adsabs/AstroCLIMB huggingface dataset:
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: Left panel: the evolution of the particle mass distribution (multiplied by mass squared to convert to integrated mass) in the outer PPB. The absolute scaling of the distribution (C) depends on the binning used. Right panel: the SEDs calculated from the particle-size distributions shown in the left panel. As the smallest particles are reduced in number density, the mid-IR emission hump from the system drops, as then does the scaling of the complete excess profile as the system evolves.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: The eight final processed images at 25.5 μm, at the four extended dither positions and two rotations, shown with the masks used to produce the final combined image. Images are shown in logarithmic stretch, between −20 and 1800 MJy sr−1.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: Top: the radial profile of the color temperature of the disk derived from the ratio of the F2550W and F1500W MIRI images. Bottom: the associated optical depth. For an optically thin disk, the optical depth can be approximated by the ratio of the observed flux to the product of the Planck function evaluated for the dust temperature (the color temperature above is used as a proxy for the dust temperature) and the disk solid angle.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: The radial profile of the disk color temperature shown in Figure 16 (black line and shaded uncertainties) is compared to the dust temperature profiles for several dust species (colors) and dust particle sizes (0.3 μm, top line; 1 μm, middle line; 3 μm, bottom). The observations are most comparable to the amorphous olivine or carbonaceous dust with grain sizes of ∼1 μm. Larger ∼3 μm amorphous carbon grains are also compatible. Water ice is too cold to dominate the dust population in the ϵ Eri disk.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: The iterative reduction sequence (top to bottom) for the ϵ Eri F2550W data set at each of the four dither positions at Rotation 1 (levels in megajanskys per steradian given on the right side of each row). The “Clean product” images contain row/column artifacts that were removed by similar artifacts present in the PSF images, as the artifacts are estimated on the PSF-subtracted images.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: The relative change in particle number density in the parent belt over the age of the ϵ Eri system as a function of particle size. Within about 10 Myr of collisional evolution, the SW drag and collisional production reach a quasi-steady state, with the same fractional losses at all particle sizes up to 10 cm.
Paper: Identification of Galactic H I Counterpart of the Large [O III] Emission Structure 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 Southeast of M31
Authors: Tiantian Liang, Jie Wang, Tao Wang, Haibo Yuan, Ruoyi Zhang, Zhiyu Zhang, Chao-Wei Tsai, Ping Zhou, Xiaohui Sun, Hu Zou, Yingjie Jing, Chen Xu, Zhipeng Hou, Yann Sainty, Marcel Drechsler, Xavier Strottner, Ziming Liu, Qingze Chen, Zerui Liu
Figure caption: PV diagrams of the H I counterpart and surrounding gas. The left top panel shows the same integrated intensity H I map as Figure 1 right panel with a contour whose level is 1.79 Jy km s−1. The contours mark the central high-flux structures of the H I counterpart and nearby structures, labeled as A–G. The white arrows mark the direction of the I to IV, and the width is 3′. The central structures are marked with white dashed circles in panels I–IV. To best illustrate the gas structures in different PV diagrams, different color scales were used in each subplot.
Paper: Identification of Galactic H I Counterpart of the Large [O III] Emission Structure 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 Southeast of M31
Authors: Tiantian Liang, Jie Wang, Tao Wang, Haibo Yuan, Ruoyi Zhang, Zhiyu Zhang, Chao-Wei Tsai, Ping Zhou, Xiaohui Sun, Hu Zou, Yingjie Jing, Chen Xu, Zhipeng Hou, Yann Sainty, Marcel Drechsler, Xavier Strottner, Ziming Liu, Qingze Chen, Zerui Liu
Figure caption: Left: [O III] 5007 Å narrowband image (M. Drechsler et al. 2023). Two bright strips and one faint strip are marked with O1, O2, and O3. A yellow dashed ellipse marks the faint strip because it is not obvious. Right: the image of SDSO1 is in red, and the H I counterpart is in blue. The three corresponding H I structures are marked with H1, H2, and H3. The H I image is integrated from −79 to −56 km s−1.
Paper: Identification of Galactic H I Counterpart of the Large [O III] Emission Structure 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 Southeast of M31
Authors: Tiantian Liang, Jie Wang, Tao Wang, Haibo Yuan, Ruoyi Zhang, Zhiyu Zhang, Chao-Wei Tsai, Ping Zhou, Xiaohui Sun, Hu Zou, Yingjie Jing, Chen Xu, Zhipeng Hou, Yann Sainty, Marcel Drechsler, Xavier Strottner, Ziming Liu, Qingze Chen, Zerui Liu
Figure caption: Similar to Figure 2 but with a broader velocity range. (a)–(n) Integrated H I intensity maps from −700 to 0 km s−1 in 50 km s−1 steps. (o) Integrated intensity image in the velocity range −400 to −200 km s−1. The black contour levels represent 0.12, 0.2, and 0.31 Jy beam−1 km s−1, corresponding to data convolved to a 9′ resolution.
