adsabs/AstroCLIMB huggingface dataset:
Paper: A Search for Radio Technosignatures at the Solar Gravitational Lens Targeting Alpha Centauri
Authors: Nick Tusay, Macy J. Huston, Cayla M. Dedrick, Stephen Kerby, Michael L. Palumbo III, Steve Croft, Jason T. Wright, Paul Robertson, Sofia Sheikh, Laura Duffy, Gregory Foote, Andrew Hyde, Julia Lafond, Ella Mullikin, Winter Parts, Phoebe Sandhaus, Hillary H. Smith, Evan L. Sneed, Daniel Czech, Vishal Gajjar
Figure caption: Observations of the possible probe positions for communication with α Cen on UT 2021 November 6. The blue and orange lines mark the positions for receiving and transmitting probes, respectively, with light travel time taken into account. Tics along the probe position lines show where a probe at certain distances from the Sun would lie. The FWHM beam positions of each observation are represented by black circles, labeled by filter.
Paper: A Search for Radio Technosignatures at the Solar Gravitational Lens Targeting Alpha Centauri
Authors: Nick Tusay, Macy J. Huston, Cayla M. Dedrick, Stephen Kerby, Michael L. Palumbo III, Steve Croft, Jason T. Wright, Paul Robertson, Sofia Sheikh, Laura Duffy, Gregory Foote, Andrew Hyde, Julia Lafond, Ella Mullikin, Winter Parts, Phoebe Sandhaus, Hillary H. Smith, Evan L. Sneed, Daniel Czech, Vishal Gajjar
Figure caption: View of the solar system from a probe opposite α Cen at 550 au on the night of our observations. The Sun lies at the origin, and the inner solar system planets’ orbits are shown. Gray filled circles indicate beam widths for various transmitter diameters at 10 cm wavelengths. For a probe located at a distance d  > 550 au, these orbital axes would scale down by a factor of d/(550 au).
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Example images of sources with “resolved” morphology; one source from each subclass is shown. The first column shows each object’s arcminute-wide SDSS color image. The second column shows the corresponding ∼3.″5 resolution 6 GHz image from Kellermann et al. (2016), where all sources appeared unresolved. The third column shows the source’s higher-resolution (∼0.″33) A-configuration image, where the size of the image relative to the lower-resolution one is indicated by the green inset region from the second column; each source’s A-configuration morphology subclassification is noted in the upper left corner of this panel. The fourth column further displays contour maps of the A-configuration images to highlight extended features; the number in the upper left corner of each contour map indicates the base contour value (typically equivalent to a detection with S/N ≈ 3.5–4; consecutive contours are spaced by multiples of ﹩\sqrt{2};﹩ see Column (4) of Table 1 for exact σ rms values). An approximate linear size scale is given in each contour map. The SDSS location of each QSO is indicated by the magenta cross in the contour maps. The approximate FWHM of the synthesized beam (resolution element) for each radio observation is indicated by the ellipse in the lower left corner of each image. Image cutouts and individual notes for all resolved sources in the sample are included in Appendix A.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Histogram of projected physical size of RQQ radio emission, computed as the geometric mean of the major and minor axes (deconvolved). For multicomponent sources, the size corresponds to the component that is colocated with the optical QSO. For extended sources (i.e., with emission connected to the core component), the size corresponds to the extent of the extended emission. Upper limits are shown for unresolved sources. A total of 90/128 sources are included in this figure; the remaining 38 are too faint to derive accurate size estimates (see Table 1).
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Histogram showing ratio of core to total 6 GHz emission detected in A configuration for the 55 resolved sources. For sources without a core clearly separated from more extended structure, S core is the peak flux density (determined by Gaussian fit) of the source. The 67 unresolved sources are not included in this figure; core-to-total ratio for unresolved sources is by definition equal to unity.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Total 6 GHz flux density in A configuration vs. that associated with the SDSS optical counterpart for all detections. The core is the dominant radio component for all RQQs except for J0935+4819, J1118+3103, J1146+3715, and J1233+6443 (marked by star symbols)—all of which exhibit edge-brightened, extended morphology.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Distributions of the radio properties of the RQQ targets observed at ∼0.″33 resolution. Top: total 6 GHz flux density measured with the VLA. Middle: 6 GHz luminosity. Bottom: base-10 logarithm of R  i , where R  i  represents the ratio between our measured 6 GHz flux density and the source’s optical i-band flux density (Schneider et al. 2010).
