adsabs/AstroCLIMB huggingface dataset:
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Recovery of the injected RV signal with 9 cm s−1 amplitude by averaging over bisectors of 19 lines and binning to a resolution of 0.05 in orbital phase. The solid curve is the injected signal, and the dashed line is the best fit to the data and is consistent with the injected signal to within the errors (see text).
Paper: Precise Radial Velocities Using Line Bisectors
Authors: Drake Deming, Joe Llama, Guangwei Fu
Figure caption: Distribution of deviations in the bisector span, normalized by their observed standard deviation and divided into quiet-Sun and active-Sun periods. The measured distributions include all of the lines in Table 1. The blue curves are fitted Gaussian distributions.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). VI. Nuclear Star Clusters
Authors: Mika Lambert, Donghyeon J. Khim, Dennis Zaritsky, Richard Donnerstein
Figure caption: Environmental properties of UDGs with and without NSCs. We compare the local measures of environment, σ ENV and N ENV, measures of the local velocity dispersion and richness provided by Zaritsky et al. (2023), for UDGs with NSCs (red stars) and UDGs without NSCs (smoothed blue distribution). The dotted lines mark the regions set by Zaritsky et al. (2023) to differentiate environments of low density (N ENV < 15 and σ ENV < 500) and high density (N ENV > 15 and σ ENV > 500).
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Complex nebulosity and substructures in the disk, as seen in F2300C. The stretch is adjusted to bring up fainter features observed in the outer regions. Relevant features are annotated including the main and secondary disk planes and the cat’s tail. The nebulosity to the west (top) includes both irregular clumps or knots, and also some apparent linear striations or tendrils. To the east (bottom) the clumps are fainter and fewer but still present, including one particular bright clump at the bottom center. These clumps are consistently detected in identical positions on the sky seen in the two distinct rolls, confirming they are astrophysical in origin rather than any instrumental artifact.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: The β Pic debris disk as seen with NIRCam and MIRI. The top six panels show the NIRCam result from MCRDI PSF subtraction as described in Section 2.5.2, while the bottom two panels for MIRI are from classical PSF subtractions as described in Section 2.5.1. In the NIRCam data, looking closely the planet β Pic b can be seen just to the left (NE) of the occulted star (indicated with an arrow in the F300M data), along with the edge-on debris disk and its subtle warp already known from prior observations. In the MIRI data, a highly asymmetric curved feature we dub the cat’s tail is seen to the SW, apparently bending sharply away from the disk plane (see Figure 4 and Section 3.2). A mask has been applied to the F2300C image only to block the pixels behind the opaque classical Lyot occulter and its supports. All images are shown rotated by 60.°9 to align the main disk major axis horizontally, on identical asinh stretches and identical spatial scales, though with a larger vertical field of view shown for the more extended nebulosity seen with MIRI.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Same data as Figure 1 after deconvolution of the off-axis coronagraphic PSFs as described in Section 2.6. The presence of a vertical warp from the inclined secondary disk is seen more clearly in the deconvolved NIRCam data. Many complex asymmetric substructures are visible in the deconvolved MIRI data, consistently detected in both filters. Note that the deconvolution of the F1550C data is more challenging and thus has higher resulting uncertainties, as discussed in the text. Also the masked region around the F2300C Lyot occulter and its supports has been expanded to block edge regions that are not reliably deconvolved. Similarly to Figure 1, the images were rotated by 60.°9 to align the main disk horizontally.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: An example illustrating the components of the MCRDI model for the F335M data. Left: the reduced MCRDI image. Middle left: the best-fit PSF-convolved disk model. Middle right: the composite disk and planet model. Right: the final residual map for this model. The field of view is chosen to show the model within approximately the r < 2.″34 optimization region used for MCRDI. As in Figure 1, the images were rotated by 60.°9 to align the main disk with the horizontal axis.
