adsabs/AstroCLIMB huggingface dataset:
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: The difference between MWM [M/H] and literature [Fe/H] as a function of ASPCAP raw Teff and log g from APOGEE DR17 (top panels), GALAH DR4 (second row from the top), Gaia-ESO DR5 (second row from the bottom) for stars with S/N > 50 from both surveys, and no BAD flags from MWM. The bottom panels show the comparison with the GBS sample. The solid black line shows the running median value.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Kiel diagram showing raw Teff and log g values. Dartmouth isochrones with ages of 12 Gyr, and [M/H] = −1.5 to 0.5 dex are overplotted. The light-gray line shows a 1 Gyr old solar-metallicity isochrone. Note that the log g discrepancy between the isochrones and ASPCAP increases below 4500 K in the main sequence.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Differences of DR19 ASPCAP spectroscopic raw Teff and APOGEE DR17 (Abdurro’uf et al. 2022), GALAH DR4 (S. Buder et al. 2025), Gaia-ESO DR5 (S. Randich et al. 2022), and GBS (C. Soubiran et al. 2024) temperatures as a function of ASPCAP raw Teff color coded by raw metallicity. The solid black line shows the running median value.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Differences of DR19 ASPCAP raw surface gravities and APOGEE DR17 (Abdurro’uf et al. 2022), GALAH DR4 (S. Buder et al. 2025), Gaia-ESO DR5 (S. Randich et al. 2022), and GBS (C. Soubiran et al. 2024) values as a function of ASPCAP raw Teff color coded by raw metallicity. The solid black line shows the running median value.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Differences of DR19 ASPCAP spectroscopic and astroseismic log g as a function of ASPCAP metallicity and raw surface gravity. The top panel shows the RGB, the middle panel shows the RC stars from the APOKASC3 sample, and the bottom panel shows all TESS stars.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Top panel: the 2D histogram of the difference between [M/H] and [Fe/H] as a function of raw Teff. Bottom panel: the difference between [M/H] and [Fe/H] as a function of raw log g color coded by [M/H]. Only stars with S/N > 50 and no bad flags are shown.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Scatter of metallicity in 12 open and 16 globular clusters. A slight anticorrelation with average [M/H] can be seen as lines in the H band get weaker with decreasing metallicity.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Corrected abundances published in DR19 as a function of [M/H] of stars with S/N > 50, no BAD flags, and e_x_h < 0.2. Features seen in the calibrated abundances are discussed in the individual abundance sections. Stripes seen in the low-density regions of some abundances (Na, P, K, V, Cr, Co, Cu, Ce, and Nd) indicate noding problems at low abundance values. All abundances are plotted, except those that are within 0.03 dex of the grid edge. Abundances of Cglobal and Nglobal are from the global fit.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Comparison between MWM DR19 and APOGEE DR17 abundances as a function of Teff color coded by MWM [M/H]. S/N was restricted to be larger than 50 in both surveys. Abundances of Cglobal and Nglobal are from the global fit. The solid black line shows the running median value.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: The median DR19 uncertainties (blue dots) for each element compared to scatter measured in the solar neighborhood sample (red dots), in 12 open clusters (yellow dots), and 348 wide binaries (black dots). The range of Teff is between 4000 and 6000 K, S/N > 50.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Comparison between MWM DR19 and GALAH DR4 abundances as a function of Teff color coded by MWM [M/H]. S/N was restricted to be larger than 50 in both surveys. Abundances of Cglobal and Nglobal are from the global fit. The solid black line shows the running median value.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Raw abundances of giants (log g < 3.8) as a function of Teff with S/N > 50 and no BAD flags. The orange coloring indicates the parameter region from Table 6 where the abundances might not be reliable. The yellow region identifies the cool and carbon-rich stars with Teff < 4250 K and [C/M] > 0.1.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Same as in Figure 12 but for dwarfs.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: [X/M] abundances as a function of Teff using 358 giant stars in 12 open clusters from the OCCAM survey. The solid line shows the derived calibration equation. Stars with S/N > 50, log g < 3.8, Teff < 6000 K, and no BAD flags were kept in the sample.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: [C/M] as a function of Teff below 5000 K for the entire sample with S/N > 50 and no BAD flags. The group of stars with Teff < 4250 K and [C/M] > 0.1 are shown with yellow dots.
