adsabs/AstroCLIMB huggingface dataset:
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: Two-dimensional distribution of redshift versus i-band magnitude for all of the HSC+WISE objects in the HSC–DESI overlap fields in GAMA defined in Section 2.4.2, colored by the fraction of objects that were spectroscopically observed by DESI. We again split the sample by the photometric AGN classification described in Section 2.3 in to Type I (left panel) and Type II AGNs (right panel). From the fraction of DESI-observed objects as a function of brightness and redshift, we observe the characteristic DESI S/N threshold as a function of redshift that selects for the brightest objects available. Thus, DESI poorly samples from the obscured and faint population of AGNs in the HSC+WISE catalog, and is much more complete for the characteristically brighter Type I AGNs.
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: Redshift comparison for all DESI-matched HSC+WISE AGNs that did not already have a spectroscopic redshift, as a 2D histogram colored by number of objects per cell N. We compare the photometric redshift from the HSC+WISE catalog (described in Section 2.3) with the DESI-provided spectroscopic redshift for all objects with z < 1.4. We overlay a reference 1:1 relation as a black dashed line, and an uncertainty envelope of δz = 0.1 × (1 + z) as a pair of dotted lines. We split the matched sample into Type I (unobscured and reddened) and Type II (obscured) AGNs from the photometric classification we use in R. Córdova Rosado et al. (2024) and reference in Section 2.3. We note that the Type I AGNs are more numerous, and their redshifts follow the 1:1 line with a median absolute deviation (MAD) in their difference of ∼0.05, while the Type II AGNs have a tilt of approximately δz = 0.05 × (1 + z) and the MAD in their difference of ∼0.07. The HSC photo-z’s slightly overestimate the spectroscopic redshift, with the effect being most dramatic at z > 1.0. The bottom panels show the difference between redshift estimates represented by (zphot − zspec)/(1 + zspec).
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: WISE and optical photometric color–color distribution for the parent HSC+WISE AGN catalog and the objects with a match in DESI. As in Figure 2, we split the HSC+WISE AGN catalog using their photometric classifications into Type I (unobscured and reddened, left column) and Type II (obscured, right column). Top row: the MIR W2−W3 versus W1−W2 color space of our AGNs. We overlay the D. Stern et al. (2012) AGN selection threshold (W1−W2 = 0.16 in AB magnitudes) as a dashed line, the AB magnitude-converted S. Mateos et al. (2012) wedge in dotted lines, and the T. H. Jarrett et al. (2011) box in dotted–dashed lines. Our unsupervised ML-selected AGN sample includes a significant number of objects that fall outside these canonical selection choices. The matched HSC×DESI sample follows the color distribution of the parent HSC+WISE sample, although the higher DESI S/N leads to an apparent undersampling of the bottom-right color space for the Type II AGN, discussed in Section 2.4.2. Bottom row: the optical r − i versus g − r color space of our AGNs. The color distribution of the matched sample follows the contours of the parent sample closely, as expected given the similar optical selection constraints between the HSC+WISE catalog and DESI.
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: The HSC+WISE-selected AGN sample from A. D. Goulding et al. (2025, in preparation) for the HSC GAMA field, and its matches in the DESI Early Data Release (EDR.) The HSC GAMA field, centered at approximately at R.A., decl. (11.7 hr, 0∘), includes all masking choices detailed in Section 2.2. Our procedure to select matches in the DESI EDR catalog is detailed in Section 2.4.2. The three contiguous regions of overlap—which we label GAMA10h, GAMA12h, and GAMA14h after their approximate hour coordinate in R.A.—are treated independently in the analysis. The angular scales for the x- and y-axes are stretched inhomogeneously, making the circular DESI fields appear elongated.
Paper: Curious Case of CGRaBS J0211+1051: Observational Evidence of the Lepto-hadronic Origin of High-energy Emission?
Authors: Sunil Chandra, Pankaj Kushwaha, Pranjupriya Goswami, Michael Zacharias
Figure caption: (a) X-ray spectra fitted with a simple absorbed power-law model (TBabs*powerlaw). (b) Same as (a) but with Γ tied to the one from the 2011 observations. (c) The contour plots for the Γ–N distribution showing confidence intervals for three different X-ray spectra. (d) Simultaneous X-ray and UV spectral modeling. The black data points refer to optical–X-ray data taken from 2021 December 9 to 15, representing a fainter quiescence state of the source. The red and cyan data are unfolded data points in UV X-rays from F2011 and F2109. S1 in the legends refers to test scenario 1 (Section 2.6; the spectral slopes for the UV and X-ray bands are the same, only the norms are different), whereas S2 belongs to scenario 2 (both norms and indices are kept free while modeling). The black X-ray data are pn spectra, whereas the orange X-ray data are from the MOS observations.
