adsabs/AstroCLIMB huggingface dataset:
Paper: Challenging the Disk Instability Model. I. The Case of YZ LMi
Authors: Raymundo Baptista, and Wagner Schlindwein
Figure caption: Top: disk and gas stream midplane densities as a function of mass-transfer rate for a disk radius of Rd = 0.65 RL1. Red lines show the MTIM disk midplane density ρd0(Rd) for α = 3.5 (solid), 3 and 4 (dashed), while blue lines show the DIM disk midplane densities ρ+(Rd), ρ−(Rd) (dashed) and ρmed(Rd) (solid) for αc = 0.02, αh = 0.1, and γ = 0.27. Black lines show the gas stream midplane density ρs0(Rd) for T2 = 1900 K (solid), 1000 K, and 3700 K (dashed). Vertical dotted lines mark the mass-transfer rate ranges ﹩{\dot{M}}_{2}(\mathrm{quiescence})=(1.3-6.3)\times {10}^{15}\,{\rm{g}}\,{{\rm{s}}}^{-1}﹩ (Section 5) and ﹩{\dot{M}}_{2}(\mathrm{outburst})=16\,{\dot{M}}_{2}(\mathrm{quiescence})=(2.1-10.0)\times {10}^{16}\,{\rm{g}}\,{{\rm{s}}}^{-1}﹩. Bottom: the penetration radius (in units of RL1) as a function of ﹩{\dot{M}}_{2}﹩ for α = 3.5. Labels depict the corresponding T2 value.
Paper: Challenging the Disk Instability Model. I. The Case of YZ LMi
Authors: Raymundo Baptista, and Wagner Schlindwein
Figure caption: Disk and gas stream midplane densities as a function of disk radius. Red lines show the MTIM disk densities ρd0(R) for α = 3.5, ﹩{\dot{M}}_{2}(\mathrm{quiescence})=3\times {10}^{15}\,{\rm{g}}\,{{\rm{s}}}^{-1}﹩ (solid), and ﹩{\dot{M}}_{2}(\mathrm{outburst})=4.8\times {10}^{16}\,{\rm{g}}\,{{\rm{s}}}^{-1}﹩ (dashed), while blue lines show the DIM disk densities ρ+(R), ρ−(R) (dashed), and ρmed(R) (solid) for αc = 0.02, αh = 0.1, and γ = 0.27. Black lines show the gas stream midplane density ρs0(R) for ﹩{\dot{M}}_{2}(\mathrm{quiescence})﹩ (solid) and ﹩{\dot{M}}_{2}(\mathrm{outburst})﹩ (dashed). Labels depict the corresponding T2 values. Vertical ticks mark the position of the penetration radius, Rp, at each ﹩{\dot{M}}_{2}﹩ for T2 = 1900 K.
Paper: An Atomic Spectral Survey of WASP-76b: Resolving Chemical Gradients and Asymmetries
Authors: Aurora Y. Kesseli, I. A. G. Snellen, N. Casasayas-Barris, P. Mollière, and A. Sanchez-Lopez
Figure caption: Results of our test on the observability for each element and select ions that have absorption lines at optical wavelengths for (a) a temperature of 2500 K and (b) 4000 K. We only show a portion of the periodic table for the ions (bottom of both panels (a) and (b)) as these ions are the only ones that have significant absorption lines in the optical. Neutral atoms and ions that do not have any absorption lines above the expected continuum, set by the opacity due to collision-induced absorption and H−, are shown in gray. Elements and ions with higher observability have deeper and more numerous absorption lines and are abundant enough that these lines significantly contribute to the overall opacity. For both cases, transition metals, alkali metals, and alkaline metals are particularly observable.
Paper: An Atomic Spectral Survey of WASP-76b: Resolving Chemical Gradients and Asymmetries
Authors: Aurora Y. Kesseli, I. A. G. Snellen, N. Casasayas-Barris, P. Mollière, and A. Sanchez-Lopez
Figure caption: Example model atmospheres showing the relative transit depth vs. wavelength for Na and Cr in WASP-76b. We show how changing the two free parameters, temperature and pressure at the opacity base due to continuum opacity sources (Pcloud), change the relative absorption of each species. At higher temperatures, more absorption lines are present, and the scale height of the atmosphere is increased. When the base opacity is moved higher in the atmosphere, the weaker lines and line wings are hidden. Moving the base opacity higher in the atmosphere has the same effect as decreasing the abundance. The results we present for each species use a temperature of 3000 K and a base opacity at 1 mbar (unless stated otherwise), but in Section 6.1 we discuss how different models might affect our results.
