adsabs/AstroCLIMB huggingface dataset:
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Flowchart illustrating the extraction of line profile properties for 12CO J = 3−2 emission from the disk of LkCa 15.
Paper: exoALMA. III. Line-intensity Modeling and System Property Extraction from Protoplanetary Disks
Authors: Andrés F. Izquierdo, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Cartoon illustrating our adopted geometric parameter conventions and the projected rotation velocity of a disk with positive inclination and clockwise rotation.
Paper: Contribution of Alfvénic Waves on the Formation and Deflection of Switchbacks: Insights from Two Decades of WIND Spacecraft Data
Authors: Hui Li, Fanzhuo Dai, Chi Wang, Wence Jiang, Haoyu Li
Figure caption: (a) and (b) show the proportions and purity of Alfvén waves in the solar wind at different speeds. PSP data (orange) covers the period from 2018-11-01 to 2018-11-11. (c) Relationship between switchback occurrence rate and solar wind speed. PSP data (orange) are from the first 17 encounters (heliocentric distances less than 0.25 au), while WIND data (blue) cover the entire time. Green indicates period with large-amplitude Alfvén waves (﹩\overline{\,\rm{Err}\,}\lt 0.3﹩ and δB⊥/B0 > 0.2).
Paper: Contribution of Alfvénic Waves on the Formation and Deflection of Switchbacks: Insights from Two Decades of WIND Spacecraft Data
Authors: Hui Li, Fanzhuo Dai, Chi Wang, Wence Jiang, Haoyu Li
Figure caption: The high-speed stream and its surrounding regions (leading edge, trailing edge, upstream, and downstream): (a) switchback occurrence rate, (b) maximum deflection angle of switchbacks, (c) Alfvén wave contribution, and (d) Alfvén wave purity. Here, upstream and downstream correspond to 1 day outside the leading edge and trailing edge, respectively.
Paper: Contribution of Alfvénic Waves on the Formation and Deflection of Switchbacks: Insights from Two Decades of WIND Spacecraft Data
Authors: Hui Li, Fanzhuo Dai, Chi Wang, Wence Jiang, Haoyu Li
Figure caption: (a) Distribution of switchback occurrence rate with Alfvén wave purity. (b) Distribution of switchback occurrence rate with Alfvén wave amplitude during hours when the average Alfvén wave purity is less than 0.3. (c) and (d) are the same format as (a) and (b), but with occurrence rate replaced by maximum deflection degree. (e)–(h) are the corresponding marginal probability distributions.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Fitting results for the fiducial temperature assumption. (a) Gas (blue) and dust (orange) surface density profiles. The dust surface density is multiplied by 100 for visibility purposes. The black bar at the upper-right corner indicates the spatial resolution of the CO image. (b) Midplane gas pressure profile (blue) with an arbitrarily scaled dust surface density profile (orange). The dust surface density peaks at the gas pressure maximum. Note that there are uncertainties from the undetermined XCO in panels (a) and (b). (c) Gas surface density profile for various XCO with criteria for gravitational instability and streaming instability.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: (Left) Azimuthally stacked CO spectra. The upper and lower panels show the same data, but in the lower panel, we convolved the spectrum at each radius with a flat kernel of three channels and use the symmetric logarithm color map in order to enhance the faint emission in the line wings. The horizontal dotted lines indicate the radial range of the dust ring. The dashed ellipse marks the faint line wings we analyze in this Letter. (Middle) The best-fit model of the CO spectra. (Right) The residual between the observed and model spectra.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Log–log plot of the radially averaged spectrum at ﹩r=0\mathop{.}\limits^{{\rm{^{\prime\prime} }}}4-0\mathop{.}\limits^{{\rm{^{\prime\prime} }}}8﹩ as a function of ∣v∣. The wing (∣v∣ > 1 km s−1) emission follows v−2, which is predicted for pressure-broadened line wings. The orange dotted line indicates the best-fit model if we interpret the wing as a high-temperature component. As discussed in Section 3.1, the derived temperature from the line width is 4.8 × 103 K, which is unrealistically high for CO molecules.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: (Top) 331 GHz continuum image. (Bottom) The integrated intensity map of the 12CO J = 3–2 line. Both images are obtained as part of the exoALMA project (P. Curone et al. 2025; R. Teague et al. 2025). The J1604 disk is close to face on and consists of a single well-defined continuum ring.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: The same as Figure 5, but for the high midplane temperature case with T100 = 30 K.
