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Paper: Roles of Supernova and Active Galactic Nucleus Feedback in Shaping the Baryonic Content in a Wide Range of Dark Matter Halo Masses
Authors: Emanuele Contini, Changjo Seo, Jinsu Rhee, Seyoung Jeon, Sukyoung K. Yi
Figure caption: Fraction of gas ejected beyond the virial radius by SN (solid lines) and AGN (dashed lines) feedback, as a function of halo mass and at various redshifts (indicated by different colors), for the AGNeject1 (left panel) and AGNeject2 (right panel) models. The fractions shown represent the contribution of each feedback mode relative to the total ejected gas (i.e., SN plus AGN). The figure highlights the marked differences between the two models. In AGNeject1, AGN feedback dominates over SN feedback in the halo-mass range ﹩11.5\lt {\mathrm{log}}\,{M}_{{\rm{halo}}}\lt 13.5﹩, depending on redshift, with the dominance centered at ﹩{\mathrm{log}}\,{M}_{{\rm{halo}}}\sim 13﹩ at z = 0. In contrast, AGNeject2 shows negligible AGN ejection until z ≤ 1, after which it becomes efficient and overtakes SN feedback in the range ﹩12.3\lt {\mathrm{log}}\,{M}_{{\rm{halo}}}\lt 13.2﹩ at z = 0. At the high-mass end (﹩{\mathrm{log}}\,{M}_{{\rm{halo}}}\gt 14﹩), SN and AGN feedback contribute comparably in both models.
Paper: Roles of Supernova and Active Galactic Nucleus Feedback in Shaping the Baryonic Content in a Wide Range of Dark Matter Halo Masses
Authors: Emanuele Contini, Changjo Seo, Jinsu Rhee, Seyoung Jeon, Sukyoung K. Yi
Figure caption: Baryon fraction normalized to the Universal value as a function of halo mass at z = 0, as predicted by AGNeject1 (left) and AGNeject2 (right). Predictions are compared with the EAGLE (J. Schaye et al. 2015, red), IllustrisTNG (A. Pillepich et al. 2018, green), and SIMBA (R. Davé et al. 2019, brown) simulations. Neither model matches the simulations across the full halo-mass range, but AGNeject2 resembles IllustrisTNG and SIMBA by producing a distinct “cavity” in the baryon fraction, though with different depth and location. Unlike the simulations, which rise toward the Universal fraction on cluster scales, our models still predict a ∼25% baryon deficit, implying a substantial reservoir of baryons remains beyond the virialized region.
Paper: The Molecular Inventory of TMC-1 with GOTHAM Observations
Authors: Ci Xue, Alex N. Byrne, Larry Morgan, Gabi Wenzel, P. Bryan Changala, Zachary T. P. Fried, Ryan A. Loomis, Anthony Remijan, Edwin A. Bergin, Ilsa R. Cooke, David Frayer, Andrew M. Burkhardt, Steven B. Charnley, Martin A. Cordiner, Andrew Lipnicky, Michael C. McCarthy, Brett A. McGuire
Figure caption: GOTHAM DRV observations and simulations. The top panel shows the calibrated observed spectra in black in kelvin (left axis) and the noise level per channel in gray in millikelvin (right axis). The receivers used in each frequency range are shown as colored bars. Data between 34,250 and 35,686 MHz in the Ka band are flagged due to abnormally high Tsys (see Appendix A for details). The bottom panel shows the simulated spectrum in red in kelvin, generated from the MCMC fitting of 102 analyzed molecules. The absorption lines and some bright emission lines contributed by molecules that need special treatment are not included in the simulation. See the main text for details.
Paper: The Molecular Inventory of TMC-1 with GOTHAM Observations
Authors: Ci Xue, Alex N. Byrne, Larry Morgan, Gabi Wenzel, P. Bryan Changala, Zachary T. P. Fried, Ryan A. Loomis, Anthony Remijan, Edwin A. Bergin, Ilsa R. Cooke, David Frayer, Andrew M. Burkhardt, Steven B. Charnley, Martin A. Cordiner, Andrew Lipnicky, Michael C. McCarthy, Brett A. McGuire
Figure caption: Zenith sky opacity of the default values used in GBTIDL (black dashed line) and the dynamic values retrieved from CLEO associated with the session 08 of AGBT18B–007 as examples (color solid lines). Different colors represent linear interpolation between observation times, while the cubic spline represents interpolation between frequencies. Left: frequency range of 0–50 GHz; Right: zoom-in frequency range near the 22 GHz water vapor line.
