 2017; HV+21, Genesis data from V. S. Heber et al. 2021) compared with spectroscopic determinations (AG89, E. Anders & N. Grevesse 1989; GS98, N. Grevesse & A. J. Sauval 1998; AGSS09, M. Asplund et al. 2009; EM+22, E. Magg et al. 2022). All uncertainties are reported here as 1σ. The gray band represents the adopted range in this work. While past fractionation models based on in situ mass spectrometry data in the Ulysses mission (vSZ16) and the Apollo lunar foil experiment (B07) reported estimates with large error bars, returned samples from Genesis allow more precise estimates with multiple concordances (JML+2017). The value in K. Lodders (2003) is the same as that in AGSS09; therefore, it is not shown in this figure.
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: The predicted uncompressed density of the Pluto–Charon system (colored curves) as the fraction of the protosolar C inventory contained in refractory organics increases from 0% to 100%, assuming the canonical protosolar abundances in K. Lodders (2021; see Table 1). The horizontal black dashed line represents the average uncompressed density of the system, ∼1800 kg m−3 (A. C. Barr & M. E. Schwamb 2016; W. B. McKinnon et al. 2017), taken to be the most representative value we have for the bulk composition of large KBOs. The gray area shows the 3σ uncertainty (±20 kg m−3; M. Brozović et al. 2015; W. B. McKinnon et al. 2017; F. Nimmo et al. 2017).
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: The predicted uncompressed density of the Pluto–Charon system (colored curves) as the fraction of the protosolar C inventory contained in refractory organics increases from 0% to 100% under C/O ∼ 0.63. The horizontal black dashed line represents the average uncompressed density of the system, ∼1800 kg m−3 (A. C. Barr & M. E. Schwamb 2016; W. B. McKinnon et al. 2017), taken to be the most representative value we have for the bulk composition of large KBOs. The gray area shows the 3σ uncertainty (±20 kg m−3; M. Brozović et al. 2015; W. B. McKinnon et al. 2017; F. Nimmo et al. 2017).
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: Solar C/O ratio (0.73 ± 0.10) from this work (red box) compared with estimates in the literature through time. All uncertainties are reported here as 1σ. AG89, E. Anders & N. Grevesse (1989); GS98, N. Grevesse & A. J. Sauval (1998); L03, K. Lodders (2003); AGS05, M. Asplund et al. (2005); AGSS09, M. Asplund et al. (2009); L21, K. Lodders (2021); AAG21, M. Asplund et al. (2021); EM+22, E. Magg et al. (2022); TNT+24, this work.
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: The predicted uncompressed density of the Pluto–Charon system (colored curves) as the fraction of the protosolar C inventory contained in refractory organics increases from 0% to 100% under the new protosolar abundances (Table 2). The horizontal black dashed line represents the average uncompressed density of the system, ∼1800 kg m−3 (A. C. Barr & M. E. Schwamb 2016; W. B. McKinnon et al. 2017), taken to be the most representative value we have for the bulk composition of large KBOs. The gray area shows the 3σ uncertainty (±20 kg m−3; M. Brozović et al. 2015; W. B. McKinnon et al. 2017; F. Nimmo et al. 2017).
Paper: The Ancient Star Formation History of the Extremely Low-mass Galaxy Leo P: An Emerging Trend of a Post-reionization Pause in Star Formation
Authors: Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman, O. Grace Telford, Alyson Brooks, Elizabeth A. K. Adams, Danielle A. Berg, Martha L. Boyer, John M. Cannon, Andrew E. Dolphin, Anthony J. Pahl, Katherine L. Rhode, John J. Salzer, Roger E. Cohen, Steve R. Goldman
Figure caption: The SFH of Leo P based on the F090W − F150W CMD and the PARSEC library compared with the SFHs of the gas-rich isolated low-mass galaxies Aquarius, Leo A, and WLM. The SFHs for Aquarius and Leo A were derived from deep HST imaging (A. A. Cole et al. 2014, 2007), and the SFH for WLM was derived from deep JWST NIRCam imaging (K. B. W. McQuinn et al. 2024b). The shaded regions for each solution represent only the statistical uncertainties. The log of the present-day stellar mass in units of solar masses are listed next to the galaxy names. The approximate Epoch of Reionization is shown as a shaded gray bar, and the dotted line represents a constant star formation rate across all lookback times.
