adsabs/AstroCLIMB huggingface dataset:
Paper: Architectures of Compact Super-Earth Systems Shaped by Instabilities
Authors: Max Goldberg, Konstantin Batygin
Figure caption: Mass ratios and orbital period ratios of five well-characterized resonant chains. Center: colored points represent adjacent pairs of planets and are placed according to mass and orbital period ratio computed from outside in. Colored lines connect adjacent pairs in the same system, and horizontal black lines mark orbital resonances. Adjacent pairs missing at least one measured mass were discarded. Top: kernel density estimates of the distribution of mass ratio for the five resonant chains (red) vs. all sub-Jovian systems (gray). Right: histogram of period ratios of adjacent planets with the same color scheme as the top panel. Overall, resonant chains exhibit tighter clustering in both period ratios and mass ratios than the overall sample of sub-Jovian exoplanets.
Paper: Architectures of Compact Super-Earth Systems Shaped by Instabilities
Authors: Max Goldberg, Konstantin Batygin
Figure caption: Runs of 50 integrations of nearly the same initial conditions, with N = 11, ﹩\overline{m}\sim 10{M}_{\oplus }﹩, and initial resonance 4:3, but differing initial mass dispersion ﹩{ \mathcal D }﹩. The dashed line marks the evolution for run 9, which has different initial conditions (see Table 2). The red and black horizontal lines represent ﹩{ \mathcal D }﹩ for the resonant chains from Section 2 and all systems, respectively. For the run starting around ﹩{ \mathcal D }\approx 0.35﹩, plotted darker in blue, translucent vertical lines indicate the time of a collision, which triggers a change in ﹩{ \mathcal D }﹩.
Paper: Architectures of Compact Super-Earth Systems Shaped by Instabilities
Authors: Max Goldberg, Konstantin Batygin
Figure caption: Eight collisional outcomes for the same initial system with N = 11, ﹩\overline{m}=8.6{M}_{\oplus }﹩, initial resonance 4:3, and initial mass dispersion ﹩{ \mathcal D }\approx 0.1﹩. For each planet, the semimajor axis a, pericenter distance a(1 − e), and apocenter distance a(1 + e) are plotted in the same color. When two planets collide, the traces retain the color of the inner planet. Instability-driven evolution leads to wider orbital spacing, while retaining a degree of mass uniformity that is compatible with the data.
Paper: Architectures of Compact Super-Earth Systems Shaped by Instabilities
Authors: Max Goldberg, Konstantin Batygin
Figure caption: Collisional energetics of impacts in our simulations. Left panel: the distribution of the relative speed just before a collision, scaled by the escape velocity of the new planet. Collisions with V imp/V esc < 1 are expected to be perfect mergers. One event with V imp/V esc ≈ 12.4 has been omitted for clarity. Right panel: the distribution of specific collision energy to the energy required for catastrophic disruption. The event omitted from the left panel lies just below ﹩Q/{Q}_{D}^{* }=1﹩.
Paper: Architectures of Compact Super-Earth Systems Shaped by Instabilities
Authors: Max Goldberg, Konstantin Batygin
Figure caption: Cumulative frequency of period ratios for the postinstability synthetic systems (colored lines) and real systems (black line). Blended samples are constructed by mixing the two populations of low- and high-mass planets in the listed fractions.
Paper: Architectures of Compact Super-Earth Systems Shaped by Instabilities
Authors: Max Goldberg, Konstantin Batygin
Figure caption: Period ratios of outer planet pairs and inner planet pairs for the well-characterized systems in Weiss et al. (2018; left) and synthetic systems (right). In the right panel, blue and green dots correspond to the low-mass and high-mass samples, respectively. The Pearson r correlation between the orbital period ratios is statistically significant (p < 10−4) in both cases.
Paper: Setigen: Simulating Radio Technosignatures for the Search for Extraterrestrial Intelligence
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Steve Croft, John Hoang, Cherry Ng, Danny C. Price, Sofia Sheikh, Zihe Zheng
Figure caption: Radio spectrogram plots created from setigen frames. A: Frame with only synthetic chi-squared noise. B: Frame from panel (A) with an injected synthetic signal at S/N = 30. C: “Real” GBT observation of Voyager I carrier signal at the X band. D: Frame from panel (C) with an injected synthetic signal at S/N = 1000, with the same drift rate as the injected signal in panel (B).
Paper: Setigen: Simulating Radio Technosignatures for the Search for Extraterrestrial Intelligence
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Steve Croft, John Hoang, Cherry Ng, Danny C. Price, Sofia Sheikh, Zihe Zheng
Figure caption: Basic layout of a voltage pipeline written using setigen.voltage.
