adsabs/AstroCLIMB huggingface dataset:
Paper: Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass Loss
Authors: Su Wang, 素 王, D. N. C. Lin, 潮 林
Figure caption: The evolution of the system in Case 6, where A = 0.1 and τ  m  = 104 yr. The system becomes unstable at about 0.35 Myr. Panel (a) shows the evolution of the innermost planet. In this case, the innermost planet will lose about 0.3 Earth-mass, which is about 10% of the initial mass. Panel (b) shows the evolution of a, a(1-e), and a(1+e) of all of the planets. Panel (c) shows the evolution of the resonant angles. The resonant angles tend to librate in a large range from 0–2π. Panel (d) shows the evolution of eccentricities of planets in the system. The different colors represent the same as those in Figure 9.
Paper: Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass Loss
Authors: Su Wang, 素 王, D. N. C. Lin, 潮 林
Figure caption: The amplitude of resonant angles in the system with different gas disk depletion timescales. Amji (1 ≤ i ≤ 8, j = i + 1) has the same definition as in Figure 5. Red circles, blue asterisks, and black squares represent depletion timescales of 105, 106, and 3 × 106 yr, respectively.
Paper: Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass Loss
Authors: Su Wang, 素 王, D. N. C. Lin, 潮 林
Figure caption: The evolution of relative separation between adjacent planets in different cases with different gas density. Panels (a), (b), and (c) correspond to the cases with f  g  = 1, 0.5, and 0.2, respectively. f  g  is the enhancement factor of the gas density as shown in Equation (10). f  g  = 1 refers to the gas density profile of the MMSN model. The colors of different lines represent the relative separation between different planet pairs as the legend shown in panel (a).
Paper: Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass Loss
Authors: Su Wang, 素 王, D. N. C. Lin, 潮 林
Figure caption: The results of G2. In this Group, the transition radius locates at 3 au. Thus, planets 7, 8, and 9 undergo inward migration, while the other planets migrate outward. Planet pairs can be trapped into 3:2 (k = 14.2) and 4:3 MMRs (k = 10.1). Panel (a) shows the evolution of semimajor axis, pericenter, and apocenter of the nine planets. The black lines display the evolution of semimajor axis, and the gray lines show the evolution of the pericenter and apocenter of the nine planets. Panel (b) shows the evolution of the relative space between adjacent planet k  ji , and k  ji  represents the same separation as in Figure 4. Panel (c) shows the evolution of resonant angles ﹩\theta =(p+q)\lambda ^{\prime} -p\lambda -q\varpi ^{\prime} ﹩, where the unprimed and primed parameters refer to the inner and outer planets, respectively, two planets are in or near (p+q):p resonance, and λ and ϖ are the mean longitude and longitude of pericenter. Amji represents the resonant angle amplitude of the planet pair  Pi  and P  j  (i represents the serial number of the planet from inner to outer, 1 ≤ i ≤ 8, j = i + 1).
Paper: Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass Loss
Authors: Su Wang, 素 王, D. N. C. Lin, 潮 林
Figure caption: The distribution of planetary systems that contain more than three planets observed by TESS mission. The gray circles depict the innermost planet in the system, and the inner planet in a planet pair is labeled in red if the planet pair is in or near 2:1 MMR. Red solid dots represent period ratio deviations of 2.0 by no more than 2%, while the red open circles represent period ratio deviations of 2.0 by no more than 10%. The green solid dots and open circles show the period ratio results of 3:2 MMR, and the blue solid dots show the results of 4:3 MMR. The gray solid dots represent no obvious sign of a first-order MMR relationship between two adjacent planets.
Paper: Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass Loss
Authors: Su Wang, 素 王, D. N. C. Lin, 潮 林
Figure caption: The evolution of a typical stable system. In this run, the masses of planets in the system are 3 M ⊕, the initial separation between planets is 14 R hill, and the timescale of mass loss is 106 yr. The system is stable for more than 10 Myr. The innermost planet loses 5% of its total mass in this process. Panel (a) shows the evolution of the semimajor axis and mass of the innermost planet. The red line shows the evolution of mass, and the black line represents the evolution of semimajor axes. Panel (b) represents the semimajor axis evolution of nine planets in the system. The black lines represent the evolution of the semimajor axis, and the gray lines depict the evolution of the pericenter and apocenter. Panel (c) displays the evolution of the relative space k  ji  between two adjacent planets  Pi  and P  j  (here, “i” represents the serial number of the planet from inner to outer, 1 ≤ i ≤ 8, j = i + 1), and different colors display different k  ji  as shown in the legend in panel (c).
