adsabs/AstroCLIMB huggingface dataset:
Paper: The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: R. Santra, R. Kale, S. Giacintucci, D. R. Wik, T. Venturi, D. Dallacasa, R. Cassano, G. Brunetti, D. C. Joshi
Figure caption: uGMRT 400 MHz full-resolution image (color) IMG1 obtained with Robust = 0.5. We have marked the tailed radio galaxies and discrete sources with red “+” signs. We highlight the newly detected diffuse source, named “U”, with a dashed red circle. In the central region, low-surface-brightness radio halo emission is seen. The green contours show the cluster X-ray emission as imaged by Chandra (Figure 8).
Paper: Forecasting the Population of Globular Cluster Streams in Milky Way–type Galaxies
Authors: Sarah Pearson, Ana Bonaca, Yingtian Chen, Oleg Y. Gnedin
Figure caption: The SBs for the 1814 surviving model streams from MW1 (red) and examples of observed MW GC streams (yellow stars) vs. Galactocentric radius. Most model streams are fainter than the MW streams, but some are similar.
Paper: Evidence for Abiotic Dimethyl Sulfide in Cometary Matter
Authors: Nora Hänni, Kathrin Altwegg, Michael Combi, Stephen A. Fuselier, Johan De Keyser, Niels F. W. Ligterink, Martin Rubin, Susanne F. Wampfler
Figure caption: Measured vs. expected intensities for the two combinations methanethiol + DMS (top) and methanethiol + ethanethiol (bottom). Color coded are the individual contributions in percent of the observed intensity. Reference spectra have been taken from NIST (S. E. Steins 2018) and were scaled to C2H6S on m/z = 62 for both DMS and ethanethiol and to CH4S on m/z = 48 for methanethiol as those species can be unambiguously assigned to the respective M. The hatched contribution to C2H4S on m/z = 60 can be assigned to thiirane and/or thioacetaldehyde (parent), fragments of which we do not indicate as no reference spectrum is available for thioacetaldehyde. Details are given in the main text.
Paper: Evidence for Abiotic Dimethyl Sulfide in Cometary Matter
Authors: Nora Hänni, Kathrin Altwegg, Michael Combi, Stephen A. Fuselier, Johan De Keyser, Niels F. W. Ligterink, Martin Rubin, Susanne F. Wampfler
Figure caption: Time variability of DFMS mass spectra collected around 67P’s outbound equinox and for the set masses m/z = 61 (a) and m/z = 62 (b). The measured intensities per pixel are plotted with line points and in arbitrary units (a.u.). To improve the visibility, statistical uncertainties are indicated as error bars for the March 15 03:55 UTC spectrum only.
Paper: Evidence for Abiotic Dimethyl Sulfide in Cometary Matter
Authors: Nora Hänni, Kathrin Altwegg, Michael Combi, Stephen A. Fuselier, Johan De Keyser, Niels F. W. Ligterink, Martin Rubin, Susanne F. Wampfler
Figure caption: DFMS mass spectra collected on 2016 March 15 around m/z equal to 62 (a) and 61 (b). The measured intensities per pixel are plotted with black squares, in arbitrary units (a.u.), and with their statistical uncertainties. The peaks are fitted with Gaussian functions. We show the individual Gaussians in gray, highlighting those representing the relevant S-bearing species in magenta, and the overall fit in purple. The exact mass positions of the different chemical species are indicated by dashed lines. The standard deviation of the fitted peak position is ≈6 × 10−4.
Paper: Evidence for Abiotic Dimethyl Sulfide in Cometary Matter
Authors: Nora Hänni, Kathrin Altwegg, Michael Combi, Stephen A. Fuselier, Johan De Keyser, Niels F. W. Ligterink, Martin Rubin, Susanne F. Wampfler
Figure caption: Juxtaposed NIST reference fragmentation patterns of the two structural isomers DMS and ethanethiol (S. E. Steins 2018). The relative intensity (rel. intensity; normalized to the highest signal in the spectrum) is plotted as a function of mass per charge (m/z).