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Radially averaged spectrum at ﹩r=0\mathop{.}\limits^{{\rm{^{\prime\prime} }}}4-0\mathop{.}\limits^{{\rm{^{\prime\prime} }}}8﹩ (see Figure 2). The lower panel shows a zoomed-in view of the upper panel. Colored lines indicate models with different gas surface densities, as discussed in Section 4.1
Paper: exoALMA. XIV. Gas Surface Densities in the RX J1604.3−2130 A Disk from Pressure-broadened CO Line Wings
Authors: Tomohiro C. Yoshida, Pietro Curone, Jochen Stadler, Stefano Facchini, Richard Teague, Munetake Momose, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Brianna Zawadzki
Figure caption: Observed dust surface density profile (black) and calculated profiles from the observed gas surface density for different αturb.
Paper: exoALMA. XVII. Characterizing the Gas Dynamics around Dust Asymmetries
Authors: Lisa Wölfer, Marcelo Barraza-Alfaro, Richard Teague, Pietro Curone, Myriam Benisty, Misato Fukagawa, Jaehan Bae, Gianni Cataldi, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Francois Menard, Anika Nath, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: PLUTO simulations of a vortex triggered by the RWI at the edge of a dead zone (top row) and a Jupiter-mass planet (bottom row), using a scaling radius of 70 au to convert from code units to physical units. Shown are the gas density (left panels), radial velocity (middle panels), and azimuthal velocity (right panels). The density field and sub-Keplerian rotation velocity of a smooth disk have been removed (in case of vr this is zero), and the quantities are normalized. The location of the planet is marked with a circle in the bottom row panels.
Paper: exoALMA. XVII. Characterizing the Gas Dynamics around Dust Asymmetries
Authors: Lisa Wölfer, Marcelo Barraza-Alfaro, Richard Teague, Pietro Curone, Myriam Benisty, Misato Fukagawa, Jaehan Bae, Gianni Cataldi, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Francois Menard, Anika Nath, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Polar-deprojected residuals of the centroid velocity, peak intensity, and line width, shown for both CO lines and the HD 135344B (top) and MWC 758 (bottom) disks. The deprojection of the NIR scattered-light emission is included in the fourth panel of each row (T. Stolker et al. 2017; B. B. Ren et al. 2023), highlighting the observed spiral features that are overlaid as contours on the other three panels. The SPHERE images are normalized to the peak value and shown with a logarithmic normalization of the color map. Note the different spatial scale of the rows.
Paper: exoALMA. XVII. Characterizing the Gas Dynamics around Dust Asymmetries
Authors: Lisa Wölfer, Marcelo Barraza-Alfaro, Richard Teague, Pietro Curone, Myriam Benisty, Misato Fukagawa, Jaehan Bae, Gianni Cataldi, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Francois Menard, Anika Nath, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Velocity residuals of the data (top two rows) and dead-zone vortex model (bottom row). The model was postprocessed with RADMC-3D and convolved with the beam of the observation. For each disk, the model has been adapted such that that the geometry and vortex location match the data. For MWC 758, two representations are included to account for both vortex features. In the first two rows, the continuum observations are overlaid, highlighting the dust asymmetries. The beam of the observation is shown in the lower left corner of each panel in the first row.
Paper: exoALMA. XVII. Characterizing the Gas Dynamics around Dust Asymmetries
Authors: Lisa Wölfer, Marcelo Barraza-Alfaro, Richard Teague, Pietro Curone, Myriam Benisty, Misato Fukagawa, Jaehan Bae, Gianni Cataldi, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Francois Menard, Anika Nath, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Andrew J. Winter, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Velocity perturbations of the dead-zone vortex simulation, postprocessed with RADMC-3D and adapted to each dust asymmetry observed in the data. Shown are the unconvolved models (top row) and models convolved with the beam of the observation (bottom row). The continuum observations are overlaid in all panels to highlight the location of the dust asymmetries.
Paper: Detection of Methane in the Closest Extreme Metal-poor T Dwarf WISEA J181006.18−101000.5 
Authors: Jerry J.-Y. Zhang, 俊䶮 章, Nicolas Lodieu, Eduardo L. Martín, Pascal Tremblin, María Rosa Zapatero Osorio, Víctor J. S. Béjar, Nikola Vitas, Bartosz Gauza, Yakiv V. Pavlenko, Rafael Rebolo
Figure caption: New WISE1810 JHK spectrum normalized at 13000 Å compared with ATMO2020++ best-fit model matching in the H band (red). Upper: the whole spectral energy distribution, combined with multiband photometry, GTC/OSIRIS red optical spectrum (8000–10000 Å), and GTC/EMIR YJ spectrum (10000–11700 Å) from N. Lodieu et al. (2022); lower: the JHK bands, with model matched in the H band but moved onto the observed spectra to compare features in the J and K bands. Note: the original data are plotted in light gray, and solid black or blue lines are data smoothed by a factor of 7.
