adsabs/AstroCLIMB huggingface dataset:
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Upper: fraction of corotating satellite pairs in bins of opening angles between the pairs. We follow the convention of (Phillips et al. 2015), such that a pair of satellites on opposite sides of a host have an opening angle of 0°. The green-filled squares show the corotating fraction from pairs of satellites that are within 150 kpc of their hosts. The blue points show the same but include all confirmed satellites up to 300 kpc from their hosts. The dark and light gray bands show the 1σ  and 2σ of corotation fraction when all satellites are assigned a position angle (relative to their hosts) uniformly at random. Lower: the number of pairs in bins of opening angles. Same as above, green and blue lines indicate satellites that are within 150 and 300 kpc, respectively. The gray bands show the 1σ distribution of the number of pairs when all satellites are assigned a position angle (relative to their hosts) uniformly at random. See Section 5.8 for details about how the corotating fraction is calculated.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: The color–magnitude distribution of (A) all galaxies (top left), (B) confirmed satellites (top center), (C) probability of finding a SAGA satellite (top right), (D) galaxies with literature redshifts (lower left), (E) galaxies with SAGA redshifts (lower center), and (F) the fraction of confirmed redshifts (lower right). Each panel is plotted in the (g − r) o  color vs. r 0 magnitude photometric space; color indicates the number of galaxies per hexagon bin for panels (A), (B), (D), and (E), and the fraction per bin for panels (C) and (F). Panel (A) includes all galaxies in the cleaned photometric catalogs within 300 kpc of each SAGA host galaxy. Panel (B) shows the number of confirmed satellites; the red points indicate the individual satellites. Panel (C) shows the ratio of panel (B) to panel (A), with the incompleteness correction predicted by the model described in Appendix B.1. Panel (F) shows the ratio of the sum of panels (D) and (E) to panel (A).
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Average cumulative radial distribution of confirmed satellites around 101 SAGA hosts (thick green line), and satellites of MW and M31 (orange-dashed and purple-dotted–dashed lines). For the latter, we calculated the projected distance using a random set of sight lines, and the 1σ range is shown as shaded areas around the median lines. The thin green line shows the average radial distribution of the 25% of SAGA hosts (25 hosts) that have the most concentrated distribution. The blue-dotted line shows a projected NFW profile with a concentration parameter c = 10. We did not attempt to obtain any redshifts within 10 kpc of the host galaxy and that inner region (gray vertical band on the left) is excluded from the radial profile calculation.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Satellite quenched fraction as a function of stellar mass for SAGA satellites (green points with error bars), MW and M31 satellites (orange crosses and shaded region; Wetzel et al. 2015), and isolated SDSS field galaxies (purple-shaded region; Geha et al. 2012). See Section 5.3 for the quenching definition. We also show the quenched fraction with only confirmed SAGA satellites (i.e., no incompleteness correction) as empty squares. The green error bars show binomial (Poisson) error on the fraction values. The solid green curves indicate the [16%, 84%] system-to-system scatter of the SAGA quenched fractions. The gold and silver vertical lines show the corresponding stellar mass limit of the Gold and Silver samples. The SAGA quenched fraction data points are also provided in Table C6.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Distribution of satellite abundance, shown as the fraction of systems (y-axis) that have a specific number of satellites down to M ⋆ > 107.5 M ⊙ (gold sample, x-axis). The black points show the incompleteness-corrected SAGA observations, where the error bars indicate the scatter among the realizations of the incompleteness correction. The gray solid line shows the predictions from the best-fit galaxy–halo connection model UM-SAGA, as presented in Paper V. The associated dark (light) gray bands indicate the 1σ (2σ) intervals of the prediction. The satellite abundance of MW (M31) is shown as a dashed (dotted–dashed) gray line.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Dependence of satellite abundance (color) on the estimated group halo mass (x-axis) and the stellar mass of the most massive confirmed satellite (y-axis) of each system. The group mass was estimated by Lim et al. (2017). Typical errors are shown in the upper left corner. The direction of the color gradient of the points shows that the satellite abundance primarily varies with the stellar mass of the most massive satellite. At a fixed most massive satellite mass, there is no strong dependence of the satellite abundance on group mass.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Same as the lower panel of Figure 4 but in bins of effective surface brightness (x-axis) and r-band magnitude (x-axis).