Paper: Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies
Authors: Neven Tomičić, Ariel Werle, Benedetta Vulcani, Alessandro Ignesti, Alessia Moretti, Anna Wolter, Koshy George, Bianca M. Poggianti, Marco Gullieuszik
Figure caption: Observed surface brightness maps of Hα emission line (left-hand column), FUV (middle column), and NUV (right-hand column) of galaxies JO201, JO60, and JW100 (from top to bottom respectively). The stellar disks are indicated by thick contours and their disk centers are marked with yellow crosses on the black circle. Here, the Hα tracer maps are matched with the UV angular resolution and pixel sizes. The SNR threshold used for this figures is SNR > = 4 for the Hα and the UV maps.
Paper: The Study of Jet Formation Mechanism in Fermi Blazars
Authors: Shangchun Xie, Zhihao Ouyang, Jingyu Wu, Hubing Xiao, Shaohua Zhang, Yongyun Chen, Zhijian Luo, Junhui Fan
Figure caption: The distribution of the ﹩\mathrm{log}\lambda ﹩ of our sample. The red denotes FSRQs and the blue denotes BL Lacs. The dashed curves are the Gaussian fit of the histogram.
Paper: The Study of Jet Formation Mechanism in Fermi Blazars
Authors: Shangchun Xie, Zhihao Ouyang, Jingyu Wu, Hubing Xiao, Shaohua Zhang, Yongyun Chen, Zhijian Luo, Junhui Fan
Figure caption: The comparison between jet power in the MAD scenario and that estimated by 15 GHz flux density for BL Lacs. The black line is the equality line. The blue and red crosses are the same as those in Figure 1.
Paper: The Study of Jet Formation Mechanism in Fermi Blazars
Authors: Shangchun Xie, Zhihao Ouyang, Jingyu Wu, Hubing Xiao, Shaohua Zhang, Yongyun Chen, Zhijian Luo, Junhui Fan
Figure caption: The maximal BP and BZ jet power calculated by Equations (7) and (9) vs. the observed jet power of samples. The upper panel shows the calculated theoretical maximal BZ jet power vs. the observed jet power, and the bottom panel shows the calculated theoretical maximal BP jet power vs. the observed jet power. The black lines are the equality lines. The blue and red crosses are the same as those in Figure 1.
Paper: The Study of Jet Formation Mechanism in Fermi Blazars
Authors: Shangchun Xie, Zhihao Ouyang, Jingyu Wu, Hubing Xiao, Shaohua Zhang, Yongyun Chen, Zhijian Luo, Junhui Fan
Figure caption: The correlation between jet power calculated by radio flux density and that by BP and BZ mechanism. The blue and red crosses are the same as those in Figure 1.
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: Lyα halos of G1 (top) and N1 (bottom). The colored dots are the galaxy continuum size and location as measured from HST/F160W (s cont,G1 = 3.12 kpc, scont,N1 = 2.26 kpc), the white dashed circle highlights the continuum location. We show newly discovered objects as black labels. Left: Lyα surface brightness spatial map. Right: Lyα velocity map showing the peak of Lyα emission in each spaxel in velocity space with respect to the systemic redshifts z G1 = 2.4313 and z N1 = 3.1509. Red is showing redshifted gas, and blue shows blueshifted gas.
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 CGM absorption and best fits centered at z G1 = 2.4312. Best-fit models are shown as colored lines, and contamination from intervening absorption is shown as light gray lines. Note that H I (top) is on a different velocity scale. The darkest gray region shows the velocity range associated with the DLA, which is defined by the Fe-peak elements' velocity range, the lighter gray shaded region shows the full extant of the low-ionization metal absorption, and the lightest gray regions shows the velocity of the intermediate- and high-ionization absorption (discussed in Section 5.4). Left panel: the product of the individual Voigt profiles. Right panel: The decomposed Voigt profiles. The error spectrum is shown at the bottom as a red solid line.
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: CGM abundance ratios for G1 (star) and N1 (plus). Top row: blue filled symbols are direct non-dust-corrected metallicity measurements. Bottom row: purple filled symbols have been dust corrected following empirical prescriptions from A. De Cia et al. (2016). The left column shows Fe-peak abundance; the middle column panel shows [α/Fe] ratios; and the right column show Carbon and odd number elements. The light red and dark red squares show the DLA mean metallicity (and typical dispersion) from a compilation/analysis by M. Rafelski et al. (2012; references therein); the gray squares show the median abundance ratios for very metal-poor DLAs compiled by E. H. Nuñez et al. (2022).