Paper: Setigen: Simulating Radio Technosignatures for the Search for Extraterrestrial Intelligence
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Steve Croft, John Hoang, Cherry Ng, Danny C. Price, Sofia Sheikh, Zihe Zheng
Figure caption: Spectrogram derived from synthetic raw voltages, showing the edge of the coarse channel bandpass shape and a bright, slightly drifting cosine signal. The top panel shows an integrated profile, showing the PFB scalloping loss toward the left and the synthetic signal toward the right.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Comparison of the retrieved LDCs u 1 and u 2 from the TESS data with the one calculated from the model stellar atmospheres using the code provided by Espinoza & Jordán (2015). In the upper panels, the y-axis represents the theoretical LDCs, while the x-axis shows the empirical values of LDCs. The black dashed line is the line of equality between the x- and y-axes. The lower panels show the distribution of residuals between the theoretical and empirical LDCs.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Comparison of the retrieved LDCs u 1 and u 2 from the TESS data with the SPAM LDCs. The latter made use of nonlinear LDCs from the code provided by Espinoza & Jordán (2015). In the upper panels, the y-axis represents the SPAM LDCs, while the x-axis shows the empirical values of LDCs. The black dashed line is the line of equality between the x- and y-axes. The lower panels show the distribution of residuals between the SPAM and empirical LDCs.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Comparison of the retrieved u 1 and u 2 coefficients from the TESS data with the one calculated from the model stellar atmospheres using tabulated values from Claret (2017) using the r-method and q-method.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Comparison of the retrieved u 1 and u 2 coefficients from the TESS data with the SPAM LDCs that made use of tabulated values of nonlinear LDCs from Claret (2017) using the r-method and q-method.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Comparison of the retrieved LDCs u 1 and u 2 from the TESS data with the SPAM LDCs. The latter made use of nonlinear LDCs from the code provided by Claret (2017). In the upper panels, the y-axis represents the SPAM LDCs, while x-axis shows the empirical values of LDCs. The black dashed line is the line of equality between the x- and y-axes. The lower panels show the distribution of residuals between the SPAM and empirical LDCs.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Comparison of the retrieved u 1 from the TESS data with the one calculated from the model stellar atmospheres using the tabulated values from Claret (2017). In the upper panels, the y-axis represents the theoretical LDCs, while the x-axis shows the empirical values of LDCs. The black dashed line is the line of equality between the x- and y-axes. The lower panels show the distribution of residuals between the theoretical and empirical LDCs.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Temperature variation of offsets in u 1 and u 2 when, theoretically, LDCs are calculated using LDCs provided by Claret (2017). The dashed–dotted lines show the best-fit model to the residuals.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Third transit of WASP-7b observed by TESS in Sector 27. An event suggestive of a spot-crossing event is seen about 24 minutes before mid-transit.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Same as Figure 10 but using SPAM LDCs.
Paper: Investigating the Baryon Cycle in Interacting Dwarfs with the Very Large Array and Pan-STARRS
Authors: N. Luber, Sarah Pearson, Mary E. Putman, Gurtina Besla, Sabrina Stierwalt, Joel P. Meyers
Figure caption: Left: the measured H I mass as a function of expected H I mass for the 10 systems in the P16 sample (black outlined circles), the Swaters et al. (2002) sample (black outlined stars), and the three dwarf systems NGC 3264, the square, NGC 3664, the triangle, and UGC 4638, the diamond. For all systems except for UGC 4638, the H I measurements are from single-dish telescopes. The expected value is derived through the H I mass to B-band optical radius relationship for dwarf galaxies in Swaters et al. (2002), using Equation (1) and the values from Section 4. The gray shaded region illustrates the ±1σ error on the fit calculated from the 73 isolated dwarf galaxies with H I masses in the range 107.5–10.0 M ⊙ in Swaters et al. (2002). Note that this figure only shows those galaxies with an observed H I mass greater than 108.7 M ⊙. The dwarf systems presented in this paper and the dwarf pairs from P16 do not appear significantly H I deficient when compared to the Swaters et al. (2002) sample of isolated dwarfs. Right: the relationship between measured single-dish H I masses and interferometric H I masses for the same systems. The interferometric measurements for the P16 sample come from their Table A2 and the single-dish measurements are compiled from the literature (Bottinelli et al. 1978; Shostak & Allen 1980; Richter et al. 1994; Putman et al. 2003; Koribalski et al. 2004; Koopmann et al. 2008; Matthews & Uson 2008). The values for NGC 3264 and NGC 3664 are those reported in Table 3. The single-dish masses are generally larger than the interferometric masses, which means there is significant extended gas in these systems.