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Vertically integrated surface brightness profiles of the disk in the different JWST filters, as labeled. Only regions with S/N > 15 were investigated. The top panels show the surface brightness vs. stellocentric distance to the star for the SW and NE sides (left and right, respectively). The middle and bottom panels show the contrast to the stellar flux and the contrast corrected for the projected distance dependence for the SW (left) and NE (right) sides. Shaded gray areas correspond to the 3σ range, color coded for each filter. The vertical dashed line in second panel (NE) indicates the location of β Pic b.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: Atmospheric retrieval posteriors (lower-left corner pairs) and range of spectral fits (upper right) from our coadded NIRCam observations of GJ 341b reduced with Tiberius. A subset of model parameters and covariances are shown, with H2O, CH4, and CO not displayed (nor constrained) for clarity.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: Atmospheric retrieval posteriors (lower-left corner pairs) and range of spectral fits (upper right) from our coadded NIRCam observations of GJ 341b reduced with Tswift. A subset of model parameters and covariances are shown, with H2O, CH4, and CO not displayed (nor constrained) for clarity.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: Column-wise: CO(1–0), 13CO(1–0), and C18O(1–0) moment maps (m-0, m-1, and linewidth maps in respective rows) constructed using emission regions, which display emission above 3σ level (σ being the rms noise level of the respective cubes). In panels (b) and (c), C18O(1–0) clumps where spectra were extracted (see Figure 11) have been marked by boxes. These boxes are labeled in panel (c). In panels (g) and (h), the regions of high dispersion have been marked by boxes and labeled p1 and p2, respectively. Spectra was extracted at these two locations as well. The red box is our targeted region, as shown in panel (a) of Figure 1. Locations of YSOs are also shown on the top-left panel.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: Panel (a): Herschel column density map. Panel (b): Herschel temperature map. Panel (c): Color-composite image (Red: Spitzer 4.5 μm; Green: Spitzer 3.6 μm; Blue: UKIDSS 2.2 μm). Panel (d): Spitzer ratio map of 4.5 μm/3.6 μm emission, smoothed using Gaussian function. The ratio map overlaps the NVSS 1.4 GHz radio continuum contours (magenta). The lowest level to generate these contours is 1.5 mJy beam−1 with a step size of 1 mJy beam−1. All the panels show the location of the identified massive stars (red circles) and the cluster region (red polygon). Panels (a), (b), and (c) also show the location of Class I (cyan circles) and Class II (green/blue circles) YSOs. The convex hull for identified YSO cores and ARs are also shown in Panel (a) and (b). Panel (c) and (d) are zoomed-in images for the NGC 2316 cluster region.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: Panel (1) and (2): PM vector-point diagrams (panel (1)) and Gaia DR3 G vs. (G BP − G  RP ) CMDs (panel (2)) for stars located in the NGC 2316 cluster region. The left subpanels (1(a) and 2(a)) show all-stars, while the middle (1(b) and 2(b)) and the right subpanels (1(c) and 2(c)) show the probable cluster members and field stars, respectively. Panel 3: Membership probability P  μ , PM errors  σ  PM  and parallax of stars as a function of the G magnitude for stars in the NGC 2316 cluster region. Stars with P  μ   ≥  80 are considered members of the NGC 2316 cluster and are shown by blue circles. Square box symbols represent the stars with PM errors  ≤ 0.4 mas (considered for estimating the distance of the NGC 2316 cluster).