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: Combined rest-optical and SED properties of G1 (blue outlined star) and N1 (orange outlined cross). The symbols and colored lines are the same as Figure 5. Top: stellar mass–excitation plot. Bottom: sSFR–excitation plot. Light red filled points show sSFR calculated from SFR(Hα) (Hβ for N1), and yellow filled points are calculated from SFR(SED). N1s Hβ SFR(Hβ) (lower limit) and SFR(SED) are roughly the same, so appear as one point.
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: Dust extinction of G1 (blue outlined star) and N1 (orange outlined plus) in the ISM (red fill) and CGM (light blue fill). Extinction measurements using (1) the Balmer decrement are denoted as “Hα/Hβ,” (see Section 3.2.1), (2) the best-fit SED models as “SED” (see Section 3.3), and (3) from the CGM as “CGM” (see Section 4.2.4). We show typical DLA dust extinction as a blue horizontal dashed line from A. De Cia et al. (2016) and C. Konstantopoulou et al. (2023), average dusty DLA extinction (K. E. Heintz et al. 2018), and a very dusty DLA that was analyzed by C. Konstantopoulou et al. (2024). We use R V = 3.1 (J. A. Cardelli et al. 1989).
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: Lyα emission kinematics (filled points) compared to CGM absorption kinematics (shaded regions) for the DLA associated with G1 (top; blue shaded region) and the DLA associated with N1 (bottom; orange shaded region). Red outlined markers show the Lyα red-peak velocity (Section 4.1, 3.1), black outlined markers are the systemic velocity (Section 2.2, 3.2), and blue outlined markers show blue peak velocity, all with respect to z sys (nebular emission) of G1 and N1. Each marker is labeled in the center of the figure.
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: BPT diagrams showing G1 (blue filled star) and N1 (orange filled plus). Green points are z ∼ 2–3 KBSS star-forming galaxies, magenta points are KBSS AGN, and gray points are z ∼ 0 SDSS star-forming galaxies. Light green lines are fits to the KBSS galaxies from S17. Note that N1 does not have an observation of [N II], Hα, or S II, so we show it is an unbound point and orange horizontal bar whose width is equal to its O3 error. Top: N2-BPT diagram. Bottom: S2-BPT diagram.
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: N1's CGM absorption centered at its systemic redshift zN1 = 3.1509. The lines and colors are the same as Figure B3.
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: Error associated to the ﹩{f}_{\mathrm{NL}}^{\mathrm{local}}﹩ prediction as a function of the number of simulations used to train the model. See caption of Figure 10.
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 vanilla LH parameter predictions analyzing either the power spectrum or the compressed power spectrum, as a function of the training sample size. Notice that the x axis is not uniformly spaced.
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 12 for the ﹩{f}_{\mathrm{NL}}^{\mathrm{equil}}﹩ parameter and combining the power spectrum with the marked power spectrum.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Luminosity vs. velocity for Class 3 stars, non-Class 3 classical sgB[e] stars, and sgB[e]-WL stars, color-coded as shown. Circles and triangles indicate LMC and SMC objects, respectively.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Comparison of velocity distributions for Classes 1, 2, and 3 in the LMC.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Comparison of velocity distributions for Class 3 and the remaining sgB[e] 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 of Class 1 LBVs and sgB[e] stars in the LMC.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Luminosity vs. velocity for LMC LBV Classes 1 and 2, and sgB[e] Class 3 and non-Class 3 objects, color-coded as shown.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Normalized velocity distributions of LMC sgB[e] stars and SMC field OBe stars, with Class 3 and non-Class 3 stars stacked and color-coded as shown.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Luminosity vs. velocity for all stars in the SMC. LBVc stars are shown with open circles; the Class 2 object is HD 5980, whose LBV status is especially questionable.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Normalized velocity distributions for the sgB[e] and field OBe stars in the SMC.
Paper: Kinematic Insights into Luminous Blue Variables and B[e] Supergiants
Authors: Julian A. Deman, M. S. Oey
Figure caption: Velocity distributions for the sgB[e]-WL stars and the SMC field OBe stars. Blue and green correspond to LMC and SMC objects, respectively.