Paper: Identification of Galactic H I Counterpart of the Large [O III] Emission Structure 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 Southeast of M31
Authors: Tiantian Liang, Jie Wang, Tao Wang, Haibo Yuan, Ruoyi Zhang, Zhiyu Zhang, Chao-Wei Tsai, Ping Zhou, Xiaohui Sun, Hu Zou, Yingjie Jing, Chen Xu, Zhipeng Hou, Yann Sainty, Marcel Drechsler, Xavier Strottner, Ziming Liu, Qingze Chen, Zerui Liu
Figure caption: Spectra of points A0–G0, which are localized peak points of structure A–G in Figure 4. The shaded area indicates the integrated velocity range depicted in the upper left panel of Figure 4. Vertical lines mark the velocities corresponding to the localized signal peaks of the spectral lines at points A0–G0.
Paper: Identification of Galactic H I Counterpart of the Large [O III] Emission Structure 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 Southeast of M31
Authors: Tiantian Liang, Jie Wang, Tao Wang, Haibo Yuan, Ruoyi Zhang, Zhiyu Zhang, Chao-Wei Tsai, Ping Zhou, Xiaohui Sun, Hu Zou, Yingjie Jing, Chen Xu, Zhipeng Hou, Yann Sainty, Marcel Drechsler, Xavier Strottner, Ziming Liu, Qingze Chen, Zerui Liu
Figure caption: The intensity maps of H I gas integrated every 5 km s−1 from −90 to −45 km s−1, where the dashed green polygon delineates the spatial extent of SDSO1. The color scales in different panels range from 3% to 87% of their data value.
Paper: Identification of Galactic H I Counterpart of the Large [O III] Emission Structure 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 Southeast of M31
Authors: Tiantian Liang, Jie Wang, Tao Wang, Haibo Yuan, Ruoyi Zhang, Zhiyu Zhang, Chao-Wei Tsai, Ping Zhou, Xiaohui Sun, Hu Zou, Yingjie Jing, Chen Xu, Zhipeng Hou, Yann Sainty, Marcel Drechsler, Xavier Strottner, Ziming Liu, Qingze Chen, Zerui Liu
Figure caption: Multiwavelength analysis of SDSO1’s Galactic environment. (a) H I distribution integrated over −79 to −56 km s−1 in the LSR frame, with contour levels at 1.4 and 1.7 Jy beam−1 km s−1. The dashed white rectangle indicates the spatial extent shown in the top-left panel of Figure 4. (b) Dust map within d = 1.4–2.3 kpc, overlaid with H I counterparts from panel (a). (c) Infrared emission from IRIS 100 μm (M.-A. Miville-Deschênes & G. Lagache 2005), showing morphological correspondence with both HI structures (green contours) and dust features. (d) The LAMOST star color excess E(B − V) values as a function of distance toward regions 0–3: signal region 0 and control regions 1–3 (solid white polygons in panel (a)). The four lines represent the best-fitting models to the LAMOST data in regions 0–3, with corresponding shaded regions indicating the 68% confidence intervals of the fits. The numbers following each region’s label in the legend indicate the number of LAMOST data points used in the fitting for the respective regions. During initial LAMOST fitting, the >3σ data points have been removed.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption:                         Geometry of lens systems and their caustics. Each panel shows a different regime of caustic structure, defined using the criteria from Equation (5). The star, plus, and square indicate the positions of the star, planet, and moon, respectively. sp and sm indicate the distances between the star and planet, and the moon and planet, respectively. ψ indicates the orientation of the moon relative to the planet–star axis. The red lines show the location and shape of the planetary caustic(s), or, in the case of the resonant regime, the resonant caustics. These caustics do not include the effect of the moon. For illustrations of the effect of moons on the planetary caustics, see Figures 2, 6, and 11. For the close and wide regimes, xcen shows the distance between the star and the center of the caustic. Δξ and Δη are the vertical and horizontal widths of the planetary caustic, respectively. The cross section of the planetary caustic, scaus, is the geometric mean of Δη and Δξ. Note that this figure is not drawn to scale.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption: A histogram of the rms deviation between light curves computed using our inverse-ray-shooting algorithm and light curves computed using MulensModel (R. Poleski & J. C. Yee 2019). We use a subset of 2590 light curves computed as part of the simulations described in this work. For the rms calculation, we only use the region of the light curve calculated using ray shooting and exclude the parts calculated with MulensModel. The gray filled histogram shows the rms between ray-shooting light curves with only a planet and a MulensModel light curve calculated with the same parameters. The blue hatched histogram uses light curves that include a moon compared to the same MulensModel light curve. The open histogram shows the rms between planet-only ray shooting light curves (no moon), including expected photometric noise (see Section 5), compared to the same MulensModel light curve. The blue histogram with the moon is essentially the gray (planet-only) histogram shifted to larger deviations, resulting in a slight excess compared to the planet-only histogram at high rms that comes from the perturbations due to the moons.