adsabs/AstroCLIMB huggingface dataset:
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Same as Figure 3, but for pulsars in the Sagittarius Arm.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Derived longitudinal magnetic field strengths (positive is CCW) along our Sagittarius Arm zone as a function of Galactic latitude. Outliers are denoted with a cross and listed in Table 3.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: Left: diagram (not to scale) of the cylindrical region of interest, around which the mass flux of the gas is calculated. Right: mass flow history across the boundary of the cylinder of interest, of the in-disk favored (zeta0.1, top panel), isotropic (zeta1, middle panel), and out-of-disk favored (zeta10, bottom panel) runs, and the associated star formation history (red) in the interior of the cylinder. Radial gas flows (Equation (15)) are shown in blue, and vertical flows (Equation (16)) are shown in green. Notably, in the isotropic run, starburst episodes (red peaks) are preceded by a inward bulk gas motion (blue and green dips) followed by peaks of outward motion (blue and green peaks) within the disk, consistent with a more turbulent gas disk. In the in-disk favored run, the vertical gas cycles are suppressed, and in the out-of-disk favored run, the radial gas cycles are suppressed. However, only in the out-of-disk favored run produces bursty star formation and the overall mass flows are suppressed, indicating that radial gas flows are more effective at driving turbulence.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: Magnitude of momentum injected by SNe per mass of stars formed, for each run over 2 Gyr. We calculate the total magnitude in two ways: linear (top panel, Equation (19)), and in quadrature (bottom panel, Equation (20)). For the same weighting scheme, there is no dependence of the magnitude of momentum injected on the anisotropy factor γ. However, between solid-angle weighting (red), volume weighting (blue), and mass weighting (green), the magnitude of momentum injected can differ by as much as a factor of ∼5. These behaviors hold using both calculation methods (although the values do depend on the calculation method).
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: Dark matter density profiles between 1 and 2 Gyr. The median density across snapshots at each radius is plotted as a solid line, and the interquartile range at each snapshot is shaded. Consistent with the understanding of core formation, the out-of-disk favored run, which has a nonbursty star formation history, has a dark matter cusp, and the isotropic and in-disk favored runs, which have bursty star formation histories, have dark matter cores. For comparison, the initial cuspy density profile (measured as the median density from the stellar center of mass over the first 200 Myr, similar across all runs considered) is shown by the gray dashed line.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: Top: total stellar mass formed. Higher-γ runs (i.e., runs with more momentum directed outside the disk), form a lower total stellar mass. The difference in the stellar mass formed can vary by up to half an order of magnitude, across all runs considered. Bottom: burstiness parameter B as defined by Equation (14). Higher-γ runs tend to be less bursty according to this parameter, over a wide range of SFR averaging timescales. The horizontal error bars are the uncertainties in γ, as discussed in Equation (13) and Table 2.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: The effective anisotropy (γ, as defined in Equation (13)), and its associated uncertainty, as a function of the nominal anisotropy (ζ, as defined in Equations (11) and (12)). The nominal anisotropy controls the ratio of momentum injected in the polar (z) direction to the in-plane (x, y) directions, by every star particle, before postprocessing effects are considered. The effective anisotropy measures the ratio between the total momenta actually injected in these directions.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: Vertical (green) and in-plane (purple) stellar velocity dispersion of stars as a function of anisotropy. Changing the degree of anisotropy does not affect the vertical velocity dispersion of the stars, even when we inject more momentum in that direction. Conversely, the radial velocity dispersion of stars is inversely correlated with the anisotropy factor, so that higher radial velocity dispersions are observed when the momentum is injected preferentially within the disk. This may occur either as stars tend to be born on more radial trajectories, or as stellar orbits are dynamically heated by radial flows.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: Star formation histories of the entire galaxy in the in-disk favored (green, left), isotropic (purple, center), and out-of-disk favored (orange, right) momentum injection runs. The top row shows the star formation rate (SFR) in linear scale, the middle row shows the SFR in log scale, and the bottom row shows the cumulative stellar mass formed. The burstiness of the SFR depends substantially on the injection model, with the in-disk favored and isotropic models resulting in more bursty histories and a greater stellar mass than the out-of-disk favored model.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: Gas column density of the in-disk favored (left), isotropic (center), and out-of-disk favored (right) runs at snapshot time 1.2 Gyr. The box width of each panel is 10 kpc on a side. Runs with higher injected momentum within the disk exhibit more diffuse structures and larger gas void regions, but slightly less turbulence in the vertical directions, than runs with more injected momentum out of the disk.
Paper: Bursty Star Formation in Dwarfs is Sensitive to Numerical Choices in Supernova Feedback Models
Authors: Eric Zhang, Laura V. Sales, Federico Marinacci, Paul Torrey, Mark Vogelsberger, Volker Springel, Hui Li, Rüdiger Pakmor, Thales A. Gutcke
Figure caption: Stellar column density of the in-disk favored (left), isotropic (center), and out-of-disk favored (right) runs for snapshot at 1.2 Gyr. The stellar half-mass radius about the stellar center of mass is shown by the white dashed lines. The box width of each panel is 10 kpc on a side.