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The Dst indices of all simulated cases in the ensemble cases 1–16, at three longitudes at 1 au. Each panel in (a) shows the time series of the Dst index for different cases. The values of “Min” indicate the minimum Dst value during the event for each longitude, while “Sum” represents the integrated Dst index over time. The subplots (b) at the bottom compare the Dst indices at 0° longitude of Case 0 (the single-CME case), with the cases having 45° and 0° tilt between the CMEs.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: These plots illustrate the southward magnetic field (Bz ) at the location of the three virtual spacecraft used in this study, showcased at −10° (orange), 0° (blue), and +10° (green) longitudinal positions. The entire set of 16 cases within the CME–CME interaction ensemble is represented here.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Amount of mixing between CME1 and CME2 upon the interacting structure’s arrival at 1 au. Subplots (a) and (b) show the mixing factor (﹩{ \mathcal M }﹩) for cases with 45° and 0° relative tilt between the CMEs, along with the number of grid cells corresponding to each bin. Subplots (c) and (d) present the mean percentage of CME1-CME2 mixing along the three longitudes (0° and ±10°) in the equatorial plane.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Histogram plots of the minimum Dst value corresponding to the change in initial density ((a1)–(a3)), speed ((b1)–(b3)), tilt ((c1)–(c3)), and magnetic flux ((d1)–(d3)), at three longitudes at 1 au.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The panels showcase the scaled density (in log10 scale, N cm−3) for the considered CME–CME–SIR interaction scenario in the inner heliosphere. Panels (a1)–(a4) represent the temporal evolution of the scale density for the case LSLDLF0, while panels (b1)–(b4) depict the scenario for the case LSHDLF0.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Temporal evolution of the percentage change in the radial width of CME1 compared to the single-CME case. Results are presented along three longitudes (0° and ±10°) for all cases.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The subplots demonstrate the temporal evolution of change in the radial momentum, total KE, and total ME of CME1 for cases 1–16, with respect to the single-CME case.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Comparison of observed Dst and the estimated values as described in Equations (A1)–(A5). The (a1), (b1), and (c1) panels show the observed in situ SW speed, density, and Bz  values at the Sun–Earth L1 point for CR2270, CR2194 and CR2165, respectively. The (a2), (b2), and (c2) panels show the observed vs. estimated Dst values for these three CRs, along with their difference.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Histogram plots of the cumulative Dst values corresponding to the change in initial density ((a1)–(a3)), speed ((b1)–(b3)), tilt ((c1)–(c3)), and magnetic flux ((d1)–(d3)), at three longitudes at 1 au.
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: 2D distribution of specific intensity I  ν  (in log scale), blurred with a Gaussian beam, in the plane of the sky at frequency ν = 1 GHz and time t = 50 (in code units) after integrating the specific emissivity J  ν  along the line of sight. Shown are the maps for steady (left), variable (center), and precessing (right) jets with inclination ﹩{\hat{{\boldsymbol{n}}}}_{\mathrm{los}}=90^\circ ﹩ (top panel), 45° (middle panel), and 10° (bottom panel), respectively. The color bars indicate the level of specific intensity in ﹩\mathrm{erg}\ {{\rm{s}}}^{-1}{\mathrm{cm}}^{-2}{\mathrm{str}}^{-1}{\mathrm{Hz}}^{-1}﹩ (in log scale). The black contours indicate 0.01%, 0.1%, 1%, 5%, and 10% of maximum intensity in all panels. Additionally, contours at 10−5 of the maximum intensity are added in the middle panel for better visualization.
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: 2D distribution of specific intensity I  ν  (in log scale) in the plane of the sky at frequency ν = 1 GHz and time t = 50 (in code units) after integrating the specific emissivity J  ν  along the LOS. Shown are the maps for steady (left), variable (center), and precessing (right) jets with inclination ﹩{\hat{{\boldsymbol{n}}}}_{\mathrm{los}}=90^\circ ﹩ (top panel), 45° (middle panel), and 10° (bottom panel) respectively. The color bars indicate the level of specific intensity in ﹩\mathrm{erg}\ {{\rm{s}}}^{-1}{\mathrm{cm}}^{-2}{\mathrm{str}}^{-1}{\mathrm{Hz}}^{-1}﹩ (in log scale).