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Angular offsets between radio and optical positions of our targets. Typical SDSS positional uncertainties are ≈0.″1, indicated by the circle centered at the origin. Not pictured is J1102+0844, which has an angular offset of 0.″81.
Paper: Kiloparsec-scale Radio Structure in z ∼ 0.25 Radio-quiet QSOs
Authors: Trevor V McCaffrey, Amy E Kimball, Emmanuel Momjian, Gordon T Richards
Figure caption: Luminosity distributions at 6 GHz for the different morphology classes of our sample. The open histogram with arrows emphasizes that the nondetections are plotted as 3σ rms upper limits. See Section 4 for descriptions of morphology classes.
Paper: Revisit of Open Clusters UPK 39, UPK 41, and PHOC 39: A New Binary Open Cluster Found
Authors: Xianhao Ye, Jingkun Zhao, Terry D. Oswalt, Yong Yang, Gang Zhao
Figure caption: [M/H]] vs. age. The gray shadows show the coverages of PARSEC isochrones used in this paper. The colored crosses present the top 1% of isochrones that have smallest ﹩\bar{{d}^{2}}﹩ for the three clusters.
Paper: Revisit of Open Clusters UPK 39, UPK 41, and PHOC 39: A New Binary Open Cluster Found
Authors: Xianhao Ye, Jingkun Zhao, Terry D. Oswalt, Yong Yang, Gang Zhao
Figure caption: Relative distances among c1, c2, and c3 vs. time. The gray shaded areas present the uncertainties of relative distances and the green shaded areas denote their relative distances in multiples of ﹩\bar{{r}_{{\rm{t}}}}﹩.
Paper: Revisit of Open Clusters UPK 39, UPK 41, and PHOC 39: A New Binary Open Cluster Found
Authors: Xianhao Ye, Jingkun Zhao, Terry D. Oswalt, Yong Yang, Gang Zhao
Figure caption: Left panel: orbits of c1, c2, and c3 traced back to their birthplaces. c3 was close to c1 and c2 when they were born and c2 was near c1 in the time of the formation of c1. Right panel: circles are where these clusters were born and crosses are their locations after 400 Myr. They did and will orbit together in the thin disk. The arrow in each panel shows the direction of motion.
Paper: Revisit of Open Clusters UPK 39, UPK 41, and PHOC 39: A New Binary Open Cluster Found
Authors: Xianhao Ye, Jingkun Zhao, Terry D. Oswalt, Yong Yang, Gang Zhao
Figure caption: CAMD for c1, c2 and c3 (left to right), along with adopted ages and the corresponding isochrones with [M/H] between −0.5 to 0.3 dex (interval 0.05 dex) are shown.
Paper: Revisit of Open Clusters UPK 39, UPK 41, and PHOC 39: A New Binary Open Cluster Found
Authors: Xianhao Ye, Jingkun Zhao, Terry D. Oswalt, Yong Yang, Gang Zhao
Figure caption: Distributions of member stars of c1, c2 and c3 in Cartesian coordinates xyz centered at Sun. The solid circles are the tidal radii based on the total cluster mass, and the dashed circles are ﹩\bar{{r}_{{\rm{t}}}}\sim 24﹩ pc.
Paper: Revisit of Open Clusters UPK 39, UPK 41, and PHOC 39: A New Binary Open Cluster Found
Authors: Xianhao Ye, Jingkun Zhao, Terry D. Oswalt, Yong Yang, Gang Zhao
Figure caption: Distributions of [M/H] vs. G for c1, c2, and c3. The colored lines present the median values of [M/H] for the clusters.
Paper: Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Grace Ochs, Mireya Arora, Arjun Savel
Figure caption: Emission spectra generated throughout the orbit of our 3G model planet. The solid lines show spectra that have been calculated including Doppler shifting from winds and rotation, while the dashed spectra do not include those effects. The bottom of the plot starts with the spectrum at phase 0 (corresponding to transit, when the nightside of the planet faces us), and moving up the y-axis moves forward with time (including arbitrary offsets in flux to separate the spectra). On the side panel to the right, a single feature is isolated, with the gray vertical dashed line showing the line center for the Doppler off case. The feature begins as absorption at phase 0, due to the fact that we are viewing entirely the nightside of the planet. Moving forward with time (increasing orbital phase), we can see the feature switch to emission as parts of the planet with temperature inversions come into view (with full dayside at a phase of 0.50), then back to absorption again. Additionally, the line center is redshifted and blueshifted slightly throughout the orbit, due to line-of-sight velocities from the planetary winds and rotation.
