adsabs/AstroCLIMB huggingface dataset:
Paper: CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50
Authors: Weihua Guo, Xuepeng Chen, Jiancheng Feng, Li Sun, Shiyu Zhang, Chen Wang, Yang Su, Yan Sun, Qingzeng Yan, Shaobo Zhang, Xin Zhou, MiaoMiao Zhang, Min Fang, Ji Yang
Figure caption: Zoomed-in views of the nine green circles indicated in Figure 18. The red, yellow, and green crosses represent the candidate YSOs of Class I, Class II, and the flat type, respectively. The white contours are the 13CO intensities integrated in the velocity interval of [−39.5, −33.5] km s−1, which are set from 3σ (1σ ∼ 0.28 K  km s−1) to the peak value (27 K  km s−1) in a 6% average step.
Paper: Double Shells of the Planetary Nebula NGC 7009 Minor Axis
Authors: Seong-Jae Lee, Siek Hyung, Masaaki Otsuka
Figure caption: The spectral scan, showing the [S II] 6716 Å and [S II] 6731 Å lines in one echelle order. The flux on the y-axis is in units of erg−1 Å−1 cm−2 s−1 (e.g., 2.0(−15) stands for 2.0 × 10−15). The spectral scan is from one spatial component or a single row of the CCD, corresponding to the 4″ N-NW position from the center (see Figure 2(a)). Each pixel corresponds to ∼0.″39 × Δλ, where Δλ = λ/(3R). The continuum level has been adjusted. See the text.
Paper: Double Shells of the Planetary Nebula NGC 7009 Minor Axis
Authors: Seong-Jae Lee, Siek Hyung, Masaaki Otsuka
Figure caption: The slit monitoring camera images (left) and the reduced 2D Hα spectral images (right). Observation date: 1998 August 14 UT (first night) and 1998 August 15 UT (second night). The spectral image is on a log scale showing that a white color represents an intense flux. The x-axis: The full size is 3 Å. The right side of the 2D spectrum is the redder side, i.e., receding wavelengths. The y-axis: 14″ or 10″ in the sky. (a) The 14″ slit at the CSPN position along the minor axis. (b) and (c) The 10″ slit at the S-SE and N-NW directions, respectively. See the text and Table 1.
Paper: Double Shells of the Planetary Nebula NGC 7009 Minor Axis
Authors: Seong-Jae Lee, Siek Hyung, Masaaki Otsuka
Figure caption: HST image of NGC 7009 and Keck HIRES slit direction on the nebular image. The HST WFPC2 image with the F658N filter shows the main shell, outer shell, and caps/ansae (NASA/ESO). The 10″ or 14″ × 0.″862 slit entrance was placed at the S-SE area, the center (CEN), and the N-NW area along the minor axis (PA = +347°). South is upward, and north is downward. See the text.
Paper: BASS. XXXVI. Constraining the Local Supermassive Black Hole–Halo Connection with BASS DR2 AGNs
Authors: M. C. Powell, S. W. Allen, T. Caglar, N. Cappelluti, F. Harrison, B. E. Irving, M. J. Koss, A. B. Mantz, K. Oh, C. Ricci, R. J. Shaper, D. Stern, B. Trakhtenbrot, C. M. Urry, J. Wong
Figure caption: Left: projected correlation functions of each M BH bin (small M BH: cyan; large M BH: maroon; same bins as Figure 1) disaggregated by the two main mass estimation methods. Type 1 AGNs, whose M BH are estimated by broad-line measurements, are shown by the filled circles. Type 2 AGNs, whose mass estimates rely on the M BH–σ * relation, are shown by the lighter triangles. Right: projected correlations functions of each M BH bin using black hole masses calculated solely with velocity dispersion measurements.
Paper: BASS. XXXVI. Constraining the Local Supermassive Black Hole–Halo Connection with BASS DR2 AGNs
Authors: M. C. Powell, S. W. Allen, T. Caglar, N. Cappelluti, F. Harrison, B. E. Irving, M. J. Koss, A. B. Mantz, K. Oh, C. Ricci, R. J. Shaper, D. Stern, B. Trakhtenbrot, C. M. Urry, J. Wong
Figure caption: Projected correlation functions of the large black hole mass bin (maroon data points) and small black hole mass bin (cyan data points), compared to the two model predictions (Model 1: dotted lines; Model 2: solid lines). Both models show clustering differences between each bin on all scales; however, the differences are greater for Model 2, especially on scales of the one-halo term (<1 h −1 Mpc). This model, in which SMBH mass tightly correlates with halo mass, better matches the data measurements on one-halo scales.