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: Required number of simulations to constrain the true-positive rates (top panels) and false-positive rates (bottom panels). Subsamples of size ﹩{N}_{\mathrm{sim}}﹩ are drawn from a sample of 100,000 simulations, and true- and false-positive rates are calculated for each subsample. One can observe high variability for subsamples with low ﹩{N}_{\mathrm{sim}}﹩, but as ﹩{N}_{\mathrm{sim}}﹩ increases the calculated quantities converge to a given value. These simulations were from a scenario with ΔA = 0.4 and NEEC = 25. Left and right columns represent different threshold values for the Bayes factor required for detection of a trend.
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: Sensitivity of the results of our analysis to the choice of kernel for the kernel density estimate. Simulations are the same as those in Figure 4, but change the bandwidth parameter (bw) of the Gaussian kernel used.
Paper: The MiMO Catalog: Physical Parameters and Stellar Mass Functions of 1232 Open Clusters from Gaia DR3
Authors: Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Zhaozhou Li, 昭洲 李, Xiaoting Fu, 晓婷 符
Figure caption: Comparison of age, distance modulus, and AV (rows) measured by MiMO (x-axis) vs. D. Bossini et al. (2019), T. Cantat-Gaudin et al. (2020), W. S. Dias et al. (2021), E. L. Hunt & S. Reffert (2023) and L. Cavallo et al. (2024; columns). Each point represents a star cluster. Error bars indicate the reported fitting uncertainties for each method (except for T. Cantat-Gaudin et al. 2020, which does not provide error bars). The rms difference between the best fits, ΔRMS, and the mean fitting uncertainties of each catalog, ϵMiMO and ϵother, are indicated in the upper-right corner of each panel.
Paper: The MiMO Catalog: Physical Parameters and Stellar Mass Functions of 1232 Open Clusters from Gaia DR3
Authors: Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Zhaozhou Li, 昭洲 李, Xiaoting Fu, 晓婷 符
Figure caption: Comparison of cluster parameter estimates using different metallicity priors. Results with the Spectroscopic Prior (a) are shown on the horizontal axes. The orange points represent the Global Prior (b), and the blue points represent the Uniform Prior (c), both shown on the vertical axes.
Paper: The MiMO Catalog: Physical Parameters and Stellar Mass Functions of 1232 Open Clusters from Gaia DR3
Authors: Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Zhaozhou Li, 昭洲 李, Xiaoting Fu, 晓婷 符
Figure caption: CMDs for six example clusters that show significant differences in age estimates between MiMO and D21. Small dots represent the MiMO input sample, with likely field stars (pmemb < 1 − ffs) shown in gray, while crosses indicate the sample used by D21.
Paper: The MiMO Catalog: Physical Parameters and Stellar Mass Functions of 1232 Open Clusters from Gaia DR3
Authors: Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Zhaozhou Li, 昭洲 李, Xiaoting Fu, 晓婷 符
Figure caption: Distribution of the separation index, Esep, for the full catalog and MF-prime samples, respectively. Esep indicates the level of separation between the distributions of cluster and field populations in the CMD.
Paper: JWST-TST DREAMS: Sulfur Dioxide in the Atmosphere of the Neptune-mass Planet HAT-P-26 b from NIRSpec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Natasha E. Batalha, Nicholas Wogan, Lili Alderson, Dominic Doud, Néstor Espinoza, Ryan J. MacDonald, Hannah R. Wakeford, Jeff A. Valenti, Nikole K. Lewis, Sara Seager, Kevin B. Stevenson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Ana Glidden, Jingcheng Huang, Zifan Lin, Dana R. Louie, Cathal Maguire, Elijah Mullens, Kristin Sotzen, Daniel Valentine, Mark Clampin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Comparison of the temperature–pressure structure of HAT-P-26 b from the free retrieval analysis using an isothermal (magenta) and N. Madhusudhan & S. Seager (2009; orange) parameterization, alongside the self-consistent computation from the PICASO grid (black dotted line).
