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Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: The bottom row shows the three MIRI images of the Vega debris system at the same orientation and field of view. Slight artifacts from the coronagraph persist in the 15.5 μm image, while it and the 23 μm image have a central region eliminated by the coronagraphs; the 25.5 μm image is missing the core because of saturation. The millimeter disk emission detected by ALMA (L. Matrà et al. 2020) is superimposed as contours on the 25.5 μm image for comparison. The top panel is an enlarged disk image at 25.5 μm, with the major disk features labeled for reference as they are discussed further in this paper. These features are: (1) the halo, visible at 25.5 μm to a radius of ∼33″ (∼250 au); (2) the outer disk (Kuiper-belt analog), extending from ∼10″ to 22″ (∼78–170 au) and the dominant feature in the ALMA image at 1.34 mm; (3) the inner disk, extending from the inner edge of the outer disk to as close as the images penetrate to the star; and (4) the dip in surface brightness of the inner disk from ∼5″ to 10″ (∼40−78 au).
Paper: Icarus Revisited: An Ancient, Metal-poor Accreted Stellar Stream in the Disk of the Milky Way
Authors: Paola Re Fiorentin, Alessandro Spagna, Mario G. Lattanzi, Michele Cignoni, Sara Vitali
Figure caption: Top panels: 3D velocity space for the 622 chemically selected nearby stars color coded according to eccentricity. Icarus stars are highlighted as filled dots within the Icarus locus (solid line). The dashed line encircles GSE (V. Belokurov et al. 2018; A. Helmi et al. 2018). Here we identify 376 objects with e > 0.7. A few stars from Thamnos (H. H. Koppelman et al. 2019), Sequoia (G. C. Myeong et al. 2019), and HS (A. Helmi et al. 1999) are present. Bottom panel: the V  ϕ –[Fe/H] distribution of the chemically selected ex situ sample, as above. In the background the full sample within 3 kpc of the Sun is shown. The chemokinematical selection thresholds, 140 < V  ϕ  < 160 km s−1 and [Fe/H] < −1 for the Atari disk/MWTD by M. K. Mardini et al. (2022) and V  ϕ  > 180 km s−1 and [Fe/H] < −0.8 for the metal-poor thin disk by S. Nepal et al. (2024), are represented by the dashed/solid lines, respectively.
Paper: Icarus Revisited: An Ancient, Metal-poor Accreted Stellar Stream in the Disk of the Milky Way
Authors: Paola Re Fiorentin, Alessandro Spagna, Mario G. Lattanzi, Michele Cignoni, Sara Vitali
Figure caption: Chemical validation of Icarus. Top panels: the [Y/Eu]–[Fe/H] and [Eu/Mg]–[Fe/H] distributions are shown for the subset of sources that have estimates of europium and yttrium abundance relative to iron without warnings from GALAH (left and right, respectively). Icarus, GSE, and the remaining chemically accreted/unevolved members are represented as in Figure 4. Solid boxes define the “accreted regions” that enclose the low-α stars from P. E. Nissen & W. J. Schuster (2010) and the “blob stars” reported by A. Carrillo et al. (2022). Bottom-left panel: as above, but the [Ba/Y]–[Fe/H] plane for all the sources with GALAH estimates of barium and yttrium abundance relative to iron with no warnings. Bottom-right panel: the [Ba/Mg]–[Mg/H] plane that identifies the contributions from AGB stars with respect to SNe II. In particular, for [Ba/Mg] ≳ 0.9, the AGB contribution is dominant.
Paper: Icarus Revisited: An Ancient, Metal-poor Accreted Stellar Stream in the Disk of the Milky Way
Authors: Paola Re Fiorentin, Alessandro Spagna, Mario G. Lattanzi, Michele Cignoni, Sara Vitali
Figure caption: Comparison to Simulations. Left panel: Toomre diagram of the chemically selected accreted/unevolved sample, color coded according to eccentricity, as in Figure 3. Along Icarus stars (filled dots), GSE, Thamnos, and HS members are present. The (conservative) kinematical selection threshold for halo stars, ∣∣ v  −  v  LSR∣∣ > 230 km s−1, is represented by the dashed line. The locus of Icarus is shown with solid line. The debris of the simulated 10°-inclination prograde satellite produced by G. Murante et al. (2010) and analyzed in P. Re Fiorentin et al. (2015, 2021) are overplotted (diamonds). Right panel: space of adiabatic invariants, L  xy –L  z , for Icarus stars. Again, the debris of the simulated 10°-inclination prograde satellite are overplotted for comparison (diamonds).
