adsabs/AstroCLIMB huggingface dataset:
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: [X/H] vs. [Fe/H] for SAGA (gray points) and dwarf galaxy stars (blue is classical dSph, yellow is ultra-faint dwarf). J0931 + 0038 is shown as a large red square. The dotted line indicates [X/Fe] = 0, and the dashed line is the best fit to the SAGA stars that we use as an empirical ISM composition. Note that the comparison abundances have been shifted by the NLTE and evolutionary corrections for J0931 + 0038.
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: Light element ratios vs. initial mass for CCSNe (left column; HW10, G18, NKT13, LC12, LC18, E20, R18), HNe and PISNe (center column; HW10, G18, NKT13, HW02), and rotation velocity (right column; LC18 only). N and Na are not plotted for E20. In the right column, the same mass and metallicity at different rotation velocities are connected by solid lines (< 50 M ⊙) or dashed lines (≥ 50 M ⊙). These figures explain the first rows of Table 2.
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: Iron-peak element ratios vs. initial mass for CCSNe (left column; HW10, G18, NKT13, LC12, LC18, E20, R18), HNe and PISNe (center column; HW10, G18, NKT13, HW02), and rotation velocity (right column; LC18 only). In the right column, the same mass and metallicity at different rotation velocities are connected by solid lines (< 50 M ⊙) or dashed lines (≥ 50 M ⊙). These figures explain the middle rows of Table 2.
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: Kinematics of J0931 + 0038 (red star) compared to red giants observed by the SDSS-V halo program. Stars plausibly belonging to the GSE merger are highlighted in blue.
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: Results of grid search through CCSN, PISN, and HN models for different permutations of elements. The best-fit model is shown in the legend: dashed blue = CCSN, dotted orange = PISN, solid green = HN. Reduced χ 2 is shown in the legend. See text for details.
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: Chemical abundances of J0931 + 0038 compared to four other notable stars. LAMOST J1010 + 2358 has a pure signature of a PISN, while the other three are metal-poor stars whose compositions are currently best explained with HN models.
Paper: Constraints on Cosmological Coupling from the Accretion History of Supermassive Black Holes
Authors: Mark Lacy, Athena Engholm, Duncan Farrah, Kiana Ejercito
Figure caption: The allowed values of the cosmological coupling strength k (Equation (1)) and the Salpeter time (Equation (10)) t  S  for quasars assuming accretion-dominated growth of the supermassive black hole density. Left: assuming the GD07 estimate of ρ •(0), middle assuming the best estimate from this paper and right assuming the value from the peaks of the GWB posterior fits. The hatched blue regions represent the parameter space where the Salpeter time is too long to grow enough black holes at z = 4 to explain the observed luminosity function and the red regions are those where the Eddington ratio needs to exceed unity to do this. The yellow hatched regions are excluded based on the plausible range of 0.05 < η < 0.3.
Paper: New Horizons Venetia Burney Student Dust Counter Observes Higher than Expected Fluxes Approaching 60 au
Authors: Alex Doner, Mihály Horányi, Fran Bagenal, Pontus Brandt, Will Grundy, Carey Lisse, Joel Parker, Andrew R. Poppe, Kelsi N. Singer, S. Alan Stern, Anne Verbiscer
Figure caption: Left: the flight path of the New Horizons spacecraft up through 55 au with the minimum detectable mass represented in the color scale. The decrease in spacecraft speed with increasing distance results in a higher minimum detectable mass. New Horizons is heading along the ecliptic longitude λ NH ≃ 293° compared to the ISD inflow of λ ISD = 259°, indicated by the parallel upward-pointing arrows at the bottom. Therefore, ISDs impact SDC at an angle of α ≃ 23° off of normal (Bernardoni et al. 2022). ISDs currently impact SDC at 39 km s−1 while IDPs only impact at 14 km s−1. Therefore, despite their size difference, ISD impacts can be measured and interpreted as small IDPs (Bernardoni et al. 2022). Based on the current model, ISD assumed IDP size should not exceed 0.68 μm. Right: all noncoincident data up to 2023 July 25. Each detector has an independent mass threshold. For flux and density computation a common threshold was set at r  g  ≥ 0.63 μm (m ≥ 2.62 × 10−12 g) such that all of the detectors provide an equal statistical contribution to the calculated flux and density (Bernardoni et al. 2022). The gray blocks represent regions of exceptionally high thresholds due to high spacecraft activity during close encounters with Pluto and Arrokoth. Other periods of missing data are due to SDC being powered off for spacecraft operational reasons.