Paper: BASS. XXXVI. Constraining the Local Supermassive Black Hole–Halo Connection with BASS DR2 AGNs
Authors: M. C. Powell, S. W. Allen, T. Caglar, N. Cappelluti, F. Harrison, B. E. Irving, M. J. Koss, A. B. Mantz, K. Oh, C. Ricci, R. J. Shaper, D. Stern, B. Trakhtenbrot, C. M. Urry, J. Wong
Figure caption: Median SMBH mass–halo mass relations predicted by each model (Model 1: blue; Model 2: orange) compared to those reported in the literature that were measured using individual galaxies and various proxies for halo mass (gray lines). The dashed lines correspond to the relations predicted by the best-fit models when imposing the third constraint.
Paper: Double Shells of the Planetary Nebula NGC 7009 Minor Axis
Authors: Seong-Jae Lee, Siek Hyung, Masaaki Otsuka
Figure caption: Density vs. [S II] 6716/6731 Å ratio. The P-I model by Ferland et al. (2017) is indicated with open circles, assuming T e = 10,000 K. See the text.
Paper: BASS. XXXVI. Constraining the Local Supermassive Black Hole–Halo Connection with BASS DR2 AGNs
Authors: M. C. Powell, S. W. Allen, T. Caglar, N. Cappelluti, F. Harrison, B. E. Irving, M. J. Koss, A. B. Mantz, K. Oh, C. Ricci, R. J. Shaper, D. Stern, B. Trakhtenbrot, C. M. Urry, J. Wong
Figure caption: Corner plots of the covariances of ERDF parameters.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: As in Figure 12, but for a box size of ﹩4\times 8\times 2{\lambda }_{\mathrm{MRI}}^{3}﹩.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Left: evolution of the average Lorentz factor for electrons, positrons, and for the two species combined in the 3D pair-plasma MRI simulation of Figure 13 (ω C/Ω0 = 15, β 0 = 312, and box size ﹩4\times 8\times 2{\lambda }_{\mathrm{MRI}}^{3}﹩). As in 2D, electrons heat significantly more than positrons. Right: evolution of the particle energy distribution during the nonlinear stage (t ≃ 4.7–15P 0) of the same simulation. Right after the onset of reconnection at t ≃ 4.7P 0, the distribution has developed a nonthermal tail following a power law (the slopes of power laws with indices 2.5 and 3 are shown to guide the eye). The nonthermal population persists until the end of the run, while a separated high-energy peak develops around γ ∼ 100 (dotted line), which corresponds to the maximum attainable energy, due to the system size in the z-direction.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Left: trajectories of test particles (an electron and a positron) moving in the xy-plane when a uniform and constant magnetic field  B  = (0, 0, B 0) is present. The particle motion is computed by solving the equations employed in the shearing-box paradigm. Right: spatial distribution of the radial and toroidal magnetic field (top row) after the formation of channel flows in a small-box, 2D MRI simulation of size ﹩2\times 2{\lambda }_{\mathrm{MRI}}^{2}﹩ (with ω C/Ω0 = 120, β 0 = 624). The corresponding spatial distribution of particle drift velocity along z (bottom row) shows that electrons are pulled toward current sheets, and positrons are pushed away.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Isotropic power spectrum of the poloidal (red line) and toroidal (blue line) magnetic field for the 3D pair-plasma MRI simulation of Figure 13 (ω C/Ω0 = 15, β 0 = 312, and box size ﹩4\times 8\times 2{\lambda }_{\mathrm{MRI}}^{3}﹩). The spectra are averaged over one channel disruption/creation cycle during the nonlinear stage (between t ≃ 9P 0 and t ≃ 11P 0), showing a persistent peak around the most-unstable MRI wavenumber k MRI. The spectra feature characteristic slopes indicating an inertial range, and a spectral break in the vicinity of the average Larmor-radius wavenumber k  ρ  measured at t ≃ 10P 0.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Left: evolution of the volume-averaged Alfvén speed (calculated with the nonrelativistic expression) for several 3D PIC simulations of the pair-plasma MRI, compared with a 2D simulation using the same initial physical parameters. In the 3D runs, the constraint ﹩{v}_{{\rm{A}}}^{\mathrm{NR}}/c\lt 1﹩ is much better respected. Right: evolution of the volume-averaged pressure anisotropy, which influences the MRI growth rate, in the same runs. The 3D runs develop smaller anisotropy over longer times.