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Electron energy spectrum of all particles in the domain for the simulation run Std90 (in blue), Var90 (in orange), and Prc90 (in green) at t = 50. The injected spectrum for each particle normalized to the total number of particles at t = 50 is shown by the black dashed line. The blue and green dashed lines show the slope of spectra with power-law index α = 2.6 and 3.1, respectively, for comparison with the particle spectra. The magenta dashed line shows the asymptotic limit of α = 2.23 for ultrarelativistic shocks. Taken from (Paper-I).
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: SFMS, panel (a)) and MZR, panel (b)). The red star represents the total galaxy, while other specific regions with ALM-spaxel numbers are plotted in different shapes and colors. The gray contours and dots represent the sample of 21,642 galaxies from the NASA-Sloan Atlas catalog (M. R. Blanton et al. 2011). The magenta circles are 33 local dwarf galaxies from the Spitzer LVL (D. A. Dale et al. 2009) survey, which were selected by Li et al. (2024, in preparation) with spatially resolved observations. In panel (a), the SFMS of local star-forming galaxies is derived by D. Elbaz et al. (2007), shown in the black solid and dashed lines. In panel (b), the MZR in the local universe is from M. Curti et al. (2020) by adopting different metallicity calibrations, shown in solid lines, while the MZR with stellar mass M * < 107.5 M ⊙ is extrapolated, depicted by black dashed lines. The dashed cyan line with the shaded region marks the value of solar abundance (i.e., Z ⊙ = 8.69 ± 0.05) (C. Allende Prieto et al. 2001).
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: Distributions of the EWs of the broad He II  λ4686 (top panels) and C/N λ4650 (bottom panels) bumps vs. that of Hβ. The simulated evolutionary models from SB99 are divided into two metallicities, i.e., Z = 0.02 (solar, in blue) and 0.008 (subsolar, in green), and three IMF slopes, α = 3.30 (steeper slope, in dashed line), 2.35 (Salpeter slope, in solid line), and 1.00 (flatter slope, in the dashed–dotted line). The red-filled triangle marks the result of this work, and the corresponding errors are estimated by the method of R. Cayrel (1988). The title of each top panel expresses the adopted burst duration (Δt) and the upper cutoff mass (M up) in each case. In the middle panels, we additionally consider three extended burst models with durations of Δt = 0.2 (SFR = 100 M ⊙ yr−1), 2 (10 M ⊙ yr−1), and 200 Myr (0.1 M ⊙ yr−1) in the case of Salpeter IMF (α = 2.35), shown in different blue-like colors (moved slightly up/down for clarity). The top panels (bottom panels) share the same range of axes for visual comparison.
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: Integrated intensity maps of CO(1–0) emission (panel (a)) and 3 mm continuum (panel (b)). The white contours represent the CO(1–0) intensity at levels of 0.2, 0.3, and 0.4 Jy beam−1 km s−1, respectively. The black polygons and circles show the W-R region and three star-forming regions, respectively. The red contours in panel (b) correspond to the distribution of Hα flux in Figure 4 at 5%, 10%, and 30% of the peak flux. Black plus signs mark the galaxy center. The beam sizes of CO(1–0) emission (4.″2 × 3.″14) and continuum (4.″84 × 3.″61) are plotted in white ellipses in the left bottom corner of each panel.
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: The CO(1–0) line profile with a velocity interval of 5.2 km s−1. In panel (a), the black histogram represents the original stacked spectrum within the mom0 map. We adopt Gaussian profiles to fit the redshift (in red) and the blueshift (in blue) parts of the line profile, in which corresponding centroids are shown in dashed lines. The green curve is the superposition of the two Gaussian profiles as the best-fit model. The spectra of pixels distributed in the ALM area are selected to be stacked in the same specific star-forming region. The corresponding stacked spectrum (black) and the best-fit single Gaussian profile (green) are shown in panels (b)–(e). The region names are labeled at the top right of each panel.