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: CO(1–0) (gray), 13CO(1–0) (blue), and C18O(1–0) (red) spectra at the locations marked in Figure 10(c), (g), and (h). The C18O(1–0) spectra (shown for c1–c4 only) have been scaled up by a factor of 3. For clumps c1–c4, the Gaussian fit to C18O(1–0) spectra, has been shown by yellow line, and the peak position is indicated by a dashed line. The peak location (velocity ± dispersion) is also specified on the images.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: Panel (a): MST for the location of YSOs. The isolated cores (blue dots) and ARs (Blue + Yellow dots) are shown by their respective Convex hulls. Panel (b): Histogram for the MST branch length. Panel (c): J vs. (J − H) CMD for the YSOs located inside the CC (filled triangles (Class II)/filled asterisks (Class I)) and CAR (triangles (Class II)/asterisks (Class II)). Panel (d): Same as panel (c) but for WC and WAR. The red solid curve in panels (c) and (d) represents the isochrone of 3 Myr and Z  =  0.02 given by Pastorelli et al. (2019), which is shifted along the reddening vector for A  V   = 4 mag and the distance of 1.3 kpc.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption:  V vs. (V − I  c ) CMD for the YSOs (Class II) located inside the CC (filled triangles) and CAR (triangles). The red solid curve represents the isochrone of 3 Myr and Z  =  0.02 given by Pastorelli et al. (2019), which is shifted along the reddening vector for A  V   =  4 mag and the distance of 1.3 kpc. Black lines are the evolutionary tracks for different mass stars.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: pv slices along the vectors (L1–L6) marked on the (a) 13CO(1–0) m-0 and (b) 13CO(1–0) linewidth images. The contour levels in the 13CO(1–0) m-0 map are at 1.2, 2.5, 4, 7, and 10 K  km s−1. The four boxes on 13CO(1–0) linewidth image mark the locations of C18O(1–0) clumps (c1, c2, c3, and c4) from Figure 10(c). The red box is our targeted region as shown in panel (a) of Figure 1. L1–L6 pv slices have contours marked at 0.45, 1, 1.5, 2, 2.5, 3, 3.5, 4, and 5 K.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption:  13CO(1–0) Channel Map of the larger region. Two nearly parallel SE-NW elongated (filamentary) structures, delineated best in ∼[8.63, 9.13] km s−1 and ∼[12.12, 12.62] km s−1 channels respectively, can be seen. The redshifted (filamentary) cloud shows many filaments joining it. The red box is our targeted region as shown in panel (a) of Figure 1.
Paper: Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A
Authors: Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit
Figure caption: 1comp (top row), 2comp (middle row), and 3comp (bottom row) posterior data and models for the 2013 June 5 (left column), 2013 June 24 (middle column), and 2022 June 21 (right column) HST reverse scan observations of HD 189733 A. Spectra are given in units of flux at the stellar surface. The flux level varies between models because the conversion from raw counts depends on the free parameter a scale. Notably, the simplest 1comp retrievals settle on a distinct value of a scale in order to optimize the fit to the spectral slope with a single spectral component. In addition to the mean (gray line) and standard deviation (gray shaded region) of total model flux, contributions from individual spectral components are shown as colored lines (means) and shaded regions (standard deviations). Below each panel with spectral fluxes, another panel shows the residuals between the data and models in units of the standard deviation of the set of posterior models. Over all observation dates, the 2comp model fits the data better than the 1comp model, while the 3comp model does not significantly improve the fit. Note that the higher precision of the 2022 June 21 observations leads to better constraints on the contributions from the individual components (right middle panel).
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: Evolutionary tracks based on the PISA pre-main-sequence stellar evolution models (Tognelli et al. 2011). These models have a metalicity Z = 0.02, a helium abundance Y = 0.2880, a mixing length α = 1.90, and a deuterium abundance X  D  = 4 × 10−5. The blue, red, and green data squares indicate stars with T eff = 17,000 K and L = 2120 L ⊙, T eff = 15,700 K and L = 1430 L ⊙, and T eff = 14,000 K and L = 730 L ⊙, respectively. These correspond to the three SED models of the same colors in Figure 6. The gray square shows the locus of a star with T eff = 14,000 K, L = 300 L ⊙, which would be consistent with a 4 M ⊙ star shortly before reaching the ZAMS.