Paper: The Molecular Inventory of TMC-1 with GOTHAM Observations
Authors: Ci Xue, Alex N. Byrne, Larry Morgan, Gabi Wenzel, P. Bryan Changala, Zachary T. P. Fried, Ryan A. Loomis, Anthony Remijan, Edwin A. Bergin, Ilsa R. Cooke, David Frayer, Andrew M. Burkhardt, Steven B. Charnley, Martin A. Cordiner, Andrew Lipnicky, Michael C. McCarthy, Brett A. McGuire
Figure caption: Carbon abundances probed by each molecule detected in GOTHAM (Table 2) as a function of the number of carbon atoms (#C), colored by elemental composition. Hydrocarbons are shown in gray, nitrogen-bearing species in blue, oxygen-bearing species in red, and sulfur-bearing species in yellow. Molecules containing more than one heteroatom are marked in purple.
Paper: The Molecular Inventory of TMC-1 with GOTHAM Observations
Authors: Ci Xue, Alex N. Byrne, Larry Morgan, Gabi Wenzel, P. Bryan Changala, Zachary T. P. Fried, Ryan A. Loomis, Anthony Remijan, Edwin A. Bergin, Ilsa R. Cooke, David Frayer, Andrew M. Burkhardt, Steven B. Charnley, Martin A. Cordiner, Andrew Lipnicky, Michael C. McCarthy, Brett A. McGuire
Figure caption: Individual line detection of C3N transitions in the GOTHAM DRV data. Each panel provides a window context of 7 km s−1 and the quantum numbers in a format of (N, J, F) of the covered transitions. The observed spectra are displayed in black while the simulated spectra using the MCMC-derived parameters are overlaid in red. Simulated spectra of the individual velocity components are shown in yellow (5.64 km s−1), green (5.80 km s−1), brown (5.96 km s−1), and blue (6.07 km s−1).
Paper: The Molecular Inventory of TMC-1 with GOTHAM Observations
Authors: Ci Xue, Alex N. Byrne, Larry Morgan, Gabi Wenzel, P. Bryan Changala, Zachary T. P. Fried, Ryan A. Loomis, Anthony Remijan, Edwin A. Bergin, Ilsa R. Cooke, David Frayer, Andrew M. Burkhardt, Steven B. Charnley, Martin A. Cordiner, Andrew Lipnicky, Michael C. McCarthy, Brett A. McGuire
Figure caption: Statistics of system temperatures of all GOTHAM observations, grouped by spectral windows and polarization. The black solid line represents the typical Tsys reported in the GBT Proposer’s Guide. The dashed lines show a threshold of 3 times the typical values.
Paper: The Molecular Inventory of TMC-1 with GOTHAM Observations
Authors: Ci Xue, Alex N. Byrne, Larry Morgan, Gabi Wenzel, P. Bryan Changala, Zachary T. P. Fried, Ryan A. Loomis, Anthony Remijan, Edwin A. Bergin, Ilsa R. Cooke, David Frayer, Andrew M. Burkhardt, Steven B. Charnley, Martin A. Cordiner, Andrew Lipnicky, Michael C. McCarthy, Brett A. McGuire
Figure caption: Schematic diagram for the data flow of the DRV data calibration and reduction pipeline.
Paper: The Molecular Inventory of TMC-1 with GOTHAM Observations
Authors: Ci Xue, Alex N. Byrne, Larry Morgan, Gabi Wenzel, P. Bryan Changala, Zachary T. P. Fried, Ryan A. Loomis, Anthony Remijan, Edwin A. Bergin, Ilsa R. Cooke, David Frayer, Andrew M. Burkhardt, Steven B. Charnley, Martin A. Cordiner, Andrew Lipnicky, Michael C. McCarthy, Brett A. McGuire
Figure caption: Fractions of the amount of flagged data per channel of GOTHAM DRV. The reasons for flagging include channels with interference, integrations with abnormal Tsys, and spectral window edges.
