adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: The RVs during the transit event of HD 93963 Ac on 2024 May 3 (UTC), measured by Keck/KPF spectra. For each data point, the black error bar is the observational uncertainty while the additional gray one indicates the extra jitter from the fitting. In the upper subplot, the solid red line is the final best-fit model (﹩\lambda =1{4}_{-19}^{+17}﹩ degrees), incorporating the RM effect, Gaussian process (GP), and RV long-term trend, and the red shade shows the 1σ uncertainty. The solid blue line is also the final best-fit model but without the GP plotted. In the lower panel, the residuals are given by subtracting the best-fit model, including the RM, GP, and long-term trend.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: Time-varying probability that an observer at a fixed position could detect both HD 93963 Ab and Ac transiting their host star. The left and right panels are coplanar and noncoplanar initialization, respectively, obtained from analytical solutions. The color of the solid lines indicate the initial true stellar obliquity. A comparison derived from N-body simulations is shown in Figure 14 in the Appendix.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: The estimated mutual inclination between HD 93963 Ab and Ac as a function of the initial true stellar obliquity (ψ). The left and right panels are respectively initialized from coplanar and noncoplanar configurations. The purple and olive colors represent results from the N-body simulations and the analytical solution, respectively. The red dotted lines mark the prediction by Equation (16) in C. Spalding & K. Batygin (2016) under the coplanar initialization.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: The estimated probability of both HD 93963 Ab and Ac transiting their host star on the whole celestial sphere as a function of the initial true stellar obliquity (ψ). The left and right panels are respectively initialized from coplanar and noncoplanar configurations. The purple and olive colors represent results from the N-body simulations and the analytical solution, respectively.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Comparison of our work to previous SLS publications in angular separation vs. physical separation. Confirmed and candidate companions in this work (orange stars) are plotted against known SLSs from B. Zuckerman (2014, red), H13 (and references there in; blue), WD–MS systems in Gaia DR3 from H. T. Noor et al. (2024, purple), wide PCEBs in Gaia from N. Yamaguchi et al. (2024, magenta), and two SLSs detected via astrometric acceleration and AO imaging in B. P. Bowler et al. (2021, yellow). The gray density gives an adaptation of W04 Figure 10 (right) to our parameter space, with contours marking 1σ, 2σ, and 3σ confidence intervals. We illustrate the approximate limits of MagAO-X search space between 120 mas (5λ/D in ﹩{i}^{{\prime} }﹩, a conservative estimate of smallest angular resolution achievable) and 3” (half the detector field of view) by gray dashed–dotted lines; the light gray dotted line marks the expected capabilities of fully optimized coronagraphs on MagAO-X with an ≈1λ/D inner working angle. Our survey can bridge a gap between SLS direct imaging and detection via other means.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Number of WDs expected and observed within 100 pc local volume. The dashed blue line is the number of WDs predicted by theory (see text for details); the purple line is the 100 pc Gaia sample from F. M. Jiménez-Esteban et al. (2023); the magenta line is the 100 pc SLS sample from A. Rebassa-Mansergas et al. (2021), corrected for the 80% completeness of their sample and the 9% completeness of their sample from the total underlying SLS population; the orange line is the new SLS sample from P. K. Nayak et al. (2024); and the black line is the sum. We did not include SLS surveys for which the objects are resolved by Gaia, since they would be captured in the F. M. Jiménez-Esteban et al. (2023) catalog. The dotted gray line (a) shows the approximate detection limit for Gaia for a WD at 100 pc, assuming a detection limit of G = 20 mag; the dashed gray line (b) shows the detection limit at the background limit of the deepest observations in this work, a flux contrast of approximately 5 × 10−5, to a G0 type star at 100 pc; and the dotted–dashed gray line (c) shows the background limit if we are able to achieve a 5× deeper contrast. The purple dotted lines mark the WD absolute V-band magnitudes as a function of cooling age (Eqution (5)). The faintest WDs are still being missed, however the number of observed WDs from 11 to 14 mag much more closely matches theory than in B. Katz et al. (2014). Our survey is already probing all but the oldest WDs in the background-limited regime.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Completeness maps for nondetections. Orange horizontal lines mark the WD companion Teff and uncertainty predicted in R20. (a) TYC 1262-1500-1, (b) HD 87147, (c) BD-09 3292, (d) CD-28 10038, (e) HD 109439, (f) TYC 169-1942-1, (g) TYC 1447-1616-1, (h) HD 146740, (i) HD 7918, (j) CD-27 191, (k) HD 680, and (l) BD-01 220.