Paper: Investigating the Baryon Cycle in Interacting Dwarfs with the Very Large Array and Pan-STARRS
Authors: N. Luber, Sarah Pearson, Mary E. Putman, Gurtina Besla, Sabrina Stierwalt, Joel P. Meyers
Figure caption: The neutral hydrogen morphology (left) and kinematics (right) for the NGC 3664 (top), NGC 3264 (middle), and UGC 4638 (bottom) dwarf systems, overlaid on Pan-STARRS r-band images (Chambers et al. 2016). The magenta lines correspond to column densities of, at top, 0.13, 0.40, 1.20, 3.60, 10.8, and 15.00 × 1020 atoms cm−2; in the middle, 0.35, 1.3, 2.5, 5.0, 10.0, and 11.9 × 1020 atoms cm−2; and at bottom, 1.5, 3, 4.5, 6, 7.5, 9, 10.5, and 12 × 1020 atoms cm−2. The black contour in all plots corresponds to a column density of 7 × 1019 atoms cm−2. The blue arrows point to the location of the dwarf members in each system. All images are oriented with north pointing up and east pointing left, and the beams are the hatched ellipses appearing in the southwest corners.
Paper: Investigating the Baryon Cycle in Interacting Dwarfs with the Very Large Array and Pan-STARRS
Authors: N. Luber, Sarah Pearson, Mary E. Putman, Gurtina Besla, Sabrina Stierwalt, Joel P. Meyers
Figure caption: Position−velocity slices taken along the H I morphological and kinematic major axis for (left) NGC 3664A, the barred Magellanic primary galaxy in the NGC 3664 system, (middle) the entire NGC 3264 system, and (right) the entire UGC 4638 system. In all cases the contours are adjusted to best trace out the extended emission. The position–velocity slices are taken over the position angles, where the position angle is, measured clockwise going north−south with 0° being north, 48°, 5°, and 62°, for NGC 3664A, the NGC 3264 system, and the UGC 4638 system, respectively. The velocity offset axis is centered at the systemic velocity for each system. In each case, the position–velocity slices do not show the characteristic flattening out at a high offset from positional center. The white circle in the slice for NGC 3264 (middle) is the approximate location of the secondary galaxy, and the gas outside of this circle is all from the primary dwarf. The dense concentration of gas in the right panel represents the positions of the galaxies in the UGC 4638 system.
Paper: Investigating the Baryon Cycle in Interacting Dwarfs with the Very Large Array and Pan-STARRS
Authors: N. Luber, Sarah Pearson, Mary E. Putman, Gurtina Besla, Sabrina Stierwalt, Joel P. Meyers
Figure caption: Left: a zoom-in on the Pan-STARRS r-band image of the UGC 4638 dwarf triplet. The gray scale is logarithmic, and the window has a physical size of 28.3 × 23.8 kpc. We clearly see extended diffuse starlight coming off of the primary galaxy (lower left corner), which is similar to the diffuse extended starlight from the NGC 4490 dwarf in Pearson et al. (2018). We also see clumpy star formation north of the primary, as well as diffuse starlight extending from the two smaller dwarfs in the central west and northwest (upper right) part of the image. Right: same as left, but showing a Pan-STARRS i-, r-, and g-band composite image of the UGC 4638 triplet, with the color scale from red to blue corresponding to the intensity of the bands i, r, and g, in that order, with the transfer function weighted more toward the g band such that fine color distinctions can be made. This image reveals that the diffuse stellar extensions follow the overall color distribution of the galaxies and are therefore likely associated with the triplet. The thin, dense stellar feature between the three dwarfs is redder and appears to have a central bulge. It is therefore likely a background galaxy.
Paper: Investigating the Baryon Cycle in Interacting Dwarfs with the Very Large Array and Pan-STARRS
Authors: N. Luber, Sarah Pearson, Mary E. Putman, Gurtina Besla, Sabrina Stierwalt, Joel P. Meyers
Figure caption: Ultraviolet images for (top) NGC 3664, (middle) NGC 3264, and (bottom) UGC 4638 2.′58. The images are taken from the Galaxy Evolution Explorer (GALEX) Allsky Imaging Survey (AIS; Bianchi et al. 2014). In each image, the transfer function is the native color map produced by the GALEX AIS team, as output by the Aladin Sky Atlas (Bonnarel et al. 2000; Boch & Fernique 2014).
