adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: (a) F CO is plotted as a function of L bol. ALMASOP observations are shown with gray squares. Blue, green, brown, and magenta points represent YSOs, VeLLOs, proto−brown dwarfs, and candidate FHSCs, respectively. Proto−brown dwarfs are also in the VeLLO category. These data points have been adopted from Palau et al. (2014), Hsieh et al. (2016), and Dutta et al. (2022a). Open squares indicate single-dish observations. A linear fit of the whole sample (ALMASOP and literature) is shown with the black line. (b) F CO is shown as a function of M Env. The filled circles are single systems. Tringles indicate binary or other multiple systems. Colors are for bolometric temperature (T bol), where those with T bol > 70 K are condered as Class I objects. The black filled circles with red open squares do not have a T bol estimation. A linear fit of the data points is also shown.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G205.46-14.56M1 (HOPS 317). (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 10 km s−1. All symbols are the same as in Figure 3. (c) CO emission maps integrated over −18 to −2 km s–1 and +2–12 km s−1 with sensitivity 7.4 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.11 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission integrated over −102 to −28] km s–1 and +4–12 km s−1 with sensitivity 3.7 K km s−1, with similar symbols and contours to those in Figure 5(a). (f) SiO PV diagram with sensitivity 0.16 K, with similar symbols and contours to those in Figure 5(b). The “?” mark indicates that the present observations could not confirm the candidacy of the knot.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G205.46-14.56S1 (HOPS 358). (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 11 km s−1. All symbols are the same as in Figure 3. (c) CO emission integrated over −20 to −4 km s–1 and +2–20 km s−1 with sensitivity σ ∼ 14.8 K km s−1, with similar symbols to those in Figure 4(a). The contours are at (3, 9, 18, 36, 72) × σ . (d) CO PV diagram with sensitivity 0.11 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission integrated over −20 to +20 km s−1 with sensitivity 3.4 K km s−1, with similar symbols and contours to those in Figure 5(a). (f) SiO PV diagram with sensitivity 0.14 K, with similar symbols and contours to those in Figure 5(b). The “?” mark indicates that the present observations could not confirm the scenario.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: (a) Jet mass-loss rates (﹩{\dot{M}}_{j}﹩) are plotted as a function of (a) bolometric luminosity (L bol) and (b) envelope mass M Env. The color bar indicates the ratio of mass-loss rate to accretion rate (﹩{\dot{M}}_{j}﹩/﹩{\dot{M}}_{\mathrm{acc}}﹩). Stars in panel (a) are data points for different well-known SiO jet objects adopted from the literature (e.g., Lee 2020). The triangles in panel (b) are multiple sources within a common envelope. A linear fit of the data points is also shown in panel (b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: Mean ejection periods (﹩{{ \mathcal T }}_{\mathrm{knot}}﹩) are plotted as a function of (a) bolometric luminosity (L bol) and (b) envelope masses (M env). Single and multiple sources are shown with circles and triangles, respectively. The color scale indicates the mass accretion rate (﹩{\dot{M}}_{\mathrm{acc}}﹩). The straight line in panel (b) is the linear fit to the data points.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: CH3OH ice lines (﹩{R}_{{\mathrm{CH}}_{3}\mathrm{OH}}﹩) of the known hot corinos are plotted as a function of bolometric luminosity (L bol). Observed CH3OH radius and the acronyms of ALMASOP objects are adopted from Hsu et al. (2022). The diagonal lines indicate the ice-line radius at 100 K for luminosity L bol = 1, 10, 70, and 100 L ⊙.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: Keplerian radii corresponding to the observed mean periods of episodic events are plotted as a function of envelope masses. A stellar mass M * = 0.1 M ⊙ is assumed for all protostars. All notations are the same as in Figure 15(b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G192.32-11.88N. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.9 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 12 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 6.4 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.13 K, with similar symbols and contours to those in Figure 4(b). (e) Integrated SiO emission with sensitivity 2.7 K km s−1, with similar symbols and contours to those in Figure 5(a). (f) SiO PV diagram with sensitivity σ = 0.47 K, with similar symbols to those in Figure 5(b). The SiO contour labels are at (1.5, 2, 3, 4) × σ.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G211.47-19.27S. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 4 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 8.6 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.15 K, with similar symbols and contours to those in Figure 4(b). (e) Integrated SiO emission with sensitivity 1.9 K km s−1, with similar symbols and contours to those in Figure 5(a).