Paper: Icarus Revisited: An Ancient, Metal-poor Accreted Stellar Stream in the Disk of the Milky Way
Authors: Paola Re Fiorentin, Alessandro Spagna, Mario G. Lattanzi, Michele Cignoni, Sara Vitali
Figure caption: CMD diagram M G vs. ﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}﹩ for the (accreted) Icarus stars as shown in Figure 3. We show 71 Icarus stars with high-quality photometry: 68 objects have been corrected for extinction using 3D maps from J. L. Vergely et al. (2022; filled circles) while for three objects (open diamonds) more accurate A  V  estimates by means of the EXOFASTv2 code (J. D. Eastman et al. 2019) are derived. These stars are color coded according to metallicity [Fe/H]. Isochrones of ages 10, 12, 14 Gyr for [M/H] = –1.0 (magenta) and [M/H] = –1.3 (gray) are from A. Bressan et al. (2012) and P. Marigo et al. (2017).
Paper: Icarus Revisited: An Ancient, Metal-poor Accreted Stellar Stream in the Disk of the Milky Way
Authors: Paola Re Fiorentin, Alessandro Spagna, Mario G. Lattanzi, Michele Cignoni, Sara Vitali
Figure caption: Chemical validation of Icarus. The [(C+N)/O]–[Ni/Fe] plane for the subset of high-quality APOGEE giants (gray dots). Icarus and GSE members are shown respectively as filled and open circles, color coded by eccentricity. These are highlighted among the chemically selected accreted/unevolved stars (black open circles).
Paper: Icarus Revisited: An Ancient, Metal-poor Accreted Stellar Stream in the Disk of the Milky Way
Authors: Paola Re Fiorentin, Alessandro Spagna, Mario G. Lattanzi, Michele Cignoni, Sara Vitali
Figure caption:  N-body numerical simulation by G. Murante et al. (2010) of the disruption of an LMC-like galaxy, on a 10° inclination prograde orbit, progressively destroyed by the gravitational pull of a MW-like galaxy (see also G. Murante et al. 2010; P. Re Fiorentin et al. 2015, 2021). Top panels: the spatial distribution in the x–y plane are shown, from left to right, after T = 1.8 Gyr and T = 3 Gyr, as well as the final configuration for the particles of the 10° inclination satellite. Bottom panels: as above, but for the x–z plane.
Paper: Icarus Revisited: An Ancient, Metal-poor Accreted Stellar Stream in the Disk of the Milky Way
Authors: Paola Re Fiorentin, Alessandro Spagna, Mario G. Lattanzi, Michele Cignoni, Sara Vitali
Figure caption: Top panels: chemical distribution, [Mg/Mn]–[Al/Fe] (left) and [Mg/Fe]–[Fe/H] (right), for the 149,826 Gaia-APOGEE stars. The solid lines represent the adopted selection of 551 accreted/unevolved stars (color coded according to eccentricity), separated from in situ thick/thin-disk stars (gray). Bottom panels: same distribution as top panels for the 71 selected stars among the 237,979 Gaia–GALAH stars.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: Upper panel: disk color temperature radial profile derived from the flux ratios of two observed bands (the red color using F1550C and F2550W and the blue color using F2550W and PACS70). The spatial resolutions of MIRI and PACS are shown as horizontal bars for reference. Due to the different resolutions, limited field of view, and flux calibration uncertainties at different bands, the solid lines are the adopted dust temperature profile for the Vega system for the radial range of 1″−33″ and an r −0.5 extrapolation (green dotted–dashed line) outside that range. Bottom panel: disk optical depth radial profile derived from the color temperatures (upper panel), which is used to define several major radial zones (color shaded regions), as detailed in Section 4.2.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: Excess SED of the Vega system using the infrared photometry tabulated in Table A1 for constraining the hot/warm excess. The large blue squares are the photometry for constraining the hot excess emission (ν 2.8 spectral slope), where the points between 3 and 8 μm were obtained by subtracting a very accurate photospheric model from integrated measurements of Vega, and the other three points were measured with interferometers. The pink asterisks mark the values from interferometric measurements. The large red dots are the photometry using larger apertures and are well described by the warm dust emission with temperatures of 130−170 K, in contrast to the cold (∼50 K) outer disk emission.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: The model 25.5 μm disk morphology at 2 Myr for a PR-dominated disk, compared to the observed Vega F2550W image (first panel), all on the same display scale. The second panel assumes no planet (for details, see Section 5.2.2), while the third and fourth panels assume a 1 and 6 M ⊕ mass planet at 65 au (marked by white circles), respectively (for details, see Section 5.2.3). The models do not include the entire outer planetesimal disk and halo, hence the difference with the observed images at large radii.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: The color temperature distribution inferred from the flux ratio between F1550C and F2550W data. The red circles are derived using the observed F1550C and F2550W radial profiles, as shown in Figure 2. The acceptable temperatures using the ring-like parametric models are depicted as the pink color. The maximum dust temperature inside the 1″ region is ≲270 K, consistent with the warm excess SED (Figure 6) and no significant residual flux after PSF subtraction.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: The left panel shows some examples of the acceptable parametric models at F1550C (colored lines) in comparison with the WebbPSF off-axis 1550C PSF (dashed line). The power-law-only model extending to 0.″3 underpredicts the brightness in the region of 0.″6−0.″8, while the ring plus PL models produce slightly higher values. Both narrow (1 au) and broad (3 au) rings with the same total flux of 0.14 Jy at 15 μm produce satisfactory fits. The right panel shows some examples of the acceptable parametric models at F2550W for three different peaked ring locations (r  p ) and widths (r  w ) for the inner disk shown on the plot. The hashed areas depict the region either under the coronagraphic mask for F1550C or affected by the saturation for F2550W.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: Vega disk radial-surface-brightness profiles observed at four different wavelengths—F1550C (15.5 μm), F2300C (23 μm), and F2550W (25.5 μm) from JWST and PACS70 (70 μm) using Herschel—that are well described as broken power laws (i.e., linear behaviors in a log-log plot). The shading shows radial zones of different optical depth (see Figure 3).