Paper: New Horizons Venetia Burney Student Dust Counter Observes Higher than Expected Fluxes Approaching 60 au
Authors: Alex Doner, Mihály Horányi, Fran Bagenal, Pontus Brandt, Will Grundy, Carey Lisse, Joel Parker, Andrew R. Poppe, Kelsi N. Singer, S. Alan Stern, Anne Verbiscer
Figure caption: Left: temporal variation due to PR drag of the semimajor axis (a) and eccentricity (b) of olivine-type particles with β = 0.3 starting with initial a = 70 au and e = 0.4 (blue lines) and β = 0.4 with initial a = 120 au and e = 0.7 (red). These initial conditions were motivated by the peak of the a and e distributions as illustrated in Figure 4. The shaded regions show the range of their radial motion a(1 − e) ≤ r ≤ a(1 + e). Right: temporal variation over 2 Myr of the semimajor axis (c), eccentricity (d) dotted lines, and radius (d) bottom solid lines of 1 (blue line) and 5 μm (red) photo-sputtered ice particles, launched with an initial semimajor axis a = 45 au and eccentricity e = 0.1. Small ice grains continuously gain energy and drift outwards out of the solar system, while bigger particles initially drift inward until their mass loss results in a large enough β to reverse the direction of their drift and eventually also leave the solar system.
Paper: New Horizons Venetia Burney Student Dust Counter Observes Higher than Expected Fluxes Approaching 60 au
Authors: Alex Doner, Mihály Horányi, Fran Bagenal, Pontus Brandt, Will Grundy, Carey Lisse, Joel Parker, Andrew R. Poppe, Kelsi N. Singer, S. Alan Stern, Anne Verbiscer
Figure caption: (a) The semimajor axis, a, distribution of the low-inclination (i ≤ 10°) KBOs (blue line), and of the newly released particles, a*, for β = 0.3 (green) and 0.4 (red); (b) The eccentricity distributions of parent bodies, e, and the new dust particles, e*; (c) the radial density distributions, each curve normalized to the total number of KBOs (2320) or dust particles (2290 and 2200); (d) the fraction of the ejected particles generated from all low-inclination KBOs as a function of β. The dots show the results of a full numerical solution of the equation of motion for various radii (measured in μm) olivine-type particles (Poppe 2016).
Paper: New Horizons Venetia Burney Student Dust Counter Observes Higher than Expected Fluxes Approaching 60 au
Authors: Alex Doner, Mihály Horányi, Fran Bagenal, Pontus Brandt, Will Grundy, Carey Lisse, Joel Parker, Andrew R. Poppe, Kelsi N. Singer, S. Alan Stern, Anne Verbiscer
Figure caption: SDC flux estimates for particles with a radius greater than 0.63 μm from 1 to 55 heliocentric au. Each point, with 1σ error bars, is an average of the flux measured by each detector across each 3 au traversed by the New Horizons spacecraft. The orange curve represents the ISD flux values calibrated from Ulysses measurements (Bernardoni et al. 2022). While ISD grains are much smaller (∼0.28 μm), they are also traveling at higher relative velocities and, as a result, SDC interprets them as small IDPs (Bernardoni et al. 2022). The red line shows a model from Poppe (2016) that is normalized to the SDC measurements and assumes SDC is impacted only by IDPs. The black line is a sum of the orange and red models to provide a more representative model of the total flux that SDC is measuring up to 42 au.
Paper: New Horizons Venetia Burney Student Dust Counter Observes Higher than Expected Fluxes Approaching 60 au
Authors: Alex Doner, Mihály Horányi, Fran Bagenal, Pontus Brandt, Will Grundy, Carey Lisse, Joel Parker, Andrew R. Poppe, Kelsi N. Singer, S. Alan Stern, Anne Verbiscer
Figure caption: SDC density measurements above four cutoff sizes: 0.63, 0.68, 0.82, and 1.50 μm. The overall shape and upward trend, within error bars, is consistent between 0.63, 0.68, and 0.82 μm. Above 1.50 μm, there are insufficient detections to make any confident claims about the density of the grains throughout the New Horizons flight path. The 0.63, 0.82, and 1.50 μm cutoffs are chosen based on the onboard threshold table for different flight conditions, while the 0.68 μm cutoff is selected to observe the flux without any potential effects from interstellar grains.