Paper: Curious Case of CGRaBS J0211+1051: Observational Evidence of the Lepto-hadronic Origin of High-energy Emission?
Authors: Sunil Chandra, Pankaj Kushwaha, Pranjupriya Goswami, Michael Zacharias
Figure caption: Long-term optical lightcurve showing strong variability throughout. The magnitudes in the ZTF filters are shifted by a constant value to fit in the frame. The vertical dashed lines represent different epochs used for SED extraction.
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: Broadband modeling including optical rebrightening results. Multiband light curves fitted with a two-component uniform (top-hat) jet model. X-ray (Swift/XRT; 1 keV), optical/near-infrared (r, z, J; M. Busmann et al. 2025), and 15.5 GHz radio (AMI-LA; F. Carotenuto et al. 2024) data are shown. Downward arrows mark 3σ upper limits; open symbols indicate points excluded in the fit. Solid lines show the best-fitting two-component jet model, with contributions from the first component (dashed) and the second component (dotted) indicated separately. Band-dependent scaling factors are applied for clarity.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: A cluster phase-space sampled with an increasing number of tracers. The data were generated using the AGAMA framework (see the text) for an M200 = 1015 M⊙ cluster at redshift z = 0.01 with β = 0.25. The black points are the inferred line-of-sight velocities from a single line-of-sight draw. The down-sampled edge profile (black dotted lines) corresponds to the maximum absolute velocity within each radial bin. The blue (solid) lines correspond to the 3D escape profiles (Equation (4)). Note the increased suppression of the edge as sampling decreases.
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: Broadband modeling results. Best-fit afterglow light curves for an on-axis jet (model top hat) compared with observations at multiple frequencies. The X-ray (Swift/XRT; 1 keV) and optical and near-infrared observations in the r, z, and J filters are from M. Busmann et al. (2025). Radio observations at 15.5 GHz from AMI-LA (F. Carotenuto et al. 2024). Downward arrows indicate 3σ upper limits. Empty symbols show data not used for model fitting. A scaling factor has been applied to different frequencies for plotting purposes.
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: Radio luminosity light curves. EP241021A (red circles) is compared to other FXRTs (e.g., EP240315A, R. Ricci et al. 2025; EP240414A, J. S. Bright et al. 2025) as well as other high-energy transients, including GRBs (circles; P. Chandra & D. A. Frail 2012), relativistic TDEs (squares; B. A. Zauderer et al. 2011; I. Andreoni et al. 2022), and FBOTs (diamonds; R. Margutti et al. 2019; D. A. Perley et al. 2019, 2021).
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: Broadband modeling including optical rebrightening results. Posterior distributions of the fitted parameters for the uniform (top-hat) jet model.
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: Variability timescale on 2024 October 29 with data sampled at 40 minute intervals.
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: Broadband modeling results. Corner plot showing the posterior distributions of the fitted model parameters using a uniform (top-hat) jet model.
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: Spectral index evolution between 5.5–9 GHz (red circles) and 9–17 GHz (blue squares) over time since the EP trigger. The dashed line indicates β = 0.75.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: Phase-space diagrams of 45 clusters in the sample (AS1063 not shown; see A. Rodriguez et al. 2024). The black points indicate member galaxies, the red points indicate interlopers, the red lines indicate the identified phase-space edge, the blue lines indicate the dynamical fits, and the green lines indicate the suppressed lensing profiles.
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: The HG SPF as a function of scattering angle for TWA 20, AU Mic (K. Lawson et al. 2023), and TWA 7 (K. A. Crotts et al. 2025), based on disk models fit to scattered-light observations with JWST/NIRCam. In addition to the SPF constructed with the best-fit values of g1, g2, and w1 for TWA 20 (thick blue line), SPFs based on 1000 random draws from the posterior distributions of g1, g2, and w1 are plotted to demonstrate the spread in possible SPF structure. In most of these draws, a notable backward-scattering peak is visible in addition to the forward-scattering peak characteristic of the SPF of all three plotted disks.
