adsabs/AstroCLIMB huggingface dataset:
Paper: Relative Intrinsic Scatter in Hierarchical Type Ia Supernova Sibling Analyses: Application to SNe 2021hpr, 1997bq, and 2008fv in NGC 3147
Authors: Sam M. Ward, Stephen Thorp, Kaisey S. Mandel, Suhail Dhawan, David O. Jones, Kirsty Taggart, Ryan J. Foley, Gautham Narayan, Kenneth C. Chambers, David A. Coulter, Kyle W. Davis, Thomas de Boer, Kaylee de Soto, Nicholas Earl, Alex Gagliano, Hua Gao, Jens Hjorth, Mark E. Huber, Luca Izzo, Danial Langeroodi, Eugene A. Magnier, Peter McGill, Armin Rest, César Rojas-Bravo, Radosław Wojtak
Figure caption: Hubble Space Telescope image of NGC 3147 (z Helio = 0.00938), with the SN Ia trio’s locations marked and the length scale in the bottom left. Overlaid is a 15.″8 × 15.″8 (3 kpc on a side) inset region of SN 2021hpr from 2021 December 30th (≈9 months after SN detection).
Paper: Relative Intrinsic Scatter in Hierarchical Type Ia Supernova Sibling Analyses: Application to SNe 2021hpr, 1997bq, and 2008fv in NGC 3147
Authors: Sam M. Ward, Stephen Thorp, Kaisey S. Mandel, Suhail Dhawan, David O. Jones, Kirsty Taggart, Ryan J. Foley, Gautham Narayan, Kenneth C. Chambers, David A. Coulter, Kyle W. Davis, Thomas de Boer, Kaylee de Soto, Nicholas Earl, Alex Gagliano, Hua Gao, Jens Hjorth, Mark E. Huber, Luca Izzo, Danial Langeroodi, Eugene A. Magnier, Peter McGill, Armin Rest, César Rojas-Bravo, Radosław Wojtak
Figure caption:  BAYESN fit to the SN 2021hpr grizy photometry (Table 1), along with kernel density estimates of the posterior distributions.
Paper: Early Results from GLASS-JWST. XXIII. The Transmission of Lyα from UV-faint z ∼ 3–6 Galaxies
Authors: Gonzalo Prieto-Lyon, Charlotte Mason, Sara Mascia, Emiliano Merlin, Namrata Roy, Alaina Henry, Guido Roberts-Borsani, Takahiro Morishita, Xin Wang, Kit Boyett, Patricia Bolan, Marusa Bradac, Marco Castellano, Amata Mercurio, Themiya Nanayakkara, Diego Paris, Laura Pentericci, Claudia Scarlata, Michele Trenti, Tommaso Treu, Eros Vanzella
Figure caption: Lyα velocity offset vs. UV magnitude and implied halo mass, using the mapping derived in the UV luminosity function model of Mason et al. (2015), color coded by redshift. Our new sample is shown as colored stars. For comparison, we show values from the literature at z ∼ 2–3 (Erb et al. 2014; Steidel et al. 2014; gray squares), at 4 < z < 7.5 (Bradač et al. 2017; Stark et al. 2015; Willott et al. 2015; Inoue et al. 2016; Pentericci et al. 2016; Stark et al. 2017; Mainali et al. 2018; Cassata et al. 2020; Endsley et al. 2022; colored squares), at z > 7.5 (Tang et al. 2023; blue circles), and GN-z11 (Bunker et al. 2023; black diamond). We also show the model of Mason et al. (2018a) which was derived from z ∼ 2 literature samples. The new GLASS-ERS sample extends this measurement to galaxies ∼2 mag fainter than previously possible. Δv Lyα  error bars are dominated by the uncertainty of the centroid in the MUSE Lyα emission observations.
Paper: Early Results from GLASS-JWST. XXIII. The Transmission of Lyα from UV-faint z ∼ 3–6 Galaxies
Authors: Gonzalo Prieto-Lyon, Charlotte Mason, Sara Mascia, Emiliano Merlin, Namrata Roy, Alaina Henry, Guido Roberts-Borsani, Takahiro Morishita, Xin Wang, Kit Boyett, Patricia Bolan, Marusa Bradac, Marco Castellano, Amata Mercurio, Themiya Nanayakkara, Diego Paris, Laura Pentericci, Claudia Scarlata, Michele Trenti, Tommaso Treu, Eros Vanzella
Figure caption: Fraction of Lyα flux transmitted through the IGM as a function of the radius of the ionized bubble and emitted Δv Lyα , color coded by transmission through the IGM. We show the contour of 30% transmission as a white curve. The IGM transmission values are calculated assuming a Lyα-emitting galaxy is in the center of a single ionized bubble in a neutral IGM, as described in Section 5.2. This figure shows that Lyα emission lines with Δv Lyα  ≲ 200 km s−1 must reside at least ≳1 pMpc from the neutral IGM in order to transmit a significant fraction of their flux through the IGM.
