adsabs/AstroCLIMB huggingface dataset:
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: For Option 3, Zoe is a contact binary with semimajor axes of 18 × 17 × 16 km and 16 × 15 × 14 km and Logos is also a contact binary. Zoe is rotating with a rotational period of 3 days. In this Figure, we report four screenshots centered on Logos at different times (T1 to T4) to show the system configuration before (T1), during (T2 and T3), and after (T4) the 2027-3 mutual event (see Table 5). Logos will cast its shadow on Zoe (inferior event) during this mutual event. In the lower plot, we represent the brightness variation of the system as a function of time (black continuous line). The vertical cyan lines indicate the timings of the screenshots while the red vertical lines delimit the duration of the mutual event. The “first contact” red line indicates when the mutual event starts and the “last contact” red line indicates when the mutual event stops.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: For Option 1, Zoe is a spherical object and Logos is a contact binary. In this Figure, we report four screenshots centered on Logos at different times (T1 to T4) to show the system configuration before (T1), during (T2 and T3), and after (T4) the 2027-3 mutual event (see Table 5). During this mutual event, Logos will cast its shadow on Zoe (inferior event). In the lower plot, we represent the brightness variation of the system as a function of time (black continuous line). The timings of the screenshots are indicated by the vertical cyan lines while the red vertical lines delimit the duration of the mutual event. The “first contact” red line indicates when the mutual event starts and the “last contact” red line indicates when the mutual event stops.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: We model the event 2027-3 assuming that Zoe is a triaxial ellipsoid with b/a=0.58 and c/a=0.42, but we use different rotational periods for Zoe. One can appreciate that Zoe’s rotational period dictates the morphology and depth of the event.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2026-1 event assuming that Zoe is a spherical object.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2026-1 event assuming that Zoe is an ellipsoidal object.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2027-4 event assuming that Zoe is a triaxial ellipsoid.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2027-4 event assuming that Zoe is a contact binary.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2027-4 event assuming that Zoe is a spherical object.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2029-7 event assuming that Zoe is a contact binary.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2028-5 event assuming that Zoe is an ellipsoidal object.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2028-6 event assuming that Zoe is an ellipsoidal object.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2029-7 event assuming that Zoe is an ellipsoidal object.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2028-5 event assuming that Zoe is a spherical object.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2028-6 event assuming that Zoe is a spherical object.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2028-6 event assuming that Zoe is a contact binary.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2028-5 event assuming that Zoe is a contact binary.
Paper: Logos-Zoe: A Contact Binary Triple System in the Trans-Neptunian Belt
Authors: Audrey Thirouin, Keith S. Noll, William M. Grundy, Scott S. Sheppard, Felicity Escarzaga, Brian Donnelly
Figure caption: Modeling of the 2029-7 event assuming that Zoe is a sphere.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: Keck OSIRIS K-band jackknife image from the 2023 observing run. The images have a pixel size of ∼9.942 mas pixel−1. Panel (A) marks the target as the pink dot and the approximate position of the residual with a green dot. Panel (B) shows the residuals from a 1-star fit, and panel (C) shows the smooth residuals from a 2-star fit. All stars in the frame are fitted with the PSF model and subtracted to produce the residual frame.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: Best-fit MCMC contours (68.3%, 99.5%, 99.7%) of stellar X and Y pixel positions. Top panels: Lens (green) and one source star (pink). Bottom panels: Lens (green) and two source stars (pink and blue). These contours are overplotted on the 2023 jackknife K-band OSIRIS image (left), and the residuals of that image (right). Each frame is ∼0﹩\mathop{.}\limits^{\unicode{x02033}}﹩35 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩35.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: OGLE identification of OB161195. Red dots on the OGLE image are OGLE detected stars. The target is shown as a blue dot, which is the centroid measured at the peak of magnification. In the OGLE reference image, it is a blend of faint stars. The Keck image shows the OGLE stars transformed to the Keck grid, in red, and the target in blue. The Keck OSIRIS frame is 9.942 mas pixel−1, and the OGLE frame is 260 mas pixel−1.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: Best-fit MCMC contours of the source and lens pixel positions (X, Y) for 2020, 2021, and 2023. The left panels show the target, and the right panels show the 1-star residual with the source subtracted. The lens best-fit positions are in green and the source in red.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: CMD for the OB161195 field. In black are the OGLE-III stars within 90″ of the target, and with the HST CMD of the Stanek window in green (K. Z. Stanek et al. 1994; S. K. Terry et al. 2020). The red spot is the Red Clump centroid, the orange and blue are source 2 and source 1, respectively. In purple is the location of the lens.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: The OB161195 best-fit 2L2S light curve with constraints from the high angular resolution Keck data—using the full data set (MOA, OGLE and KMTNET).