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption: An example magnification map generated using inverse ray shooting and the following parameters: qp = 0.0026, qm = 0.01, sp = 2.058, sm = 0.9648, Ψ = 43°. On this scale, darker color indicates higher magnification. The moon introduces additional structure to the caustic that is not present with just a planet.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption: Panel (a) shows the range of semimajor axes ap and planet masses Mp for which we simulated companion moons. We assume a 0.3M⊙ host star, which is approximately the mean mass of the stars in our simulation. We assume a distance to the lens, Dl of 7.37 kpc, which is approximately the front of the Galactic bulge. The black solid lines show contours of constant sHill ≡ aHill/RE,p, e.g., the ratio of the Hill radius of the planet to the Einstein ring radius of a planet. The dashed blue curves show contours of constant scaus, the mean caustic cross section (see Equations (14) and (17)). Note that the definitions of scaus for the close and wide regimes are slightly different. For the wide regime, scaus is simply related to the size of the planetary caustic. For the close regime, scaus also takes into account the vertical separation between the two planetary caustics. The gray shaded region shows the region of the resonant caustic topology that we do not include in our simulations. Each offset panel (b)–(g) shows the caustic structures (in red), the Hill radius (in black), and the planetary Einstein ring radius (in blue) centered at the location of the planet (the plus symbol). The caustics were calculated using the triplelens package (R. Kuang et al. 2021). The gray shaded region in the inset is the region around the planet where we simulated moons (0.1–0.5 Hill radii). A moon with a randomly chosen semimajor axis and orbital phase is shown as a square. The arrows in each panel point to the locations of the small caustics from the moon. These panels are connected to the corresponding planet mass and semimajor axis in the main panel. This figure is discussed in more detail at the end of Section 3.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption: Examples of simulated Roman light curves with detectable moons. For each light curve, the left panel shows the region of the light curve near the planet and moon perturbations. The inset plot shows the full light curve. The black points with uncertainties are the simulated data points. The orange curve is the best-fit binary lens model, and the blue curve is the actual event including the moon. The bottom panel on the left shows the residuals of the planet+moon event from the binary lens fit. The right panel shows the magnification map for this event. The dashed line shows the source trajectory, with the direction of the source given by the arrow. The circle along the source trajectory shows the size of the source. A variety of parameters for each event are listed above each plot. The events displayed here were chosen to display a variety of the features present from exomoons in our simulations.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption: Magnification maps for planetary systems with four moons. In both cases, the host star has a mass of M = 0.37 M⊙, is located at a distance of Dl = 7.9 kpc, and has an Einstein ring radius of RE = 3.0 au. The planet has a mass of Mp = MJup and mass ratio qp = 2.6 × 10−3, and an instantaneous projected separation of 6.2 au or sp = 2.08. The Hill radius is aHill = 0.59 au. The ratio of the Hill radius to the planetary Einstein ring radius is ﹩{a}_{{\rm{Hill}}}/({q}_{p}^{1/2}{R}_{{\rm{E}}})=3.9﹩. In each case, the planet hosts four moons with semimajor axes of 0.15, 0.25, 0.35, and 0.45 times the Hill radius. The moons have the same mass and coplanar orbits with an inclination of i = 45°. The phases of the orbits of the moons were chosen at random. The left panels show the locations of the planet and each moon as black dots, as well as the size of the Hill radius as the black circle and the planetary Einstein Ring as the blue circle. The gray shaded area is the region from 0.1 to 0.5 of the Hill radius in which we simulated moons. The right panels show the resulting magnification maps. In the top row, the mass ratio of each moon is qm = 10−2 (Mm ≃ 3.2 M⊕), and in the bottom row it is 10−3 (Mm = 0.32 M⊕ ≃ 3 MMars.)
