adsabs/AstroCLIMB huggingface dataset:
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: Similar to Figure 1, but for dark matter particles from TNG300.
Paper: How Do the Velocity Anisotropies of Halo Stars, Dark Matter, and Satellite Galaxies Depend on Host Halo Properties?
Authors: Jiaxin He, Wenting Wang, Zhaozhou Li, Jiaxin Han, Vicente Rodriguez-Gomez, Donghai Zhao, Xianguang Meng, Yipeng Jing, Shi Shao, Rui Shi, Zhenlin Tan
Figure caption: Similar to Figures 1 and 2 above, but for subhalos from TNG300. Wide radial bins are adopted for subhalos, due to their much smaller sample size.
Paper: Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2
Authors: K. R. Gold, D. R. Schmidt, L. M. Ziurys
Figure caption: Spectra of molecular transitions observed toward the planetary nebula M4-17 obtained with the ARO telescopes (1, 2, and 3 mm) and the IRAM 30 m (2 mm); see Table 1. Among the new detections in this PN are HNC, CN, CCH, CS, and H2CO, identified by the various transitions indicated. H13CN has also been observed, as shown. The N = 2 → 1 line of CCH and the J Ka,Kc = 21,1 → 11,0 line of H2CO were observed at both the ARO 12 m and the IRAM 30 m, as indicated. The fine-structure splittings for CCH (N = 2 → 1 and N = 3 → 2) and CN (N = 2 → 1) are shown underneath the spectra, except for the CN N = 1 → 0 line, where separate spectra are displayed. Improved data are also shown for CO, HCN, and HCO+ (see text). The spectra were observed with 0.3–0.5 km s−1 (IRAM), 1.1–1.8 km s−1 (12 m), and 1.1–1.3 km s−1 (SMT) resolution and smoothed to 4.5–6.5 km s−1. The temperature scale is ﹩{T}_{A}^{* }﹩ (mK).
Paper: Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2
Authors: K. R. Gold, D. R. Schmidt, L. M. Ziurys
Figure caption: Spectra of molecular transitions observed toward the planetary nebula M1-59 obtained with the ARO telescopes (1, 2, and 3 mm) and the IRAM 30 m (2 mm); see Table 1. New detections in this PN are HNC, CN, CCH, and CS, identified by the transitions indicated, as well as H13CN. Also presented (lower left corner) is the spectrum of the J Ka,Kc = 11,0 → 10,1 transition of H2S, a new molecule in PNe. The fine-structure splittings for CCH (N = 3 → 2) and CN (N = 2 → 1) are shown underneath the spectra. Improved data are also shown for CO, HCN, and HCO+ (see text). Channels containing galactic contamination in the CO: J = 1 → 0 panel are omitted. Hydrogen radio recombination lines appear in the HCO+; J = 1 → 0 and CS: J = 3 → 2 panels, as indicated. The spectra were observed with 0.3–0.5 km s−1 (IRAM), 1.1–1.8 km s−1 (12 m) and 1.1–1.3 km s−1 (SMT) resolution and have been smoothed to 3–5 km s−1. The temperature scale is ﹩{T}_{A}^{* }﹩ (mK).
Paper: Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2
Authors: K. R. Gold, D. R. Schmidt, L. M. Ziurys
Figure caption: Spectra of molecular transitions observed toward the planetary nebula Hu 1-1 obtained with the ARO telescopes (1, 2, and 3 mm) and the IRAM 30 m (2 mm); see Table 1. New detections are HNC, CN, CCH, CS, H2CO, and c–C3H2, identified by the transitions indicated. H13CN has also been observed, as shown. The N = 2 → 1 line of CCH and the J Ka,Kc = 21,1 → 11,0 line of H2CO were observed at both the ARO 12 m and the IRAM 30 m, as indicated. The fine-structure splittings for CCH (N = 2 → 1 and N = 3 → 2) and CN (N = 2 → 1) are shown underneath the spectra. Improved data are also shown for HCN and HCO+ (see text). The spectra were observed with 0.3–0.5 km s−1 (IRAM), 1.1–1.8 km s−1 (12 m), and 1.1–1.3 km s−1 (SMT) resolution and have been smoothed to 4–6 km s−1. The temperature scale is ﹩{T}_{A}^{* }﹩ (mK).