Paper: Roles of Supernova and Active Galactic Nucleus Feedback in Shaping the Baryonic Content in a Wide Range of Dark Matter Halo Masses
Authors: Emanuele Contini, Changjo Seo, Jinsu Rhee, Seyoung Jeon, Sukyoung K. Yi
Figure caption: Baryon fraction normalized to the Universal value (Y200) as a function of halo mass for the AGNeject1 (left) and AGNeject2 (right) models. Solid lines indicate different redshifts, compared with predictions from NewCluster (filled circles) and literature data (symbols in the legend). AGNeject1 shows almost no evolution with time, while AGNeject2 predicts a strong late-time decline in baryon content between ﹩11.8\lt {\rm{log}}{M}_{{\rm{halo}}}\lt 13.4﹩. On small scales, NewCluster supports the near-constant trend of AGNeject1. On cluster scales, both models agree with I. Chiu et al. (2016) and D. Akino et al. (2022), but fall below M. Angelinelli et al. (2023). The most distinctive feature is the deep z = 0 cavity in AGNeject2, signaling enhanced baryon depletion at late times.
Paper: Roles of Supernova and Active Galactic Nucleus Feedback in Shaping the Baryonic Content in a Wide Range of Dark Matter Halo Masses
Authors: Emanuele Contini, Changjo Seo, Jinsu Rhee, Seyoung Jeon, Sukyoung K. Yi
Figure caption: Hot-gas fraction normalized to the Universal baryon fraction as a function of halo mass at different redshifts (separate panels), predicted by AGNeject1 (blue) and AGNeject2 (red). Results are compared with observational constraints and simulations at z = 0 and z = 1, and with simulations only at higher redshifts. Predictions from NewCluster are also shown at z ≥ 1 (magenta circles). Both models broadly agree with observations at z = 0 and show hints of convergence at z = 1, though they predict lower fractions than MAGNETICUM (M. Angelinelli et al. 2023) at all epochs. The main difference arises in Milky Way–like halos: AGNeject1 is more effective until z = 1, while AGNeject2 becomes dominant in the last ∼7 Gyr. At z = 3, NewCluster gives slightly lower values but follows the same trends. This explains the deep baryon fraction cavity at z = 0 in AGNeject2 (Figure 1).
Paper: Roles of Supernova and Active Galactic Nucleus Feedback in Shaping the Baryonic Content in a Wide Range of Dark Matter Halo Masses
Authors: Emanuele Contini, Changjo Seo, Jinsu Rhee, Seyoung Jeon, Sukyoung K. Yi
Figure caption: Efficiency of AGN feedback in ejecting gas beyond the virial radius as a function of halo mass. The efficiency is defined as the total gas mass expelled by AGN up to a given redshift (including all progenitors), normalized by the halo mass at that epoch. Predictions from our two models are shown: AGNeject1 (left) and AGNeject2 (right), with colors indicating different redshifts. In AGNeject1, efficiency gradually rises with time, peaking between ﹩12.5\lt {\mathrm{log}}\,{M}_{{\rm{halo}}}\lt 13﹩, depending on redshift, and flattening to ∼5% on cluster scales. By contrast, AGNeject2 remains negligible until z = 1, then increases sharply at ﹩{\mathrm{log}}\,{M}_{{\rm{halo}}}\gt 12﹩, reaching a peak near ﹩{\mathrm{log}}\,{M}_{{\rm{halo}}}\sim 13﹩ at z = 0. This highlights the contrasting timing and strength of AGN-driven gas ejection in the two models.
Paper: Roles of Supernova and Active Galactic Nucleus Feedback in Shaping the Baryonic Content in a Wide Range of Dark Matter Halo Masses
Authors: Emanuele Contini, Changjo Seo, Jinsu Rhee, Seyoung Jeon, Sukyoung K. Yi
Figure caption: Stellar-to-halo mass relation for central galaxies at different redshifts (panels), as predicted by AGNeject1 (blue) and AGNeject2 (red). At z = 0, predictions are compared with the SHARK2 SAM (C. d. P. Lagos et al. 2024), the empirical relation of B. P. Moster et al. (2013), and observational estimates from A. B. Romeo et al. (2020), G. Hinshaw et al. (2013), A. H. Gonzalez et al. (2013), A. V. Kravtsov et al. (2018), and P. E. Mancera Piña et al. (2025). At z ≥ 1, results are compared with B. P. Moster et al. (2013) and the NewCluster simulation. Both models agree well with semianalytic, empirical, and observational constraints at z = 0. At higher redshifts, NewCluster tends to overpredict stellar masses in low-mass halos. Matching this relation over cosmic time is crucial, especially in low-mass halos where the central galaxy contains most of the stellar mass within the virial radius.