Paper: The First TESS Self-lensing Pulses: Revisiting KIC 12254688
Authors: Nicholas M. Sorabella, Silas G. T. Laycock, Dimitris M. Christodoulou, Sayantan Bhattacharya
Figure caption: Synthetic light curves of a self-lensing binary system containing a 1.1M ⊙ star with a radius of 1.5R ⊙ and a 0.35M ⊙ WD (left panels) or a 7M ⊙ BH (right panels), with orbital periods of 270 and 9 days, respectively. The top panels simulate the light curves as viewed by the 475 s (∼8 minutes) cadence TESScut exposures, and the bottom panels are the same light curves as viewed by the 30 minute cadence of Kepler.
Paper: The First TESS Self-lensing Pulses: Revisiting KIC 12254688
Authors: Nicholas M. Sorabella, Silas G. T. Laycock, Dimitris M. Christodoulou, Sayantan Bhattacharya
Figure caption: Binned light curves of KIC 12254688 for TESS Sectors 41 and 56, respectively. We have zoomed in to the locations of the pulses (near the middle of each plot) so that they are more easily noticeable. The midpoint of the Sector 41 pulse is at 2424.734 BTJD and Sector 56 is at 2843.449 BTJD. Sector 56 has a small downward trend to the right of the pulse that we subsequently remove using a second-order polynomial fit, in which we exclude the pulse itself.
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: Best-fit results of fitting abundances of J0931 + 0038 (red points) combining CCSNe, HNe, and PISNe with Type Ia and ISM. Same lines as Figure 12. References: Bravo et al. (2019, B19), E20, Fink et al. (2014, F14), G18, HW10, R18. See Section B.3 for discussion.
Paper: The First TESS Self-lensing Pulses: Revisiting KIC 12254688
Authors: Nicholas M. Sorabella, Silas G. T. Laycock, Dimitris M. Christodoulou, Sayantan Bhattacharya
Figure caption: Our joint fits to the phase folded light curves of KIC 12254688 from TESS (top left) and Kepler (bottom left) with updated radial velocity data (right panels) from Masuda et al. (2020). The orange lines represent the 95% confidence intervals, and the dark gray lines represent the 50th percentile estimates.
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: Best-fit results of fitting abundances of J0931 + 0038 (red points) combining CCSNe, HNe, and PISNe with each other. The large panels shows the fits in [X/H], while the smaller panels indicate the residual (data–model). The blue and orange lines indicate two different models described in the top left legend of each panel, and the black line indicates their sum. The top right corner of the large panels shows reduced chi-squares and the error-normalized MAD. References: E20, G18, HW02, HW10, N13, R18. See Section B.3 for discussion.
Paper: The First TESS Self-lensing Pulses: Revisiting KIC 12254688
Authors: Nicholas M. Sorabella, Silas G. T. Laycock, Dimitris M. Christodoulou, Sayantan Bhattacharya
Figure caption: Detrended light curves of KIC 12254688 from TESS Sectors 41 and 56. The projected pulse midpoints are expected to lie at 2424.734 BTJD and 2843.449 BTJD in Sectors 41 and 56, respectively.
Paper: The First TESS Self-lensing Pulses: Revisiting KIC 12254688
Authors: Nicholas M. Sorabella, Silas G. T. Laycock, Dimitris M. Christodoulou, Sayantan Bhattacharya
Figure caption: The 1D and 2D projections of the posterior probability distributions of the model parameters for the TESS data fit. The returned values are obtained from the 16th, 50th, and 84th percentiles, utilizing the final 4000 steps of 100 independent MCMC walker chains.
Paper: The First TESS Self-lensing Pulses: Revisiting KIC 12254688
Authors: Nicholas M. Sorabella, Silas G. T. Laycock, Dimitris M. Christodoulou, Sayantan Bhattacharya
Figure caption: As in Figure A1, but for the Kepler data fit.
