adsabs/AstroCLIMB huggingface dataset:
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: The near-IR transmission spectrum of HD 219666 b observed over two visits with HST/WFC3 G141. The spectra derived from each individual visit are shown as the gray diamond and square points, with a uniform 205 ppm offset applied to all points from the second visit. The error-weighted average of our two visits is shown as the black points, and the median retrieved model spectrum is shown as the green line with its 1 and 2σ uncertainties represented by the green shaded regions.
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: Allan variance plots, showing the rms of residuals as a function of temporal bin size (N), for each of our fits to the two HST observations presented in this work. The black lines were calculated for our fits to each visit’s broadband light curve, and the gray lines for each visit’s spectroscopic light curves. The first visit’s residuals are consistent with pure white noise whose rms falls off as ﹩1/\sqrt{N}﹩. The second visit’s rms values fall off shallower than the white-noise expectation, suggesting excess red noise is present in the data.
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: Atmospheric volume mixing ratios of water as inferred from retrievals on HST/WFC3 data (black circles) vs. JWST data (blue triangles) in the literature for planets in the  <5 R⊕ regime. Note that in this speculation we do not carefully consider exactly which retrieval method or JWST instrument is used. In each case (except our target HD 219666 b, which has not been followed up by JWST), the HST-only analysis underestimated the abundance of water relative to the JWST analysis. Values are taken from T. Mikal-Evans et al. (2023) and B. Benneke et al. (2024) for TOI-270 d, B. Benneke et al. (2019b) and N. F. Wogan et al. (2024) for K2-18 b, and B. Benneke et al. (2019a) and T. G. Beatty et al. (2024) for GJ 3470 b.
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: Detrended observed data, best-fit models, and data-model residuals from our simultaneous fit of the broadband transit and RV data. The HST/WFC3 broadband light curves from each visit are shown in the top row, and the 12 TESS light curves, after phase-folding them all together, are shown in the middle-left panel. The HARPS RV data from M. Esposito et al. (2019) are shown in the middle-right panel. Also shown in the bottom row are the observed fluxes of the star HD 219666, converted from the magnitudes listed in Table 1, along with our best-fitting stellar SED model. From these simultaneous fits, we precisely constrained the properties of HD 219666 b’s orbit.
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: Corner plot from our joint transit and RV fit described in Section 3.4.
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: Corner plot from our fit to the spectroscopic HST/WFC3 G141 light curve at ∼1.40 μm from Visit 2.
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: Corner plot from our fit to the spectroscopic HST/WFC3 G141 light curve at ~1.40 μm from Visit 1.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Left: 5σ contrast limits of the F410M data overlaid with Keck/NIRC2 contrast limits (﹩{L}^{{\prime} }﹩ band, N. L. Wallack et al. 2024; Ms band, this study; see Appendix E). The inset is a zoomed-in version of the contrast limits at separations from the central star around 1″. The star symbol indicates the contrast and separation of the source candidate from the F410M data. The vertical dashed black lines indicate the separations of the ALMA velocity kinks. The light-green, gray, sky-blue, and pink shaded areas correspond to the projected separation ranges of the ALMA dust gaps (D10, D45, D86, and D145, respectively; J. Huang et al. 2018; A. Isella et al. 2018). Right: the contrast limits obtained from the F200W data overlaid with a rough SPHERE 5σ contrast limit we inspected visually from D. Mesa et al. (2019), where we applied the disk inclination to the separations for consistency with our contrast limits.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: NIRCam F410M (left) and F200W (right) maps as in the bottom panels of Figure 1, with symbols representing the predicted locations of putative protoplanets from the velocity kinks observed with ALMA (indicated by magenta circles with the kink IDs; C. Pinte et al. 2020), a point-like source candidate (white and blue circles in the left and right panels, respectively), and ring features (R0–R3).