Paper: Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2
Authors: K. R. Gold, D. R. Schmidt, L. M. Ziurys
Figure caption: Plots of observed fractional abundances from this work and the literature (P. Cox et al. 1992; R. Bachiller et al. 1997; J. L. Edwards & L. M. Ziurys 2013, 2014; J. L. Edwards et al. 2014; D. R. Schmidt & L. M. Ziurys 2016, 2017a, 2017b, 2019; D. R. Schmidt et al. 2018a, 2018b, 2022) vs. ages of PNe (in year). Left column shows plots for CCH (green circles), CN (red stars), and HNC (teal triangles). Right column displays data for H2CO (navy crosses), c–C3H2 (yellow squares), and CS (purple diamonds). Predictions from the M. P. Redman et al. (2003) model are also shown for CCH, CN, HNC, and CS by dashed lines. As these plots illustrate, observed abundances remain constant across the >12,000–25,000 yr PN lifespan for all six molecules, within factors of 10–60. In contrast, the model predicts decreases in abundance of three to four orders of magnitude, up to ∼10,000 yr.
Paper: Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2
Authors: K. R. Gold, D. R. Schmidt, L. M. Ziurys
Figure caption: Spectra of molecular transitions observed toward the planetary nebula Na 2 obtained with the ARO telescopes (1 and 3 mm); see Table 1. The new detections are CN, observed in both the N = 1 → 0 and N = 2 → 1 transitions, and CCH, N = 3 → 2. The fine-structure splittings for CCH (N = 3 → 2) and CN (N = 2 → 1) are shown underneath the spectra. One (J = 5/2 → 3/2) spin component of CCH, which is quantum-mechanically expected to be weaker, has a low intensity. Improved data are also shown for CO and HCO+ (see text). The spectra were observed with 1.1–1.8 km s−1 (12 m) and 1.1–1.3 km s−1 (SMT) resolution and have been smoothed to 3–5 km s−1. The temperature scale is ﹩{T}_{A}^{* }﹩ (mK).
Paper: Scintillation Bandwidth Measurements from 23 Pulsars from the AO327 Survey
Authors: Sofia Sheikh, Grayce C. Brown, Jackson MacTaggart, Thomas Nguyen, William D. Fletcher, Brenda L. Jones, Emma Koller, Veronica Petrus, Katie F. Pighini, Gray Rosario, Vincent A. Smedile, Adam T. Stone, Shawn You, Maura A. McLaughlin, Jacob E. Turner, Julia S. Deneva, Michael T. Lam, Brent J. Shapiro-Albert
Figure caption: An example of the analysis pipeline described throughout Section 3 for a scan of pulsar B2315+21. Subplot (1): The dynamic spectrum after loading into PyPulse with a pulse template. Time is shown on the horizontal axis and frequency on the vertical axis. The pulsar fades in as it enters the drift-scan beam and then fades out as it leaves the beam a few minutes later. Scintillation is visible in the horizontal striping across the pulsar’s signal from top-to-bottom. Subplot (2): The 2D autocorrelation function (2D ACF) of the dynamic spectrum, showing the correlation of the signal with a delayed copy of itself as a function of lag (delay) in time and frequency. The correlation coefficient is a measure of similarity between the signal and its copy, with the central peak normalized to unity. The frequency lag is shown on the vertical axis and the time lag is shown on the horizontal axis. The horizontal extent (in time lag) only indicates the time that the pulsar was in the beam, not the scintillation timescale, and is thus unimportant for this study. The width of the narrowest horizontal stripe in the 2D ACF is indicative of the scintillation bandwidth corresponding to the stripes in Subplot (1). Subplot (3): The 2D ACF “slice,” created by summing the 2D ACF in Subplot (2) along the time axis. The narrowest peak in this image can be fitted with a Gaussian or Lorentzian to measure the scintillation bandwidth. For some faint pulsars, the bounds of the fit will be determined by crossing points where the correlation coefficient becomes negative (dashed line). Subplot (4): The 2D ACF slice from Subplot (3), but zoomed in to the middle few MHz and overplotted with both a best-fit Lorentzian (green) and a best-fit Gaussian (blue) to the points between the vertical gray dashed lines, using a least squares fitting method. These are the measurements reported in Table 1.