Paper: Detection of Methane in the Closest Extreme Metal-poor T Dwarf WISEA J181006.18−101000.5 
Authors: Jerry J.-Y. Zhang, 俊䶮 章, Nicolas Lodieu, Eduardo L. Martín, Pascal Tremblin, María Rosa Zapatero Osorio, Víctor J. S. Béjar, Nikola Vitas, Bartosz Gauza, Yakiv V. Pavlenko, Rafael Rebolo
Figure caption: Images of the position of WISE1810 on 2024 July 21 from GTC/EMIR in the J, H, and Ks bands. The object is marked with a red circle. The field of view of each image is 45″ × 45″. North is up and east is left.
Paper: Detection of Methane in the Closest Extreme Metal-poor T Dwarf WISEA J181006.18−101000.5 
Authors: Jerry J.-Y. Zhang, 俊䶮 章, Nicolas Lodieu, Eduardo L. Martín, Pascal Tremblin, María Rosa Zapatero Osorio, Víctor J. S. Béjar, Nikola Vitas, Bartosz Gauza, Yakiv V. Pavlenko, Rafael Rebolo
Figure caption: Comparison between old spectrum from A. C. Schneider et al. (2020) and new GTC/EMIR spectrum. While GTC/EMIR photometry agrees with photometry from A. C. Schneider et al. (2020), the two spectra are not matched.
Paper: Detection of Methane in the Closest Extreme Metal-poor T Dwarf WISEA J181006.18−101000.5 
Authors: Jerry J.-Y. Zhang, 俊䶮 章, Nicolas Lodieu, Eduardo L. Martín, Pascal Tremblin, María Rosa Zapatero Osorio, Víctor J. S. Béjar, Nikola Vitas, Bartosz Gauza, Yakiv V. Pavlenko, Rafael Rebolo
Figure caption: Temperature–pressure profile (left) and abundance–pressure profiles of the most frequent molecules (right) in the atmosphere of WISE1810 from the adjusted ATMO2020++ model with nonequilibrium chemistry.
Paper: Detection of Methane in the Closest Extreme Metal-poor T Dwarf WISEA J181006.18−101000.5 
Authors: Jerry J.-Y. Zhang, 俊䶮 章, Nicolas Lodieu, Eduardo L. Martín, Pascal Tremblin, María Rosa Zapatero Osorio, Víctor J. S. Béjar, Nikola Vitas, Bartosz Gauza, Yakiv V. Pavlenko, Rafael Rebolo
Figure caption: Comparison between WISE1810 and the 2MASS2030 T1.5 dwarf in the region of three KI lines. The lighter-colored curves are original data and the dark ones are smoothed by a factor of 7.
Paper: Detection of Methane in the Closest Extreme Metal-poor T Dwarf WISEA J181006.18−101000.5 
Authors: Jerry J.-Y. Zhang, 俊䶮 章, Nicolas Lodieu, Eduardo L. Martín, Pascal Tremblin, María Rosa Zapatero Osorio, Víctor J. S. Béjar, Nikola Vitas, Bartosz Gauza, Yakiv V. Pavlenko, Rafael Rebolo
Figure caption: 15300–15800 Å feature compared with transmission absorption spectra of HCN and H2S obtained using gas chamber under room temperature and 1 atm pressure.
Paper: Detection of Methane in the Closest Extreme Metal-poor T Dwarf WISEA J181006.18−101000.5 
Authors: Jerry J.-Y. Zhang, 俊䶮 章, Nicolas Lodieu, Eduardo L. Martín, Pascal Tremblin, María Rosa Zapatero Osorio, Víctor J. S. Béjar, Nikola Vitas, Bartosz Gauza, Yakiv V. Pavlenko, Rafael Rebolo
Figure caption: Normalized CCFs against radial velocity (in blue) with their maximum (red dot) and Gaussian fits (in gold) in the JHK bands.