Paper: Early Results from GLASS-JWST. XXIII. The Transmission of Lyα from UV-faint z ∼ 3–6 Galaxies
Authors: Gonzalo Prieto-Lyon, Charlotte Mason, Sara Mascia, Emiliano Merlin, Namrata Roy, Alaina Henry, Guido Roberts-Borsani, Takahiro Morishita, Xin Wang, Kit Boyett, Patricia Bolan, Marusa Bradac, Marco Castellano, Amata Mercurio, Themiya Nanayakkara, Diego Paris, Laura Pentericci, Claudia Scarlata, Michele Trenti, Tommaso Treu, Eros Vanzella
Figure caption: Δv Lyα  vs. velocity dispersion of the optical lines. We present our data as stars color coded by redshift. In gray squares are z ∼ 2–3 sources from Erb et al. (2014). We show upper limits for measurements below ﹩{\sigma }_{\mathrm{res}}=47﹩ km s−1. Uncertainties are dominated by the MUSE Lyα centroid measurements. Both samples suggest a correlation between the optical line velocity dispersions and Δv Lyα .
Paper: Early Results from GLASS-JWST. XXIII. The Transmission of Lyα from UV-faint z ∼ 3–6 Galaxies
Authors: Gonzalo Prieto-Lyon, Charlotte Mason, Sara Mascia, Emiliano Merlin, Namrata Roy, Alaina Henry, Guido Roberts-Borsani, Takahiro Morishita, Xin Wang, Kit Boyett, Patricia Bolan, Marusa Bradac, Marco Castellano, Amata Mercurio, Themiya Nanayakkara, Diego Paris, Laura Pentericci, Claudia Scarlata, Michele Trenti, Tommaso Treu, Eros Vanzella
Figure caption: Δv Lyα  against rest-frame EW of Lyα. Our data are shown as stars color coded by redshift. We present values from the literature at z ∼ 2–3 (Erb et al. 2014; Steidel et al. 2014; gray squares), at 3 < z < 7.5 (Bradač et al. 2017; Stark et al. 2015; Willott et al. 2015; Inoue et al. 2016; Pentericci et al. 2016; Stark et al. 2017; Mainali et al. 2018; Cassata et al. 2020; Tang et al. 2021; Endsley et al. 2022; colored squares), z > 7.5 (Stark et al. 2017; Tang et al. 2023; blue circles), and GN-z11 (Bunker et al. 2023; black diamond). Both the literature data and our sample show low Δv Lyα  at higher EW.
Paper: A Fundamental Mechanism of Solar Eruption Initiation in a Multipolar Magnetic Field
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Temporal evolution of the thickness of the current layer that formed in the core field in simulations with friction. Panels (A) and (B) represent simulations M0 and M1, respectively. The details are similar to those in Figure 4(c).
Paper: A Fundamental Mechanism of Solar Eruption Initiation in a Multipolar Magnetic Field
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Evolution of the specific magnetic field line and its height with time in simulations with friction. Panels (A) and (B) represent simulations M0 and M1, respectively. The details are similar to those in Figure 5.
Paper: Early Results from GLASS-JWST. XXIII. The Transmission of Lyα from UV-faint z ∼ 3–6 Galaxies
Authors: Gonzalo Prieto-Lyon, Charlotte Mason, Sara Mascia, Emiliano Merlin, Namrata Roy, Alaina Henry, Guido Roberts-Borsani, Takahiro Morishita, Xin Wang, Kit Boyett, Patricia Bolan, Marusa Bradac, Marco Castellano, Amata Mercurio, Themiya Nanayakkara, Diego Paris, Laura Pentericci, Claudia Scarlata, Michele Trenti, Tommaso Treu, Eros Vanzella
Figure caption: Example spectra from this sample, with the velocity axis centered at the systemic redshift given by Hα. We show galaxies 70003 and 80070, which have low and high Δv Lyα , respectively. Spectra are from JWST/NIRSpec Hα (purple) and VLT/MUSE Lyα (yellow). Vertical lines mark the Hα (solid) and Lyα (dashed) peaks.