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: The PR drag timescale of particles with β values of 0.1 and 0.5 to the inner edge of 69 au. The black solid and dashed lines mark the estimated collisional timescales, 0.5 Myr for the β = 0.5 and 0.7 Myr for the β = 0.1 particles within the model region, highlighting that they are able to travel to the inner edge unimpeded from a distance of 78 au (for details, see Section 5.2.2). Note that the collisional timescales are inversely proportional to ﹩\sqrt{r}﹩, which is ∼10% different in this narrow model region.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: Azimuthal disk brightness distribution in the “enhanced” F2550W disk image estimated by two metrics: the left panel as the residual flux, by subtracting the median value at each of the radii, and the right panel as the ratio between the observed and broken-power-law models. An annular width of 10 pixels (1.″1 ∼resolution) and azimuthal segments of 20° are used for the computation (for details, see Section 4.4). The red points with a connected line represent the gap area, while the blue points represent the outer disk.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: The upper panel shows the disk radial profiles in the r ∼ 4″−12″ region, using the three MIRI filters, in comparison to power-law profiles (solid lines). The bottom panel shows the dip profiles defined as the observed divided by the power-law model (i.e., the flux deficit). The dip is broad (∼20 au) and of similar depth (∼20%) in both F2550W and F2300C, but narrower and shallower in F1550C. The green solid line is the inner side of the F2550W profile but flipped to allow close comparison with the outer side. It implies that there is a slight asymmetry before and after the bottom of the dip.
Paper: Fast Methods for Computing Photometric Variability of Eccentric Binaries: Boosting, Lensing, and Variable Accretion
Authors: Daniel J. D'Orazio, Paul C. Duffell, Christopher Tiede
Figure caption: The 2D periodograms of the total accretion rate from prograde (left) and retrograde (right) CBDs onto binaries with orbital eccentricity e ranging from 0.0 to 0.8. The y-axis indicates the timescale in units of orbital periods. Black indicates regions where there is low power (see color bars), while purple and yellow regions have increasingly more power (on a log10 scale).
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: Disk surface brightness simulations highlighting the PR-drag transport of dust particles from the inner zone of the planetesimal belt located between 69 and 85 au. Each row represents a different time stamp of the evolution, starting from time zero at the top to 4 Myr at the bottom. The first column has no planet, while the following columns show the simulations where a 1, 3, and 6 M ⊕ planet, indicated as the white circle, is placed at 65 au. All images were convolved with a F2550W WebbPSF and are shown on the same display scale.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: The iterative reduction sequence for the F2550W data set. The columns show the four dither positions of the Vega data displayed on logarithmic scale with the boundaries (in megajanskys per steradian) given on the right side of each row. Details of the sequence (from top to bottom) are itemized in Section D.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: Locating the best PSF, using a scaling factor of 1.43, for the first rotation of Vega observations. The subtractions are shown for all nine SGD PSF positions, laid out in spatial order. For the first rotation, position 6 (marked with the yellow font) was clearly the best PSF to use.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: Top row: the F2550W PSF (HD 169305) images following the stage 1 and 2 pipeline reduction steps, without background or other corrections applied at the four dither positions (P1–P4). Image scaling is logarithmic between 911 and 2066 MJy sr−1. Bottom row: the same images, but with background correction applied, row and column artifacts removed, and the background base level adjusted. The images are scaled logarithmically here as well, between −6.9 and 1147 MJy sr−1.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: Left panel: the radial surface brightness profile of the no-planet dynamical model at various evolution times, compared to the observed JWST/MIRI F2550W profile. Right panel: the SED of the inner disk for the no-planet simulation at various stages of evolution, compared to the mid-infrared photometry.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: The background-subtraction process for the F2300C coronagraphic observations, shown for one of the Vega (top row) and one of the PSF observations (bottom row). All images are in logarithmic scaling but at different levels, to highlight their features.
