adsabs/AstroCLIMB huggingface dataset:
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the mass fraction of N2+ (left) and O2+ (right) contributed by the additional plasma component for different densities and temperatures. The temperature range is that indicated by the N II λλ4041/5680 and O II λλ4089/4649 line ratios (Section 3.2.3). The N II λλ5666/5680 and O II λλ4662/4649 line ratios imply electron densities >5000–100,000 cm−3. If so, the additional plasma component accounts for up to about half of the N2+ and O2+ mass fractions.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: The top two panels present the [O III] electron temperature using the raw PV diagrams and those corrected for contamination due to recombination and charge exchange. The third panel presents the PV diagram of the difference map between the corrected and raw temperature maps. In all panels, the contours are of the [O III] λ4363 intensity. At the bottom, we plot the mean and median for the difference map as a function of the relative intensity in the [O III] λ4363 line. The error bars span from the 5th–95th percentiles.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: We present the PV diagram of the density derived from the [O II] λλ3726,3729 lines. The contours are those of the intensity of the emission in the O II λ4649 line (see Figure 6). Overall, the density implied by the [O II] lines is higher than implied by the [S II], [Cl III], or [Ar IV] lines. In addition, there is a similar structure of high densities where the [N II] λλ5755/6583 ratio is high (Figure 28).
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present PV diagrams for [O III] λ4363 (left) and [O III] λ4959 (right) of the observed emission (top), the contamination due to recombination (second), the contamination due to charge exchange (third), and the emission due to collisional excitation (bottom). The PV diagrams in the bottom row are the result of subtracting those in the second and third rows from the PV diagrams in the top row. Since the emission due to recombination and charge exchange is so faint, the normalization value for the intensity/color scale varies in the middle two rows by factors of 10–1000 with respect to the top and bottom rows. While recombination makes a small contribution to the [O III] λλ4363,4959 PV diagrams, charge exchange is much less relevant.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: Diagnostic time series on the night of 2MASS J0835+1953's candidate transit. From top to bottom: x centroid position, y centroid position, air mass, seeing FWHM (″), sky background (ADU), intrapixel position, and ALC. Unfilled circles with error bars show the mean of individual measurements (filled circles) over each block. In the x and y centroid panels, red lines indicate the intended guide field position of the target. None of the diagnostics were found to correlate significantly with target flux.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: Top: The full PINES light curve for 2MASS J0835+1953. Middle: The first night of data, showing the candidate transit event in more detail. The plot elements match those of Figure 3. The optimized QP-GP model fit no apparent variability and appears as a flat line with a narrow 1σ confidence region. Bottom: The corrected light curve, which is largely unchanged due to the flat QP-GP model in the middle panel. The S/N′ of the suspected transit event is indicated with an offset arrow.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: An example of a transit recovery in a single night of synthetic data. Panel (a) shows a simulated light curve of a time-variable target. The gray points show photometry with a 60 s exposure time and the black circles with error bars show the data binned over 12 minute intervals. We injected a transiting planet into the light curve with the properties given in the lower-right of panel (a). The blue line shows the composite transit+variability model. In panel (b), the light curve is resampled to mimic PINES observations, with 12 minute blocks of data obtained once per hour. The third block of data (colored in orange) is decremented by more than 2σ and initiates the QP-GP model fit shown in panel (c). The blue curve in panel (c) shows the mean of the QP-GP model that was fit to the unbinned data excluding points in the third block, and the shaded region indicates the 1σ uncertainty of the model. In panel (d), the flux has been corrected for the QP-GP model. The corrected S/N of the third block is indicated with an black arrow that is offset for clarity.