Paper: Scintillation Bandwidth Measurements from 23 Pulsars from the AO327 Survey
Authors: Sofia Sheikh, Grayce C. Brown, Jackson MacTaggart, Thomas Nguyen, William D. Fletcher, Brenda L. Jones, Emma Koller, Veronica Petrus, Katie F. Pighini, Gray Rosario, Vincent A. Smedile, Adam T. Stone, Shawn You, Maura A. McLaughlin, Jacob E. Turner, Julia S. Deneva, Michael T. Lam, Brent J. Shapiro-Albert
Figure caption: DM vs. scattering time in ms, shown on logarithmic axes. The orange points indicate the DM and τ  s  values from our measurements, while the brown line shows the best fit of the form A × DM a . We find that the DM scaling method somewhat matches our data set, with best-fit parameters of A = 2.1 × 10−1 and a = 2.6, but there is still significant scatter. We display 1σ errors for the converted scattering time, as calculated in Section 3.7. Note that the sizes of the error bars span four orders-of-magnitude, and points with smaller error bars are significantly upweighted in the fit; this can be difficult to gauge visually given that points with different magnitudes of error bars can look deceptively similar in log–log plotting.
Paper: Scintillation Bandwidth Measurements from 23 Pulsars from the AO327 Survey
Authors: Sofia Sheikh, Grayce C. Brown, Jackson MacTaggart, Thomas Nguyen, William D. Fletcher, Brenda L. Jones, Emma Koller, Veronica Petrus, Katie F. Pighini, Gray Rosario, Vincent A. Smedile, Adam T. Stone, Shawn You, Maura A. McLaughlin, Jacob E. Turner, Julia S. Deneva, Michael T. Lam, Brent J. Shapiro-Albert
Figure caption: Correlations between DF (Gaussian fit vs. NE2001) and DM (top left-hand panel), period (top right-hand panel), galactic longitude (bottom left-hand panel), and galactic latitude (bottom right-hand panel). While no universal trends are visible, the presence of measurements with negative DF at low DMs and periods, and the high DF on the pulsar furthest from the galactic plane, could point to differing accuracy of NE2001 in certain directions and distances. The 1σ errors are displayed for the DF, calculated using only measurement errors from Section 3.7 (not model errors). The two points with large DF and error bars near 250° galactic longitude belong to B1237+25, whose measured scintillation bandwidths were significantly larger than the prediction when compared to the rest of the sample. Large measured bandwidths are associated with larger absolute errors, which are exaggerated in this case by the small predicted bandwidth.
Paper: Scintillation Bandwidth Measurements from 23 Pulsars from the AO327 Survey
Authors: Sofia Sheikh, Grayce C. Brown, Jackson MacTaggart, Thomas Nguyen, William D. Fletcher, Brenda L. Jones, Emma Koller, Veronica Petrus, Katie F. Pighini, Gray Rosario, Vincent A. Smedile, Adam T. Stone, Shawn You, Maura A. McLaughlin, Jacob E. Turner, Julia S. Deneva, Michael T. Lam, Brent J. Shapiro-Albert
Figure caption: Two Sankey diagrams generated with Sankeymatic (S. Bogart 2024) illustrating (1) the path of pulsars from initial identification in the data set to selection for analysis in Section 3 and (2) the result of each PUPPI PSRFITS file from each of those pulsars, leading to the 38 measurements we report in Section 4. In subfigure (1), there are two separate NE2001 filtering steps, indicating the original incomplete filtering described in Section 2.2.
Paper: Scintillation Bandwidth Measurements from 23 Pulsars from the AO327 Survey
Authors: Sofia Sheikh, Grayce C. Brown, Jackson MacTaggart, Thomas Nguyen, William D. Fletcher, Brenda L. Jones, Emma Koller, Veronica Petrus, Katie F. Pighini, Gray Rosario, Vincent A. Smedile, Adam T. Stone, Shawn You, Maura A. McLaughlin, Jacob E. Turner, Julia S. Deneva, Michael T. Lam, Brent J. Shapiro-Albert
Figure caption: A scatterplot comparing the Lorentzian (x-axis) and Gaussian (y-axis) scintillation bandwidth measurements below 1 MHz. The Gaussian and Lorentzian measurements for each scintillation bandwidth are generally similar, but the Lorentzians start trending larger at larger scintillation bandwidths (this trend continues into the four measurements above 1 GHz but was omitted for plot readability). The 1σ errors are displayed for each fit, as calculated in Section 3.7.