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Reproduction of Figure 1 from K. El-Badry (2024) showing the sensitivity regimes of various multiplicity metrics for a 2 M⊙ binary. The purple filled region indicates the regime of the targets in our survey, at ≈100–700 pc; the inner and outer astronomical unit ranges of the purple region are the inner and outer angular sensitivities from Figure 9 converted to physical separation as a function of distance. The orange filled region shows the sensitivity regime for fully optimized coronagraphs (see Section 4.3) They fall outside the regime for which RUWE and PMa are most sensitive, and even fall inside the regime eventually resolvable by Gaia. Our detected companions are too faint to be resolved by Gaia even if they do fall within the spatially resolvable region. That these metrics are useful but incomplete for assessing WD multiplicity, and our survey will probe a regime not probed by any other multiplicity metric.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Contrast curves for nondetections. The colored regions mark the 2σ, 3σ, and 5σ limits as a function of separation for each system and reduction method given. Separation is given in both λ/D units (bottom) and milliarcseconds (top); contrasts are given in flux contrast units. The black line gives the 1σ noise floor for each observation. The classical ADI reduction got lower limits for BD-09 3292 than KLIP ADI. Contrast curves were computed using the method described in Section 3.2.1.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: PMa plot for HD 92588 and HD 104018 using the methodology of P. Kervella et al. (2022). This plot describes the (minimum) mass of an object as a function of separation that would produce the observed PMa between the Hipparcos and Gaia observations. Top: the orange vertical line marks the separation of HD 92588 CC1 from HD 92588, and the horizontal orange line marks the approximate mass of a mid M dwarf. If HD 92588 CC1 is an M dwarf–WD binary, it would lie even higher on this plot. Bottom: the orange vertical line marks the separation of HD 104018 CC1 from host, and the horizontal vertical line marks the approximate mass of the WD. Both companions fall well above the sensitivity curve, suggesting that neither is responsible for the observed acceleration and may be unassociated.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Common proper motion plot for TYC 4831-473-1 B. The offset from TYC 4831-473-1 in R.A. and decl. are given on the x- and y-axis respectively, with our observed position in 2022 and 2024 are given by the blue and red circles. If TYC 4831-473-1 B were an unmoving background star, it would follow the black track relative to TYC 4831-473-1, given by the host star’s proper motion and parallax; we would have observed TYC 4831-473-1 B at the location of the red diamond in 2024. Our observed location is highly discrepant with this predicted location and moving in the opposite direction in R.A. We conclude that TYC 4831-473-1 B is not a background star, and posit that the apparent motion of TYC 4831-473-1 B is due to orbital motion. More observations are required to begin to pin down orbital parameters.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Map of completeness to hydrogen-dominated WD companions in our survey to date. The contours and shading mark the fraction of WD companions we would have detected in our survey in regions of (SMA,Teff) space, with 1.0 being all hydrogen-dominated WDs hotter than 5000 K being detected, and 0.0 being none detected.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Reduced images for the systems without a candidate signal. Each system was reduced using the method indicated. All point-source-like signals have been determined to be speckles.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: Basic properties of the sample of LITTLE THINGS dIrrs (black) and the subsample with ultradeep imaging (red). SFRD is the SFR divided by the area encompassed by one disk scale length. ﹩{\mu }_{0}^{V}﹩ is the central surface brightness in the V band. The sample of LITTLE THINGS dIrrs with ultradeep imaging data (red) samples the range of characteristics of the larger LITTLE THINGS sample.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: DDO 43’s objects with FUV emission in the far outer disk are circled in black/yellow on the V (top) and FUV (bottom) images. The red ellipses define the far outer disk. The blue circles are other objects identified in the far outer disk but without FUV emission.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: DDO 46’s objects with FUV emission in the far outer disk are circled in black on the V (top) and yellow on the FUV (bottom) images. The red ellipses and blue circles are as in Figure 4.
Paper: Ultradeep Imaging of Nearby Dwarf Irregular Galaxies: Young Objects in the Far Outer Disk
Authors: Deidre A. Hunter, Hong-Xin Zhang, Bruce G. Elmegreen, Ella R. Castelloe, Hannah Michaye Ledford, Ishara Nisley, Ryuga Hatano
Figure caption: V-band image of DDO 46. Green contours and red ellipses are as in Figure 2. The outer ellipse has been adjusted in x and y to include the stellar extension to the south.
Paper: Survey of Oxygen-rich AGB Stars Using the KVN 4 Receiving Bands—SMASTES. I.
Authors: Hyeon Baek, Se-Hyung Cho, Jaeheon Kim, Seung-Min Son, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: Distributions of the peak and integrated flux (P.F and I.F) ratios of H2O to SiO11. (a) P.F of SR, (b) I.F of SR, (c) P.F of Mira, (d) I.F of Mira, (e) P.F of OH/IR, and (f) I.F of OH/IR. The solid line represents the average value of the flux ratios.
Paper: Survey of Oxygen-rich AGB Stars Using the KVN 4 Receiving Bands—SMASTES. I.
Authors: Hyeon Baek, Se-Hyung Cho, Jaeheon Kim, Seung-Min Son, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: Distributions of the P.F and I.F ratios of SiO12 to SiO11. (a) P.F of SR, (b) I.F of SR, (c) P.F of Mira, (d) I.F of Mira, (e) P.F of OH/IR, and (f) I.F of OH/IR. The solid line represents the average value of the flux ratios.
