adsabs/AstroCLIMB huggingface dataset:
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: Keck/KCWI and Keck/MOSFIRE spectra of G1. Top: Smoothed FUV spectrum from the QSO-spectrally subtracted cube (black), nonsubtracted cube (yellow-orange), and error spectrum (red). Vertical colored lines show emission and absorption based on G1's systemic redshift. Bottom panels: Optical spectrum. The top of each panel shows the 1D spectrum (black), offset error spectrum (red), and modeled emission lines (green dashed). The bottom shows the 2D spectrogram.
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: The evolution in the frequency derivative ﹩\dot{\nu }﹩ modeled with the combination of spin-down terms and damped harmonic oscillator (blue curve; E. Gügercinoğlu et al. 2023) and free precession (red curve; G. Ashton et al. 2017), as indicated in the top panel. The residuals (data – model) are shown in the bottom panel, which clearly demonstrate significant scatter (indicating that these models are likely unsuitable to describe the full complex ﹩\dot{\nu }﹩ evolution). To obtain a statistically acceptable fit, we fit the models to a smaller section of the data (i.e., MJD 59,055–59,135). We find for the damped SHO, χ 2/dof = 51.5/46, while for the free precession model, χ 2/dof = 50.5/45.
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: Surface brightness (SB) profiles of the three XMM-Newton observations in three different energy bands up to a radial distance of 250″ from the position of PSR J1846−0258. In each case, the radial profile was fit with a King point-spread function model (after excluding the radial range of 35″–160″ to avoid the contribution from the SNR; see text; blue lines) with the addition of a constant background (black solid lines) in order to analyze the extension of the source. The residuals to the best fit are shown in the bottom panel.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: Keck/KCWI and Keck/MOSFIRE spectra of N1. Hα is not accessible from the ground at N1's redshift. Same lines and colors as Figure 2.
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: The evolution in the best-fit blackbody temperatures and radii (top panels), and the pulsed flux and total flux (bottom panels) during the 2020 outburst of PSR J1846–0258. The values derived in this study (black points) are compared with those derived in C.-P. Hu et al. (2023, blue points). The upper limits (quoted at the 1σ confidence level) are indicated by the arrows.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: Best-fit SEDs from BPASSv2.2 for galaxies G1 (top) and N1 (bottom). Black points show observed AB magnitudes (after QSO subtraction and bright emission line correction), and red points/curves are from the best-fit model. The best-fit parameters for the galaxy are shown at the bottom right of plot and are tabulated in Table 5. Top: G1. Bottom: N1.
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: The 1σ Fisher error bars from different combinations of summary statistics measured in the QUIJOTE halo catalogs at z = 0, after marginalizing over ﹩{M}_{\min }﹩. From left to right we consider the local, equilateral, or orthogonal PNG shapes jointly with cosmological parameters. The dark blue line corresponds to power spectrum + bispectrum (P0 + B) constraints, the green line to power spectrum + marked power spectrum (P0 + MP0), both are combined to obtain the light blue lines (P0 + B + MP0), and finally the red lines also include the marked bispectrum (P0 + B + MP0 + MB). The bold values are the largest 1σ Fisher error bars obtained for each parameter, used as normalization for the others. Marked statistics contain new information with respect to their standard counterparts on all parameters, which is significant for ﹩{f}_{\mathrm{NL}}^{\mathrm{equil}}﹩, ﹩{f}_{\mathrm{NL}}^{\mathrm{ortho}}﹩, σ 8, and Ωm.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: Extracted rest-FUV Keck/KCWI spectra as a function of extraction aperture size (used in the QSO subtraction input). Lyα emission peak is marked as a blue dashed line in each spectrum. Left: Sum of spaxels that contain galaxy G1. The blue end of the spectrum shows the largest difference (in flux) between the apertures size, but are still ≲10% of one another while the shape stays identical. Right: Sum of spaxels that contain galaxy N1. Similar behavior is seen except the percent differences between the aperture sizes are ≲5%.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: G1's intermediate- and high-ionization metal CGM absorption and and best-fit Voigt profiles centered at z G1 = 2.4312. The magenta dashed–dotted lines shows a metal absorption complex at v ∼ −750 km s−1, and brown dashed–dotted lines show metal absorption at v ∼ −500 km s−1. The lines and colors are the same as Figure 8.