Paper: Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass Loss
Authors: Su Wang, 素 王, D. N. C. Lin, 潮 林
Figure caption: The results of G1. In this Group, all planets undergo inward type I migration. The transition radius is 0.5 au. The planets are labeled “1” to “9” from the innermost to the outermost. Panel (a) shows the evolution of semimajor axes of nine planets with black lines, and the evolution of the pericenter and apocenter of the nine planets are shown with gray lines. Panel (b) displays the evolution of the relative separation between planets. kji refers to the relative separation between two adjacent planets  Pi  and Pj (here, i represents the serial number of the planet from inner to outer, 1 ≤ i ≤ 8, j = i + 1), and different colors display different k  ji  as shown in the legend in panel (b).
Paper: Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass Loss
Authors: Su Wang, 素 王, D. N. C. Lin, 潮 林
Figure caption: The stabilities of multiple planetary systems are shown with varied mass-loss timescales and fractions. “k” represents the relative Hill radius between two adjacent planets initially. The y-axis represents the logarithm of mass-loss timescale. The systems that are stable for at least 107 yr are labeled in dark blue, while the systems with orbital crossing before the end of the simulations are labeled in light blue. The upper three panels show the stabilities of systems with different planetary masses, but with the same mass-loss fraction (A = 0.05). The cases in the upper three panels correspond to those listed in Table 1. The lower three panels show the stabilities of systems with different mass-loss fractions, but with the same planetary masses (m = 10M ⊕). The cases with A = 0.2 and A = 0.1 correspond to that listed in Table 2. The results shown in the upper and lower panels of the rightmost column are the same cases.
Paper: Single-band VLBI Absolute Astrometry
Authors: Leonid Petrov
Figure caption: Differences in declination from the X-band solution XIR with respect to the dual reference solution RIR using data from the R1/R4 VLBI, similar to Figure 7. The default TEC GNSS mapping function (ΔH = 0, α = 1.0, and k = 1.00) was used for this comparison.
Paper: Single-band VLBI Absolute Astrometry
Authors: Leonid Petrov
Figure caption: Similar to Figure 15 but derived from an analysis of observations from the R1/R4 VLBI network. The statistics are computed for one year intervals.
Paper: Single-band VLBI Absolute Astrometry
Authors: Leonid Petrov
Figure caption: The empirical declination bias corrections D(δ) computed from the coefficients presented in Table 5 for three VLBI networks: the Southern Hemisphere network marked with S (red), R1/R4 marked with R (blue), and VLBA marked with V (green).
Paper: MAVEN Observations of Whistler-mode Waves Within the Magnetic Dips in the Martian Ionopause/Ionosphere
Authors: Jing Wang, Jiang Yu, Zuzheng Chen, Xiaojun Xu, Kun Li, Jun Cui, Jinbin Cao
Figure caption: Overview of magnetic dip structures observed by MAVEN in the Martian ionopause. The projections of MAVEN orbit (pink curve) in the (a) X MSO–Y MSO and (b) X MSO–Z MSO planes in MSO coordinates. The solid and dashed black curves represent the locations of the bow shock and MPB from Trotignon’s empirical models (Trotignon et al. 2006), respectively. (c)–(g) The magnetic field strength ∣B∣, the electron density N  e , the omnidirectional ion energy spectra, the ion mass spectra and the omnidirectional electron energy spectra. The vertical shaded area in panels (c)–(g) marks out the region of magnetic dip structures. The horizontal lines in panel (f) marks the O+ and O2 + ions.
Paper: MAVEN Observations of Whistler-mode Waves Within the Magnetic Dips in the Martian Ionopause/Ionosphere
Authors: Jing Wang, Jiang Yu, Zuzheng Chen, Xiaojun Xu, Kun Li, Jun Cui, Jinbin Cao
Figure caption: Growth analysis of whistler-mode waves. (a) The magnetic field strength (black) and electron number density (red). (b) The ratio of electron plasma frequency (f pe) to electron gyrofrequency (f ce). (c) The electron energy spectra. The pitch angle distribution for (d) 5–10 eV, (e) 10–20 eV, (f) 20–50 eV and (g) 100–1000 eV electrons. (h) The electric spectral density and (i) the convective growth rate in the frequency range between 1 Hz and 100 Hz. The superimposed black curve in panel (c) denotes the minimum electron cyclotron resonant energy (E min). The lower and upper black curves in panels (h) and (i) represent the lower hybrid frequency and 0.2 f ce, respectively.