Paper: Scintillation Bandwidth Measurements from 23 Pulsars from the AO327 Survey
Authors: Sofia Sheikh, Grayce C. Brown, Jackson MacTaggart, Thomas Nguyen, William D. Fletcher, Brenda L. Jones, Emma Koller, Veronica Petrus, Katie F. Pighini, Gray Rosario, Vincent A. Smedile, Adam T. Stone, Shawn You, Maura A. McLaughlin, Jacob E. Turner, Julia S. Deneva, Michael T. Lam, Brent J. Shapiro-Albert
Figure caption: Predicted scintillation bandwidths using M. A. Krishnakumar et al. (2015) (YMW16) plotted against the measured scintillation bandwidths from this study fitted with Gaussians (blue) and Lorentzians (green). Upper limits are shown with gold triangles. Even more strongly than with NE2001, the measurements were larger than their corresponding predictions. The 1σ errors are displayed for the measured scintillation bandwidth, as calculated in Section 3.7.
Paper: Scintillation Bandwidth Measurements from 23 Pulsars from the AO327 Survey
Authors: Sofia Sheikh, Grayce C. Brown, Jackson MacTaggart, Thomas Nguyen, William D. Fletcher, Brenda L. Jones, Emma Koller, Veronica Petrus, Katie F. Pighini, Gray Rosario, Vincent A. Smedile, Adam T. Stone, Shawn You, Maura A. McLaughlin, Jacob E. Turner, Julia S. Deneva, Michael T. Lam, Brent J. Shapiro-Albert
Figure caption: A histogram comparing the distribution of DF (i.e., the consistency of the model with the data) for YMW16 vs. NE2001 predictions compared to data with Gaussian fits. Even with a small sample size, it is clear that the NE2001 distribution peaks closer to zero than the YMW16 distribution in the left-hand plot, indicating that NE2001 is a better fit to the data.
Paper: Scintillation Bandwidth Measurements from 23 Pulsars from the AO327 Survey
Authors: Sofia Sheikh, Grayce C. Brown, Jackson MacTaggart, Thomas Nguyen, William D. Fletcher, Brenda L. Jones, Emma Koller, Veronica Petrus, Katie F. Pighini, Gray Rosario, Vincent A. Smedile, Adam T. Stone, Shawn You, Maura A. McLaughlin, Jacob E. Turner, Julia S. Deneva, Michael T. Lam, Brent J. Shapiro-Albert
Figure caption: Predicted scintillation bandwidths from NE2001 plotted against the measured scintillation bandwidths from this study fitted with Gaussians (blue) and Lorentzians (green). Upper limits are shown with gold triangles. In general, the measurements were larger than their corresponding predictions. The 1σ errors are displayed for the measured scintillation bandwidth, as calculated in Section 3.7.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: ETVs for TIC 356896561 determined from the SC (top) and FFI (bottom) light curves. Blue and red diamonds refer to the primary and secondary eclipse times, respectively, derived as explained in Section 3.2. The best-fit ETV solution is overplotted as a solid line. Fitting residuals are shown in lower panels.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Difference in standard deviations between the system parameter estimates obtained from the two data sets. The top, middle, and bottom panels show the difference in ﹩{a}_{{\rm{A}}}\sin {i}_{\mathrm{AB}}﹩, P AB, and M B, respectively.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: The TESS SC (top) and FFI (bottom) light curves of TIC 356896561 (presented here is Sector 57). Red symbols denote the observations while the solid line corresponds to the best-fit model of the SC light curve determined using the procedure described in Section 3.2.
Paper: Impacting Atmospheres: How Late-stage Pollution Alters Exoplanet Composition
Authors: Emilia Vlahos, Yayaati Chachan, Vincent Savignac, Eve J. Lee
Figure caption: Mass fraction of evaporated H2O relative to the total gas. The left panel shows accretion into the fiducial model of a 5M ⊕ core with a gas-to-core ratio (gcr) of ∼0.06. The center panel shows accretion into a planet with a gas-to-core ratio of ∼0.4 (core mass fixed at 5M ⊕) and the right panel shows accretion into a planet with a 10M ⊕ core (gas-to-core ratio fixed at 0.06). The vertical line marks the advective-radiative boundary. All profiles are calculated for f gas = 10−2 at an orbital distance of 3.5 au. The change in deposition mass fraction with respect to gas-to-core mass ratio or core mass is negligible compared to the variations caused by a different history of pollution.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Top panels: ETVs for TIC 219900027 (left) and TIC 424461577 (right) extracted using the method presented in this study. Blue and red diamonds refer to the primary and secondary eclipse times, respectively. No outliers have been removed. Middle panels: same as top panels but using the KvW method. Bottom panels: difference between the mideclipse times measured by the two methods.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Same as Figure 1 but for TIC 219900027 (presented here is Sector 19). The eclipse profile and the contribution of the O’Connell and proximity effects are shown as the dotted and dashed lines, respectively. To account for the eclipse depth difference between the SC and FFI light curves, we derived an independent light-curve solution for each of the two data sets.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Same as Figure 1 but for TIC 229771234 (presented here is Sector 52). To account for the eclipse depth difference between the SC and FFI light curves, we derived an independent light-curve solution for each of the two data sets.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Same as Figure 1 but for TIC 259006185 (presented here is Sector 55).