Paper: The Evaporating Massive Embedded Stellar Cluster IRS 13 Close to Sgr A*. I. Detection of a Rich Population of Dusty Objects in the IRS 13 Cluster
Authors: Florian Peißker, Michal Zajaček, Lauritz Thomkins, Andreas Eckart, Lucas Labadie, Vladimír Karas, Nadeen B. Sabha, Lukas Steiniger, Maria Melamed
Figure caption: Finding chart for the dusty sources associated with a zoomed view toward the IRS 13 cluster. While the Greek-named sources are previously analyzed in the literature, we find additional sources that we enumerate to avoid confusion. The sources E1–E7 belong to IRS 13E and are marked for clarity. The bow-shock source X3 is analyzed in Peißker et al. (2023b). In addition, IRS 13W is associated with an M3 giant star (Maillard et al. 2004). The data shown were observed with NACO in 2004. Whereas the left image displays a continuum overview of the direct vicinity of Sgr A* (about 0.45 × 0.50 pc), the right represents a zoomed-in high-pass-filtered view toward IRS 13. Please consult Appendix D and Appendix E for the H- and K-band counterparts of the sources marked. In addition, Appendix F displays all newly identified dusty sources in the H, K, and L band, including their related light curve. Every source not marked in this finding chart is not considered to be a cluster member because of its proper motion or previous studies (Pfuhl et al. 2014; Gautam et al. 2019).
Paper: The Evaporating Massive Embedded Stellar Cluster IRS 13 Close to Sgr A*. I. Detection of a Rich Population of Dusty Objects in the IRS 13 Cluster
Authors: Florian Peißker, Michal Zajaček, Lauritz Thomkins, Andreas Eckart, Lucas Labadie, Vladimír Karas, Nadeen B. Sabha, Lukas Steiniger, Maria Melamed
Figure caption: Anisotropy parameter ﹩{\gamma }_{{TR}}﹩ for the investigated sources in IRS 13. In the upper row, we illustrate ﹩{\gamma }_{{TR}}﹩ for the E stars (left) and the dusty sources (right). Dividing the anisotropy parameter into four bins reveals an overdensity for some of the sources close to ﹩{\gamma }_{{TR}}\approx \pm 1﹩ implying the existence of substructures. In the lower-left plot, we show all investigated sources of the IRS 13 cluster. The uncertainties of the anisotropy parameters are determined with error propagation of the related standard deviation of the proper motion values (Appendix 3.2). The gray numbers and dashed vertical lines represent the related bin. The lower-right plot shows the normalized number of sources for each bin as a function of ﹩{\gamma }_{{TR}}﹩. The magenta-colored line represents the normalized theoretical probability distribution that one would expect for a uniform cluster. The comparison of the observed structure of IRS 13 with a uniform cluster suggests anomalies that are responsible for a nonuniform distribution.
Paper: The Evaporating Massive Embedded Stellar Cluster IRS 13 Close to Sgr A*. I. Detection of a Rich Population of Dusty Objects in the IRS 13 Cluster
Authors: Florian Peißker, Michal Zajaček, Lauritz Thomkins, Andreas Eckart, Lucas Labadie, Vladimír Karas, Nadeen B. Sabha, Lukas Steiniger, Maria Melamed
Figure caption: Monte Carlo simulations of ﹩{\gamma }_{{TR}}﹩ for 10,000 stars. As we have shown in Figure 6, the anisotropy parameter peaks at ±1, which indicates a nonuniform cluster. In comparison, we show a Gaussian distribution.
Paper: The Evaporating Massive Embedded Stellar Cluster IRS 13 Close to Sgr A*. I. Detection of a Rich Population of Dusty Objects in the IRS 13 Cluster
Authors: Florian Peißker, Michal Zajaček, Lauritz Thomkins, Andreas Eckart, Lucas Labadie, Vladimír Karas, Nadeen B. Sabha, Lukas Steiniger, Maria Melamed
Figure caption: Gaussian distribution of the DS around the geometrical center of IRS 13. The blue-colored histogram shows the number of sources inside the bin of the size of 0.″09. The brown dashed line represents a Gaussian fit of the blue-colored projected surface density. Because the geometrical center of the cluster is in an empty region, the Gaussian probability density drops toward the origin of the stellar distribution.