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G192.12-11.10. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼1.5 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 10 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 11.5 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.16 K, with similar symbols and contours to those in Figure 4(b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G200.34-10.97N. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 14 km s−1. All symbols are the same as in Figure 3. (c) CO map integrated over −20 to +12 km s−1 with sensitivity 9.9 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.14 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission map integrated over −10 to +10 km s−1 emission with sensitivity 3.7 K km s−1, with similar symbols and contours to those in Figure 5(a). (f) SiO PV diagram with sensitivity σ = 0.12 K, with similar symbols to those in Figure 5(b). The SiO contour labels are at (2, 3, 4) × σ. The “?” mark indicates that the present observations could not confirm the scenario.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G209.55-19.68N1. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 7 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 7.8 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.12 K, with similar symbols and contours to those in Figure 4(b). (e) Integrated SiO emission with sensitivity 2.6 K km s−1, with similar symbols and contours to those in Figure 5(a). (f) SiO PV diagram with sensitivity σ = 0.15 K, with similar symbols to those in Figure 5(b). The “?” mark indicates that the present observations could not confirm the candidacy of the knot.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G205.46-14.56M2. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼4.5 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 14 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 6.15 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) Integrated SiO emission with sensitivity 2.1 K km s−1, with similar symbols and contours to those in Figure 5(a).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G196.92-10.37. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼1.2 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 11 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 9.6 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.1 K, with similar symbols and contours to those in Figure 4(b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G203.21-11.20W1. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼3.36 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 10 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 5.14 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.11 K, with similar symbols and contours to those in Figure 4(b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G205.46-14.56N2. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼0.8 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 10 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 4.5 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) Integrated SiO emission with sensitivity 1.15 K km s−1, with similar symbols and contours to those in Figure 5(a).
Paper: Investigating the Atmospheric Mass Loss of the Kepler-105 Planets Straddling the Radius Gap
Authors: Aaron Householder, Lauren M. Weiss, James E. Owen, Howard Isaacson, Andrew W. Howard, Daniel Fabrycky, Leslie A. Rogers, Hilke E. Schlichting, Benjamin J. Fulton, Erik A. Petigura, Steven Giacalone, Joseph M. Akana Murphy, Corey Beard, Ashley Chontos, Fei Dai, Judah Van Zandt, Jack Lubin, Malena Rice, Alex S. Polanski, Paul Dalba, Sarah Blunt, Emma V. Turtelboom, Ryan Rubenzahl, Casey Brinkman
Figure caption: The mass–radius relationship for transiting exoplanets with combined fractional mass and radius uncertainties less than 50% (plotted in gray as a function of fractional uncertainty), based on the NASA Exoplanet Archive (Akeson et al. 2013; queried on 2022 September 22). We also depict the radius gap (Fulton et al. 2017) from 1.5 R ⊕ to 2.0 R ⊕ (light gray) as well as the planetary compositions (light blue, dashed) from Zeng et al. (2019). Additionally, we include the 1σ radius (Fulton & Petigura 2018) and mass measurements of Kepler-105b (blue, 2.53  ± 0.07R ⊕, 10.8  ± 2.3M ⊕) and Kepler-105c (brown, 1.44  ± 0.04R ⊕, 5.6  ± 1.2M ⊕). We also show the EvapMass (Owen & Campos Estrada 2020b) predicted 1σ minimum mass distribution for Kepler-105b that is consistent with photoevaporation (red, 8.7  ± 2.4M ⊕). If the measured mass of Kepler-105b is greater than the EvapMass prediction, then the difference in gas content between Kepler-105b and Kepler-105c can be explained by photoevaporation. Comparing these distributions, we conclude that the difference in gas envelopes of the Kepler-105 planets is entirely attributable to photoevaporation in 76% of scenarios (i.e., M  b,measured  >  M  b,predicted).