Paper: Roles of Supernova and Active Galactic Nucleus Feedback in Shaping the Baryonic Content in a Wide Range of Dark Matter Halo Masses
Authors: Emanuele Contini, Changjo Seo, Jinsu Rhee, Seyoung Jeon, Sukyoung K. Yi
Figure caption: SN feedback efficiency as a function of halo mass for the AGNeject1 (left) and AGNeject2 (right) models, shown at different redshifts (color-coded lines as indicated in the legend), following the same format as Figure 4. SN feedback is most effective in low-mass halos and progressively declines with increasing halo mass. The two panels are identical, reflecting the fact that the AGN feedback implementations in these models do not influence the SN feedback.
Paper: Observational Properties of β Cephei Stars: 88 New Samples Discovered Based on TESS and Gaia Data
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, David Mkrtichian, Farkhodjon Khamrakulov, Wen-xu Lin
Figure caption: The Hertzsprung–Russell (H-R) diagram of BCEP stars. In this diagram, confirmed BCEP stars and candidates from this work are marked as filled red circles. For comparative analysis, previously published BCEP and SPB stars from Papers I–III are also plotted as open red circles and black circles, respectively. Theoretical stellar evolution frameworks are shown. Black solid curves: zero-age main sequence and evolutionary tracks for masses 7–20 M⊙ at solar metallicity (Z = 0.02); blue/magenta dashed curves: the theoretical instability strips for SPB/BCEP stars at Z = 0.02, modeling low-degree pulsation modes l ≤ 3 (A. Miglio et al. 2007); black cross: a standard error box.
Paper: Observational Properties of β Cephei Stars: 88 New Samples Discovered Based on TESS and Gaia Data
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, David Mkrtichian, Farkhodjon Khamrakulov, Wen-xu Lin
Figure caption: The luminosity and the dominant pulsating period relation diagram of these BCEP stars and candidates. Symbols are similar to those in Figure 4. The red dashed line and the black solid line represent the relationship derived by Paper I for BCEP and SPB stars, respectively. The red solid line represents the new relation derived in Paper III.
Paper: Observational Properties of β Cephei Stars: 88 New Samples Discovered Based on TESS and Gaia Data
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, David Mkrtichian, Farkhodjon Khamrakulov, Wen-xu Lin
Figure caption: The effective temperature and the dominant pulsating period relation diagram of these BCEP stars and candidates. Similar symbols to those in Figure 2 are used, but the size of the circles denotes their pulsation amplitude at the dominant frequency.
Paper: Observational Properties of β Cephei Stars: 88 New Samples Discovered Based on TESS and Gaia Data
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, David Mkrtichian, Farkhodjon Khamrakulov, Wen-xu Lin
Figure caption: The distribution of BCEP stars according to Galactic longitude and latitude. Similar symbols to these BCEP stars in Figure 2 are used, but the size of the circles denotes their parallaxes π.
Paper: Observational Properties of β Cephei Stars: 88 New Samples Discovered Based on TESS and Gaia Data
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, David Mkrtichian, Farkhodjon Khamrakulov, Wen-xu Lin
Figure caption: Fourier spectra of new BCEP stars and candidates. The red dotted lines are the rough boundary (3 day−1) for low frequency and high frequency.
Paper: Observational Properties of β Cephei Stars: 88 New Samples Discovered Based on TESS and Gaia Data
Authors: Xiang-dong Shi, Sheng-bang Qian, Li-ying Zhu, Lin-jia Li, Er-gang Zhao, David Mkrtichian, Farkhodjon Khamrakulov, Wen-xu Lin
Figure caption: Distribution of the parallax, visual magnitude, and temperature for high-temperature stars (T > 10,​​​​​​000 K) with TESS-SC and FFI-SPOC data.