Paper: An Atomic Spectral Survey of WASP-76b: Resolving Chemical Gradients and Asymmetries
Authors: Aurora Y. Kesseli, I. A. G. Snellen, N. Casasayas-Barris, P. Mollière, and A. Sanchez-Lopez
Figure caption: Example showing how we combined the two nights and the resulting cross-correlation grids for Cr I. (a) The resulting cross-correlation grid from night 1. Each row in the 2D cross-correlation grid is a separate cross-correlation function in time between an ESPRESSO spectrum and the atmospheric transition model for Cr, divided by the average out-of-transit cross-correlation function. The four blue horizontal lines from bottom to top show the start of ingress, the end of ingress, the start of egress and the end of egress, respectively. The green dashed line shows the expected exoplanet’s velocity. Black residuals near the exoplanet’s expected velocity are due to excess absorption from Cr in the exoplanet’s atmosphere. Any velocity offset from the planet’s expected position is due to wind and dynamics in the planet’s atmosphere and will be quantified in Section 6. White residuals near 0 km s−1 are stellar residuals due to a combination of the Rossiter–McLaughlin effect, center-to-limb variations, and low flux within the stellar Cr line cores, which causes increased noise near 0 km s−1. (b) Same as (a), but for night 2. (c) The two nights have been combined by interpolating each onto a uniform grid in phase space and averaging them together, weighting them by their average S/N and the number of spectra taken during the transit. (d) The central region between −10 and +10 km s−1 has been masked as a simple method to remove all of the pixels affected by the stellar residuals.
Paper: An Atomic Spectral Survey of WASP-76b: Resolving Chemical Gradients and Asymmetries
Authors: Aurora Y. Kesseli, I. A. G. Snellen, N. Casasayas-Barris, P. Mollière, and A. Sanchez-Lopez
Figure caption: Results of our cross-correlation analysis for all of the detected and tentatively detected atoms and ions. Left: for each atom, we show the 2D cross-correlation functions, as shown in panel (d) of Figure 3, except they have now been shifted to the rest frame of the planet using the expected Kp. Therefore, any excess absorption from the planet should appear as black residuals at 0 km s−1 (shown by a green line). Center: the many cross-correlation functions in the left panel have been averaged together at the start of the transit (ϕ = −0.04 to −0.02, turquoise) and end of the transit (ϕ = +0.04 to +0.02, dark purple) separately. The dashed vertical lines show the radial velocity of the center of a Gaussian that was fit to each average 1D cross-correlation function. Right: we also searched in Kp and vwind parameter space to assess the significance of the detection and to determine the Kp and vwind values that gave the highest significance detection. The black dotted lines show the expected parameters of the system neglecting atmospheric dynamics. In many cases the most significant values deviate from the expected values. Wardenier et al. (2021) found that this deviation can be explained by including global winds and condensation of the species on the morningside of the planet.
Paper: An Atomic Spectral Survey of WASP-76b: Resolving Chemical Gradients and Asymmetries
Authors: Aurora Y. Kesseli, I. A. G. Snellen, N. Casasayas-Barris, P. Mollière, and A. Sanchez-Lopez
Figure caption:                         Scatter plots showing the relations between the derived parameters from Table 2 for all of the species detected with an S/N> 5. Top right: the Kp that exhibits the peak S/N from the right-most plots in Figure 4 vs. the radial velocity difference. Top left: amplitude 1 divided by amplitude 2 (relative amplitude difference) vs. the radial velocity difference between the first and second half of the transit. Middle left: the temperature below which the atom or ion is expected to no longer exist vs. the radial velocity difference. The temperatures for the ions are where the species are expected to become mostly neutral (ionization temperature) and are estimated using an equilibrium chemistry code from Mollière et al. (2017) assuming a pressure of 10−4 bars. The temperatures for the neutral atoms are the temperatures where each is expected to condense into a solid and are taken from either Gao et al. (2020; Mg, Cr, Mn, Fe) or Lodders (1999; Li, Na) at a pressure of 10−4 bars. Lodders (2002) stated that V condenses about 200 K above Fe, and so we use this as our estimate for V condensation. We were unable to find a condensation temperature for Ni, and so we do not include it in this plot, but given its similar behavior to the other transition metals, we expect it to condense around similar temperatures (1300 to 1500 K). We assume uncertainties of 100 K for each of these temperatures. Middle right: same temperatures, but now plotted against the peak Kp. Bottom left: FWHM of the 1D cross-correlation functions vs. the radial velocity difference; or (bottom right) the peak Kp.