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: Lyα EWs (top panel) and Lyα escape fractions (bottom panel) vs. the redshifts of the galaxies at z > 6.5 in the public NIRSpec sample. We show the Lyα EWs and Lyα escape fractions measured from the grating spectra (blue circles) and prism spectra (green squares) separately. Sources with Lyα detections are shown by filled symbols, and we put 3σ upper limits for Lyα nondetections as open symbols.
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: Lyα fraction (EW > 25 Å) as a function of redshift. We show the NIRSpec samples at 6.5 < z < 8.0, 8.0 < z < 10.0, and 10.0 < z < 13.3 as red stars. We also present the Lyα fractions of galaxies in the EGS (orange filled diamond) and the GOODS + A2744 (open magenta diamond) fields separately, both at 6.5 < z < 8.0. The top panel shows a comparison between our Lyα fractions at z > 6.5 and those at z ∼ 5–6 in M. Tang et al. (2024b, gray pentagons). The bottom panel shows a comparison with other literature values (M. A. Schenker et al. 2014; C. A. Mason et al. 2018, 2019a; L. Pentericci et al. 2018; H. Kusakabe et al. 2020; M. Nakane et al. 2024).
Paper: On the 3D Transport of Low-energy Galactic Cosmic-ray and Jovian Electrons in the Inner Heliosphere in the Presence of a Fisk-type Heliospheric Magnetic Field
Authors: N. E. Engelbrecht
Figure caption: Left panels: Galactic electron latitude gradients and relative amplitudes as a function of rigidity at 2 au and 50◦ colatitude, as well as the relationship between these quantities, using a Schwadron–Parker hybrid field (blue lines) and a pure Parker field (red dashed lines). Right panels: the same, but for Jovian electrons.
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: The fraction of galaxies with Lyα escape fraction f esc,Lyα  > 0.2 as a function of redshift. We show the NIRSpec samples at 6.5 < z < 8.0 and 8.0 < z < 10.0 as red stars, and show the EGS (orange filled diamond) and the GOODS + A2744 (open magenta diamond) samples at 6.5 < z < 8.0 separately. We overplot data at z ∼ 5 and z ∼ 6 from M. Tang et al. (2024b) as gray pentagons.
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: JWST/NIRSpec 2D and 1D medium resolution grating spectra of JADES-13041. We show the Lyα velocity profile (left panel), the C IV emission lines (middle panel), and strong rest-frame optical emission lines (Hγ, Hβ, and [O III]; right panel).
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: 2D and 1D NIRSpec medium resolution grating spectra of JADES-15423 (top) and JADES-14373 (bottom). The left panels show the Lyα velocity profiles. The right panels show the Hβ and [O III] emission lines.
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: Absolute UV magnitude (M UV) and UV continuum slope (β) of z > 6.5 galaxies identified from the public NIRSpec observations used in this study. We show the 185 galaxies with both M UV and UV slope measurements (open black stars). We mark those with Lyα detections as red filled stars.
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: JWST/NIRCam SED of JADES-13041. Observed NIRCam photometry is shown by blue circles. The BEAGLE model spectrum is shown by the black line and the synthetic photometry is presented by open red squares.
Paper: Local Interstellar Spectra and Solar Modulation of Cosmic-Ray Proton and Helium
Authors: Cheng-Rui Zhu
Figure caption: (a) Top panel: best-fit LIS fluxes (lines) and TOA fluxes (dashed lines) of p and He, multiplied by ﹩{E}_{k}^{2}﹩, compared with the measurements (colorful points) of Voyager 1 (A. C. Cummings et al. 2016), and AMS-02 (M. Aguilar et al. 2021a). Bands show the results with the 95% ranges of the spectral parameters. The middle (bottom) panel shows the the 95% credible intervals centered around J best for proton (Helium). (b) LIS ratio of proton-to-Helium, the band stands for the 95% CI.
Paper: Local Interstellar Spectra and Solar Modulation of Cosmic-Ray Proton and Helium
Authors: Cheng-Rui Zhu
Figure caption: Time series of ϕ  l  (red line) and ϕ  h  (blue line) via fitting to the AMS-02 p, He and p/He from 2011 to 2017, with 1σ bands. Previous results inferred from the neutron monitor (NM) data (I. G. Usoskin et al. 2011, 2017; yellow line) and GCR data (C.-R. Zhu et al. 2018; dark line) are also shown for comparison. The yellow band stands for the heliospheric magnetic field reversal period within which the polarity is uncertain (X. Sun et al. 2015).
