adsabs/AstroCLIMB huggingface dataset:
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: A simulation of a ∼1.′5 × 1.′5 region within the Hubble UDF in CASTOR (u, g) and Roman (F184) filters. This shows ∼2.2﹩\,{\mathrm{arcmin}}^{2}﹩, or just ∼0.06% of the area that will be covered by the proposed CASTOR Ultradeep Survey. The Roman F184W image assumes an exposure time of 1 hr. The galaxy shown in the top left cutout is the same as that in the left panels of Figure 11. While Roman's IR imaging (red) is sensitive to existing stellar mass, CASTOR picks out regions of ongoing star formation. With comparable spatial resolution from the ultraviolet to the near-infrared, CASTOR and Roman working in concert will map out stellar populations and other physical parameters across galaxies out to the epoch of cosmic noon.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: The left panels show the predicted CASTOR images of a real z = 0.6 galaxy (taken from the Hubble UDF) at depths similar to those of the proposed CASTOR Wide (left), Deep (middle), and Ultradeep (right) surveys. The right panels show representative UDF galaxies, chosen to span a grid of redshift and IR F140W magnitudes (a proxy for stellar mass) in simulated 100 hr CASTOR UV observations.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: Apparent AB magnitude (m UV) distribution in the UV band (purple histogram) illustrating the number of AGN (left y-axis) that can be observed over a range of magnitudes (x-axis), overplotted with individual AGN (black circles) over a range of redshifts (right y-axis) and m UV simulated in a sky area of 5 deg2 with a limiting m UV = 24.0. In the simulated AGN sample, the objects at lower redshifts appear fainter, implying the need for several exposures to achieve desirable S/N values for those targets (see also discussion in the text).
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: Exposure times required to reach S/N of 5 (dashed lines) and 10 (solid lines) in the UV (purple circles), u (green crosses), and g (red triangles) bands for AGN observations. The exposure times are calculated for a typical AGN spectrum in the rest frame normalized to AB magnitudes in the UV band. Brighter targets (m UV ≲ 24.5) require longer exposures in the bluer UV band compared to the redder g band.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: The time required to reach S/N = 5 per pixel for a spiral galaxy at z = 1 with uniform surface brightness μ, for each of the five CASTOR passbands. The top axis shows the corresponding physical SFR surface density, valid for z = 1 and ignoring extinction, as described in the text.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: The locus of the star-forming main sequence and its 1σ scatter, for galaxies with two stellar masses as indicated, is compared with the estimated 5σ extended source depths of the Deep (black line) and Ultradeep (cyan) curves, neglecting extinction. The main-sequence parameterization is taken from Popesso et al. (2023).
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: A point source (left), extended source (center), and galaxy (right) as seen through an optimal circular aperture (left), rectangular aperture (center), and elliptical aperture (right) in the g band. From left to right, the apertures enclose 80.60%, 58.51%, and 59.01% of the flux from these sources.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: The generated blackbody spectrum with spectral lines illustrated using MyPointSource.show_spectrum().
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Abundance ratios for the elements carbon, nitrogen, and oxygen. The observed [C, N, O/Fe] ratios for the program stars (red squares) are plotted as functions of the metallicity. Typical error bars are shown at the top of the panels. Data for field dwarf stars (gray crosses), field giant stars (black crosses), Ba giant stars (cyan squares), and Ba dwarf/CH subgiant stars (blue squares), collected from different literature sources, are also plotted. Data for field giant stars were taken from Luck & Heiter (2007); data for field dwarf stars were taken from Reddy et al. (2003), Reddy et al. (2006), and Luck & Heiter (2006); data for Ba giant stars were taken from Allen & Barbuy (2006a), de Castro et al. (2016), Karinkuzhi et al. (2018b), Shejeelammal et al. (2020), and Roriz et al. (2021b); data for Ba dwarfs/CH subgiant stars were taken from Edvardsson et al. (1993), Smith et al. (1993), North et al. (1994), Porto de Mello & da Silva (1997), Pereira & Junqueira (2003), Reddy et al. (2003), Pereira (2005), Allen & Barbuy (2006a), Pereira & Drake (2011), Karinkuzhi & Goswami (2015), Kong et al. (2018), Purandardas et al. (2019), Shejeelammal et al. (2020), Liu et al. (2021), and Karinkuzhi et al. (2021).