Paper: The Exoplanet Edge: Planets Do Not Induce Observable Transit Timing Variations with a Dominant Transit Timing Variation Period Faster than Half Their Orbital Period
Authors: Daniel A. Yahalomi, David Kipping, Eric Agol, David Nesvorný
Figure caption: Peak TTV periods recovered via LS periodograms fit to TTVFast simulated systems that pass stability and amplitude tests for all combined masses simulated. Top: TTVFast systems initialized with zero eccentricity. Middle: TTVFast systems initialized with eccentricities between 0 and 0.4. Bottom: TTVFast systems initialized with any physical eccentricity. For circular planets, TTVs with a period equal to the perturber’s period dominate for distant perturbers. When moderately eccentric systems are sampled, TTV periods commensurate with the perturber’s orbit and half-orbit are the dominant signals. For highly eccentric systems, the parameter space becomes more degenerate, but the exoplanet edge provides a lower limit for the TTV period.
Paper: Detection of Deuterated Hydrocarbon Nanoparticles in the Whirlpool Galaxy, M51
Authors: B. T. Draine, Karin Sandstrom, Daniel A. Dale, J.-D. T. Smith, Ryan Chown, Grant P. Donnelly, Sara E. Duval, Cory M. Whitcomb, Angela Adamo, L. Armus, Danielle A. Berg, Torsten Böker, Alberto D. Bolatto, Martha L. Boyer, Daniela Calzetti, B. G. Elmegreen, Brandt A. L. Gaches, Karl D. Gordon, L. K. Hunt, R. C. Kennicutt, Ralf S. Klessen, Thomas S.-Y. Lai, Adam K. Leroy, Sean T. Linden, Alex Pedrini, Noah S. J. Rogers, Julia C. Roman-Duval, Eva Schinnerer, Evan B. Skillman, Fabian Walter, Tony D. Weinbeck, Benjamin F. Williams
Figure caption: The 4–5 μm spectra (R ≈ 1100) of four star-forming regions in M51 (see text). Observed wavelengths have been corrected for redshift (see Table 1 for adopted radial velocities). Three of the spectra show CO2 ice absorption (strongest in E-Strip H II). The E-Strip H II spectrum also shows 4.56–4.69 μm XCN+CO ice absorption. A dust emission feature near 4.65 μm is present in all spectra.
Paper: The Exoplanet Edge: Planets Do Not Induce Observable Transit Timing Variations with a Dominant Transit Timing Variation Period Faster than Half Their Orbital Period
Authors: Daniel A. Yahalomi, David Kipping, Eric Agol, David Nesvorný
Figure caption: Schematic showing the rotating-tidal-distortion-induced lower exoplanet edge with an observed TTV at period Ppert/2. The gravitational influence of the distant outer perturbing planet tidal distorts the orbit of the transiting planet, with a rotational period equal to Ppert. However, the tidally distorted orbit has rotational symmetry of order m = 2 (i.e., symmetric about rotations of 180°); thus, the induced TTV will be observed with a period of Ppert/2.
Paper: The Exoplanet Edge: Planets Do Not Induce Observable Transit Timing Variations with a Dominant Transit Timing Variation Period Faster than Half Their Orbital Period
Authors: Daniel A. Yahalomi, David Kipping, Eric Agol, David Nesvorný
Figure caption: Schematic demonstrating how conjunction-induced TTVs produce an observable TTV period equal to Ppert when Ppert/Ptrans > 2. For an observer to the right of the diagram, as shown above, during the first half of the perturber’s orbit, it induces early TTVs (pulling the planet in the same direction as the orbit), and for the second half of its orbit, it induces late TTVs (pulling the planet in the opposite direction as the orbit). Thus, the observed TTV will have a period equal to Ppert.
Paper: The Exoplanet Edge: Planets Do Not Induce Observable Transit Timing Variations with a Dominant Transit Timing Variation Period Faster than Half Their Orbital Period
Authors: Daniel A. Yahalomi, David Kipping, Eric Agol, David Nesvorný
Figure caption: Two-planet KOIs from the T. Holczer et al. (2016) catalog that exhibit TTVs with ΔBIC > 6 overplotted on top of TTVFast simulated TTVs. Marker size is indicative of TTV amplitude. TTVs are split into three populations: (i) TTV periods that are greater than the period of the perturber and thus likely near MMR-induced TTVs, (ii) TTV periods consistent with exoplanet edges and thus likely driven by either aliased conjunction-induced TTVs or tidal distortions, and (iii) TTV periods that are anomalously fast and thus indicating the likely presence of additional mass in the system.