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: Debris disk radius as a function of host-star luminosity for resolved M dwarf disks. Scattered-light radii are shown as opaque and filled markers; thermal emission radii are shown as open and unfilled markers. Both radius measurements are reported for disks with both scattered-light and thermal emission data. Disk radii and stellar luminosity were taken from L. Matrà et al. (2025), É. Choquet et al. (2016), K. Lawson et al. (2023, 2024), C. Adam et al. (2021), and P. F. Cronin-Coltsmann et al. (2023). Only the inner most ring is included for TWA 7 for visual clarity; the additional rings extend well beyond 100 au. Luminosity for TWA 20 was computed from the TWA 20 photometric data. The shaded area represents the power-law relationship between R and L* determined by L. Matrà et al. (2018, 2025).
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: TWA 20 photometry data from R. M. Cutri et al. (2021), Gaia Collaboration et al. (2021), M. F. Skrutskie et al. (2006), C. A. Onken et al. (2024), SSC, S. Alam et al. (2015), and our MCFOST model stellar + disk SED. For this target, there are no observations at longer wavelengths to validate the potential excess beyond 100 μm.
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: Left: deconvolved image of the TWA 20 debris disk in the F200W filter obtained by running a deconvolution routine on the MCRDI result. The image is rotated with north up. Right: surface brightness (radial profiles) of the deconvolved disk, the raw disk model (analytical model from the fitting procedure), and the convolved disk as a function of separation from the host star.
Paper: Discovery of a Debris Disk around TWA 20
Authors: Skyler Palatnick, Maxwell A. Millar-Blanchaer, Jingwen Zhang, Kellen Lawson, Briley L. Lewis, Katie A. Crotts, Aarynn L. Carter, Beth Biller, Julien H. Girard, Sebastian Marino, Raphaël Bendahan-West, Giovanni M. Strampelli, Andrew D. James, Klaus Subbotina Stephenson, Rodrigo Ferrer-Chavez, Mark Booth, Ben J. Sutlieff, Aniket Sanghi, Clémence Fontanive, Emily Rickman, Isabel Rebollido, Kielan Hoch, William O. Balmer
Figure caption: Left: posterior distributions from the nested-sampling disk fitting routine. Some parameters, such as r0, αout, θinc, and θPA, are well constrained; other parameters, such as αin and Fs are not. Follow-up observations may improve our understanding of the structure of the TWA 20 disk.
Paper: A Visibility-based 21 cm Bispectrum Estimator for Radio-interferometric Data
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj
Figure caption: The binning scheme used by the MABS estimator. The three 2D planes correspond to frequency channels (ν1, ν2, ν3). The scattered dots in each plane show the discrete sampling of (u, v) space (gridded baseline distribution Ug) corresponding to the particular MWA observation considered here. The Ug planes are divided into annular rings. Three such rings (labeled a1, a2, and a3) with average radii (ℓ1, ℓ2, ℓ3) ≡ 2π (U1, U2, U3) are shown schematically. Note that each ring is on a different plane i.e., a different frequency. The three baselines shown here form a closed triangle Ug1 + Ug2 + Ug3 = 0. The binned MABS estimator ﹩{\widehat{B}}_{A}({\ell }_{1},{\ell }_{2},{\ell }_{3},{\nu }_{1},{\nu }_{2},{\nu }_{3})﹩ considers the average over all such triangles. Note that this figure is very similar to Figure 1 of S. S. Gill & S. Bharadwaj (2025b), except that the 2D planes there correspond to different values of k∥ instead of ν.
Paper: A Visibility-based 21 cm Bispectrum Estimator for Radio-interferometric Data
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj
Figure caption: The 3D cylindrical BS B(k1⊥, k2⊥, k3⊥, k1∥, k2∥) with ﹩{k}_{1\perp }={k}_{2\perp }={k}_{3\perp }=\frac{{\ell }_{1}}{r}=0.077\,{{\rm{Mpc}}}^{-1}﹩ fixed. The analytical predictions in the left panels are calculated using Equation (21), whereas the estimates are obtained via a 2D Fourier transform (Equation (19)) of the MABS shown in the respective panels of Figure 3. In all the panels, the values have been binned in a 20 × 20 grid in the (k1∥, k2∥) plane. The top row shows the 3D BS as a heat-map in the (k1∥, k2∥) plane, the bottom row shows 1D slices along k1∥ for three fixed values of k2∥ = {−0.17, 0.06, 0.17} Mpc−1, indicated by red, black, and green lines, respectively. The middle and right panels show the estimates without and with flagging, respectively. The error bars represent the 1σ rms statistical uncertainty.