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: Photometric redshift distribution of MaDCoWS2 and external cluster catalogs normalized by their coverage areas. The solid, dashed, and dotted lines correspond to S/NP ≥ 5, 7, and 9, respectively, for MaDCoWS2. The distributions are smoothed by a Gaussian filter with a standard deviation of 0.0375. MaDCoWS2 provides significantly more cluster candidates at z > 1.5 compared to other catalogs.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: Confusion matrix of genuine cluster detection, spurious detection from large galaxies, and spurious detection from bright stars. The majority of the validation data lie on the diagonal elements of the matrix showing the capability of the CNN to identify spurious detections in our catalog.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: Sky distribution of MaDCoWS2 cluster candidates. The colors indicate the number of cluster candidates in each bin of the two-dimensional histogram. Spatial bins span 1° in both R.A. and decl. and are not adjusted for the decrease in area with increasing absolute decl.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: The tiling for this work. We run PZWav on each of the black rectangles independently, and merge the results using the tiling from the blue rectangles.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: Cumulative S/NP distribution for MaDCoWS2 cluster candidates as a function of redshift. More than 200 cluster candidates with S/N > 7 exist at z > 1.5
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption:  f RD as a function of cluster properties for the entire redshift ranges of the external catalogs. We omit the upper error bar when f RD = 1 for clarity. Blue and yellow dots/lines indicate S/NP ≤ 5 and S/NP ≤ 7 cutoffs for MaDCoWS2. The solid lines show the function in Equation (1) fitted to the data points. ﹩{M}_{500{\rm{c}}}^{\mathrm{ACT}}﹩, ﹩{M}_{500{\rm{c}}}^{\mathrm{SPT}}﹩, ﹩{M}_{500{\rm{c}}}^{\mathrm{PSZ}2}﹩, ﹩{M}_{500{\rm{c}}}^{\mathrm{eRASS}}﹩ are in units of M ⊙, respectively.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: LS DR9 grz (left-hand panels), K  s  (middle panels), and WISE W1 (right-hand panels) images of four clusters candidates at z > 1.5 for which we have follow-up imaging. The size of the images is 1 Mpc × 1 Mpc. The circles are objects with integrated PDF > 0.2. The K  s  images were obtained from Palomar. In each panel, we provide the name of the cluster candidate, S/NP, and its photometric redshift.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: Comparison between the photometric redshifts of galaxy cluster candidates in this work and redshifts from external catalogs. Photometric and spectroscopic redshifts are shown as orange points. The spectroscopic redshifts are also overlaid in hexagonal bins with colors indicating the number of clusters in each bin. The hexagonal bin size is 0.02. The red dashed line indicates a 1:1 relation in the top panel and zero residual in the bottom panel. The bottom panel shows the residual δ z/(1 + z) as a function of redshift. ﹩{\sigma }_{z/(1+{z}_{\mathrm{Spec}})}﹩ is the standard deviation of the residual considering only spectroscopic redshifts.
Paper: The Massive and Distant Clusters of WISE Survey 2: Second Data Release
Authors: Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor, Daniel Stern, Ryan Spivey, Karolina Garcia
Figure caption: The same as Figure 8, but here the different colors show different redshift ranges for the external catalogs. Purple indicates 0.4 < z ref < 0.6, while green indicates 1 < z ref < 1.2. This figure adopts an S/NP threshold of S/NP ≥ 5. ﹩{M}_{500{\rm{c}}}^{\mathrm{ACT}}﹩, ﹩{M}_{500{\rm{c}}}^{\mathrm{SPT}}﹩, ﹩{M}_{500{\rm{c}}}^{\mathrm{PSZ}2}﹩, ﹩{M}_{500{\rm{c}}}^{\mathrm{eRASS}}﹩ are in units of M ⊙, respectively.