adsabs/AstroCLIMB huggingface dataset:
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Orbital eccentricities of TOI-1266 b (red), c (blue), and d (green) under the effects of tidal forces in a REBOUNDx model with initial planet parameters drawn from the TTV+RV joint posterior distribution. Time units are normalized by the uncertain Q/k2. The inset plot shows the last 10% of simulation steps after the eccentricities have damped to their stable long-term equilibria. For Q/k2 >  1200, the damping timescale is longer than 2 Gyr, consistent with the stellar age.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Posterior distribution for the eccentricities of TOI-1266 b and d with 1σ and 2σ contour lines (bottom) from TTV+RV joint fit, and the posterior probability distribution for the combined eccentricities of TOI-1266 b and d (top). TOI-1266 b prefers a moderate eccentricity if TOI-1266 d is not eccentric, or a small but nonzero eccentricity if TOI-1266 d is moderately eccentric.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Evolution of planetary eccentricities during the last 9.2 kyr (final 10%) of a rebound simulation with orbital parameters initialized from the TTV+RV joint fit posterior. All simulations displayed similar behavior: eccentricity oscillation around stable equilibria for the full simulation duration, with oscillation amplitudes ranging from  ∼0.01 to 0.1.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Corner plot of posteriors for planetary orbital period and initial transit time for TOI-1266 b, c, and d from the TTV+RV joint fit, made with the corner package. Modified periods are reported in units of days, while moditified initial transit times are in units of BJD–2457000.
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Corner plot of posteriors for planetary masses and eccentricities for TOI-1266 b, c, and d from the TTV+RV joint fit, made with the corner package (D. Foreman-Mackey 2016).
Paper: Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System
Authors: Michael Greklek-McKeon, Shreyas Vissapragada, Heather A. Knutson, Akihiko Fukui, Morgan Saidel, Jonathan Gomez Barrientos, W. Garrett Levine, Aida Behmard, Konstantin Batygin, Yayaati Chachan, Gautam Vasisht, Renyu Hu, Ryan Cloutier, David Latham, Mercedes López-Morales, Andrew Vanderburg, Carolyn Heffner, Paul Nied, Jennifer Milburn, Isaac Wilson, Diana Roderick, Kathleen Koviak, Tom Barlow, John F. Stone, Rocio Kiman, Judith Korth, Jerome P. de Leon, Izuru Fukuda, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Yugo Kawai, Kiyoe Kawauchi, Nobuhiko Kusakabe, John H. Livingston, Mayuko Mori, Norio Narita, Motohide Tamura, Noriharu Watanabe, Gareb Fernández-Rodríguez
Figure caption: Corner plots of the mass fractions from the four-layer ExoMDN interior structure models of TOI-1266 b (top) and TOI-1266 c (bottom).
Paper: Validating the Orbital Periods of the Coolest TESS Planet Candidates
Authors: Dillon J. Bass, Daniel C. Fabrycky
Figure caption: TOP: an example of a transit found and reported by the algorithm. The green line represents the best fit, and the dashed red line represents the predicted transit time for the alias. This specific case shows three reductions of the same data from different available pipelines. In each, a transit occurring 17.5 orbits after the originally reported transit is found. This is evidence that the reported period is at least double the true period for this particular planet. BOTTOM: an example of the table of transits produced by the algorithm. We report the sector searched, the alias of the period as the epoch after the original transit, a qualitative prediction of whether there was a transit, the measured depth, sigma heuristic, and calculated transit timing variation. These last three categories are only reported if the algorithm thinks there is a transit based on the data.
Paper: Validating the Orbital Periods of the Coolest TESS Planet Candidates
Authors: Dillon J. Bass, Daniel C. Fabrycky
Figure caption: Each X marker in this figure represents transits from six similar signal strength TOIs, plotted at the mean signal value of the group, in order to ensure a large enough number of transits for every data point. The adopted signal strength threshold marked by the red dotted line is at ﹩\delta \sqrt{D}=0.135﹩. Along the horizontal axis, we plot the 20 candidates from Sections 3.1 (in blue) and 3.3 (in black or red) with red text indicating a low signal strength candidate. The asterisks denote candidates that are in both sections.