Paper: Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Grace Ochs, Mireya Arora, Arjun Savel
Figure caption: Orthographic projections for the three models presented in this paper (in pairs of rows, from top to bottom: 0 G, 3 G, and uniform) at four orbital phases (from left to right: 0, 0.25, 0.50, and 0.75; transit would be at 0). The first row of each model shows the temperature structure at 10−4 bars (within the region probed by spectral line cores), with the wind directions plotted as arrows. The second row for each model shows the maximum vertical temperature inversion at each location. The blue and red contours show constant line-of-sight velocities in increments of ±2 km s−1 at the same pressure level as the temperature plot immediately above it. The differences in temperature structures and wind patterns will influence the high-resolution emission spectra generated from these models.
Paper: Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Grace Ochs, Mireya Arora, Arjun Savel
Figure caption: CCFs of the spectra from our three different models throughout the planet’s orbit. Each Doppler-shifted spectrum is cross correlated with its unbroadened counterpoint, with the peak cross-correlation value denoted by the colored points. The peak of the CCF quantifies the net shift of that particular spectrum. When different parts of the planet are in view, the net Doppler shift of the corresponding spectra will vary. The drag-free model differs in net Doppler shift from the active and uniform drag models early and late in orbital phase, when much of the nightside is observable. Our active magnetic drag model shows a reversal in the net shift vs. orbital phase trend around secondary eclipse (phase of 0.50), which is not seen in the drag-free and uniform drag models.
Paper: Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Grace Ochs, Mireya Arora, Arjun Savel
Figure caption: Effective retrieved net Doppler shift when using spectra generated as a function of phase (teal curve) compared to using only a dayside template (orange) or a nightside template (purple) against our 3 G model (left) and our 0 G model (right). The teal curve can be thought of as the “true” velocity shifts. While the dayside and nightside models match near their respective orbital phases, once they begin to be used at different phases, their accuracy decreases. At some points in the orbit, such as phases of 0.25 and 0.75, the dayside and nightside templates will return net shifts of opposite signs. To avoid introducing these errors, spectral templates should be generated as close to the true phase of observation as possible.
Paper: Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Grace Ochs, Mireya Arora, Arjun Savel
Figure caption: Net Doppler shifts vs. orbital phase for emission spectra over the two wavelength ranges modeled. The colored lines show the Doppler shifts for wavelength range one, where water is the dominant absorber. The gray lines correspond to the shifts of wavelength range two, where CO is the dominant absorber. The different wavelength ranges probe different pressures in the atmosphere and, due to the temperature dependence of the water abundance, the disparity between the wavelength ranges should be spatially dependent. As such, the net Doppler shifts differ slightly. The bottom right panel shows this difference in net Doppler shift as a function of phase.
Paper: Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Grace Ochs, Mireya Arora, Arjun Savel
Figure caption: Spectra from our three models at orbital phases of 0 (the bottom three spectra, when the nightside of the planet is in view), 0.25 (the middle three spectra, when the day and night are both half in view), and 0.50 (the top three spectra, when the dayside is in view). The solid lines show spectra that have been Doppler shifted by winds and rotation, while the dashed lines are the spectra without this broadening. By comparing the relative fluxes of these spectra, we can see that the 3G model has the hottest dayside and coldest nightside of all the models shown here.
Paper: Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Grace Ochs, Mireya Arora, Arjun Savel
Figure caption: The integrated line flux for the three models in this paper, as a function of orbital phase. From this plot, we see that the emission lines from the uniform drag model are consistently the strongest in the emission-dominated regime and the 0 G model has the strongest absorption features. Another interesting aspect is that the model spectra switch between being dominated by emission vs. absorption lines at different orbital phases.
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Best-fit model emission spectra (top) and reduced χ 2 maps (bottom) for HR 8799c. The five models with the lowest reduced χ 2 are shown in shades of blue, with their best-fit planet radii and reduced χ 2 given, and compared to data from this work (black circles) and previous works (gray circles; see Bonnefoy et al. 2016, and references therein). The blue squares show the filter-averaged model values. The locations of the five models in the reduced χ 2 maps are indicated by the corresponding numbers.