Paper: Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A
Authors: Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit
Figure caption: Left: median spectra divided by the exposure time for each scan direction observed flux within each observation date data set. Right: median spectra divided by the exposure time for each scan direction observed flux subtracted by the overall (six spectra) mean spectra within each observation date data set. Error bars for each spectra are smaller than the width of the lines. The left figure highlights the offset between the six scan observation spectra. Similarly, the right figure identifies the difference in curvature between the observed spectra, suggesting that a multiplicative scale factor is employed in the model spectra formulation (Equation (1)).
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: Allowed orbital configurations for the binary system S1 derived from the MCMC analysis conducted using the Orbitize! library. The black marker (star) designates the position of the primary component, and the red points represent radio observations of the secondary component. The upper right panel depicts the evolution of the angular separation over time, while the lower right panel illustrates the variation in the position angle throughout the orbits.
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: Corner plot generated from the MCMC analysis using the Orbitize! library. The diagonal panels display 1D marginalized posterior distributions for each of the orbital parameters, including a, e, i, ω, Ω, τ, and total mass. The off-diagonal panels illustrate 2D covariances between these parameters.
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: VLBA positions at epoch 2016.0 (the reference epoch of the Gaia DR3 release) of S1A (yellow triangle), S1B (purple diamond), and the center of mass of the S1 system (cyan circle). The pink square indicates the Gaia DR3 position and is taken as the origin of the coordinate system. A black cross is shown associated with each position; the sizes of these black crosses are 10 times the formal position errors in each case.
Paper: Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A
Authors: Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit
Figure caption: Bayesian evidence for different model fits over the three observation dates (rows) and two scan directions (columns). Each panel has the marginal Bayesian evidence for the specified model (“1comp,” “2comp,” and “3comp) relative to the reference (2comp), which is highlighted in green. Triangles show Bayesian evidences that represent models with >5σ preference against, demonstrating a poor fit. The 2comp model is preferred over all observation dates and scan directions; it provides a significant increase in the marginal Bayesian evidence over the 1comp model, while the additional complexity of the 3comp model does not provide a similar improvement.
Paper: Dynamical Mass of the Ophiuchus Intermediate-mass Stellar System S1 with DYNAMO-VLBA
Authors: Jazmín Ordóñez-Toro, Sergio A. Dzib, Laurent Loinard, Gisela Ortiz-León, Marina A. Kounkel, Josep M. Masqué, S.-N. X. Medina, Phillip A. B. Galli, Trent J. Dupuy, Luis F. Rodríguez, Luis H. Quiroga-Nuñez
Figure caption: PARSEC tracks (Nguyen et al. 2022) for a 4 M ⊙ solar metallicity star with different rotation velocities from ω = 0 to ω = 0.99. See the text for the definition of ω.
Paper: Dynamical Structures Associated with High-Order and Secondary Resonances in the Spin–Orbit Problem
Authors: Hanlun Lei
Figure caption: Analytical characteristic curves of the synchronous primary resonance, high-order resonances (outside the primary resonance), and secondary resonances (inside the primary resonance) in the ﹩(\dot{\theta },\alpha )﹩ space (left-hand panel) and comparisons with dynamical maps of the normalized second-derivative-based index ∣∣ΔD∣∣ (right-hand panel). In the right-hand panel, the locations of two typical binary asteroid systems are marked. The asphericity parameter is α = 1.1 for the binary asteroid system (65803) Didymos and it is 1.36 for (4383) Suruga. The vertical dashed line stands for the nominal location of the synchronous primary resonance and the shaded region in the left-hand panel represents the space where the synchronous primary resonance happens.
Paper: Dynamical Structures Associated with High-Order and Secondary Resonances in the Spin–Orbit Problem
Authors: Hanlun Lei
Figure caption: Analytical characteristic curves of the synchronous primary resonance and the secondary 1:1 spin–orbit resonance (left-hand panel) and comparisons to the associated numerical curves (right-hand panel). The vertical dashed line stands for the nominal location of the synchronous primary resonance and the shaded area represents the space where the synchronous primary resonance takes place. The agreement between analytical and numerical curves is good over the entire considered range α ∈ [0, 1.5].