Paper: The Evaporating Massive Embedded Stellar Cluster IRS 13 Close to Sgr A*. I. Detection of a Rich Population of Dusty Objects in the IRS 13 Cluster
Authors: Florian Peißker, Michal Zajaček, Lauritz Thomkins, Andreas Eckart, Lucas Labadie, Vladimír Karas, Nadeen B. Sabha, Lukas Steiniger, Maria Melamed
Figure caption: Proper motion of all observed IRS 13 sources (see Figure 3). The E stars (E1–E5) are orange-colored; the brown data points represent the bright dusty sources (α-η). We find a slight over- and underdensity regarding the shown data points in the corresponding quadrant. Please see the text for details.
Paper: The Evaporating Massive Embedded Stellar Cluster IRS 13 Close to Sgr A*. I. Detection of a Rich Population of Dusty Objects in the IRS 13 Cluster
Authors: Florian Peißker, Michal Zajaček, Lauritz Thomkins, Andreas Eckart, Lucas Labadie, Vladimír Karas, Nadeen B. Sabha, Lukas Steiniger, Maria Melamed
Figure caption: Multiwavelength view toward IRS 13 observed with NACO. To minimize the influence of dominating PSF wings, we apply an image sharpener to the H and K band observed at 1.6 μm and 2.1 μm, respectively. The prominent dust features are revealed in the MIR (here: 4.5μm) and are not treated with any filter. Every image was normalized to its peak emission flux. The contrast was adjusted to visualize the presence of the dusty sources in the related band. However, the lower cutoff resulted in regions around bright stars with apparent missing flux. We note that sources such as E3 close to E4 (see Figure 3) have an H-band emission but are suppressed because of the contrast settings.
Paper: The Evaporating Massive Embedded Stellar Cluster IRS 13 Close to Sgr A*. I. Detection of a Rich Population of Dusty Objects in the IRS 13 Cluster
Authors: Florian Peißker, Michal Zajaček, Lauritz Thomkins, Andreas Eckart, Lucas Labadie, Vladimír Karas, Nadeen B. Sabha, Lukas Steiniger, Maria Melamed
Figure caption: Comparison of raw data with processed data treated with a high-pass filter. The plot on the left shows the distance of several thousand stars with respect to Sgr A*. This plot underlines the robustness of the used high-pass filter regarding an astrometric analysis because every individual star shows the same distance to Sgr A* independent of the used approach (filter/no filter). On the right side, we show the K-band flux distribution of about 10,000 stars and estimate a difference between filtered and nonfiltered data of about 20%. Please see the text for details.
Paper: The Evaporating Massive Embedded Stellar Cluster IRS 13 Close to Sgr A*. I. Detection of a Rich Population of Dusty Objects in the IRS 13 Cluster
Authors: Florian Peißker, Michal Zajaček, Lauritz Thomkins, Andreas Eckart, Lucas Labadie, Vladimír Karas, Nadeen B. Sabha, Lukas Steiniger, Maria Melamed
Figure caption: Sketch of a class I YSO. As indicated, various components are detectable only at specific wavelengths/bands. Using this model of a class I YSO, we expect higher luminous mid-infrared (L/M band) emission compared with the near-infrared (H/K band). This sketch is inspired by a similar figure shown in Sicilia-Aguilar et al. (2016).
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: The median cumulative halo mass function of our eight fiducial mocks (red line) compared with the theoretical cumulative halo mass function from Tinker et al. (2008). The gray shading represents the range of values based on mock-to-mock variations reflecting cosmic variance.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Distributions of real and mock FoF group members’ projected relative radii (R proj,gal, left) and projected relative velocities (Δv proj,gal, right) from their average group centers as a function of group halo mass. Solid lines denote the median values, and shading encloses the 16th to 84th percentiles of each distribution. Orange represents real FoF groups from ECO (see Section 2.4), and blue represents groups extracted from the mocks using the same FoF algorithm. The mock data are drawn by combining the eight fiducial mocks into a single data set to minimize fluctuations due to cosmic variance. The agreement between real and mock FoF groups suggests that mock galaxies are populated realistically into halos.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: The group-integrated H I–halo mass relation in RESOLVE (blue) compared to ECO–RES-A (orange), both using G3 groups and HAM masses, illustrating the shape of the relation and its similarity between the RESOLVE and ECO–RES-A data sets, despite ECO’s higher reliance on photometric gas fraction H I mass estimates. Left: group-integrated H I mass as a function of group halo mass for ECO–RES-A and RESOLVE. Error bars on the medians come from bootstrapping and the blue shading represents cosmic variance errors for RESOLVE. Right: group-integrated H I mass fractions as a function of group halo mass for RESOLVE and ECO–RES-A. The red and green lines are drawn for reference and represent the median group-integrated stellar and baryonic mass fractions in ECO–RES-A. The widths of the red and green lines represent statistical error from bootstrapping.