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: Mass–distance relations for OGLE-2016-BLG-1195, obtained using the Einstein ring radius (θE) and parallax (πE) from remodeling the light curve with the measured 2023 Keck μrel constraint, and also the 2023 Keck K-band flux constraint (KL). The planet-host properties are derived from the intersection of the two most reliable mass–distance relations. The host system properties estimated by B17 and S17 are shown as crosses in blue and green, respectively. The Spitzer parallax constraint obtained by S17 is shown in gray. This is a simplified presentation of the results that include errors measured on the host star magnitudes and average errors on the θE values.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: Bayesian posterior probability distributions for the host and planetary companion mass, their separation, and lens system distance. Using only light-curve constraints are shown in blue, and with additional constraints from the follow-up Keck data in red. The center of the distributions (68.3%) are shaded in dark red and blue. The remaining 95.4% are shaded with lighter hues. The dark vertical line indicates the median of the probability distribution of each parameter.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: The 2020 and 2023 Keck narrow image data of the misidentified target star, and the 1-star fit residual image. The best-fit MCMC contours of the two stars’ pixel positions (X, Y) are shown in cyan (Star B) and in red (Star A). North is up and east is to the left.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: Two-dimensional parallax distribution for the lens in OB161195. The blue cross indicates the value obtained from this work, with constraints from Keck, and the gray crosses are the values presented in S17 using the Spitzer data set. The color-scale shows the relative probability based on a Galactic model.
Paper: OGLE-2016-BLG-1195Lb: A Sub-Neptune Beyond the Snow Line of an M-dwarf Confirmed by Keck Adaptive Optics
Authors: Aikaterini Vandorou, Lisa Dang, David P. Bennett, Naoki Koshimoto, Sean K. Terry, Andrzej Udalski, Jean-Philippe Beaulieu, Christophe Alard, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Tarik Bouchoutrouch-Ku, Andrew A. Cole, Nicolas B. Cowan, Jean-Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Sylvain Cetre, Jim Lyke, Eduardo Marin, Peter Wizinowich
Figure caption: Left panel: Three different models of the Spitzer data. The flat-line model from the 2019 baseline Spitzer data has a χ2 = 120.059. The t0 model inferred from S17 has a χ2 = 121.263. The t0 model inferred from the Keck follow-up results has a χ2 = 102.117. Right panel: S17 ’s original magnification curve from Spitzer photometry as a comparison, with magnification ranging from −1 < y < 7.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: H﹩{}_{3}^{+}﹩ emission power upper limits in the (left) Q(1,0) and (right) Q(3,0) emission lines. In both figures, the colored points are nondetections, while the lines represent model estimates. Several of the models (S. Miller et al. 2000; R. V. Yelle 2004; T. T. Koskinen et al. 2007) are only estimates of total H﹩{}_{3}^{+}﹩ power, rather than the Q(1,0) or Q(3,0) individual transition power; therefore, we have assumed that the Q(1,0) transition emits 0.5% and the Q(3,0) emits 0.3% of the total H﹩{}_{3}^{+}﹩ power. For the model from J. M. Chadney et al. (2016), we use that of AD Leo (M0V). While our upper limits are an order of magnitude below other detection limits in the literature, they are still an order of magnitude away from model estimates of H﹩{}_{3}^{+}﹩ emission power for hot Jupiters. However, these models do not include magnetic fields which could elevate the supposed H﹩{}_{3}^{+}﹩ emission.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Injection-recovery tests for WASP-80b. These results show that we would have recovered H﹩{}_{3}^{+}﹩ with strong significance for the abundances −1 > logN > −4. We would not recover −5 > logN > -6 with the current models and data.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Same as Figure 12 but for WASP-69b. In this case, a VMR of logN = −5 would be additionally be recovered with SNR > 3.
Paper: Stringent Limits on H﹩{}_{3}^{+}﹩ Emission from the Hot Jupiters WASP-80b and WASP-69b
Authors: Tyler Richey-Yowell, Evgenya L. Shkolnik, Joe Llama, James Sikora, Peter Smith
Figure caption: Same as Figure 10 but for WASP-69b.