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: PSF fitting results of the source candidate with KL = 1 (top panels), and the derived contrast and SNR values for different KL modes (bottom panels). The colors in the plot indicate the box size used for the PSF fitting, demonstrating that the extracted photometry and SNR do not largely depend on the size parameter. We finally adopted the 17-pixel box corresponding to ∼1″ × 1″ (see text). The error bars of the 17-pixel plot in the right panel correspond to the standard deviations of the SNR measurements among the range of 13–21 pixels. The gray shaded parameter space (KL ≥ 5) indicates aggressive PSF subtraction and a heavy self-subtraction effect on astronomical sources at ﹩\sim 0\mathop{.}\limits^{^{\prime\prime} }75﹩, where the source candidate is located. See also Appendix B for the PSF fitting results at different KL modes.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Comparison between the F410M map (contours) and the DSHARP ALMA continuum map (colors) at λ = 1.3 mm (6″ × 6″ map on the left and 2″ × 2″ map on the right; A. Isella et al. 2018). The location of the source candidate is indicated by a black arrow. The magenta circles show the location of the ALMA velocity kinks.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Top: post-processed JWST/NIRCam maps in the F410M (left) and F200W (right) filters, obtained with KL = 3. Bottom: zoomed-in images of the post-processed results.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Radial profiles of the surface brightness at different position angles in the F200W image. The bump feature between ∼2″ and 3″ at each position angle indicates the location of R3. The outer regions beyond R3 contain signal from background stars, as well as negative self-subtraction features, making the radial profiles noisier than in the region inside of R3.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Top left: F555W vs. F555W–F625W color–magnitude diagram (CMD) for stars inside the PDR and outside the CO cores (blue) and stars inside the PDR and projected inside the CO cores (orange). Top right: F555W vs. F555W–F625W CMD for stars outside the PDR and outside the CO cores (pink) and stars outside the PDR and projected inside the CO cores (green). Bottom left: F275W vs. F275W–F6336W CMD for stars inside the PDR and outside the CO cores (blue) and stars inside the PDR and projected inside the CO cores (orange). Bottom right: F275W vs. F275W–F336W CMD for stars outside the PDR and outside the CO cores (pink) and stars outside the PDR and projected inside the CO cores (green). Stars detected in all filters are represented by circles (∘), while stars that were not detected in the F275W filter are represented by diamonds (♢). The black arrow in each plot shows the reddening vector for AV = 0.35, the mean AV of stars in WLM measured by Y. Wang et al. (2022), assuming SMC-like extinction. The error bars in the upper-left corner of each plot demonstrate the mean uncertainty associated with the data shown. The gray dashed line shows the 5σ point-source detection limit for the given filters and exposure times (R. A. Windhorst et al. 2022).
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Multicolor image combining the five HST filters, with the outline of the PACS [C II]-detected PDR from P. Cigan et al. (2016, large gray circle) and CO cores (smaller magenta circles) overlaid (M. Rubio et al. 2015). The large black rectangle outlines the environment outside the PDR considered in this work. The legend shows the color assigned to each filter. We also include the 11﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 (55 pc) PACS beam size, which is the resolution of the PDR, in the bottom-right corner.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Left: F336W–F438W vs. F438W–F555W color–color diagram for stars inside the PDR and outside the CO cores (blue) and stars inside the PDR and projected inside the CO cores (orange). Right: F336W–F438W vs. F438W–F555W color–color diagram for stars outside the PDR and outside the CO cores (pink), and stars outside the PDR and projected inside the CO cores (green). Stars detected in all filters are represented by circles (∘), while stars that were not detected in the F275W filter are represented by diamonds (♢). The black arrow in each plot shows the reddening vector for AV = 0.35, the mean AV of stars in WLM measured by Y. Wang et al. (2022), assuming SMC-like extinction. The error bars in the upper-left corner of each plot demonstrate the mean uncertainty associated with the data shown.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: The difference between output and input magnitudes as a function of input magnitude for all artificial stars generated in the artificial star tests for each filter. The solid red horizontal line represents where the input and output magnitudes are identical, while the dashed red vertical line marks the faintest magnitude in that filter observed in the final matched catalog of stars.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Sharpness (left) and χ (right) values as a function of Vega magnitude for all sources detected in the F625W filter. Gray vertical and horizontal lines are shown to demarcate which sources were stars or galaxies. Sources with a Vega magnitude brighter than 24 were determined to be stars if their sharpness was less than zero (bottom-left quadrant in the sharpness plot), while sources with a Vega magnitude fainter than 24 were determined to be stars if both their sharpness was less than zero and their χ was less than 1 (bottom-right quadrant in both plots). Sources determined to be galaxies are shown as gold points, while sources determined to be stars are shown as purple stars.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Histograms of the ages (top left), masses (top right), and AV (bottom) for stars inside the PDR and outside the CO cores (blue), stars inside the PDR and projected inside the CO cores (orange), stars outside the PDR and projected inside the CO cores (green), and stars outside the PDR and outside the CO cores (pink). Clusters of closely packed stars may not be resolved into individual components.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Percent of fake stars recovered using DAOPHOT as a function of Vega magnitude for the F625W (orange), F555W (green), F438W (blue), F336W (purple), and F275W (pink) HST filters.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Plots showing the spatial distribution of stars, color-coded by their ages (top left), masses (top right), and AV (bottom). The large gray circle demarcates the PDR, while the smaller magenta circles show the locations and sizes of the CO cores.