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: Extracted rest-FUV KCWI spectra during all stages of QSO subtraction for G1 (left two panels) and N1 (right two panels). Top panels: orange shows the spectrum without subtraction; red shows the first subtraction (i.e., QSO continuum subtraction); and black shows the second/final subtraction (removal of QSO Lyα halo+QSO continuum removal). Bottom panels: zoom-in showing the QSO Lyα halo removal.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: G1's intermediate- and high-ionization metal CGM absorption and best-fit Voigt profiles centered at its systemic redshift zG1 = 2.4312. The lines and colors are the same as Figure 8.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: G1's neutral- and low-ionization metal CGM absorption and best-fit Voigt profiles centered at z G1 = 2.4312. The lines and colors are the same as Figure 8.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: G1's H I CGM absorption fits from R12 centered at z G1 = 2.4312. The lines and colors are the same as Figure 8.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: G1's Fe-peak element CGM absorption and best-fit Voigt profiles centered at z G1 = 2.4312. The lines and colors are the same as Figure 8.
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: Standard deviation predictions for the models in Figure 3 applied to the fiducial simulations, and the corresponding 1σ Fisher constraints. The color scale gives the ratio of each error with respect to its equivalent computed by using only the power spectrum and bispectrum, highlighting the improvements for almost every parameter with the other combinations of summary statistics. Note that the parameter ranges defining the Latin-hypercube is included as prior to the Fisher calculations.
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: Accuracy of the five ﹩{f}_{\mathrm{NL}}^{\mathrm{equil}}﹩ LH parameter predictions using power spectrum (P0), marked power spectrum (MP0), bispectrum (B), marked bispectrum (MB), and halo mass function (HMF), each column referring to a specific combination. The input of the NNs are the summary statistics either used as-is (purple cross markers) or compressed (light blue plus markers).
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: Predictions of Ωm of the best performing network trained on the compression of the P0 and MP0 statistics, and applied to the test set of the ﹩{f}_{\mathrm{NL}}^{\mathrm{equil}}﹩ LH. Left panel: comparison of the true and predicted values of Ωm. The lines span the predicted 1σ about the predicted value. Center panel: predicted standard deviations as a function of the true parameter value. The mean standard deviation is also shown, compared with the root mean squared errors (RMSE) of the mean predictions. Right panel: bias of the mean prediction in units of the predicted standard deviations.
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: Accuracy of the ﹩{f}_{\mathrm{NL}}^{\mathrm{local}}﹩ prediction as a function of the number of simulations used to train the model. Compressing the data before training the model simplifies the procedure, which needs comparatively less simulations.
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: Predictions of ﹩{f}_{\mathrm{NL}}^{\mathrm{equil}}﹩ of the best performing network trained on P0, MP0, and HMF and applied to the test set of the ﹩{f}_{\mathrm{NL}}^{\mathrm{equil}}﹩ LH. The color scale in the middle panel corresponds to the true value of Ωm, which is the cosmological parameter most correlated to the ﹩{f}_{\mathrm{NL}}^{\mathrm{equil}}﹩ standard deviation. See Figure 5 for more details.
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: Stability of the Fisher 1σ error bars under variations of the number of simulations used to compute derivatives (top row) or covariances (bottom row). The analysis includes a combination of every summary statistic considered in this work (power spectrum, bispectrum, marked power spectrum, and marked bispectrum) in the left panels, with the addition of the HMF on the right. All error bars are normalized to their values computed with the full set of simulations.
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: The 1σ Fisher error bars on several cosmological parameters from different combinations of summary statistics measured up to ﹩{k}_{\max }=0.5\,h\,{\mathrm{Mpc}}^{-1}﹩ in the QUIJOTE halo catalogs at z = 0, after marginalizing over ﹩{M}_{\min }﹩. More details can be found in Figure 1.