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Top left: evolution of α and of the volume-averaged Maxwell, Reynolds, and anisotropic stress in the 3D pair-plasma MRI simulation of Figure 13 (ω C/Ω0 = 15, β 0 = 312, and box size ﹩4\times 8\times 2{\lambda }_{\mathrm{MRI}}^{3}﹩). Top right: comparison of α for 2D and 3D simulations employing the same ω C/Ω0 and β 0 and different box sizes. Bottom left and right: comparison of the volume-averaged Maxwell and anisotropic stress for the same 2D and 3D simulations.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Energy conservation in a 2D pair-plasma MRI simulation with parameters ω C/Ω0 = 30, β 0 = 624, and box size ﹩8\times 8{\lambda }_{\mathrm{MRI}}^{2}﹩. Left: evolution of the total electromagnetic and kinetic energy compared with the modified electromagnetic and kinetic energy, where shearing-box source terms have been subtracted. The modified total energy ﹩{\bar{E}}_{\mathrm{tot}}﹩ is a conserved quantity in the absence of numerical errors. Right: evolution during the run of the error on the conserved ﹩{\bar{E}}_{\mathrm{tot}}﹩ relative to the instantaneous total energy E tot (the latter includes source terms and is not conserved).
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Differential heating in 2D pair-plasma MRI simulations, measured as the difference in kinetic energy between electrons and positrons normalized over the instantaneous total energy of the system. Simulations with small box size and variable ω C/Ω0 (left), variable box size and fixed ω C/Ω0 (center), and large box size and variable ω C/Ω0 (right) are compared.
Paper: Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha 
Authors: Eleonora Fiorellino, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: The 2019 (top panel) TESS light curve is indicated with black dots, and the contemporaneous ASAS-SN g-band light curve is shown with green points. SMARTS I-band (red), J (pink), H (burgundy), and K (brown) light curves are also added. Vertical dashed lines correspond to epochs when ESPRESSO (orange) and FEROS (magenta) spectra were taken. As Epoch 2 (FEROS) and 3 (ESPRESSO) were taken during the same night, these epochs are superimposed in the figure. The blue line (bottom panel) shows the Lomb–Scargle periodogram obtained using the 2019 TESS data. Points of the same light curve are linked with dashed lines only to help the reader follow each light curve. Horizontal lines represent false-alarm probabilities of 1% and 0.01%, respectively.
Paper: Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha 
Authors: Eleonora Fiorellino, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption:  Top: Accretion luminosity as a function of the stellar luminosity. Bottom: Mass accretion rate as a function of the stellar mass. The black stars show Cha I CTTS sample (Manara et al. 2022). In particular, the star with the error bar corresponds to WX Cha. The yellow, purple, blue, and dark green circles correspond to CR Cha, VW Cha, DR Tau, and RW Tau accretion rates (Facchini et al. 2016; Zsidi et al. 2022a, 2022b; Giannini et al. 2022, respectively). The WX Cha accretion rates computed in this work are shown in hexagons; each epoch is identified by a different color, as labeled in the legend. The black cross on the bottom right of the plot represents the uncertainty on Cha I CTTS sources. Uncertainties smaller than the symbol size are not presented. The dashed–dotted lines and the gray regions represent the best fit of Cha I sources and the relative 1σ dispersion.
Paper: Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha 
Authors: Eleonora Fiorellino, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: The 2021 (top panel) TESS light curve is indicated with black dots, and the contemporaneous ASAS-SN g-band light curve is shown with green points. The blue line (bottom panel) shows the Lomb–Scargle periodogram obtained using the 2021 TESS data. Points of the same light curve are linked with dashed lines only to help the reader follow each light curve. Horizontal lines represent false-alarm probabilities of 1% and 0.01%, respectively.