Paper: An Atomic Spectral Survey of WASP-76b: Resolving Chemical Gradients and Asymmetries
Authors: Aurora Y. Kesseli, I. A. G. Snellen, N. Casasayas-Barris, P. Mollière, and A. Sanchez-Lopez
Figure caption: Comparison between the expected observability for each atom or ion that was originally defined in Section 2 (shown as black x marks) and the S/N for the detected species (green squares) or upper limits at an S/N of 4 (purple squares) for all of the nondetections. The two y-axes have been normalized such that the Fe I signal’s S/N is equal to an observability of 1. Most of the species that are expected to be observable have a detection, but a few notable exceptions are present and are discussed in detail in the text.
Paper: An Atomic Spectral Survey of WASP-76b: Resolving Chemical Gradients and Asymmetries
Authors: Aurora Y. Kesseli, I. A. G. Snellen, N. Casasayas-Barris, P. Mollière, and A. Sanchez-Lopez
Figure caption:                         Kp vs. vwind maps for each neutral atom that we searched for, but did not detect. These maps are the same as those in the right panels of Figure 4. These are all considered nondetections, as none of them show an S/N ≥ 4 near the planet’s expected Kp and vwind value (shown by the dotted black lines). These plots show random noise peaks that often have S/Ns of 3 to 4, but we do not see any S/N peaks of 5, which is why we chose the cutoff of 5 for our detections and only consider S/N ≥ 4 signals as tentative.
Paper: An Atomic Spectral Survey of WASP-76b: Resolving Chemical Gradients and Asymmetries
Authors: Aurora Y. Kesseli, I. A. G. Snellen, N. Casasayas-Barris, P. Mollière, and A. Sanchez-Lopez
Figure caption: Same as Figure 7, but for the nondetections of each ion.
Paper: The Breakthrough Listen Search for Intelligent Life: Technosignature Search of Transiting TESS Targets of Interest
Authors: Noah Franz, Steve Croft, Andrew P.V. Siemion, Raffy Traas, Bryan Brzycki, Vishal Gajjar, Howard Isaacson, Matthew Lebofsky, David H.E. MacMahon, Danny C. Price, Sofia Z. Sheikh, Julia DeMarines, Jamie Drew, and S. Pete Worden
Figure caption: Sky map of all TESS TOIs (blue dots), with transiting TESS targets analyzed in this paper overlaid as red Xs. The gray shaded region is the zone above decl. −20° where BL targets are usually observed with the GBT; BL targets below this decl. are usually observed at the Parkes Observatory.
Paper: The Breakthrough Listen Search for Intelligent Life: Technosignature Search of Transiting TESS Targets of Interest
Authors: Noah Franz, Steve Croft, Andrew P.V. Siemion, Raffy Traas, Bryan Brzycki, Vishal Gajjar, Howard Isaacson, Matthew Lebofsky, David H.E. MacMahon, Danny C. Price, Sofia Z. Sheikh, Julia DeMarines, Jamie Drew, and S. Pete Worden
Figure caption: Fraction of the transit observed in the GBT observations. The blue bins represent all 66 cadences, while the hashed bins indicate a target that crosses the midpoint of its transit during the observation.
Paper: The Breakthrough Listen Search for Intelligent Life: Technosignature Search of Transiting TESS Targets of Interest
Authors: Noah Franz, Steve Croft, Andrew P.V. Siemion, Raffy Traas, Bryan Brzycki, Vishal Gajjar, Howard Isaacson, Matthew Lebofsky, David H.E. MacMahon, Danny C. Price, Sofia Z. Sheikh, Julia DeMarines, Jamie Drew, and S. Pete Worden
Figure caption: Histogram of the orbital periods of the observed targets.