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: The constraining power of the halo power spectrum (P0), bispectrum (B), marked power spectrum (MP0), and marked bispectrum (MB) at z = 0, and determined from the QUIJOTE halo catalogs for ﹩{k}_{\max }=0.5\,h\,{\mathrm{Mpc}}^{-1}﹩, on cosmological parameters and PNG amplitudes, after marginalizing over ﹩{M}_{\min }﹩.
Paper: Quijote-PNG: Optimizing the Summary Statistics to Measure Primordial Non-Gaussianity
Authors: Gabriel Jung, Andrea Ravenni, Michele Liguori, Marco Baldi, William R. Coulton, Francisco Villaescusa-Navarro, Benjamin D. Wandelt
Figure caption: Same as Figure 1, adding the information of the HMF to every combination of summary statistics, confirming that improvements coming from the HMF or marked statistics have different origins.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Luminosity vs. v ⊥ for Classes 1a, 1b, and 2, color-coded as shown. Circles and triangles correspond to LMC and SMC objects, respectively. The star R85 does not have an IR class and thus appears as a black circle. The SMC LBVc star HD 5980, which may not be a true LBV, is indicated with the open triangle, while the two open circles correspond to the stars R81 and R99, which also also have questionable LBV status (R. M. Humphreys et al. 2016). The four stars considered to be “classical” LBVs appear with black dots superposed on their symbols (see Section 3.2).
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Normalized comparison of LMC LBV stars with the SMC field OBe star sample. The stacked contributions of Classes 1 and 2 are color-coded as shown.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Total velocity distribution of LBV and LBVc stars in the LMC, showing the contributions of objects in Classes 1a, 1b, and 2 indicated by stacked orange, yellow, and cyan bars, respectively.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Histogram comparing velocities of LBVs and LBVc stars in the LMC.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Velocity distributions for the “classical” and “less luminous” confirmed LBVs, as identified in Section 3.2. LBVc stars are not included.
Paper: High-resolution ALMA Observations of Richly Structured Protoplanetary Disks in σ Orionis
Authors: Jane Huang, Megan Ansdell, Tilman Birnstiel, Ian Czekala, Feng Long, Jonathan Williams, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Left: a comparison of the 1.3 mm fluxes and projected separations of the sources observed in this work (light blue diamonds) and other disk detections (purple dots) and upper limits (gray triangles) in σ Orionis from M. Ansdell et al. (2017). The flux values used are all from M. Ansdell et al. (2017) for consistency. Right: a plot of the coordinates of the σ Orionis sources observed by M. Ansdell et al. (2017). Light blue dots correspond to sources observed in this work, while purple dots correspond to other disk detections and gray dots correspond to nondetections from M. Ansdell et al. (2017). The position of σ Ori is marked by an orange star. The sizes of the markers for the detected sources are scaled by the 1.3 mm flux. The dashed circles mark projected separations of 1 and 2 pc, respectively.
Paper: High-resolution ALMA Observations of Richly Structured Protoplanetary Disks in σ Orionis
Authors: Jane Huang, Megan Ansdell, Tilman Birnstiel, Ian Czekala, Feng Long, Jonathan Williams, Shangjia Zhang, Zhaohuan Zhu
Figure caption: A comparison of the parametric intensity models to the observations. First column: observations (on the same color scale as Figure 3). Second column: CLEAN images generated from the model visibilities, on the same color scale as the first column. Third column: residual images, with the color scale ranging from −5σ (blue) to 5σ (red), where σ is the rms listed in Table 3. Dashed contours correspond to the [−4, −3]σ level and solid contours to the [3, 4]σ level. Fourth column: a comparison of the deprojected, binned observed visibilities to the models. Fifth column: a comparison of the deprojected, azimuthally averaged profiles made from the observed and model CLEAN images.