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: The PINES light curves of 2MASS J0831+1538, 2MASS J0835+1953, and 2MASS J0835+2224 on the night of 2MASS J0835+1953's candidate transit event. All three light curves have been normalized ignoring the seventh block of data. Unbinned points are color-coded by time. The right-hand column shows the measured centroid positions, and the red circles show the average aperture size used for performing variable aperture photometry. For ease of comparison, the plot limits are the same in each column.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: Top: The full PINES light curve for 2MASS J1821+1414. Gray points show the 30 s photometry and black points with error bars show the photometry binned over the duration of each block. The alleged transit event (the third block on the first night) is colored in orange. The light curve was normalized ignoring this block of data. Middle: The first night of the 2MASS J1821+1414 light curve. The blue line shows the mean of the QP-GP model fit using unbinned data, excluding the block of the candidate transit. The blue shaded area indicates the 1σ uncertainty on the model. Bottom: The light curve corrected for the QP-GP model shown in the middle panel. The S/N′ of the suspected transit block, calculated as described in Section 3, is indicated with an offset arrow.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: The positions of 2MASS J0835+1953 in 2MASS (1998 November), Pan-STARRS (2010 April–2014 December), and PINES (2021 Feburary) images. All images are centered on the measured position during the PINES epoch. A red × with a surrounding circular aperture indicates the PINES position in all three panels.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: The distribution of S/N′ values for the 73 blocks of our light-curve sample that are decremented to more than 2σ.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: TESS light curves of Group-X candidate member TIC 159873822, aka TOI 2048. Data from PDCSAP (light blue), SAP (light brown), and our custom pipeline (orange) are shown; our custom pipeline was applied to the 2-minute-cadence data in this case for ease of comparison. All data have been binned to 30 minutes and offset vertically for clarity. From top to bottom, TESS sectors 16, 23, and 24  are shown. Fluxes have been normalized, and the time is given in TBJD (BJD −2,457,000). The locations of the transits of TOI 2048 b, the exoplanet we statistically validate in this work, are indicated by the vertical blue lines. The transits are evident in all three reductions, but the first (near TBJD = 1739) is affected by the systematics correction in the PDCSAP data. SAP and FFI data both show double-peaked rotational modulation; this light curve has a strong signal at both our favored P ⋆ = 8 days and at the half-period P ⋆/2 = 4 days. In the PDCSAP data, the asymmetry in the double peaks has been partially removed by the systematics correction. There is very little signal remaining at P ⋆, and rotation analysis favors P ⋆/2.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Contrast limits for close neighbors to TOI 2048, as found from Keck/NIRC2 AO imaging (at ﹩K^{\prime} ﹩ or λ = 2.124 μm; red), the absence of Gaia catalog sources (at G or λ = 0.639 μm; black), and the absence of elevated astrometric noise in the RUWE (at G; blue). These data provide the strongest constraints and are used to statistically validate TOI 2048 b. Also shown are contrast limits from Shane (at K  s , dashed green; and J, dashed cyan) and Palomar (at Brγ; dashed magenta). The detection limits rule out any binary companions above the hydrogen-burning limit at projected separations of ρ ≳ 25 au and equal-brightness binary companions at ρ ≳ 4 au.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Li EW sequences as a function of Gaia color. Colors have been corrected for reddening. Group-X candidate members from Tang et al. and Fürnkranz et al. and Friends of TOI 2048 with ﹩{\rm{\Delta }}{v}_{\tan }\lt 2﹩ km s−1 are shown as large, filled orange circles. Open gray circles are Friends with ﹩{\rm{\Delta }}{v}_{\tan }\gt 2﹩ km s−1. TOI 2048 is the green star. Group-X is compared to the Pleiades in blue (blue circles; Bouvier et al. 2018), M34 (green diamonds; Jones et al. 1997), and the Hyades (purple circles; Cummings et al. 2017). All nondetections are plotted as upper limits, denoted by downward-pointing triangles. The Group-X color–Li sequence lies above the Hyades and below Pleiades; M34 provides the closest match.