Paper: Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha 
Authors: Eleonora Fiorellino, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption:  Top: Absolute veiling measurements for WX Cha. Bottom: Accretion luminosity and the mass accretion rate as a function of time. The filled circles represent accretion rates computed by using the mean value (A  V  = 3.4 ± 0.2). The filled squares represent the accretion rates computed by using the exact value of the extinction for that epoch (see Table 3).
Paper: Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha 
Authors: Eleonora Fiorellino, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Variance profiles of a few spectral lines. The lines with different colors indicate the different epochs (as listed in the upper right panel), the black thick line shows the average line profile, and the blue shaded area illustrates the variance profile in each panel. The wavelength on the plots are the lines center in the vacuum.
Paper: Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha 
Authors: Eleonora Fiorellino, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Color–color diagram of WX Cha. The red circles are data from SMARTS observations at different epochs. The blue dashed line represents the CTTS locus. The black arrow shows the shift from the CTTS locus for a source with 1 mag of extinction. The orange solid line and the green dotted–dashed line correspond to the zero-age main sequence and the giant branch, respectively.
Paper: Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha 
Authors: Eleonora Fiorellino, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Color–magnitude diagrams of WX Cha.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Projection of the M31 satellite system along the directions that present an edge-on (left panel) and face-on (right panel) view of the planar structure described in Section 6.2. The galaxies are color-coded by the probability of belonging to the planar component, according to our model. The M31 disk (not to scale) orientation and the position of the MW are also reported. The dashed circle traces the virial radius of M31 (266 kpc; Fardal et al. 2013; Putman et al. 2021). The solid red line, in the left panel, traces the center of our planar model. The red shaded region and the gray dotted lines show the minimum (∼7 kpc) and maximum (∼23 kpc) thickness we infer in Section 6.2, respectively.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Difference between the distance modulus obtained through our PWZ modeling and that obtained by fitting the TRGB magnitude. Filled symbols represent galaxies with ﹩{M}_{V}^{\mathrm{eff}}\lt -9.5﹩, which are part of our validation sample. Empty symbols are galaxies with ﹩{M}_{V}^{\mathrm{eff}}\,\gt \,﹩−9.5. Galaxies highlighted in cyan are part of the TRGB anchor sample of Weisz et al. (2019b). RR Lyrae are necessary for accurate and precise distances to faint galaxies in and around the Local Group (e.g., those that Rubin Observatory should discover).
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Projected views of the M31 system onto the three major planes of the Cartesian coordinate system described in Section 6.1. In this reference frame, the XY-plane lies onto the M31 disk, with the positive Z-axis pointing to M31's north galactic pole and the positive X-axis having the same azimuth, in the M31 disk, as the M31-Earth vector. Galaxies are color-coded by absolute luminosity. The position of our GSS line of sight is marked as a white star. The M31 disk (not to scale) orientation and the position of the MW are also reported. The dashed circle traces the virial radius of M31 (266 kpc; Fardal et al. 2013; Putman et al. 2021).
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Difference between the distance modulus calculated in this paper and literature values from other RR Lyrae–based analyses (Pritzl et al. 2002, 2004, 2005; Bernard et al. 2010; Hidalgo et al. 2011; Yang & Sarajedini 2012; Cusano et al. 2013, 2015, 2016; Cole et al. 2017; Hatt et al. 2017; Martínez-Vázquez et al. 2017). The thick colored portion of the error bar shows the contribution to the total error budget coming from our distance measurements.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, James S. Bullock, Andrew A. Cole, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Representative observed PWZ for the galaxies in our sample, showing different data quality regimes: a populous, well-characterized RR Lyrae sample (And I, top panel); a populous, noisy sample (And VII, center); and a sparsely populated sample (And XIX, bottom). Circles and triangles represent RRab and RRc, respectively, and are color-coded by the probability of being bona fide measurements, (1 − Q  k ). The solid and dashed lines show our best-fit model for RRab and RRc, respectively. The gray lines show 100 random PWZ realizations from the MCMC chains.