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption:                         Physical parameters of the simulated events with and without detected moons. In each panel, the gray points show the events our simulation where a moon was not detected, i.e., these are the distributions of the physical parameters of the planets and moons we simulated. The stars show events where the moon was detected. The blue markers indicate the locations of the light curves shown in Figure 6 in these parameter spaces. The top left panel (a) shows the planet/star mass ratio vs. planet projected separation in units of the Einstein ring radius of the system. The lines indicate the boundaries of the resonant caustic region that we exclude from our sample. The other panels show (b) the planet mass vs. the planet semimajor axis; the (c) moon/planet mass ratio vs. the moon–planet separation in units of the Einstein ring radius of the planet; and the (d) moon mass vs. semimajor axis of the moon in units of the Hill radius.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption: These histograms show the distribution of simulated and detected events. In each panel, the solid gray bars show the distribution of events with detectable exomoons. The solid line shows the distribution of all simulated events. The height of each bin is the yield, or the number of events in each bin. The sum of the heights of all bins is the total predicted yield.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption: Improvement in Δχ2 of light curves with detected moons as a function of the sampling rate. The horizontal axis is normalized to the nominal M. T. Penny et al. (2019) sample rate of 15 minutes, whereas the vertical axis is normalized to the Δχ2 value for this sampling rate. The red points are the mean values at each sampling rate, with error bars given by the standard deviation of the points in each bin. The red dashed line is the best-fit line to the mean values. We find a slope of 0.99  ±  0.01, indicating that the Δχ2 increases linearly with sampling rate, as expected for events for which the majority of the perturbations are well-resolved at the lowest sampling rate.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption: The cumulative distribution of the number Ntot( > Δχ2) of detected moons using a given ﹩{\rm{\Delta }}{\chi }_{thr,m}^{2}﹩, normalized to the number of detected moons using ﹩{\rm{\Delta }}{\chi }_{thr,m}^{2}=90﹩, is shown as the black line. The red dashed line is the location of the adopted ﹩{\rm{\Delta }}{\chi }_{thr,m}^{2}=90﹩ threshold. The blue curve shows a power-law fit to the cumulative distribution between ﹩{\mathrm{log}}\,\left({\rm{\Delta }}{\chi }^{2}/90\right)=-2﹩ and 1. The slope of the fit is −0.638.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption: The masses of large solar system moons in Earth masses vs. their semimajor axes in units of the Hill radius. Each different symbol and color represents the moons of a different planet. The red symbols are the two exomoon candidates, Kepler-1708bi (D. Kipping et al. 2022) and Kepler-1625bi (A. Teachey et al. 2018). The gray points are our simulated moons. Each of the black stars is a detected moon in our simulation.
Paper: Predictions of the Nancy Grace Roman Space Telescope Galactic Exoplanet Survey. III. Detectability of Giant Exomoons of Wide-separation Giant Planets
Authors: Matthew Lastovka, B. Scott Gaudi, Samson A. Johnson, Matthew T. Penny, Eamonn Kerins, Nicholas J. Rattenbury
Figure caption:                         Change in the caustic structure when varying Ψ. All other parameters are the same as the light curve in Figure 6(a). The inset plot shows the orientation of the star, planet, and moon, and the location of the caustic structures. The star symbol gives the location of the star, the circle denotes the planet’s location, and the plus symbol denotes the moon’s location. Changing Ψ changes the orientation of the moon around the planet. The red box denotes the area of the map shown in the main part of the plot. This figure shows how the position and size of the lunar caustic changes with different orientations of the moon. It is clear that the lunar caustic is smaller when the moon–planet axis is perpendicular to the star–planet axis (Ψ = 90°, 270°) than when it is aligned (Ψ = 0°, 180°), and thus these configurations when the moon is aligned are more likely to be detected.
Paper: Extreme Starlight Polarization Efficiency toward ζ Ophiuchi: A Case for Line-of-sight Foreground Subtraction
Authors: Jordan A. Bartlett, Henry A. Kobulnicky
Figure caption: RGB image of the target field in equatorial coordinates at 22 μm, 12 μm, and 3.4 μm, represented as red, green, and blue, respectively. The lengths of the polarization line segments indicate the values of PV, with 1% polarization equal to the length indicated in the legend. Similarly, the angles of the line segments indicate the PA of the targets, where PA = 0° is north. The symbols indicate the three distance groups of target stars, as depicted in the legend.