Paper: A Comparison of Star Formation Rates by Different Tracers in Nearby Galaxies
Authors: Huynh Anh N. Le, Jong-Hak Woo, Yongquan Xue, Ashraf Ayubinia, Changseok Kim, Xiaozhi Lin
Figure caption: SFRs as a function of Eddington ratio for a stellar mass range from 9.5 < ﹩{\mathrm{log}M}_{* }﹩ < 11.5. SFR values are presented by SFRSED. Horizontal dashed lines in blue, pink, red, and cyan correspond to the median SFR values for star-forming, composite, Seyfert, and LINER galaxies, respectively. Vertical dashed lines indicate the median Eddington ratio values for each galaxy type.
Paper: A Comparison of Star Formation Rates by Different Tracers in Nearby Galaxies
Authors: Huynh Anh N. Le, Jong-Hak Woo, Yongquan Xue, Ashraf Ayubinia, Changseok Kim, Xiaozhi Lin
Figure caption: sSFR as a function of Eddington ratio for a total stellar mass range from 9.5 < ﹩{\mathrm{log}M}_{* }﹩ < 11.5. sSFR values are presented by sSFRSED. Horizontal dashed lines in blue, pink, red, and cyan correspond to the median sSFR values for star-forming, composite, Seyfert, and LINER galaxies, respectively. Vertical dashed lines indicate the median Eddington ratio values for each galaxy type.
Paper: A Comparison of Star Formation Rates by Different Tracers in Nearby Galaxies
Authors: Huynh Anh N. Le, Jong-Hak Woo, Yongquan Xue, Ashraf Ayubinia, Changseok Kim, Xiaozhi Lin
Figure caption: Top and middle panels: the ratios of SFR[O II]/SFRFIR and SFRHα/SFRFIR as a function of fraction of u-band light captured by the SDSS fiber, defined as the difference in magnitude, fSDSS = Ufiber − Utotal. Bottom panel: the ratio of SFR[O II]/SFRHα as a function of the fSDSS. AGN fraction (fAGN) is shown as the color scale.
Paper: A Comparison of Star Formation Rates by Different Tracers in Nearby Galaxies
Authors: Huynh Anh N. Le, Jong-Hak Woo, Yongquan Xue, Ashraf Ayubinia, Changseok Kim, Xiaozhi Lin
Figure caption: The ratios of SFR[O II]/SFRFIR and SFRHα/SFRFIR as a function of fraction of u-band light captured by the SDSS fiber, defined as the difference in magnitude, fSDSS = Ufiber − Utotal. Redshift is shown as the color scale.
Paper: A Comparison of Star Formation Rates by Different Tracers in Nearby Galaxies
Authors: Huynh Anh N. Le, Jong-Hak Woo, Yongquan Xue, Ashraf Ayubinia, Changseok Kim, Xiaozhi Lin
Figure caption: The ratio of SFRMIR/SFRFIR as a function of redshift. AGN fraction (fAGN) is shown as the color scale.
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: Stellar mass and mass surface density of various stellar systems, including star-forming galaxies (light blue dots and blue plus marks, L. Ferrarese et al. 2006; I. Trujillo et al. 2020), elliptical galaxies and early-type galaxies (open downward triangles and gray squares, P. Côté et al. 2006; L. Ferrarese et al. 2006). To compare with the dwarf galaxy population, we also show the Local Group dwarf galaxies (green crosses, I. Misgeld & M. Hilker 2011), ultracompact dwarfs (black open circles with crosses, S. Mieske et al. 2008), dwarf elliptical galaxies (dEs; orange squares and open purple circles, I. Misgeld et al. 2008, 2009; S. Côté et al. 2009), low-surface-brightness galaxies (light pink, W. Du et al. 2015), and UDGs from coma (dark red, P. G. van Dokkum et al. 2015b). The low H I mass galaxies are shown with red cross signs, which are at the similar region as dwarf elliptical galaxies. The surface density is roughly 1–2 orders of magnitude lower than the mass density of elliptical or UCDs, implying that no bright bulge formed when the dwarf galaxies were rich in H I gas. We also show the star cluster systems in gray and black dots (D. E. McLaughlin & R. P. van der Marel 2005; A. Jordán et al. 2009). The solid lines indicate the galaxy size of 100 pc, 1 kpc, and 10 kpc.