Paper: The Breakthrough Listen Search for Intelligent Life: Technosignature Search of Transiting TESS Targets of Interest
Authors: Noah Franz, Steve Croft, Andrew P.V. Siemion, Raffy Traas, Bryan Brzycki, Vishal Gajjar, Howard Isaacson, Matthew Lebofsky, David H.E. MacMahon, Danny C. Price, Sofia Z. Sheikh, Julia DeMarines, Jamie Drew, and S. Pete Worden
Figure caption: Number of hits (gray) and events (black) vs. frequency. The frequency range (band) for each GBT receiver is represented by the colored regions; the (unshaded) notch filter regions (Lebofsky et al. 2019) at L and S bands are excluded from our analysis. Values for each band, with the number of cadences, are shown in Table 1. Note that there are a different number of cadences at each band so the number of hits and events plotted here should not be directly compared across bands.
Paper: The Breakthrough Listen Search for Intelligent Life: Technosignature Search of Transiting TESS Targets of Interest
Authors: Noah Franz, Steve Croft, Andrew P.V. Siemion, Raffy Traas, Bryan Brzycki, Vishal Gajjar, Howard Isaacson, Matthew Lebofsky, David H.E. MacMahon, Danny C. Price, Sofia Z. Sheikh, Julia DeMarines, Jamie Drew, and S. Pete Worden
Figure caption: Dynamic spectra (waterfall plots) of four representative events from the 634 event sample. Each plot is a vertical stack of the 6 scans making up an ABACAD cadence. The vertical axis shows the time since the start of each scan in the cadence, and the horizontal axis shows the frequency offset from the event’s starting frequency.
Paper: The Breakthrough Listen Search for Intelligent Life: Technosignature Search of Transiting TESS Targets of Interest
Authors: Noah Franz, Steve Croft, Andrew P.V. Siemion, Raffy Traas, Bryan Brzycki, Vishal Gajjar, Howard Isaacson, Matthew Lebofsky, David H.E. MacMahon, Danny C. Price, Sofia Z. Sheikh, Julia DeMarines, Jamie Drew, and S. Pete Worden
Figure caption: Left: histograms of hits (blue) and events (red) as a function of drift rate split up by receiver. The reported drift rate is normalized by the center frequency of the hit or event, to produce a value in units of nHz (e.g., 1 nHz = 1 Hz s−1 at 1 GHz). Right: histograms of hits (blue) and events (red) as a function of S/N split up by GBT receiver. Note that not all receivers observed the same number of targets.
Paper: The Breakthrough Listen Search for Intelligent Life: Technosignature Search of Transiting TESS Targets of Interest
Authors: Noah Franz, Steve Croft, Andrew P.V. Siemion, Raffy Traas, Bryan Brzycki, Vishal Gajjar, Howard Isaacson, Matthew Lebofsky, David H.E. MacMahon, Danny C. Price, Sofia Z. Sheikh, Julia DeMarines, Jamie Drew, and S. Pete Worden
Figure caption: Transmitter Rate vs. ﹩{\mathrm{EIRP}}_{\min }﹩ for this study (represented by the four Y-shaped points) compared to past studies (none of which specifically targeted systems during transits). The two vertical lines represent the EIRP of the Arecibo S-band radar, and the solar power incident on Earth.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Primary star HGCA acceleration χ 2 as a function of companion projected separation. Orange squares are detections within 4″ with Robo-AO that have yet to be confirmed as physically associated, green circles are physically associated companions detected within 4″ with Robo-AO, and purple stars are wide comoving companions detected in Gaia EDR3. Companions linked by a dotted line have the same primary star. The horizontal dashed line marks the threshold for significant acceleration (χ 2 > 11.8).