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Illustration of the constraining power of different measurements of the CGM DM and density on a range of models. In all panels, curves show predictions of the default mNFW model of J. X. Prochaska & Y. Zheng (2019) (blue), the model of A. H. Maller & J. S. Bullock (2004) (orange; MB04), the model of M. J. Miller & J. N. Bregman (2013) (green; MB13), a U.-L. Pen (1999) model (Pen99) assuming a core radius set to the virial radius (red), and the models of Y. Faerman et al. (2017) (purple; Faerman1) and Y. Faerman et al. (2020) (brown; Faerman2). Top panels: Upper limit on the CGM DM toward M53 (left) and the LMC (right). In both cases, the minimum DM (18 pc cm−3) across the sky in either the NE2001 or YMW16 models has been subtracted. The ranges indicate the range of DMs of pulsars associated with each object. Bottom left: Upper limit on the CGM DM toward FRB 20220319D (see text for details). Bottom right: Constraints on the CGM density compared with the models. The dark disks indicate measurements using ram pressure stripping modeling of the LMC (M. Salem et al. 2015) and modeling of diffuse X-ray line emission (P. Kaaret et al. 2020). The lower limits displayed as triangles indicate estimates using ram pressure stripping modeling of a large selection of Milky Way satellites (M. E. Putman et al. 2021).
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Left: Prospector fit to the SED of the host galaxy of FRB 20220319D, IRAS 02044+7048. The SED measurements from archival Pan-STARRS, 2MASS, and WISE data are shown in red, together with representative 10% errors. Filter transmission curves are shown in gray. The MAP model photometry is shown in green, together with the MAP spectrum. The 100 spectra generated using random draws from the posterior distributions of the model parameters are shown in black. Right: Measured SFH of IRAS 02044+7048 (green). The results from 100 random draws from the posterior distributions are shown in black.
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Upper limits on the CGM mass for different assumptions for the radial density profile. We adopt a β model (see text for details), and show a limit corresponding to the conservative constraint from FRB 20220319D (black solid line), and from the most constraining pulsar in M53 (red solid line). Typical values of β found in the literature are ≳0.4. For these values, the inferred fCGM values are typically below 0.5, as indicated by blue horizontal lines.
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Total Hα flux observed at different locations within our long slit spectroscopic observations of IRAS 02044+7048. Measurements were obtained at 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 intervals along a 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 long slit oriented at a position angle of 104∘, which covered both the FRB position and the center of the galaxy. The locations of the galaxy nucleus and FRB 20220319D are indicated in the figure.
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Estimates of various contributions to the DM of FRB 20220319D, dissected according to Equation (2). Lower (upper) limits are indicated by upward (downward) arrows. The upper limit on DMCGM is derived from the observed FRB DM and the constraints on the other contributions.
Paper: Revisiting Open Clusters within 200 pc in the Solar Neighborhood with Gaia DR3
Authors: Penghui Liu, Min Fang, Yue-Lin Sming Tsai, Xiaoying Pang, Fan Wang, Xiaoting Fu
Figure caption: Comparison between our members (Gaia DR2 and DR3) and the members of CG 20 in Melotte 111. The left and middle panels display the distribution of members in sky position and proper motion respectively. The right panel presents a Venn diagram of the membership overlap. The intersection of members from this study (DR2) and CG 20 (DR2) is shown in purple, while members unique to this study (DR3) are highlighted in green. The remaining regions follow similarly.
Paper: Revisiting Open Clusters within 200 pc in the Solar Neighborhood with Gaia DR3
Authors: Penghui Liu, Min Fang, Yue-Lin Sming Tsai, Xiaoying Pang, Fan Wang, Xiaoting Fu
Figure caption: UPK 640 as a demonstrative case to highlight the variations in proper motion due to projection effect, assuming that all of its members have a common three-dimensional velocity (based on the mean value of the Hunt 23 members). By utilizing the cluster aggregate motion, the relative proper motion vectors at various positions in the sky relative to the cluster center are presented with equal distances from the Sun. The Δα and Δδ represent the angle of deviation from the cluster center in the directions of ra and dec, respectively. The length and direction of the color arrows show the relative vectors with respect to the gray dots (the selected sky coordinates).
Paper: Revisiting Open Clusters within 200 pc in the Solar Neighborhood with Gaia DR3
Authors: Penghui Liu, Min Fang, Yue-Lin Sming Tsai, Xiaoying Pang, Fan Wang, Xiaoting Fu
Figure caption: Relationship between the core fitted ages of the OCs HSC 2986, IC 2391, Melotte 22, Melotte 25, Melotte 111, NGC 2632, NGC 2451A, Platais 3, Platais 8, Platais 9, and UPK 640, and the ages fitted for their members beyond the tidal radius. The 3σ error bars are plotted for each OC. The gray dashed line denotes the identity line.
Paper: Revisiting Open Clusters within 200 pc in the Solar Neighborhood with Gaia DR3
Authors: Penghui Liu, Min Fang, Yue-Lin Sming Tsai, Xiaoying Pang, Fan Wang, Xiaoting Fu
Figure caption: Comparison between our members and the members of Hunt 23, Tar 22, and CG 20 in Melotte 111.