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: [X/Fe] (in NLTE when possible) vs. atomic number. The gray box plots for each element X are [X/Fe] from 4866 stars in the SAGA literature compilation (Suda et al. 2008) with −3.5 < [Fe/H] < −1.5 to maximize the intrinsic [X/Fe] range. The SAGA abundances have been moved to the Magg et al. (2022a) abundance scale, and they have been shifted by the NLTE correction of J0931+0038 in Table 1. The box-and-whisker plots indicate the median and 25th–75th percentile with the box and the 1st–99th percentile with the whiskers. The abundances of Na, K, Sc, and Ba are among the lowest abundances of these elements ever measured. The uncertainty for Fe is the overall metallicity uncertainty, while for other elements, it is the precision relative to Fe. Note that the plotted Li value is [Li/Fe], and A(Li) = 1.15.
Paper: Spectacular Nucleosynthesis from Early Massive Stars
Authors: Alexander P. Ji, Sanjana Curtis, Nicholas Storm, Vedant Chandra, Kevin C. Schlaufman, Keivan G. Stassun, Alexander Heger, Marco Pignatari, Adrian M. Price-Whelan, Maria Bergemann, Guy S. Stringfellow, Carla Fröhlich, Henrique Reggiani, Erika M. Holmbeck, Jamie Tayar, Shivani P. Shah, Emily J. Griffith, Chervin F. P. Laporte, Andrew R. Casey, Keith Hawkins, Danny Horta, William Cerny, Pierre Thibodeaux, Sam A. Usman, João A. S. Amarante, Rachael L. Beaton, Phillip A. Cargile, Cristina Chiappini, Charlie Conroy, Jennifer A. Johnson, Juna A. Kollmeier, Haining Li, Sarah Loebman, Georges Meynet, Dmitry Bizyaev, Joel R. Brownstein, Pramod Gupta, Sean Morrison, Kaike Pan, Solange V. Ramirez, Hans-Walter Rix, José Sánchez-Gallego
Figure caption: Spectrum of J0931+0038 (black line and gray shaded uncertainty band). For comparison, two stars with similar stellar parameters are plotted: a MIKE spectrum of a normal star from our SDSS sample in purple and a Keck/HIRES spectrum of the r-process-enhanced star BD +17°3248 in blue. Visible by eye are the low abundances of Na, Ti, Sc, and Ba; the enhancement in Sr, Y, Mn, Ni, and Zn; and the detected Mo, Ru, and Pd lines. BD +17°3248 is highly r-process-enhanced, but J0931+0038 has stronger lines of Sr, Mo, Ru, and Pd, while the Ba line is barely detected (it is blended with a weak Zr line).
Paper: Tilted Circumbinary Planetary Systems as Efficient Progenitors of Free-floating Planets
Authors: Cheng Chen, Rebecca G. Martin, Stephen H. Lubow, C. J. Nixon
Figure caption: Stability maps of a two-planet circumbinary system with e b = 0.0 (left panels) and 0.8 (right panels). The planetary system consists of one Earth-mass planet and one Jupiter-mass planet. The Jupiter-mass planet is the outer planet in the top panels and is the inner planet in the bottom panels. The inner planet has initial semimajor axis a p1 = 5 a b, and the y-axis is Δ with an interval of 0.1, while the x-axis is the initial inclination of two planets with an interval of 2.°5. The four horizontal dashed lines represent the 2:1 (cyan), 5:2 (orange), 3:1 (pink), and 4:1 (red) MMRs between the two planets. The four different colors of pixels represent two-planet stable cases (blue), the inner planet survived cases (green), the outer planet survived cases (red), and both planet unstable cases (white).
Paper: Discovery of a Large-scale H I Plume in the NGC 7194 Group
Authors: Mina Pak, Junhyun Baek, Joon Hyeop Lee, Aeree Chung, Matt Owers, Hyunjin Jeong, Eon-Chang Sung, Yun-Kyeong Sheen
Figure caption: The spectra of three blue knots (B1–B3) observed from the Doyak 1.8 m telescope of Bohyunsan Optical Astronomy Observatory long-slit spectrograph. We detected Hα emission centered at 7496, 7872, and 7766 km s−1, respectively. Instrumental flux is shown since calibration is not applied since signal-to-noise of the continuum is not sufficient enough to analyze flux calibration.