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Completeness maps to color variability in the same fashion as Figure 7.
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Same as Figure 10, but for HR 8799e.
Paper: Atmospheric Monitoring and Precise Spectroscopy of the HR 8799 Planets with SCExAO/CHARIS 
Authors: Jason J. Wang, 劲飞 王, Peter Gao, Jeffrey Chilcote, Julien Lozi, Olivier Guyon, Christian Marois, Robert J. De Rosa, Ananya Sahoo, Tyler D. Groff, Sebastien Vievard, Nemanja Jovanovic, Alexandra Z. Greenbaum, Bruce Macintosh
Figure caption: Same as Figure 10, but for HR 8799d.
Paper: Walter: A Tool for Predicting Resolved Stellar Population Observations with Applications to the Roman Space Telescope
Authors: Lachlan Lancaster, Sarah Pearson, Benjamin F. Williams, Kathryn V. Johnston, Tjitske K. Starkenburg, Erin Kado-Fong, Anil C. Seth, Eric F. Bell
Figure caption: Left: a surface brightness map of the Number 2 Bullock & Johnston (2005) halo in the F062 filter, created as described in the text. The surface brightness is indicated by the color bar. This mock observation assumes that the galaxy is at a distance of 4 Mpc, which sets the scale of the axes in degrees and the size of the RST footprints (shown as light-blue and light-green tilings, chosen to lie at disjoint locations at different representative galactic radii). We additionally show a red bar that is 50 kpc in length at the upper left, for reference. Right: the number of detected stars, ﹩{N}_{\det }﹩ (solid lines), and the fraction of the observation that is crowded, f crowd (dashed lines), for the two different locations of observations indicated in the left panel. The dotted green line represents the number of detected stars in a giant stream that overlaps the Location 2 FOV.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: CMD of the clusters under study. All stars are probable members with a membership probability higher than 90%. The curves are the isochrones of (log(age) = 9.25, 9.30, and 9.35) for Pi 2, (log(age) = 9.00, 9.05, and 9.10) for Pi 3, (log(age) = 8.90, 8.95, and 9.00) for Pi 7, (log(age) = 9.35, 9.40, and 9.45) for Pi 12, and (log(age) = 9.10, 9.15, and 9.20) for Pi 15. These ishochrones of metallicity Z = 0.008, 0.019, 0.008, 0.019, and 0.008 for clusters Pi 2, Pi 3, Pi 7, Pi 12, and Pi 15, respectively, are taken from Marigo et al. (2017). Blue filled circles are the confirmed member BSSs in Pi 2 and Pi 15.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Surface density distribution of the Pismis clusters under study. Errors are determined from sampling statistics (= ﹩\tfrac{1}{\sqrt{N}}﹩, where N is the number of cluster members used in the density estimation at that point). The smooth line represents the fitted profile of King (1962), whereas the dotted line shows the background density level. Long dashed lines represent the errors in background density.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Profiles of stellar counts across the region of clusters Pi 2, Pi 3, and Pi 7. The Gaussian fits have been applied. The center of symmetry about the peaks of R.A. and decl. is taken to be the position of the cluster’s center.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: MF histogram derived using the most probable members, where the solid line indicates the power law given by Salpeter (1955).
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Same as Figure 9, but for clusters Pi 12 and Pi 15.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: The contour plots to show the distribution of BSSs in clusters Pi 2 and Pi 15. Blue circles are BSSs, while the red circle indicates the cluster center.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Same as Figure 5, but for clusters Pi 12 and Pi 15.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Membership probability as a function of G magnitude. The red circles show the cluster members with a membership probability higher than 90% in all panels.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: LF of stars in the region of Pismis clusters.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Galactic orbits of the clusters Pi 2, Pi 3, and Pi 7 are estimated with the Galactic potential model described in text in the time interval of the age of the cluster. The left panels show the side view, and the middle panels show the top view of the orbits. The right panels show the motion of clusters in the Galactic disk with time. The filled triangles and circles denote the birth and the present-day positions of the clusters in the Galaxy.
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: AD diagram for all clusters. All stars are probable members with a membership probability higher than 90%. A plus sign indicates the mean value (Table 7) of apex coordinates.