Paper: Investigating the Baryon Cycle in Interacting Dwarfs with the Very Large Array and Pan-STARRS
Authors: N. Luber, Sarah Pearson, Mary E. Putman, Gurtina Besla, Sabrina Stierwalt, Joel P. Meyers
Figure caption: The H I morphology overlaid on a Pan-STARRS r-band image of the UGC 4638 dwarf triplet (bottom) and the nearby UGC 4640 spiral galaxy (top). The contours correspond to H I column density levels of 0.93, 1.85, 3.70, 5.55, 7.40, and 8.79 × 1020 atoms cm−2.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: IM parameter distributions across instruments for per-wavelength instrument model fits. The blue vertical line marks the center of the prior used in the initial MCMC fitting. The x-axis scale has been selected to visualize the central distribution and thus cuts off outliers, which is discussed in the text. A maximum likelihood fitted Gaussian, Lorentzian, and Student’s t distributions are displayed. The Student’s t distribution is very close to the Lorentzian distribution and provides the highest quality of fit. As a result of the outliers and empirical tail width, the fitted Gaussian distribution is significantly wider than the central distribution suggests. Additionally, the Gaussian distribution fitted only to the middle 90% of the distribution significantly underestimates the tail probabilities and fits the central distribution worse than the Student’s t.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: Empirical white-light IM parameter distributions across instruments compared to the maximum likelihood Gaussian (green) and Lorentzian (yellow) distribution fits. The x-axis range for each parameter has been set so that the central distribution can be clearly seen. This results in outliers being cut off. The behavior of these outliers will be discussed in the text. The distribution of previously used priors is represented by the dashed lines. This prior distribution, as evidenced by the width of the median prior, is consistently wider than the empirical distribution for the visit slope and orbit intercept parameters. Additionally, the orbit slope priors also show a too wide fit for G141 and G750L with G430L orbit slope the only potential exception to this.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: IM estimates for the white-light (WL) light curves plotted against the mean of the spectrum IM estimates with the standard deviation of spectrum IM estimates for that target displayed as well. The blue line represents y = x and thus if a point lies along it, this means that the spectrum value is equal to the white-light value. From this, it can be seen that for almost all targets, the white-light estimate is in close agreement to the average of the per target spectrum estimates. From this we can conclude that the spectrum estimates are not independent from the corresponding white-light estimate.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: The distribution of forward-modeled IM samples from the spectrum parent distribution for HAT-P-26 b at 1.137 microns for G141. The confidence intervals (CIs) demonstrate the magnitude of the effect the sampled systematics have on the light curve. Note that HAT-P-26 b has data from multiple visits and the overlapping CIs in the plot represent the estimates for the separate visits as each had slightly different timing data and thus different forward-modeled IM distributions.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: Histograms for 16 random samplings of a Student’s t distribution with 1.6 degrees of freedom at a sample size of 100. This plot highlights the range of possible behavior seen under a low degree-of-freedom t-distribution assumption. The x-axis is fixed across the plots so some outlier points are cut off.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: The orbit intercept parameter distribution for the first visits of HD 97658 b (top) and GJ 9827 d (bottom). Fitted Lorentzian and Gaussian distributions are superimposed and the K-S distributional fit test P value is included in the legend.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: Nontruncated histogram of all fitted parameters for the G750L visit slope. Vertical tick marks are added for each parameter estimate to display both outliers and the central distribution.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: Example behavior of the IM on a synthetic light curve. The placement and balance of the timing parameters in the formulation is overlayed. This figure represents just one set of potential IM parameters, and the synthetic parameters chosen were selected for their clarity of displaying IM effects.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: Top: distribution of the delay and τ parameters across the three instruments. Bottom: residuals of the previous naive starting value compared to the new single-parameter starting-value estimator.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: Orbit slope parameter distribution for GJ 1214 across the wavelengths of G141 with a plotted regression line fit between wavelengths and estimates for each visit. The legend identifies the north and south scanned light-curve data for the seven visits. If the exoplanet target’s characteristics were a primary influence on the IM parameters, each visit would be expected to have similar linear and mean characteristics, but the plot clearly shows that this assumption does not hold true for GJ 1214. This implies that the exoplanet characteristics are not a significant influence if any influence exists at all.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: Top: visit slope estimate distribution by wavelength for two visits of HAT-P-38 b on G141 showing one with a weak linear signal and one with a strong negative correlation to wavelength. The R 2 value of the visit fit is shown in the legend. Bottom: visit slope estimates for HAT-P-17 b on G141. This target exemplified the behavior of targets that had nonlinear parameter trends.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: The distribution of the light-curve residual standard deviation metric per wavelength for the the three filters (top: G141; middle: G430L; bottom: G750L). Left axis scales differ between the three filters. The stellar spectra for HAT-P-26 and WASP-69 are plotted for G430L and G750L to visualize correlation between stellar features and residual features.
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: Histogram of average RSDSN across targets observed by G141. 3.25 RSDSN appears to be the cutoff between the low RSDSN grouping and the extended tail of higher RSDSN outliers.