Paper: Imaging of the Vega Debris System Using JWST/MIRI
Authors: Kate Y. L. Su, András Gáspár, George H. Rieke, Renu Malhotra, Luca Matrá, Schuyler Grace Wolff, Jarron M. Leisenring, Charles Beichman, Marie Ygouf
Figure caption: The background-subtraction process for the F1550C coronagraphic observations, shown for one of the Vega (top row) and one of the PSF observations (bottom row).
Paper: Fast Methods for Computing Photometric Variability of Eccentric Binaries: Boosting, Lensing, and Variable Accretion
Authors: Daniel J. D'Orazio, Paul C. Duffell, Christopher Tiede
Figure caption: The ratio ﹩Q\equiv \left\langle {\dot{M}}_{2}/{\dot{M}}_{1}\right\rangle ﹩ of accretion rates onto each binary component, averaged over a duration shorter than the disk precession frequency. The gray x’s are measured from our reconstruction, while the blue line is an analytic approximation for the extreme values. As a check of the values derived from the eccentricity sweep, the black points show results measured from all DD21 simulations with fixed eccentricities—black points with error bars represent the average and standard deviation of ﹩\min \left(Q,{Q}^{-1}\right)﹩ over a precession period of the disk , and the triangles denote the smallest values over the same range.
Paper: Fast Methods for Computing Photometric Variability of Eccentric Binaries: Boosting, Lensing, and Variable Accretion
Authors: Daniel J. D'Orazio, Paul C. Duffell, Christopher Tiede
Figure caption: Match of accretion-rate templates constructed with our code binlite (dashed curves) compared to the simulation output (solid curves). The total accretion rate onto the binary is plotted in black, while the breakdown of accretion onto each binary component is represented by the coral and teal curves. Accretion rates are plotted in units of the steady-state value ﹩{\dot{M}}_{0}﹩. The time series is displayed over 4 binary orbits comprising the center of a ∼20 orbit segment from which the Fourier reconstruction is built. Deviations between the reconstruction and simulation output for e = 0.5, 0.6, and 0.7 derive from interorbital variability (peak-to-peak variations), whose presence is apparent from the noisy region in the top-right portion of the corresponding periodogram in Figure 1. The binary components have equal masses, but the eccentric cavity causes preferential accretion that could equivalently be favoring either black hole. Hence, labeling of coral and teal curves can be interchanged.
Paper: Fast Methods for Computing Photometric Variability of Eccentric Binaries: Boosting, Lensing, and Variable Accretion
Authors: Daniel J. D'Orazio, Paul C. Duffell, Christopher Tiede
Figure caption:  V-band apparent magnitude lightcurves for prograde systems (see Section 4). Each panel is drawn for a different azimuthal viewing angle of the binary orbit relative to the argument of pericenter ϖ, and each differently colored line is for a different binary inclination to the line of sight. The dashed line represents a face-on binary and so exhibits purely accretion-rate-induced flux variability (compare to Figure 2). The strongest Doppler and lensing effects arise for the red line, drawn for a binary inclined close to the line of sight, I = 85°. Each panel assumes a binary with M = 2 × 109 M ⊙ and P = 1 yr, at a distance of 1.5 Gpc, and accreting at 10% of the Eddington rate.
Paper: Fast Methods for Computing Photometric Variability of Eccentric Binaries: Boosting, Lensing, and Variable Accretion
Authors: Daniel J. D'Orazio, Paul C. Duffell, Christopher Tiede
Figure caption: The same as Figure 6, except each panel is for a different binary orbital eccentricity and the same viewing azimuth. Note that, as in Figure 6, viewing angles ϖ and I affect only the Doppler boost and lensing signatures, while the binary eccentricity affects both accretion variability and Doppler+lensing magnifications.
Paper: Fast Methods for Computing Photometric Variability of Eccentric Binaries: Boosting, Lensing, and Variable Accretion
Authors: Daniel J. D'Orazio, Paul C. Duffell, Christopher Tiede
Figure caption: The same as Figure 2 but for retrograde, eccentric binaries. Here the accretion rates onto the primary (coral) and secondary (teal) are nearly identical because there is no precessing, circumbinary cavity.
Paper: Fast Methods for Computing Photometric Variability of Eccentric Binaries: Boosting, Lensing, and Variable Accretion
Authors: Daniel J. D'Orazio, Paul C. Duffell, Christopher Tiede
Figure caption: The same as Figure 2 but for a prograde, e = 0.01 system, where variability at 2Ω b  and Ω b /5 coexist.