Paper: MAVEN Observations of Whistler-mode Waves Within the Magnetic Dips in the Martian Ionopause/Ionosphere
Authors: Jing Wang, Jiang Yu, Zuzheng Chen, Xiaojun Xu, Kun Li, Jun Cui, Jinbin Cao
Figure caption: Properties of electromagnetic waves at the center of magnetic dips. (a) The magnetic field strength. (b) The electric spectral density (E PSD). (c) The magnetic spectral density (B PSD). (d) The degree of polarization. (e) The wave normal angle (θ  k ). (g) The ellipticity of wave polarization. The lower and upper black curves in panel (b) represent the lower hybrid frequency and one-fifth of electron cyclotron frequency, respectively. The black curves in panels (c)–(f) represent the lower hybrid frequency.
Paper: MAVEN Observations of Whistler-mode Waves Within the Magnetic Dips in the Martian Ionopause/Ionosphere
Authors: Jing Wang, Jiang Yu, Zuzheng Chen, Xiaojun Xu, Kun Li, Jun Cui, Jinbin Cao
Figure caption: Observations of whistler-mode waves and plasma environments during the magnetic dips on 2015 January 9. (a) The magnetic field strength. (b) The electron number density. (c) The ratio of electron plasma frequency (f pe) to electron gyrofrequency (f ce). (d) The electric spectral density. The lower and upper black curves in panels (d) represent the lower hybrid frequency and 0.2f ce, respectively.
Paper: MAVEN Observations of Whistler-mode Waves Within the Magnetic Dips in the Martian Ionopause/Ionosphere
Authors: Jing Wang, Jiang Yu, Zuzheng Chen, Xiaojun Xu, Kun Li, Jun Cui, Jinbin Cao
Figure caption: VDFs of electrons outside (left) and inside (right) the dips at different times (labeled by vertical arrows in Figure 3) in the velocity space. v ∥ and v ⊥ represent the velocities parallel and perpendicular to the background magnetic field, respectively.
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: One-dimensional demonstration of speckle interference. Two sinusoidal perturbations in the pupil plane interfere to create moving speckles in the image plane. Top: 1D phase screen with interfering sinusoids over time. Middle: 1D intensity over time without a coronagraph, showing the Airy pattern. Bottom: 1D intensity over time with a coronagraph, with the speckles’ relative evolution appearing more clearly due to the lack of coherent light, C( x ). This simulation is used as a test of the space–time speckle covariance theory in Section 2.2.
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: Space–time covariance matrices for pupil plane (middle) and focal plane (bottom) of a 1D model of two sinusoids with different frequencies—as illustrated in the top panel of Figure 2—with an annotated view of the simulation (top). These matrices show a symmetric pattern that changes with the number of lags used, due to the change in the speckles’ relative locations. At lags 0 and 100, the peaks are due to the alignment of the speckles’ peaks, as marked in the top panel; lag 25 illustrates the lower covariance when the speckles are in slightly different places, and lag 50 shows two lower intensity peaks when the speckles are separated. Importantly, for a given nonzero lag, there are nonzero terms, indicating that there are temporal correlations.
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: One frame of the input sequence (left) for the simple two-sinusoid test case with a coronagraph, with the residuals after PSF subtraction using mean-subtraction, KLIP, and stKLIP, showing a clear reduction in speckle intensity. Both stKLIP and baseline KLIP reduce image variance by a factor of at least 5.7 from the original image, an improvement over simple interventions like mean-subtraction. Although stKLIP does not improve upon KLIP in this limited test case, it is important to remember that we have not optimized for modes and lags in this scenario; this step was intended for troubleshooting, not rigorous characterization of the algorithm.
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: Companion signal over number of KL modes used in the model PSF subtraction; this figure shows that signal loss begins around five modes, indicating that future iterations of this algorithm would benefit heavily from implementing measures to prevent self-subtraction. Certain choices of lag (4, 5, 6, 8) show a minor improvement in signal retention over spatial (lag = 0) KLIP.
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: Contrast curves, as well as contrast improvement (a comparison to the original image’s contrast curve), for three cases of KL modes: 5, 7, and 20. Each shows results for the image processed with baseline KLIP (zero lags) as well as stKLIP with a variety of lags. stKLIP is consistent with KLIP improvements, and in certain regions may show improvements depending on number of lags used.
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: Two-dimensional test of speckle interference. A sinusoidal phase screen (top) produces a speckle pattern imposed on an Airy disk (middle). Subtracting the PSF of a model without perturbations, we simulate observations of this sinusoidal perturbation with a “perfect” coronagraph (bottom). All images depict the intensity (I = ∣E∣2). This simulation is used as a troubleshooting step for a first implementation of the stKLIP algorithm.