Paper: The Ancient Star Formation History of the Extremely Low-mass Galaxy Leo P: An Emerging Trend of a Post-reionization Pause in Star Formation
Authors: Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman, O. Grace Telford, Alyson Brooks, Elizabeth A. K. Adams, Danielle A. Berg, Martha L. Boyer, John M. Cannon, Andrew E. Dolphin, Anthony J. Pahl, Katherine L. Rhode, John J. Salzer, Roger E. Cohen, Steve R. Goldman
Figure caption: Left two panels: the SFH and AMR derived for Leo P based on the F090W − F150W CMD (blue) and the F090W − F277W CMD (orange) using the PARSEC (solid lines) and BaSTI stellar libraries (dashed lines). Shaded regions are shown for the PARSEC SFH solutions and represent statistical uncertainties only; statistical uncertainties on the BaSTI solutions have similar amplitudes. The range in solutions between the two models gives an indication of the systematic uncertainties. The approximate Epoch of Reionization is marked with a vertical orange bar, and the dotted diagonal line represents a constant star formation rate. The shaded regions on the AMR represent the resolution of 0.15 dex used in the fitting procedure. Right panel: the SFH based on the F090W − F150W catalog and the PARSEC library (blue solid) and BaSTI library (blue dashed) compared with the SFH derived from the shallower HST ACS F475W − F814W data and the PARSEC library (purple dotted). The shaded purple envelope represents combined statistical and systematic uncertainties on the HST SFH solution. See Section 3.2 for discussion.
Paper: The Ancient Star Formation History of the Extremely Low-mass Galaxy Leo P: An Emerging Trend of a Post-reionization Pause in Star Formation
Authors: Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman, O. Grace Telford, Alyson Brooks, Elizabeth A. K. Adams, Danielle A. Berg, Martha L. Boyer, John M. Cannon, Andrew E. Dolphin, Anthony J. Pahl, Katherine L. Rhode, John J. Salzer, Roger E. Cohen, Steve R. Goldman
Figure caption: A series of four-panel plots showing the CMD-fits for the different filter combinations with two different stellar libraries. The top two sets of plots are for F090W − F150W with PARSEC (left) and BaSTI (right). The bottom two sets of plots are for F090W − F277W with PARSEC (left) and BaSTI (right). Within each four-panel plot, we show: the observed CMD as a 2D histogram or Hess diagram (top left), the modeled CMD as a Hess diagram (top right), the difference between the observed and modeled CMDs, where red (blue) indicates more (fewer) stars observed than in the model (bottom left), and the significance of the residuals or the observed – model weighted by the variance in each Hess bin (bottom right). The scales of these residual significance plots are set uniformly from a minimum of −8 to a maximum value of 8. Overall, the modeled CMDs using the PARSEC and BaSTI libraries provide excellent fits to the observed NIRCam CMDs, with offsets seen most notably on the blue side of the lower main sequence and the red side of the upper RGB (see also Figure 5).
Paper: Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy
Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela
Figure caption: Summary of four cases with the radial velocity, logarithm of temperature, radial Alfvén speed (﹩{B}_{r}/\sqrt{4\pi \rho }﹩), and velocity perturbation δ v. The (fast) Alfvén surface is shown in (dashed) white on top of each panel, while open (closed) magnetic field lines are shown in black (red). The δ v color scale varies for cases with different λ ⋆.
Paper: Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy
Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela
Figure caption: The B. E. Wood et al. (2021) ﹩\dot{M}-{F}_{X}﹩ law with updated measurements from M dwarfs and slingshot prominences. The blue line represents the fitted law (Equation (1)). The dashed lines, one-tenth and 10 times the fitted law, encompass most of the 36 data points, with only a few outliers on the subgiant/giant branch. The filled regions in red and gray correspond to the mass-loss rate estimates for TRAPPIST-1 and Proxima Cen, respectively. The black cross symbol is the upper bound for Proxima Cen (all down arrows represent upper bounds).
Paper: The Ancient Star Formation History of the Extremely Low-mass Galaxy Leo P: An Emerging Trend of a Post-reionization Pause in Star Formation
Authors: Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman, O. Grace Telford, Alyson Brooks, Elizabeth A. K. Adams, Danielle A. Berg, Martha L. Boyer, John M. Cannon, Andrew E. Dolphin, Anthony J. Pahl, Katherine L. Rhode, John J. Salzer, Roger E. Cohen, Steve R. Goldman
Figure caption: The same CMDs as shown in Figure 3, now with PARSEC isochrones overlaid. The younger isochrones (0.2, 0.4, 0.7 Gyr) have [M/H] = −1.4 while the older isochrones (7, 13 Gyr) are slightly more metal-poor ([M/H] = −1.6).
Paper: Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy
Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela
Figure caption: Profiles of the coronal temperature, radial wind speed, and wave populations along open field regions for four simulations.