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Locations of our fields overlaid on a stellar density map from SMASH DR2 (see text for details), in tangent plane coordinates assuming an LMC center of (R.A., decl.) = (82.25°, −69.5°) based on near-infrared stellar isodensity contours in the outer disk (R. P. van der Marel & M.-R. L. Cioni 2001). The dynamical center of the H I disk (T. Luks & K. Rohlfs 1992; S. Kim et al. 1998) used for our analysis of radial age gradients in Section 4 is shown as a plus sign. North is up, east is to the left, and the SMC is located to the lower right (well outside the plot). The fields we analyze are shown as filled circles, color-coded by their source as indicated in the upper left corner. Ground-based imaging fields analyzed by L. Monteagudo et al. (2018) and I. Meschin et al. (2014) are shown as green diamonds and stars, respectively, and the subset of archival J. A. Holtzman et al. (2006) WFPC2 LGSPA fields analyzed by D. R. Weisz et al. (2013) are overplotted as pink squares. Dashed lines indicate the subsets of fields in the southeast disk (magenta) and the spiral arm (orange) discussed in Section 4, and the Hubble Tarantula Treasury Project (HTTP) footprint (E. Sabbi et al. 2016) is shown in purple and labeled.
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Stacked CMD of all stars passing our photometric quality cuts, from Scylla fields and archival METAL fields, both of which were observed with WFC3/UVIS F475W and F814W filters (left) and archival LGSPA photometry observed with WFPC2 F555W and F814W (right). No correction for field-to-field differences in extinction or distance has been applied. Median photometric errors in magnitude bins, assessed using artificial star tests, are shown along the left-hand side of each CMD. PARSEC isochrones have been overplotted, indicating the main-sequence stellar mass range typical of our photometric catalogs.
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: CMDs of the four outer fields LMC_OF1−LMC_OF4 used to extend our radial coverage of the LMC, with isochrones overplotted as in Figure 2.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Photometry from DES DR1 (top left), DECaLS DR9 (top right), and DES DR2 (bottom left) cross-matched with S 5 survey targets, with target classes of BHB and BS as classified by S 5 surface gravity and temperature measurements (see Section 2). The bottom right panel uses the same photometry as the bottom left panel, but classified according to the photometric mixture model described in Section 3. The improved data quality of DES DR2 relative to DES DR1 and DECaLS DR9 is clearly visible, with both BHB and BS sequences becoming tighter and their separation more apparent. The high-quality photometry in DES DR2 is one of the key factors that enables our mixture model to accurately recover the underlying BHB and BS populations from photometric colors alone. We note that we do not include i-band photometry here for comparison since DECaLS DR9 does not include i-band data.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Same as Figure 1, but now showing the distribution of stars in three different extinction-corrected g 0 magnitude ranges in the top panel. As we extend into fainter magnitudes, the larger measurement errors cause the two well-defined sequences of BHBs and BSs to blend together, making it harder to disentangle potential BHB candidates. This motivates the use of the probabilistic mixture model described in Section 3, and the stars classified by our model as BHBs, BSs, and outliers are shown with blue circles, purple squares, and red stars, respectively, in the bottom panel. The predicted class is defined to be the one that shows the highest posterior-marginalized probability, and the color is used to represent the probability (one of p BHB, p BS, p outlier). The blue solid line and purple solid line show the ridgelines μ BHB and μ BS, calculated from the best-fit parameters in Table 1. The shaded regions with dashed lines on their boundaries along each ridgeline show the intrinsic scatters σ int for each sequence.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Left: a corner plot depicting the 2D and 1D marginal posterior probability distributions of the 14 parameters of our photometric mixture model estimated with dynesty. All values were multiplied by a factor of 100 for visualization purposes. The parameters model different aspects of the data, as noted in red at the bottom. The parameter “BHB fraction*” describes the ratio of BHBs to nonoutliers. Right: the predicted ratio of BHBs (blue), BSs (purple), and outliers (red) as a function of magnitude. Overall, our model has parameters that are well constrained, accurately trace the photometric distribution of stars, successfully identify photometric outliers, and generate physically sensible magnitude dependencies across each subgroup.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Histograms of final selected BHB candidates in DES DR2 vs. simulated samples from the best-fit density profile. Left: with heliocentric distance d; right: with Galactic radius R. We see that our best-fit density profile accurately captures the stellar density distribution, generating samples that match the data well from both heliocentric and Galactocentric points of view.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Radial distribution of BHB candidates (with p BHB ≥ 0.5 computed by our model) selected from DES DR2. Left: all candidates; right: after removing regions associated with known overdensities in Section 4. Color represents Galactic latitude b. In order of increasing heliocentric distance, our selected BHBs correctly show overdensities associated with known substructures: the Sgr stream, the LMC, and Sculptor. The removal is not exhaustive, and there are many other substructures left in the sample (see Figure 13).
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Extinction-corrected ﹩{\left(g-r\right)}_{0}﹩ vs. (i − z)0 of DES DR2 photometry for stars with magnitudes in the range 18 ≤ g 0 ≤ 20. The color–color cut used to remove contamination from WDs (lower sequence) is shown as a dashed red line. The red circles show the potential QSOs by matching our sample with the active galactic nucleus candidates from Y. Shu et al. (2019), while the blue circles show the WD sample with absolute G mag M  G  > 7.5 and good distance estimates (parallax_over_error > 10 in Gaia DR3).
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: On-sky distribution of BHB candidates, for the same samples as in Figure 6. Left: before removing substructures; right: after removing substructures. Color represents heliocentric distances. The removal of regions associated with the LMC, NGC 300, Fornax, Sculptor, and Sgr is clearly shown.