Paper: High-resolution ALMA Observations of Richly Structured Protoplanetary Disks in σ Orionis
Authors: Jane Huang, Megan Ansdell, Tilman Birnstiel, Ian Czekala, Feng Long, Jonathan Williams, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Top left: radial distribution of all gaps identified in the σ Orionis sample. Top right: radial distribution of all rings. Bottom: a stacked histogram of period ratios for pairs of gaps and pairs of rings in disks with more than one gap/ring.
Paper: High-resolution ALMA Observations of Richly Structured Protoplanetary Disks in σ Orionis
Authors: Jane Huang, Megan Ansdell, Tilman Birnstiel, Ian Czekala, Feng Long, Jonathan Williams, Shangjia Zhang, Zhaohuan Zhu
Figure caption:  A  V  of stars in σ Orionis observed by K. Maucó et al. (2023), plotted as a function of R.A. The vertical orange line marks the R.A. of σ Ori. Light blue dots correspond to sources observed in this work, while purple dots correspond to other disk detections and gray dots correspond to nondetections. The sizes of the markers for the detected sources are scaled by the 1.3 mm flux measured by K. Maucó et al. (2023).
Paper: High-resolution ALMA Observations of Richly Structured Protoplanetary Disks in σ Orionis
Authors: Jane Huang, Megan Ansdell, Tilman Birnstiel, Ian Czekala, Feng Long, Jonathan Williams, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Radial intensity profiles derived from parametric modeling and labeled with the locations of the substructures. The black curves correspond to profiles generated with the median values of the marginalized posterior distributions, while the blue curves show the results of 2000 draws from the posterior.
Paper: High-resolution ALMA Observations of Richly Structured Protoplanetary Disks in σ Orionis
Authors: Jane Huang, Megan Ansdell, Tilman Birnstiel, Ian Czekala, Feng Long, Jonathan Williams, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Azimuthally averaged, deprojected radial profiles of the disks produced from the CLEAN images. The blue shaded ribbon shows the 1σ error, which is estimated by taking the standard deviation of the pixels in each radial bin and dividing by the square root of the number of beams spanned by the corresponding annulus. The gray bar in the upper right corner of each panel denotes the major axis of the synthesized beam.
Paper: High-resolution ALMA Observations of Richly Structured Protoplanetary Disks in σ Orionis
Authors: Jane Huang, Megan Ansdell, Tilman Birnstiel, Ian Czekala, Feng Long, Jonathan Williams, Shangjia Zhang, Zhaohuan Zhu
Figure caption: 1.3 mm ALMA continuum images of the disks, sorted in descending order of projected separation from σ Ori. The synthesized beam is shown in the lower left corner of each panel. An asinh stretch is used for some of the disks in order to show the faint emission at larger radii more clearly.
Paper: High-resolution ALMA Observations of Richly Structured Protoplanetary Disks in σ Orionis
Authors: Jane Huang, Megan Ansdell, Tilman Birnstiel, Ian Czekala, Feng Long, Jonathan Williams, Shangjia Zhang, Zhaohuan Zhu
Figure caption: A zoomed-in view of SO 897, showing the emission asymmetry across the major axis. Contours are drawn at 0.6, 0.7, and 0.8× the peak intensity.
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: Cumulative satellite SMF of individual SAGA systems. Each colored curve represents one SAGA system and the color is assigned based on the number of satellites per system (same color code as in Figure 7). With 101 systems presented in one figure, the main purpose of this figure is to demonstrate the spread of the satellite SMF among these systems. The incompleteness correction is included in these SMFs (corresponding to the fractional vertical jumps). The gold-dotted and silver-dotted–dashed vertical lines show the corresponding stellar mass limit of the Gold and Silver samples. The inset shows the distribution of the number of satellites per system for the Gold sample (lower inset) and the Gold+Silver sample (upper inset). The colored points in the inset indicate the satellite numbers for individual systems; hence, they correspond to the locations where the colored curves cross the vertical lines in the main panel. The black stars and plus signs in the inset show the numbers of satellites for MW and M31, respectively.