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: The H I-to-stellar-mass ratio as a function of g − r color for the low H I mass sample presented in this work (open circles), overplotted with FASHI targets that have reliable optical counterparts (filled circles) as a reference. All points are color coded by their r-band magnitude. The similar trend between the two samples indicates the statistical reliability of the optical counterpart identification for our H I-selected galaxies.
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: Examples of the growth curve for three targets (ID from left: 40703, 35982, 40772). The left and right peaks are indicated by dashed lines in the lower-right inset of each panel. The apparent dip between the two peaks is likely caused by noise fluctuations, or not significant enough for the S/N. To account for this, we add random noise at the rms level to each channel 500 times and remeasure the K parameter. The resulting distribution of K values is shown as a histogram in the upper-left inset of each panel. In the left example, the condition K + Kerr < 0 is satisfied, and the spectrum is classified as double peaked. The right panel example also exhibits a double-peaked profile by eye, but the significance is insufficient for a robust classification in this work.
Paper: H I-detected Dwarf Galaxies in the FASHI Survey: Insights from Single- and Double-peaked Emission-line Samples
Authors: Cheng Cheng, Jia-Sheng Huang, Wei Du, Hong-Xin Zhang, Chuan-Peng Zhang, Ming Zhu, Gustavo Orellana
Figure caption: Stellar mass versus H I mass for the FASHI sample, with optical counterparts matched from the SGA catalog with spectroscopic redshifts. The H I-selected dwarf studied in this work is highlighted in red.
Paper: The Molecular Inventory of TMC-1 with GOTHAM Observations
Authors: Ci Xue, Alex N. Byrne, Larry Morgan, Gabi Wenzel, P. Bryan Changala, Zachary T. P. Fried, Ryan A. Loomis, Anthony Remijan, Edwin A. Bergin, Ilsa R. Cooke, David Frayer, Andrew M. Burkhardt, Steven B. Charnley, Martin A. Cordiner, Andrew Lipnicky, Michael C. McCarthy, Brett A. McGuire
Figure caption: Individual line detection of c-C6H5CN transitions in the GOTHAM DRV data. Each panel provides a window context of 4 km s−1 and the quantum numbers in a format of J(Ka, Kc) of the covered transitions. The observed spectra are displayed in black while the simulated spectra using the MCMC-derived parameters are overlaid in red. Simulated spectra of the individual velocity components are shown in yellow (5.61 km s−1), green (5.78 km s−1), brown (5.90 km s−1), and blue (6.03 km s−1).
Paper: Stellar Characterization, Magnesium Abundances, and Chromospheric Activity Analysis of Stars with Confirmed Exoplanets from the K2 Mission
Authors: V. Loaiza-Tacuri, Diogo Souto, F. Quispe-Huaynasi, Katia Cunha, S. Daflon, Ellen Costa-Almeida, V. V. Smith, Luan Ghezzi
Figure caption: Stellar activity as a function of planetary radius for a sample of 339 exoplanets with host star stellar activity indices derived in this study. The planetary radii (Rpl) are based on stellar radii determined using the Stefan–Boltzmann law. The blue symbols represent the median host star stellar activity index for super-Earths (Rp < 1.9 R⊕), sub-Neptunes (1.9 R⊕ ≤ Rpl < 4.4 R⊕), sub-Saturns (4.4 R⊕ ≤Rp < 8.0 R⊕), and Jupiters (Rp ≥ 8.0 R⊕). The error bars represent the median absolute deviations from these median values.
Paper: Stellar Characterization, Magnesium Abundances, and Chromospheric Activity Analysis of Stars with Confirmed Exoplanets from the K2 Mission
Authors: V. Loaiza-Tacuri, Diogo Souto, F. Quispe-Huaynasi, Katia Cunha, S. Daflon, Ellen Costa-Almeida, V. V. Smith, Luan Ghezzi
Figure caption: Average SHK as a function of Hα (left panel). Stars with rotational periods whose values are taken from T. Reinhold & S. Hekker (2020) are shown in the right panel (the black border of the red circle refers to M-type stars).