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Primary star RUWE values as a function of companion separations detected by Robo-AO, color coded by magnitude difference. Companions that are detected by Gaia, and have parallax and proper-motion measurements, are shown as circles. Those that are found in Gaia but with no parallax and proper-motion measurements are shown as diamonds, while those not found in Gaia are shown as Xs. Companions that orbit the same primary star and detected by Robo-AO within 4″ are connected by a dotted line. The horizontal dashed line marks RUWE = 1.4. It is clear that companions within 1″ are not well detected by Gaia and are causing large RUWE values, while the systems where the companions are well detected generally have smaller RUWE values.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Cumulative distribution of HGCA acceleration χ 2 values for stars with and without companions detected. The vertical dashed line marks the threshold for significant acceleration (χ 2 > 11.8). Of the 540 stars with no companions detected, 85.9% ± 4.0% (464/540) do not have significant accelerations, while 14.1% ± 1.6% (76/540) of them do. Of the 112 stars with wide (>4″) companion detections, 58.0% ± 7.2% (65/112) do not have significant accelerations, and 42.0% ± 6.1% (47/112) of them do. Of the 75 stars with companions detected within 4″, only ﹩{9}_{-2}^{+5}﹩% (7/75) do not have significant accelerations while ﹩{91}_{-4}^{+2}﹩% (68/75) of them do.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Cumulative distribution of RUWE values for stars with companions detected by Robo-AO within 1″, stars with companion beyond >1″) only, and stars with no companions detected. The vertical dashed line marks RUWE = 1.4. Large RUWE values (>1.4) indicate an issue with the astrometry fitting to a single-star model, likely caused by the presence of a close companion.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Stacked distribution comparison between the stars found in Gaia EDR3 and those not found in Gaia where distances were found in SIMBAD. There is no clear bias in the sample distance distributions. However, there are more bright stars not found in Gaia EDR3 and possibly more bright subarcsecond binaries.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Stellar multiplicity fractions as a function of spectral type for the sample of 1005 primary stars found in Gaia with both tight Robo-AO detected companions and wide comoving companions found in Gaia (colored bars) and for the full sample of 1083 primary stars with only tight companions detected by Robo-AO (dashed bars).
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Gaia color–magnitude diagram for companions detected in Gaia, including the wide comoving search and the Robo-AO tight detections found in Gaia. Color coded by companion SpT estimate from Gaia photometry.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Absolute Gaia magnitudes of 147 wide comoving companions identified in Gaia EDR3 as a function of projected separation and color coded by spectral type of the primary star.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: CU CnC system consisting of four imaged M dwarfs with the PSF-subtracted image of star A in order to see its companion. The Robo-AO image is displayed with a log stretch.
Paper: PetroFit: A Python Package for Computing Petrosian Radii and Fitting Galaxy Light Profiles
Authors: Robel Geda, Steven M. Crawford, Lucas Hunt, Matthew Bershady, Erik Tollerud, Solohery Randriamampandry
Figure caption: A unitless 1D Sérsic profile is plotted with n = 1, r  e  = 25 (black vertical lines), and I  e  = 1 (black horizontal line). The flux at the center of the profile (I 0) is equal to 5.3 and not 1 (i.e., I 0 ≠ I  e ). The dotted blue area under the curve contains half of the total flux and is equal in value to the striped green area (that also contains half of the total flux). The Sérsic profile and the green area extend to infinity.
Paper: PetroFit: A Python Package for Computing Petrosian Radii and Fitting Galaxy Light Profiles
Authors: Robel Geda, Steven M. Crawford, Lucas Hunt, Matthew Bershady, Erik Tollerud, Solohery Randriamampandry
Figure caption: The COG represents the total flux enclosed at each radius and asymptotically approaches the total flux (black dashed–dotted horizontal line). This example shows the COG of a Sérsic profile with (n = 1, I  e  = 1, r  e  = 25). The half-light radius (r  e  = 25) contains half of the total flux that is contributed by the blue dotted area in Figure 1.
Paper: PetroFit: A Python Package for Computing Petrosian Radii and Fitting Galaxy Light Profiles
Authors: Robel Geda, Steven M. Crawford, Lucas Hunt, Matthew Bershady, Erik Tollerud, Solohery Randriamampandry
Figure caption: Plot of the Petrosian profile (η(r)) of a Sérsic profile with (I  e  = 1, r  e  = 25, n = 1). Note that the profile has the property where η(0) = 1 at the center of the galaxy (r = 0) and drops to zero at the edge.
Paper: A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: Time evolution of the barycentric distance for Styx (light green), Nix (dark green), Kerberos (blue), and Hydra (purple). The very light green (blue) curve plots q  S  and Q  S  (q  K  and Q  K ) as defined in the text. The horizontal dashed gray line near the bottom of each panel indicates the location of the innermost stable distance for circular orbits in the orbital plane of the central binary (Kenyon & Bromley 2019b). The masses (in units of 1018 g) for each satellite in the simulation are listed to the right of each curve.