Paper: Validating the Orbital Periods of the Coolest TESS Planet Candidates
Authors: Dillon J. Bass, Daniel C. Fabrycky
Figure caption: A comparison between the seven longest period (if fully confirmed at current values) candidates from this paper, and the KOI catalog (S. E. Thompson et al. 2018). Equilibrium temperatures and apparent magnitudes are taken directly from the respective TOI and KOI catalogs. Note that TOI-1894’s period could be half what is reported.
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: Combined full-scale RM and PI maps for 52° < ℓ < 86°. Top: RM for pixels with PI > 0.1 K (gray denotes the masked-out regions). Bottom: PI calculated as ﹩\mathrm{PI}=\sqrt{{\langle Q\rangle }^{2}+{\langle U\rangle }^{2}}﹩, where the averages 〈Q〉 and 〈U〉 are taken over the four ST frequency channels. These maps include the region in the top panel of Figure 5 in L10, as well as previously unpublished CGPS Phase 3 data and the latitude extensions of the Ordog-Brown fields. Note the instrumental polarization in the Cygnus X region, 75° < ℓ < 85°, arising from the GMIMS-HBN data.
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: Mock observations of a full-scale Stokes U image with the GMIMS-HBN and DRAO ST telescope parameters, and the resulting combined image. (a) The full-scale image. (b) The simulated single-antenna image. (c) The simulated aperture-synthesis image. (d) The uv-plane coverage used in each of the single-antenna and aperture-synthesis mock observations (black lines with gray shading), along with the feathering functions by which we multiplied the simulated single-antenna (blue) and aperture-synthesis (red) data. (e) The resulting reconstructed image from combining the mock observations to produce the full-scale map. (f) The residuals for comparison with the input map.
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: Radial profile of GMIMS-HBN (purple squares) and DRAO ST data (blue circles) in the uv-plane. This example shows Stokes U for band C of the Ordog-Brown field “OB12” (19h 52m, ﹩19^\circ 2{5}^{{\prime} }﹩). (a) The initial GMIMS-HBN and DRAO ST visibilities as a function of radial distance (baseline), ﹩r=\sqrt{{u}^{2}+{v}^{2}}﹩, from the center of the uv-plane. Here the GMIMS-HBN data were matched to the ST gridding and tapered to approximate the ST field of view (Section 3.1, (ii)). (b) Visibilities of GMIMS-HBN data with the beam deconvolved and the image tapered to the ST primary beam (Section 3.1, (iv)). The DRAO ST visibilities remain unchanged. (c) GMIMS-HBN and DRAO ST feathered versions (Section 3.2). The dashed vertical lines indicate the feathering region boundaries.
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 distribution of ratios of GMIMS-HBN to DRAO ST polarization data in the uv-plane. The ratio is calculated separately for each band of Stokes Q and U in the region of the uv-plane where the data sets of the 403 CGPS and Ordog-Brown fields used in this experiment are assumed to have overlapping coverage. The ratio should be close to unity for reliable signal at all baselines.
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: Combined full-scale RM and PI maps for 120° < ℓ < 140°, as in Figure 7. These maps cover the same region as the bottom panel of Figure 6 in L10.
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: Sample mosaics of GMIMS-HBN (left), DRAO ST (middle), and combined data (right) for Stokes U, band B. Regions of bright positive emission covering a few square degrees that are filtered out by the ST are incorporated from the GMIMS-HBN data.
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: Combined full-scale RM and PI maps for 102° < ℓ < 122°, as in Figure 7. These maps cover the same region as the top panel of Figure 6 in L10. Note that the missing region at ℓ = 112° is due to masking around Cassiopeia A, which is too bright for the ST imaging. The hook-shaped feature in PI at ℓ = 120° is an artifact in GMIMS-HBN.
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: Combined full-scale RM and PI maps for 84° < ℓ < 104°, as in Figure 7. These maps cover the same region as the bottom panel of Figure 5 in L10.
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: Combined full-scale RM and PI maps for 138° < ℓ < 158°, as in Figure 7. These maps cover the same region as the top panel of Figure 7 in L10.