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: A schematic overview of the SAGA Survey in relation to other surveys of MW-mass satellite systems. Each gray circle represents a satellite system, and the colored points represent the satellites that are observable with current observational capacity. As the cosmological distance increases from left to right, the volume and the number of systems increase, but the depth and the number of satellites that can be surveyed in each system decrease. The SAGA Survey fills in the regime where we can survey hundreds of MW-mass satellite systems and still obtain a sizable satellite population per system. The distances and sizes shown are not to scale.
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 planet masses inferred in the σ Orionis sample in this work (turquoise dots) and those inferred from well-resolved disk gaps in the DSHARP survey of nearby star-forming regions (orange dots; S. Zhang et al. 2018). The DSHARP values correspond to α = 10−3 and the DSD1 dust distribution. The error bars show the uncertainties calculated by the linear fitting method. The gray dots correspond to confirmed exoplanets (retrieved from https://exoplanetarchive.ipac.caltech.edu/ on 2024 July 10). The solar system planets are plotted in dark blue.
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 plot of R 68 vs. L mm for the observed σ Orionis disks. Following A. Tripathi et al. (2017), L mm is defined as the flux scaled to a distance of 140 pc. The black line corresponds to the median parameters from the linear fit, while the gray shaded region shows the 68% confidence interval. (Note that the error bars on R 68 are too small to be visible.)
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: Plots of the disk optical depth as a function of radius. Substructures identified from the model radial intensity profiles are labeled. The gray bar in the SO 1153 plot shows where an optical depth cannot be derived because the estimated dust temperature is less than the brightness temperature, indicating that the dust temperatures for this source are underestimated.
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: intensity and ﹩\tfrac{{dI}}{{dr}}﹩ profiles for a disk with a gap and a ring. The locations of inflection points in the radial intensity profile are marked with dotted black lines. Right: similar to the left column but for a disk with a shoulder.
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 frank model radial profiles (calculated from the CLEAN images made from the model visibilities) to the observed profile of the SO 662 disk. Right: same but for the SO 1152 disk.
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 model intensity profiles derived from the parametric method (from Section 4) and with frank using two different sets of hyperparameters. The dashed gray lines show the rms of the CLEAN images of the observations.
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 N = 2 and N = 4 model radial profiles (calculated from the CLEAN images made from the model visibilities) to the observed profile of the SO 1152 disk.
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–mass (left), size–mass (middle), and projected distance–mass (right) relations of confirmed SAGA satellites. The blue-filled circles and red-filled squares show star-forming and quenched satellites, respectively. Large stars and plus signs indicate the satellites of the MW and M31, respectively, with faint blue and red colors indicating star forming and quenched. Here, the color shown is (g − r) o , size is the physical effective radius in kiloparsecs, distance is the projected physical separation between the satellite and its host galaxy in kiloparsecs, and mass is the estimated stellar mass. The gold and silver vertical lines show the corresponding stellar mass limit of the Gold and Silver samples. Typical errors are shown at the upper left corner of each panel; the typical errors in projected distances do not include the uncertainties in system distance measurement. In the leftmost panel, the thin diagonal brown solid line shows the color–mass relation that roughly separates star-forming and quenched satellites (i.e., combining Equations (5) and (6), the latter of which is derived from Carlsten et al. 2022).
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 correlation strength (shown as p-values) between each host property shown on the y-axis and the number of satellites per host in the Gold (shown as orange-filled squares) and Gold+Silver (shown as gray-filled circles) samples, presented as p-values from the Spearman rank correlation test. The plus and minus signs on the left show the sign of the correlation. The green-vertical-dashed and solid lines indicate p-values of 0.046 and 0.0027 (corresponding to 2σ and 3σ criteria, and correlation coefficients of  0.2 and 0.3 with 101 systems). The p-values for the correlation between the most massive satellite mass and the number of satellites in both samples are extremely low, and are not shown to scale. The inset shows a scatter plot between the most massive satellite mass and the number of satellites in the Gold sample to demonstrate the observed correlation; the black star in the inset shows where the MW system would be located in this plot. See Section 5.7 for a more thorough discussion of the host properties’ meaning.