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Rotation period vs. Gaia G BP − G RP color for stars in Group-X and comparison clusters. All colors have been corrected for reddening. Group-X candidate members from Tang et al. and Fürnkranz et al. and Friends of TOI 2048 with ﹩{\rm{\Delta }}{v}_{\tan }\lt 2﹩ km s−1 are shown as large, filled orange circles. Open orange circles are Friends with ﹩{\rm{\Delta }}{v}_{\tan }\gt 2﹩ km s−1. TOI 2048 is the green star. In the right panel, Group-X is compared to Pleiades (blue circles; Rebull et al. 2016) and Praesepe (purple circles; Rampalli et al. 2021). The Group-X color−rotation sequence lies above the Pleiades and below the Hyades. On the left, Group-X stars are compared to NGC 3532; there is excellent agreement between the Group-X color−rotation sequence and that of NGC 3532.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Galactic positions (top) and proper motions (bottom) of candidate Group-X members from Tang et al. and Fürnkranz et al. (filled pink and purple circles; pink if the star appears in only one source, and purple if it appears in both) and Friends of TOI 2048 (open orange circles). TOI 2048 is marked with a green star, falling near the extremes of the association. Friends of TOI 2048 with velocity offsets <2 km s−1 are the thick orange circles, and those with larger velocity offsets (up to the threshold of 5 km s−1) are thin orange circles. The green star marks TOI 2048; TOI 2048 is included in the candidate member list from Tang et al. (2019) but not that from Fürnkranz et al. (2019). In the position plot, the dashed circle shows the 25 pc search radius we used for FindFriends.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Absolute magnitude vs. color for candidate members from Tang et al. and Fürnkranz et al. (filled purple circles) and for Friends of TOI 2048 (open orange circles). Stars with RUWE > 1.3, indicating likely binarity, are shown as black crosses; as expected, these stars tend to lie above the main sequence. TOI 2048 is marked with a green star. The inset includes PARSEC isochrones (blue lines); the 200–400 Myr isochrones are consistent with the cluster. The magnitudes of the stars in Group-X have been corrected for extinction (although this is insignificant); the models have not. The white dwarfs and giants are discussed in Section 4.2.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Example fit from our SED analysis. The black line indicates the template spectrum (a G8V), and the blue line shows the BT-SETTL models used to fill in gaps. Synthetic photometry from the template and model is shown in green. Observed photometry is colored based on the source, with vertical errors corresponding to the measurement errors and horizontal errors corresponding to the filter width. The bottom panel shows the fit residual in units of standard deviations.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Li–age posteriors from BAFFLES. Individual age posteriors are shown as dashed lines colored by stars’ B − V magnitudes. The ensemble posterior is shown with the solid black line and has been divided by 2 for visual purposes. The median age of Group-X is 257 ± 27 Myr.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: TESS-SPOC data (gray points) and Gaussian process stellar variability model (blue curve). Time is given in TJBD, and the flux units are parts per thousand (ppt). The transits of TOI 2048 b were removed before fitting and are not shown; outliers from the preliminary fit are also not shown.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Posterior distribution of fit (i ⋆, Ω⋆) and randomly sampled (i disk, Ωdisk) for both inner and outer disks yields a posterior distribution of θ, the mutual inclination angle between the binary orbit and the disk component. As in Czekala et al. (2019), the mutual inclination of the outer disk for this system is multimodal, but dramatically misaligned (θ ≫ 3°) regardless of the choice of Ω⋆. Interestingly, one family of θ ⋆−out is nearly perpendicular, similar to the configuration described in Price et al. (2018).
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: VisAO platescale as measured in various VisAO filters over time. The orange shaded region, centered on the horizontal orange dashed–dotted line, represents the previous astrometric solution of Males et al. (2014) using data taken in the Ys filter in 2014. Note the agreement between our measurement of the same Ys data (red diamond) and their value. We note that the Hα observations suffered from poor observing conditions and an unfavorable observing strategy for astrometry, which resulted in very low signal-to-noise on the B2–B3 pair. No obvious trend in platescale with wavelength or time is present, and therefore we adopt the weighted average and standard deviation on the weighted average (represented by the blue dashed line and shaded region, respectively) as the updated platescale and platescale error for the instrument.