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Upper panel: temporal evolution of the cumulative frequency of Ba dwarf stars confirmed from detailed chemical analyses. Bottom panel: distribution of the 895 s-process-rich candidates (gray) reported by Norfolk et al. (2019), identifying the subsample labeled as Sr only (black), Ba only (red), and Sr and Ba (blue). Stars with ﹩\mathrm{log}g\geqslant 3.5﹩ represent only ∼0.3% of the total number of candidates.
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Indexes of the s-process. The upper, middle, and bottom panels show, respectively, the [hs/ls], [Pb/hs], and [s/Fe] ratios as functions of the metallicity. Symbols and the literature references are the same as in the caption of Figure 4. Typical error bars for our data are also shown in the panels.
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Combined carbon plus nitrogen abundances in the notation ﹩\mathrm{log}\epsilon ({\rm{C}}+{\rm{N}})﹩ observed in HD 15096, HD 141804, and HD 207585 as functions of the metallicity. A typical error bar is also shown. The symbols have the same meaning as in Figure 4. To illustrate the role of carbon in the CNO excess in our stars, we show the respective logarithmic carbon abundances in empty black squares. The magenta dashed line shows the initial CN abundance for a given metallicity.
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Position of the stars HD 15096 (blue), HD 37792 (red), HD 141804 (black), and HD 207585 (black) in the ﹩\mathrm{log}\,{T}_{\mathrm{eff}}﹩ vs. ﹩\mathrm{log}\,g﹩ diagram. Evolutionary tracks from Bressan et al. (2012), for Z = 0.006, 0.008, and 0.014, are also shown; the numbers correspond to stellar masses (in solar mass units, M ⊙).
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Observed (crosses) and synthetic (lines) spectra around the spectral region of the C2 molecular band at 5635 Å for the stars HD 15096, HD 141804, and HD 207585. The synthetic spectra were computed for different [C/Fe] values, as indicated in each panel. The gray lines are spectral synthesis without the contribution of the C2 molecule.
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Program stars in the [La/Fe] vs. [Eu/Fe] plane, along with data for other Ba dwarfs and Ba giants. Symbols and the literature references are the same as in the caption of Figure 4. Diamonds are data for CEMP-r (black), CEMP-s (magenta), and CEMP-r/s (green), taken from Masseron et al. (2010) and Karinkuzhi et al. (2021).
Paper: Shadowing in the Protoplanetary Disk of ZZ Tau IRS with HST
Authors: Jun Hashimoto, Ruobing Dong, Takayuki Muto, Hauyu Baobab Liu, Yuka Terada
Figure caption: The 1.6 μm NIR images of ZZ Tau IRS with PSF subtraction. The two panels show the same image with different annotations. The image is convolved by a Gaussian kernel with a size of 0.″64 in diameter and rotated by −44.73 deg to align the previously known outer disk PA horizontally, indicated by a horizontal dashed white line in panel (b). The central region is masked due to high residual noise. Black spots represent background stars added in PSF subtraction for ZZ Tau IRS and ZZ Tau, which is located at 35″ to the north. Three positive sources pointed out by white arrows in panel (b) are also background stars because their movements between observations at 1999 October 25 (Hubble Source Catalog; Whitmore et al. 2016) and 2017 August 23 (this study) are more than 1″ while it is approximately 0.″3 for ZZ Tau IRS. Four white bars at the corners indicate the direction of the diffraction pattern of the telescope spider. The black arrow represents the direction of the radial profiles at PA = 265 deg shown in Figure 2.
Paper: Shadowing in the Protoplanetary Disk of ZZ Tau IRS with HST
Authors: Jun Hashimoto, Ruobing Dong, Takayuki Muto, Hauyu Baobab Liu, Yuka Terada
Figure caption: The 12CO (3–2) moment 1 map adapted from Hashimoto et al. (2021) with the beam size of 329 × 327 mas indicated by the ellipse in right bottom corner. The image is rotated with −44.73 deg to align the disk PA horizontally. The dashed yellow line represents a direction 15 deg away from the outer disk’s minor axis. The white dashed contours represent the dust continuum at λ  =  0.9 mm at 10σ, 30σ, and 50σ (1σ = 268 μJy beam−1) taken from Hashimoto et al. (2021).
Paper: Shadowing in the Protoplanetary Disk of ZZ Tau IRS with HST
Authors: Jun Hashimoto, Ruobing Dong, Takayuki Muto, Hauyu Baobab Liu, Yuka Terada
Figure caption: Radial profiles along PA = 265 deg, as indicated by the black arrow in Figure 1(b), for the PSF-subtracted ZZ Tau IRS and the PSF reference star Gaia DR3 147869474824734208. A dip, representing the dark lane, is clearly observed at approximately r = 1″ for ZZ Tau IRS, while the PSF reference star exhibits monotonic decreasing.