Paper: TESS Light Curve of the Interacting Binary W Serpentis
Authors: Douglas R. Gies, Katherine A. Shepard, Aman Kar, Noel D. Richardson
Figure caption: Above: a schematic diagram of the components of W Ser as seen from above the orbital plane. The Roche-lobe-filling, mass-donor star (right) launches a gas stream (central dark curve) that enters the accretion torus (light gray disk) surrounding the mass gainer (white circle at left). The gas from the cool donor star mixes in with the hotter torus gas, and this results in a slightly cooler temperature in the region where the gas stream meets the torus. The gas in the outer radial parts of the torus gradually rises in temperature as the accreted gas is carried around the outer disk. The local temperatures assumed in the model are labeled in the outer regions of the disk. The dashed line indicates the Roche lobe boundary of the mass gainer, the plus sign shows the location of the center of mass, the arrows show the orbital velocities of the stars, and the orbital phases for different orientations are given in the periphery of the diagram. The spatial tick mark interval corresponds to one half of the semimajor axis (0.5 × 48.69R⊙ = 24.34R⊙). Below: the appearance of the binary model at orbital phase 0.25 for an inclination of i = 101∘. The dotted circle at left shows the location of the mass gainer star that is hidden by the vertical extent of the outer torus.
Paper: TESS Light Curve of the Interacting Binary W Serpentis
Authors: Douglas R. Gies, Katherine A. Shepard, Aman Kar, Noel D. Richardson
Figure caption: The TESS light curve of W Ser from 2024 July shown as normalized flux as a function of barycentric Julian date (tiny black symbols). The gray-shaded line shows the ELC model light curve that includes a systematic temperature drop along the rim of the accretion torus surrounding the mass gainer. The residuals from the fit are shown below (offset by +0.2) together with the sinusoidal signal from the peak in the power spectrum (dotted line).
Paper: TESS Light Curve of the Interacting Binary W Serpentis
Authors: Douglas R. Gies, Katherine A. Shepard, Aman Kar, Noel D. Richardson
Figure caption: The light curve of W Ser obtained in 1956 by A. Fresa (1957) plotted as a function of orbital phase. They gray-shaded line shows the model light curve from the TESS observations (Figure 1). The photoelectric measurements from A. Fresa (1957) are available in machine-readable format in the electronic version of this paper.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: TESS Light Curve of the Interacting Binary W Serpentis
Authors: Douglas R. Gies, Katherine A. Shepard, Aman Kar, Noel D. Richardson
Figure caption: The CLEANed discrete Fourier transform (CDFT) of the residuals from the observed minus model light curve of W Ser. The vertical dotted line marks the primary oscillatory peak at a frequency of 0.357 cycles per day.
Paper: TESS Light Curve of the Interacting Binary W Serpentis
Authors: Douglas R. Gies, Katherine A. Shepard, Aman Kar, Noel D. Richardson
Figure caption: The CDFT of the residuals from the 1956 observed minus model light curve. The markers above the main peaks indicate the frequency and uncertainty range of signals corresponding to the orbital period (1/P), half the orbital period (2/P), and the fast oscillation period found in the TESS light curve (f(TESS)). The dotted line shows the CDFT from the TESS data (Figure 3).
Paper: An Extremely Hot Pulsating Prewhite Dwarf from OGLE
Authors: Paweł Pietrukowicz, Klaus Werner, Mateusz J. Mróz, Milena Ratajczak
Figure caption: Images with star OGLE-GD-WD-0001 (in their centers) in three different bands: V (left panel) and I (right panel) from the OGLE survey and Hα (middle panel) from the VPHAS+ survey (conducted on the ESO VLT Survey Telescope; J. E. Drew et al. 2014). Each image is ﹩1\mathop{.}\limits^{^{\prime} }0﹩ on the side. North is up and east is to the left. The OGLE images are cropped templates for image subtraction that were stacked from several single frames.
Paper: An Extremely Hot Pulsating Prewhite Dwarf from OGLE
Authors: Paweł Pietrukowicz, Klaus Werner, Mateusz J. Mróz, Milena Ratajczak
Figure caption: Normalized spectrum of OGLE-GD-WD-0001 together with the best fit.
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: The steps in preparing a GMIMS-HBN map to be combined with the corresponding DRAO ST field. This example shows Stokes U for band B of one of the Ordog-Brown fields (OB12). (a) Tapered GMIMS-HBN map, regridded to match DRAO ST field grid spacing; (b) the GMIMS-HBN field transformed to the uv-plane; (c) the visibilities divided by the single-antenna beam transform to deconvolve the beam from the image; (d) the deconvolved visibilities low-pass-filtered to remove the unusable high spatial frequency components; (e) the resulting visibilities transformed back to the image plane.