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: Top left: a color–magnitude diagram of the 1000 closest stars to the center of Pal 5, after excluding those with bad photometry (Source Extractor parameter FLAGS > 3; see Section 2.1). A cubic spline interpolation along the CMD of the cluster is shown as a dashed black line, and sources with photometry consistent with being within 0.05 mag of this fitted function are in blue. The rough depth of usable Gaia DR3 proper motions (g ∼ 20.5) is indicated with a dashed gray line. The MIST isochrone with the closest age and metallicity to the values in the W. E. Harris (1996) catalog is shown as a light red line. Top middle: a density map of all sources within a 4° box around Pal 5, scaled by the standard deviation of the source density. Contours correspond to 2σ, 3σ, 5σ, 7σ, 10σ, 50σ, and 100σ overdensities. The central King limiting radius rt of the GC is masked and circled in red, and the orange circle corresponds to the Jacobi radius calculated in this work (Section 2.3). The red arrow indicates the direction of the systemic proper motion of Pal 5. Top right: a map of the effective exposure time (teff × Texp) in DELVE DR2 for the g-band photometry over the same region as the middle panels. Middle left: a background model for the top middle panel, derived by fitting a second-order two-dimensional polynomial between >4 rt and the entire 4° × 4° field of view. Middle: background-subtracted source density plot. Middle right: a map of the effective exposure time (teff × Texp) in DELVE DR2 for the r-band photometry over the same region as the middle panels. Bottom left: angular-averaged source density plot of the top middle panel, with the limiting radius derived from W. E. Harris (1996) marked in red, and the Jacobi radius calculated in Section 2.3 in yellow. The error bars on the data points are the standard error in the spatial bins averaged (1﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩8) over the annulus, in steps of 3﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩6. The dashed line corresponds to the background value plus the standard error. Bottom right: same as bottom left, but for the background-subtracted density plot.
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: A comparison of the observed Pal 5 stream in DELVE DR2 (top panels) with a simulation of the stream down to the DELVE DR2 depth (middle panels) and the LSST 10 yr depth (bottom panels). The left panels show the observed CMD (top), the simulated CMD from SPISEA (M. W. Hosek et al. 2020) with a DELVE DR2 magnitude error function (middle), and an error function for the LSST 10 yr depth (bottom). Stars selected along the isochrone for Pal 5 are shown in blue; note that stars along the red giant branch are excluded in the selection due to misalignment in the simulated and observed CMDs in that regime. The middle simulated column shows the isochrone selection applied to the simulation of Pal 5 with no Milky Way foreground, and the right simulated panels show the isochrone selection in the presence of a Milky Way foreground model populated by a fraction of stars in LSSTsim DR2 (P. Dal Tio et al. 2022) to force a rough visual match with observations at DELVE DR2 depth (g = 23.25, see Section 5). As expected, the stream becomes significantly more prominent at the forecasted full depth of LSST.
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: Same as Figure 2, but for NGC 5897. A clear photometric overdensity is seen extending from the GC beyond rJ (yellow circle). A dashed blue circle is overplotted at r =  28’ to guide the eye, roughly at the radius out to which the photometric excess exists. Note that the excess does not preferentially align with the proper motion of NGC 5897 (red arrow); this is expected given the recent pericenter passage of NGC 5897 (see Section 3.1 for more details).
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: The density of sky coverage, plotted in equatorial coordinates (R.A. and decl.), with the DECam camera and the location of 170 globular clusters (GCs) from E. Vasiliev & H. Baumgardt (2021) and the overlap with the DELVE footprint. The Dark Energy Survey (DES) covers the irregular polygon of higher star density in the lower center of the figure. The rest of the coverage is from the DELVE survey. GCs are denoted with a red cross, and those that had enough high-quality data that we could search for extratidal envelopes have a blue square around the cross. NGC 5897 (the GC with a newly detected envelope) and NGC 7492 (which has conflicting reports in the literature and for which we detect an envelope), are shown as cyan stars with coordinates ﹩(\alpha =229\mathop{.}\limits^{^\circ }35,\delta =-21\mathop{.}\limits^{^\circ }01)﹩ and ﹩(\alpha =347\mathop{.}\limits^{^\circ }11,\delta =-15\mathop{.}\limits^{^\circ }61)﹩, respectively.