Paper: Investigating the Atmospheric Mass Loss of the Kepler-105 Planets Straddling the Radius Gap
Authors: Aaron Householder, Lauren M. Weiss, James E. Owen, Howard Isaacson, Andrew W. Howard, Daniel Fabrycky, Leslie A. Rogers, Hilke E. Schlichting, Benjamin J. Fulton, Erik A. Petigura, Steven Giacalone, Joseph M. Akana Murphy, Corey Beard, Ashley Chontos, Fei Dai, Judah Van Zandt, Jack Lubin, Malena Rice, Alex S. Polanski, Paul Dalba, Sarah Blunt, Emma V. Turtelboom, Ryan Rubenzahl, Casey Brinkman
Figure caption: Observed transit times minus a linear ephemeris (black) for Kepler-105b (top) and Kepler-105c (bottom). The plot also includes the best fit TTVFaster (Agol & Deck 2016) solution to the TTVs (dark green) as well as the 1σ  confidence intervals from our model (light green). Our TTV model is strongly preferred to a linear ephemeris (ΔAIC  =   − 27, where AIC is the Akaike information criterion; Akaike 1974), indicating the presence of dynamical perturbations affecting the transit times. Based on the TTVs alone, we detected Kepler-105c with 4σ  confidence (5.9 ± 1.4 M ⊕) and Kepler-105b with 2σ confidence (﹩{9.3}_{-4.6}^{+4.9}﹩                   M ⊕). Furthermore, we ran two additional MCMC runs where the mass of Kepler-105c was constrained to be either  ≤3.1 M ⊕ or  ≥8.7 M ⊕. Our best-fit TTVFaster analytic solution was strongly preferred over these MCMC models (ΔAIC  =   − 11 for both cases).
Paper: Investigating the Atmospheric Mass Loss of the Kepler-105 Planets Straddling the Radius Gap
Authors: Aaron Householder, Lauren M. Weiss, James E. Owen, Howard Isaacson, Andrew W. Howard, Daniel Fabrycky, Leslie A. Rogers, Hilke E. Schlichting, Benjamin J. Fulton, Erik A. Petigura, Steven Giacalone, Joseph M. Akana Murphy, Corey Beard, Ashley Chontos, Fei Dai, Judah Van Zandt, Jack Lubin, Malena Rice, Alex S. Polanski, Paul Dalba, Sarah Blunt, Emma V. Turtelboom, Ryan Rubenzahl, Casey Brinkman
Figure caption:  Phase-folded RVs (red) and the RadVel (Fulton et al. 2018) fit to the RVs (blue) for Kepler-105b (left) and Kepler-105c (right). The RadVel two-planet fit without a GP yielded a 4σ detection of Kepler-105b (10.7 ± 2.8 M ⊕) but did not strongly detect Kepler-105c, despite imposing a planetary signal at its known orbital period. Thus, we can only place a 95% upper limit of 4.6 M ⊕ on the mass of Kepler-105c based on only the RVs.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Schematic of the network architecture. A single donut is passed through a convolutional neural network (CNN), generating a set of image features. These features are concatenated with a flag that indicates if the donut is intra-/extra-focal, the field angle of the source, and the effective wavelength of the observation. A dense neural network then estimates the Zernike coefficients associated with the optical wave front.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Example of donuts simulated with Batoid and Galsim. This set represents the diversity of the simulation: the simulated donuts have varying S/N, some are sharply vignetted by the Rubin camera (top right and bottom left), some are blended with a single other donut, and a small fraction are blended with many donuts.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Comparing the increase in PSF FWHM due to wave-front aberrations for 1000 simulated stars with random Zernike amplitudes. The x-axis is the increase in FWHM as measured from the simulated images, while the y-axis is the value estimated from our weighted Zernike scheme. The dashed line indicates perfect correspondence. The two methods agree for FWHM increases below 0.″25. Above this level, the weighted Zernike scheme overestimates the increase in FWHM.