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: One frame of the input sequence (left) from MEDIS, with the residuals after PSF subtraction using mean-subtraction, KLIP, and stKLIP. Both stKLIP and baseline KLIP reduce image variance by a factor of ∼1.85 from the original image for the listed case of 10 modes and 2 time steps lag in stKLIP.
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: Examples of MEDIS simulations. (Top) Pupil plane, illustrating the phase screen. (Bottom) Focal plane, with a clearly bright companion object. These simulations are used as a preliminary test of stKLIP’s efficacy and potential; however, there is a large parameter space to explore beyond the scope of this work.
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: Companion signal-to-noise ratio (S/N) compared to the original image S/N over number of KL modes used in the model PSF subtraction; this figure shows a 10%–20% improvement over the original image using stKLIP and KLIP, with stKLIP having a slight edge (on the order of a few percent) for certain choices of lag.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: a) An example of an event in the 1165–1185 MHz region, consistent with GPS L5. This event is RFI, as it appears in multiple different targets in consecutive observations. The dashed red line represents turboSETI's best-fit drift rate for the detected hit. b) An example of an event in the 1375–1385 MHz region. These events occur for only a fraction of the observation (here, about 100 s) within a single scan—this makes it difficult to determine whether they are impulsive RFI or whether they are true transient signals localized on the sky. However, because we observe the same morphology of signal in multiple targets, and because of the match to the GPS L3 downlink, we can assign these events as RFI. c) An example of an event in the 1570–1580 MHz region. These events are similar to the example shown in subfigure b in that they are degenerate between transient and localized signals; this is a common challenge for single-dish technosignature searches. The same signals were identified in multiple targets, however, indicating that they are indeed RFI—likely the GPS L1 downlink. d) An example of a high-drift-rate signal around 1626 MHz. We attribute this event to an Iridium satellite. It is clearly present in all three panels, and therefore RFI, but the changing slope of the signals over time confounds the linear search algorithm.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: A histogram showing the frequency distribution of the hits (lighter) and events (darker) in a logarithmic (left) and a linear (right) scale. The notch filter is responsible for the absence of hits between 1200–1340 MHz. Three distinct frequency regions contain more than 100,000 hits each: 1165–1185 MHz, 1375–1385 MHz, and 1570–1580 MHz. These three regions are discussed in further detail in Section 5.1.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: Confirmed transiting exoplanets in the Kepler field as observable from the Green Bank Telescope (GBT) during on 2018 March 25. The horizontal errorbars depict the transit duration, whereas the color of the markers represent the stellar effective temperature. Points without visible errorbars have extremely well-defined transit midpoints. The gray region marks our observing window, whereas the targets observed are circled in black. We did not include a habitability requirement in planet selection.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: A plot of all exoplanetary systems (blue stars) observed with the GBT for this project, overlaid on the Kepler field of view, which covers 115 square degrees on sky (Mullally et al. 2016). The name of each system as it appears in Table 4 is shown. Boyajian’s star (an off-source target) is also included for reference.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: A histogram showing the frequency distribution of the hits (light gray), events (light purple), and signals of interest (purple). The signals of interest are distributed relatively evenly throughout the spectrum. Note the gap from 1.20 to 1.34 GHz due to the GBT L-band receiver’s notch filter.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: A histogram showing the S/N distribution of the hits (light gray), events (light green), and signals of interest (green). The signals of interest are primarily faint. There are also 5 hits with S/N > 10, 000, which are not shown on this plot for readability.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: A histogram showing the drift rate distribution of the hits (light gray), events (light orange), and signals of interest (orange). The signals of interest are found only at low absolute drift rates.
Paper: Resolved SPLASH Chemodynamics in Andromeda’s PHAT Stellar Halo and Disk: On the Nature of the Inner Halo along the Major Axis
Authors: Ivanna Escala, Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, J. Leigh Wojno, Lara Cullinane, Benjamin F. Williams, Julianne Dalcanton
Figure caption: IR (F110W, F160W) PHAT v2 CMD (Dalcanton et al. 2012; Williams et al. 2014) for the RGB stars in SPLASH (Appendix C). The RGB classification is based on the foreground reddening–corrected optical CMD (Section 4.1). The RGB stars follow a tight sequence that is insensitive to metallicity and age. Note that the axes are not shown to equal scale, for clarity. The black dashed lines are the estimated 2σ widths expected for an unreddened RGB CMD, taking into account stellar surface density variations (Dalcanton et al. 2015). The lack of a second broader sequence at redder colors suggests that the majority of stars are in front of the dust layer and not significantly reddened.