Paper: Shadowing in the Protoplanetary Disk of ZZ Tau IRS with HST
Authors: Jun Hashimoto, Ruobing Dong, Takayuki Muto, Hauyu Baobab Liu, Yuka Terada
Figure caption: The surface density of large and small dust grains in our model.
Paper: Shadowing in the Protoplanetary Disk of ZZ Tau IRS with HST
Authors: Jun Hashimoto, Ruobing Dong, Takayuki Muto, Hauyu Baobab Liu, Yuka Terada
Figure caption: (a) Schematic view of the geometry in the inner and outer disks in our modeling. The inner and outer disks are separated by the gap at r = 1 to 60 au. The inner disk is inclined by 15 deg relative to the outer disk. The whole system is viewed at θ = 0 deg and ϕ = 60 deg. Refer to text in Section 4.1 for details. (b) and (c) Synthesized scattered light image at λ = 1.6 μm and dust continuum image at λ = 0.9 mm at raw resolution in our modeling.
Paper: Shadowing in the Protoplanetary Disk of ZZ Tau IRS with HST
Authors: Jun Hashimoto, Ruobing Dong, Takayuki Muto, Hauyu Baobab Liu, Yuka Terada
Figure caption: ALMA images of dust continuum (a) and brightness temperature of 12CO 3–2 (b) for ZZ Tau IRS adapted from Hashimoto et al. (2021). These images are rotated with −44.73 deg to align the disk PA horizontally. (c) The radial profiles along disk PA in panels (a) and (b). (d) The contours representing the dust continuum at 10σ, 30σ, and 50σ (1σ = 268 μJy beam−1) are superposed on the HST image in Figure 1.
Paper: Shadowing in the Protoplanetary Disk of ZZ Tau IRS with HST
Authors: Jun Hashimoto, Ruobing Dong, Takayuki Muto, Hauyu Baobab Liu, Yuka Terada
Figure caption: The HST image with a wide field of view, encompassing ZZ Tau, ZZ Tau IRS, and the PSF reference star Gaia DR3 147869474824734208 within the same field for ZZ Tau IRS. The PSF reference star for ZZ Tau, U Car, is in a separate field.
Paper: Shadowing in the Protoplanetary Disk of ZZ Tau IRS with HST
Authors: Jun Hashimoto, Ruobing Dong, Takayuki Muto, Hauyu Baobab Liu, Yuka Terada
Figure caption: Schematics of the ZZ Tau IRS system in an edge-on view, i.e., viewed at θ = 0 deg and ϕ = 90 deg. Earth-bound observers view the disks at θ = 0 deg and ϕ = 60 deg. In addition to the misaligned inner disk and the shadowed outer disk, the outer disk of large dust grains (dots), warmer CO gas (red), and CO gas in the gap (blue) are illustrated. Refer to the text in Sections 4.1 and 5.1 for further details.
Paper: Shadowing in the Protoplanetary Disk of ZZ Tau IRS with HST
Authors: Jun Hashimoto, Ruobing Dong, Takayuki Muto, Hauyu Baobab Liu, Yuka Terada
Figure caption: Comparison between the HST image and the convolved model image. (a) The HST image, as shown in Figure 1(a). (b) The model image from Figure 5(b) convolved with a Gaussian kernel with a diameter of 0.″64, same as the Gaussian kernel applied in panel (a).
Paper: Post-Newtonian Orbital Effects Induced by the Mass Quadrupole and Spin Octupole Moments of an Axisymmetric Body
Authors: Lorenzo Iorio
Figure caption: Plot of the amplitudes, in m yr−1 and 10−8 yr−1, respectively, of Equations (58)–(59), calculated for the polar orbital configuration of Equations (53)–(54), as functions of the apocenter height h apo for a fixed value of the pericenter height h peri = 4200 km. The dashed vertical line corresponds to h apo = 3.2 × 106 km, which was the originally planned apocenter height of Juno before the problems encountered by its propulsion system.
Paper: Post-Newtonian Orbital Effects Induced by the Mass Quadrupole and Spin Octupole Moments of an Axisymmetric Body
Authors: Lorenzo Iorio
Figure caption: Plot of Equations (62)–(63), in mas yr−1, calculated for the polar orbital configuration of Equations (53)–(54) with the condition of Equation (73), as functions of the apocenter height h apo for a fixed value of the pericenter height h peri = 4200 km. The dashed vertical line corresponds to h apo = 3.2 × 106 km, which was the originally planned apocenter height of Juno before the problems encountered by its propulsion system.