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: Channel maps of the CO(1–0) emission with a velocity range of 20.8 km s−1 <v < −26.0 km s−1 and a velocity interval of Δv = 5.2 km s−1. The corresponding value of the velocity is shown in the upper right corner. The galaxy center and beam size are marked with a black plus sign and a black ellipse, respectively. The positions of triple star-forming (and W-R) regions are the same as those in Figure 4 and are marked in panel (e) by black dotted circles (solid polygon). The CO(1–0) intensity in white contours starts and increases at 3σ rms (σ rms = 1.85 mJy beam−1). The increments are marked in white on the right-side color bar.
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: Moment maps of the CO(1–0) emission with a threshold of >4σ rms. The mom0 map in panel (a) is the integrated intensity, and the mom1 (panel (b)) and mom2 (panel (c)) maps show the mean velocity and line width (FWHM) of CO(1–0), respectively. The symbols of the black plus signs and the bottom left ellipse indicate the center of the galaxy and the beam size (4.″20 × 3.″14), respectively. The positions of triple star-forming (and W-R) regions are the same as in Figure 4 and are marked in panel (a) by black dotted circles (solid polygon).
Paper: Two Intermittent Eruptions of a Minifilament Triggered by a Two-step Magnetic Reconnection Within a Fan-spine Configuration
Authors: Liping Yang, Zhike Xue, Jincheng Wang, Liheng Yang, Qiaoling Li, Yian Zhou, Yang Peng, Xinsheng Zhang
Figure caption: A sketch showing the whole scenario of the two-step reconnection process associated with the two eruptions. In all the panels, the letter “P” (“N”) indicates the positive (negative) polarity. The cyan curve represents the minifilament, and the orange (green) lines represent the inner spine. The black line indicates the small-scale low-lying magnetic loops and the filled red stars mark the reconnection sites. The light green (magenta) lines represent the brightening B1 (the bright loop BL1 or the reconfigured inner spine ). In panel (d), the purple lines represent the newly formed inner spine and outer spine after null point reconnection. The green arrows point to the high-lying field lines of the outer spine. In addition, the light green (magenta) arrows point to B1 (BL1).
Paper: Two Intermittent Eruptions of a Minifilament Triggered by a Two-step Magnetic Reconnection Within a Fan-spine Configuration
Authors: Liping Yang, Zhike Xue, Jincheng Wang, Liheng Yang, Qiaoling Li, Yian Zhou, Yang Peng, Xinsheng Zhang
Figure caption: The reconfigured large-scale magnetic structures overlying the eruptive region (indicated by the green lines) from the global PFSS model, which was overlaid on the AIA 171 Å image at 23:41:10 UT on April 7. The white rectangle outlines the region of interest with the same FOV as Figure 2(b3). The jet is denoted by the red arrows, and it propagates in the direction of the white arrow.
Paper: Why Do Semianalytic Models Predict Higher Scatter in the Stellar Mass–Halo Mass Relation Than Cosmological Hydrodynamic Simulations?
Authors: Antonio J. Porras-Valverde, John C. Forbes, Rachel S. Somerville, Adam R. H. Stevens, Kelly Holley-Bockelmann, Andreas A. Berlind, Shy Genel
Figure caption: Instantaneous AGN feedback model: black hole mass as a function of halo mass colored by the quenched fraction (﹩{\mathrm{log}}_{10}\left(\mathrm{sSFR}\ \left[{\mathrm{yr}}^{-1}\right]\right)\lt -11.0﹩) for DARK SAGE fiducial (top left), TNG (bottom left), SMBH seeding, and several σ runs with a fixed conditional distribution. For the fixed conditional distribution case, we assume a scatter of 0, 0.2, and 0.4 dex. In the case of SMBH seeding, the quenching transition happens around a black hole mass of 108 M ⊙, like in DARK SAGE fiducial and TNG. In the case of the fixed conditional distribution model, both black hole mass and halo mass contribute to suppressing star formation.