Paper: Survey of Oxygen-rich AGB Stars Using the KVN 4 Receiving Bands—SMASTES. I.
Authors: Hyeon Baek, Se-Hyung Cho, Jaeheon Kim, Seung-Min Son, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: Distributions of the P.F and I.F ratios of SiO21 to SiO11. (a) P.F of SR, (b) I.F of SR, (c) P.F of Mira, (d) I.F of Mira, (e) P.F of OH/IR, and (f) I.F of OH/IR. The solid line represents the average value of the flux ratios.
Paper: Binary Star Orbits. VI. The Interferometric-spectroscopic Binary 73 Leo
Authors: Brian D. Mason, R. Elizabeth M. Griffin, R. T. Zavala, Christian A. Hummel, Haley M. Hurowitz, Jonathan L. Hurowitz, William I. Hartkopf, Ellyn K. Baines, Stephen J. Williams, Rachel A. Matson
Figure caption: Radial-velocity data from Table 4, with the new RV-orbit solution fitted to them. Open triangles are the seven early (1978–9) Cambridge Coravel RVs, filled squares are the 44 later ones from the Cambridge Coravel, and include four values measured on other Coravel-type instruments, while the 47 red triangles represent the velocities from DAO spectroscopy.
Paper: Binary Star Orbits. VI. The Interferometric-spectroscopic Binary 73 Leo
Authors: Brian D. Mason, R. Elizabeth M. Griffin, R. T. Zavala, Christian A. Hummel, Haley M. Hurowitz, Jonathan L. Hurowitz, William I. Hartkopf, Ellyn K. Baines, Stephen J. Williams, Rachel A. Matson
Figure caption: Plot of measurements for 73 Leo made with the NPOI. The ellipse represents the final (i.e., combined) orbit (Section 3). The location of the primary is at the origin; the relative positions of the secondary are plotted together with their error ellipses. The vector from the origin indicates the periastron point. The scales (in milliarcseconds, mas) in R.A. and decl. are marked on the bottom and left axes, respectively.
Paper: Binary Star Orbits. VI. The Interferometric-spectroscopic Binary 73 Leo
Authors: Brian D. Mason, R. Elizabeth M. Griffin, R. T. Zavala, Christian A. Hummel, Haley M. Hurowitz, Jonathan L. Hurowitz, William I. Hartkopf, Ellyn K. Baines, Stephen J. Williams, Rachel A. Matson
Figure caption: NPOI measures of the magnitude difference of 73 Leo. The weighted mean of 3.62(0.06) (P. R. Bevington & D. K. Robinson 2003) is shown as a dashed line.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Southern μ-Sagittariids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Southern δ-Aquariids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Southern η-Aquariids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Northern June Aquilids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the November Orionids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Northern Taurids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Perseids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Orionids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Leonids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the ϕ-Piscids.
Paper: TESSELLATE: Piecing Together the Variable Sky with TESS
Authors: Hugh Roxburgh, Ryan Ridden-Harper, Andrew Moore, Clarinda Montilla, Brayden Leicester, Zachary G. Lane, James Freeburn, Armin Rest, Michele T. Bannister, Andrew R. Ridden-Harper, Lancia Hubley, Qinan Wang, Rebekah Hounsell, Jeff Cooke, Dave A. Coulter, Michael M. Fausnaugh
Figure caption: The light curves of known exoplanet host star WASP-62 (top panels) and a previously undiscovered exoplanet candidate TSS J0547-6921 (bottom panels). The left panels are replotted in their respective right panels after being phase-folded and fit with a standard Gaussian model (red line), which is used in the TESSELLATE exoplanet vetting criteria.
Paper: TESSELLATE: Piecing Together the Variable Sky with TESS
Authors: Hugh Roxburgh, Ryan Ridden-Harper, Andrew Moore, Clarinda Montilla, Brayden Leicester, Zachary G. Lane, James Freeburn, Armin Rest, Michele T. Bannister, Andrew R. Ridden-Harper, Lancia Hubley, Qinan Wang, Rebekah Hounsell, Jeff Cooke, Dave A. Coulter, Michael M. Fausnaugh
Figure caption: A section of the 10 minute cadence light curve of asteroid (5254) Ulysses from sector 29.
Paper: When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST
Authors: R. Arun
Figure caption: Composite figure showing continuum-subtracted, normalized PAH spectra from T Cha and four reference sources. Top panel (6.2 μm): spectra are normalized to unity at their 6.2 μm peak. Shown are the JWST H II PDR template (blue), HD 97300 (black), PDS 144N (green), SR 21A (orange), and T Cha (red). Middle panel (7.7 μm): the normalized spectra reveal variations in the 7.7 μm complex, with peak positions shifting from ∼7.6 μm in class A environments to ∼8.1 μm in T Cha, indicative of different PAH excitation conditions. Bottom panel (11.2 μm): the 11.2 μm feature, normalized similarly. The gray band highlights the minor class A feature identified in T Cha.