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: The group-integrated H I–halo mass relation from this study compared with several observational and theoretical results. The G3 median relation for ECO+RES-B is illustrated by the black data points. The observational mean relation and error of Guo et al. (2020) is shown in green shading, and inferred forms of the relation from Obuljen et al. (2019) and Li et al. (2022) are shown in solid red and dashed yellow, respectively. Theoretical predictions from Baugh et al. (2019), Chauhan et al. (2020), and Calette et al. (2021) are shown in dashed brown, dashed blue, and dotted purple, respectively.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Violin plots illustrating distributions of group purity (P  g , blue) and group completeness (C  g , orange) for G3 groups in all 32 mocks, with additional black markers to illustrate mean P  h  and C  h  values. Violin widths are as in Figure 6. The four panels organize the mocks by fiducial, central-offset, b  v  = 0.8, and b  v  = 1.2 types, and the markers show the median and mean quantities. The mocks are labeled 1–8 in order of increasing galaxy number density, corresponding to 0.138, 0.158, 0.159, 0.183, 0.185, 0.223, 0.224, and 0.369 Mpc−3. To improve clarity by ensuring that neighboring violins do not overlap, the horizontal positions of the violins are placed nonlinearly in number density.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Conditional distributions of group median errors between “observed” HAM halo masses (group finding + HAM applied to mocks) and true halos masses (supplied with mocks), as a function of HAM mass. The upper four panels show the distributions for the G3 group finder applied to the fiducial, central-offset, and velocity bias mocks. To contrast with G3, the lower panel shows the distribution resulting from FoF group finding with false-pair splitting (E17). In each panel, the orange circles mark the median values at fixed M HAM and dashed orange lines are drawn to enclose 68%, 90%, and 95% of the error distribution at fixed mass. For reference, the green shading in each panel shows the distribution from the G3 algorithm applied to fiducial mocks. These distributions show that the G3 algorithm consistently recovers HAM halo masses independent of halo velocity bias or central galaxy location bias.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Scatter in the group-integrated H I–halo mass relation. Both panels use G3 groups and HAM masses. Left: scatter plot of absolute-valued residuals between individual M H I,grp values and best-fitting median relations (Equation (9)) as in Table 2. RESOLVE is shown in blue and ECO–RES-A in red. Black lines denote the median, 68th percentile, and 9th percentile of the ECO–RES-A residuals as a function of halo mass. Right: scatter plot of M H I,grp vs. M halo for RESOLVE and ECO–RES-A, with the best-fitting model for ECO–RES-A overplotted. Dashed lines mark ±0.5 dex and ±1 dex offsets from the median ECO–RES-A relation, open circles show median M H I,grp values for ECO–RES-A, and black stars show mean M H I,grp values for ECO–RES-A.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Violin plots illustrating distributions of purity and completeness as a function of halo mass for the G3 group finder (blue) and FoF (orange) for comparison. Both purity and completeness mappings are pictured (see Section 4.1). Violin widths are as in Figure 6. FoF (as implemented by our team with false-pair splitting) attains somewhat higher purity than the G3 algorithm, but G3 attains higher completeness, with dramatic improvement at high masses.
Paper: The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H I–Halo Mass Relation
Authors: Zackary L. Hutchens, Sheila J. Kannappan, Andreas A. Berlind, Mehnaaz Asad, Kathleen D. Eckert, David V. Stark, Derrick S. Carr, Ella R. Castelloe, Andrew J. Baker, Kelley M. Hess, Amanda J. Moffett, Mark A. Norris, Darren Croton
Figure caption: Inconsistency of extinction corrections performed with and without GALEX NUV data. Top left: GALEX NUV coverage of ECO, with “deep” defined as >1000 s exposure time. We note that RESOLVE (decl. 0°–5°) has full deep GALEX NUV coverage. Top right: model u − r color vs. stellar mass for RESOLVE and ECO galaxies (all M  r  < − 17.33). There is no model u − r offset between ECO and RESOLVE. Bottom left: model u − r color corrected for internal extinction vs. stellar mass for RESOLVE (in which all galaxies have deep GALEX NUV) and for ECO (just galaxies without deep GALEX NUV). RESOLVE and ECO show a visible offset. Bottom right: model u − r color corrected for internal extinction vs. stellar mass for RESOLVE and for ECO (just galaxies with deep GALEX NUV). The offset seen in the lower left panel disappears.