Paper: A Visibility-based 21 cm Bispectrum Estimator for Radio-interferometric Data
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj
Figure caption: MABS BA(ℓ1, ℓ2, ℓ3, Δν1, Δν2) as a function of (Δν1, Δν2) for an equilateral configuration with ℓ1 = ℓ2 = ℓ3 = 711. The top panel shows the analytical prediction; the middle and bottom panels show the estimates without and with flagging, respectively. The black solid line in each inset shows a 1D slice of the MABS along Δν1 at fixed Δν2 = 0. The green points in the inset show the estimated values, and the orange-shaded region denotes the 1σ rms statistical fluctuations.
Paper: A Visibility-based 21 cm Bispectrum Estimator for Radio-interferometric Data
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj
Figure caption: The sampling Nν(Δν1, Δν2), which counts the number of frequency channel triplets (ν1, ν2, ν3) corresponding to each set of frequency separations (Δν1, Δν2). The left panel shows Nν(Δν1, Δν2) without flagging, while the right panel shows the same with flagging i.e., it incorporates the periodic pattern of missing channels present in the MWA data. In both panels, the region where ∣Δν2 − Δν1∣ > Bbw is not sampled at all. The black line encloses the region that we have used for the 2D FFT (Equation (19)) to evaluate the 3D BS. This is the largest regular region that avoids the frequency separations that are not sampled. Note that there are no missing frequency separations (Δν1, Δν2) introduced due to the flagging.
Paper: A Visibility-based 21 cm Bispectrum Estimator for Radio-interferometric Data
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj
Figure caption: The 3D BS monopole ﹩\bar{B}({k}_{1},\mu ,t)﹩ for all the triangle configurations where we have estimates. Each panel, which corresponds to a different (μ, t) (shape), shows the estimated value ﹩\bar{B}﹩, with 1σ error bars, as a function of k1. The analytical predictions ﹩{[\bar{B}]}_{d}﹩ are also shown for comparison.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: Weak lensing and escape masses for the 46 clusters in our sample, assuming our fiducial cosmology. The bias (lensing versus escape) and correlation are significantly improved from using caustics in Figure 7. The embedded histograms (purple being escape, yellow being lensing) show the distribution of z-scores compared to the expectation of a Gaussian centered at 0 with σ = 1, for which we find very good agreement for the escape velocity (lensing errors are marginally underestimated). This indicates our errors are consistent with the intrinsic scatter.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: Left panel: we infer unbiased escape masses for the halos in the Millennium simulation using the AGAMA analytic model for the suppression. When the skewness in the suppression distribution is ignored, the bias increases by 0.1 (green points). The embedded histograms show the distributions of z-scores, compared to the expectation of a Gaussian centered at μ = 0 with σ = 1. The dashed line shows unity slope. Right panel: same as the left panel, except for when the true mass has a 0.6 dex uncertainty. The bias is statistically consistent.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: We show the effect of the choice of the initial estimate of r200 on the inferred escape mass (y-axis). The initial r200s are determined after scatting the true mass by δM. The posterior M200 is centered about its mean for visual purposes. We use N = 100 different phase-space realizations of ﹩{\hat{M}}_{200}﹩ for a fixed line-of-sight projection. The inner blue circle denotes the 1σ confidence level, with the outer ones denoting 2σ and 3σ. The ellipse is nearly horizontal, such that the induced correlation while present, is very weak. The embedded histogram shows the marginalized posterior. The shaded region defines the range of initial r200s used, which has little influence on the mass.
Paper: The Concordance of Weak Lensing and Escape-velocity Mass Estimates for Galaxy Clusters
Authors: Alexander Rodriguez, Christopher J. Miller
Figure caption: Random velocity draws (assumed to be from a normal distribution) that are added to the galaxy velocities in an example halo in Millennium, then used to measure the standard deviation in the resulting down-sampled edge profile (﹩{\sigma }_{{v}_{\,\rm{esc,DS}\,}}﹩), over 10,000 velocity draws. These are shown for different bin numbers, as shown by the different colored lines. The uncertainty in the down-sampled edge profile is always less than or equal to the error on the velocity itself. The star shows the value of σ = 30 km s−1 assumed in the data. The black solid line shows unity slope.