Paper: Post-Newtonian Orbital Effects Induced by the Mass Quadrupole and Spin Octupole Moments of an Axisymmetric Body
Authors: Lorenzo Iorio
Figure caption: Plot of Equations (66)–(67), in mas yr−1, calculated for the polar orbital configuration of Equations (53)–(54) with the condition of Equation (73), as functions of the apocenter height h apo for a fixed value of the pericenter height h peri = 4200 km. The dashed vertical line corresponds to h apo = 3.2 × 106 km, which was the originally planned apocenter height of Juno before the problems encountered by its propulsion system.
Paper: Post-Newtonian Orbital Effects Induced by the Mass Quadrupole and Spin Octupole Moments of an Axisymmetric Body
Authors: Lorenzo Iorio
Figure caption: Plot of the amplitudes, in m yr−1 and 10−8 yr−1, respectively, of Equations (58)–(59), calculated for the polar orbital configuration of Equations (53)–(54), as functions of the apocenter height h apo for a fixed value of the pericenter height h peri = 4200 km.
Paper: Post-Newtonian Orbital Effects Induced by the Mass Quadrupole and Spin Octupole Moments of an Axisymmetric Body
Authors: Lorenzo Iorio
Figure caption: Plot of Equations (66)–(67), in mas yr−1, calculated for the polar orbital configuration of Equations (53)–(54) with the condition of Equation (73), as functions of the apocenter height h apo for a fixed value of the pericenter height h peri = 4200 km.
Paper: Post-Newtonian Orbital Effects Induced by the Mass Quadrupole and Spin Octupole Moments of an Axisymmetric Body
Authors: Lorenzo Iorio
Figure caption: Plot of Equations (62)–(63), in mas yr−1, calculated for the polar orbital configuration of Equations (53)–(54) with the condition of Equation (73), as functions of the apocenter height h apo for a fixed value of the pericenter height h peri = 4200 km.
Paper: Resonant Chains and the Convergent Migration of Planets in Protoplanetary Disks
Authors: Ka Ho Wong, Man Hoi Lee
Figure caption: (a) Boundary between inward and outward migration according to Equation (6) for an adiabatic disk with power-law indices α for surface density and β for temperature. (b) Boundary between faster forced migration of inner planet and faster forced migration of outer planet according to Equations (7) and (8) for m 1 = m 2. (c) Combined plot, with the convergent outward and inward migration regions corresponding to the regions bounded by the red and blue lines in Figure 3.
Paper: Resonant Chains and the Convergent Migration of Planets in Protoplanetary Disks
Authors: Ka Ho Wong, Man Hoi Lee
Figure caption: Same as Figure 1(c) but for P 2/P 1 = 3/2 and (a) m 2/m 1 = 2 and (b) m 2/m 1 = 1/2. The convergent inward and outward migration zones are marked.
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Fitting of theoretical σ N  s  curves (red lines) and observed σ N  s  values (black squares). The data are plotted in logarithmic scale; σ is expressed in millibarn and N  s  in the scale ﹩\mathrm{log}\epsilon (\mathrm{Si})=6.0﹩. The estimated neutron exposures are shown in the bottom of panels.
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Comparison between the observed abundance profiles (black squares with error bars) and the predicted profiles (curves) from the Monash (blue) and FRUITY (red) nucleosynthesis models that best fit the observational data set, after dilution is applied. The derived dilution factors are also shown.
Paper: High-resolution Spectroscopic Analysis of Four Unevolved Barium Stars 
Authors: M. P. Roriz, N. Holanda, L. V. da Conceição, S. Junqueira, N. A. Drake, A. Sonally, C. B. Pereira
Figure caption: Ba dwarfs analyzed in this work (red squares) in the Toomre diagram of ﹩{({U}_{\mathrm{LSR}}^{2}+{W}_{\mathrm{LSR}}^{2})}^{1/2}﹩                   vs. V LSR. Ba dwarfs previously analyzed by Pereira & Drake (2011), Escorza et al. (2019), and Pereira (2005) are shown in red crosses. The classical Ba giant stars of the thin disk (black crosses), transition thin/thick disk (green crosses), thick disk (blue crosses), and halo (magenta crosses), taken from de Castro et al. (2016), are also plotted in this diagram.