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: RMs and peak Faraday depths as a function of Galactic longitude in the latitude range −3﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 ≤ b ≤ 5﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 for diffuse synchrotron emission compared to compact polarized point sources. (a) Aperture-synthesis-only data: extragalactic point-source RMs from CGPS (green), and the surrounding extended diffuse emission RMs (DRAO ST; blue). (b) Single-antenna-only diffuse emission RMs (GMIMS-HBN; purple) and full-scale combined diffuse emission RMs (red), both using the CGPS four-channel, 35 MHz bandwidth as in Figures 7–13. (c) Single-antenna-only diffuse emission peak Faraday depth from RM synthesis applied to the full GMIMS-HBN 1280–1750 MHz band. In all three panels, data are binned into 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 independent longitude bins, following A. Ordog et al. (2019). For all diffuse emission data bins the error bars are one standard deviation divided by the square root of the average number of beams contributing data to the bin. For the CGPS point-source RMs the error bars are the standard deviation divided by the square root of the number of sources in each bin.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Spectroscopic light curves from first, second, and third visits (top to bottom) from the Eureka! (left panel) and SPARTA (middle panel) pipelines binned to wavelength resolution of 0.1 μm and time resolution of 1 minute for better visualization. The ratio between the two pipeline products (SPARTA/Eureka) is shown in the right panel. Each red tick at the top and bottom of each plot indicates trimming applied to each visits (20 minutes for first and second visit). Note that in visit 3, a clear flux offset is seen near -0.06 days, so we trim an additional 50 minutes to avoid it. Dashed horizontal orange lines indicate the edges of each wavelength bin in 20 bins scheme. The planet’s eclipse is too shallow to see with this color bar.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Possible stellar spectra of LTT 1445A, including our adopted SPHINX model and other theoretical or empirical options. Spectra are shown both as surface flux (top) and as a ratio to the adopted SPHINX spectrum (bottom). The blue shading indicates the effect on the spectra of changing stellar effective temperature by ±150 K (1σ). Wavelengths beyond 10.6 μm (shaded in gray) fall within the shadowed region and may have less reliable observed absolute fluxes.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Posterior histograms of ﹩e\cos \omega ﹩ (top) and ﹩e\sin \omega ﹩ (bottom) along with physical interpretation axes for ﹩e\cos \omega ﹩, which sets secondary eclipse timing (Equation (4)), and ﹩e\sin \omega ﹩, which sets secondary eclipse duration (Equation (5)). Each vertical colored-region in the top panel indicates the observing duration of each visit. The purple dashed lines indicates the adopted values, which are the inverse-variance weighted average of the best fits from the three visits.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Top panel: a plot showing the measured scatter in the model residuals with 20 wavelength binning for each of the three visits (σresiduals) from the Eureka! (solid line) and SPARTA (dashed line) pipelines. Bottom panel: the ratio of measured scatter from Eureka!/SPARTA (σres,Eureka/σres,SPARTA). The gray bands show shadowed region at 10.6–12 μm. The measured scatter is calculated as the standard deviation of the 1 minute time bin residuals for each of the 20 wavelength bins described in Section 3.5.2.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Panchromatic systematics-corrected light curves for three individual visits (left to right) and an inverse-variance weighted average across all visits (far-right column). Data are shown from the SPARTA extracted fluxes; Eureka! light curves are similar. Light curves are binned in wavelength to dλ = 0.35 μm (20 wavelengths) and in time to dt = 2 minutes (transparent error bars) and dt = 20 minutes (opaque error bars). Eclipse models are shown in solid lines using depths from the individual-visit and weighted-average emission spectra in Table 2.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Broadband (5–10.62 μm) systematics-corrected light curves for three individual visits and a weighted average across all visits. Data are shown from the SPARTA extracted fluxes. Light curves are binned in wavelength in time to dt = 2 minutes (transparent error bars) and dt = 20 minutes (opaque error bars) for visualization purposes only. Eclipse models are shown with solid lines using depths from the individual-visit and weighted-average values in Table 2.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Maps of the systematics-corrected and visit-combined flux of the system, binned into large dλ = 0.35 μm wavelength bins and dt = 20 minutes time bins to decrease noise for visual display. Flux is normalized to 1 during eclipse, when the planet is behind the star. Both data (left) and best-fit eclipse models (middle) generally show the planet contributing more flux at longer wavelengths; residuals (data—model; right) are consistent with noise.
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 2, Zoe is a triaxial ellipsoid with a = 52 km, b = 30 km, and c = 13 km and Logos is a contact binary. Zoe is rotating along its c-axis 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). 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.