adsabs/AstroCLIMB huggingface dataset:
Paper: Wide Binary Orbits Are Preferentially Aligned with the Orbits of Small Planets, but Probably Not Hot Jupiters
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Adam L. Kraus, Logan Pearce, Karen A. Collins, Malena Rice, Eric L. N. Jensen, David Baker, Valerio Bozza, Paul Benni, Allyson Bieryla, Avraham Binnenfeld, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Phil Evans, Marshall C. Johnson, Eric Girardin, Joao Gregorio, Pablo Lewin, Tsevi Mazeh, Felipe Murgas, Aviad Panahi, Francisco J. Pozuelos, Don J. Radford, Howard M. Relles, Fabian Rodriguez Frustaglia, Richard P. Schwarz, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, William C. Waalkes, Gavin Wang, Justin Wittrock, Shay Zucker
Figure caption: Results of simulations to determine whether higher false-positive rates for giant planets can explain the difference in the inclination distribution compared to small-planet systems (described in Section 4.3.1). Left: an image showing the median p-value from 1000 simulations performed for a given false-positive fraction and semimajor-axis cutoff. Right: an image showing the percentage of p-values from each of the 1000 simulations that are below 0.05. The horizontal and vertical lines visible in the figure are the separations between the grid points used in the simulation. In both panels, a blue cross marks our expectation for the semimajor-axis delineation and false-positive rate. Our grid points have a much finer resolution in semimajor axis than false-positive rate. We find that for plausible values of the false-positive rate (expected to be roughly less than 25%) and semimajor-axis cutoff (≈700 au) we would probably still expect to see a significant alignment if giant planets were similar to small planets. Since we do not see a significant alignment, we infer that giant planets are probably less strongly aligned than small planets.
Paper: Wide Binary Orbits Are Preferentially Aligned with the Orbits of Small Planets, but Probably Not Hot Jupiters
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Adam L. Kraus, Logan Pearce, Karen A. Collins, Malena Rice, Eric L. N. Jensen, David Baker, Valerio Bozza, Paul Benni, Allyson Bieryla, Avraham Binnenfeld, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Phil Evans, Marshall C. Johnson, Eric Girardin, Joao Gregorio, Pablo Lewin, Tsevi Mazeh, Felipe Murgas, Aviad Panahi, Francisco J. Pozuelos, Don J. Radford, Howard M. Relles, Fabian Rodriguez Frustaglia, Richard P. Schwarz, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, William C. Waalkes, Gavin Wang, Justin Wittrock, Shay Zucker
Figure caption: The variation of the p-value between binaries with exoplanets above and below a specific semimajor axis and the control sample, as measured through a KS test. Explicitly, denoting the control sample as c and the binaries with exoplanets as b, the blue line is computed as KS(b[ai < a and r < 6], c), the orange line as KS(b[ai > a and r < 6], c), the red line as KS(b[ai < a and r > 6], c), and the green line as KS(b[ai > a and r > 6], c). Because we are doing many comparisons, per K. C. Schlaufman (2015), the minimum of the p-value distribution should not be interpreted as an exact probability, but the dip at ≈700 au suggests that there is some change in the inclination distribution around roughly that semimajor axis.
Paper: Wide Binary Orbits Are Preferentially Aligned with the Orbits of Small Planets, but Probably Not Hot Jupiters
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Adam L. Kraus, Logan Pearce, Karen A. Collins, Malena Rice, Eric L. N. Jensen, David Baker, Valerio Bozza, Paul Benni, Allyson Bieryla, Avraham Binnenfeld, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Phil Evans, Marshall C. Johnson, Eric Girardin, Joao Gregorio, Pablo Lewin, Tsevi Mazeh, Felipe Murgas, Aviad Panahi, Francisco J. Pozuelos, Don J. Radford, Howard M. Relles, Fabian Rodriguez Frustaglia, Richard P. Schwarz, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, William C. Waalkes, Gavin Wang, Justin Wittrock, Shay Zucker
Figure caption: Left: the distribution of ∣90∘ − i∣ for all systems with exoplanets when the temperature of the host star of the exoplanet has a temperature greater than or less than 6100 K. Unlike the distribution of spin–orbit angles for hot Jupiters, we find no evidence of a difference in the distribution of planet/binary orbit angles above and below the Kraft break. Right: the same as the left panel, but restricted to less than 700 au, and with counts shown instead of relative density.
Paper: Wide Binary Orbits Are Preferentially Aligned with the Orbits of Small Planets, but Probably Not Hot Jupiters
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Adam L. Kraus, Logan Pearce, Karen A. Collins, Malena Rice, Eric L. N. Jensen, David Baker, Valerio Bozza, Paul Benni, Allyson Bieryla, Avraham Binnenfeld, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Phil Evans, Marshall C. Johnson, Eric Girardin, Joao Gregorio, Pablo Lewin, Tsevi Mazeh, Felipe Murgas, Aviad Panahi, Francisco J. Pozuelos, Don J. Radford, Howard M. Relles, Fabian Rodriguez Frustaglia, Richard P. Schwarz, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, William C. Waalkes, Gavin Wang, Justin Wittrock, Shay Zucker
Figure caption: Left: comparison of the distributions of binary inclination for systems with small planets with binary semimajor axes less than 700 au (left) and with binary semimajor axes greater than 700 au (right) between our sample and that of S. Christian et al. (2022). In both panels, our results are consistent with those of S. Christian et al. (2022), but our considerably larger sample lets us make inferences with higher statistical confidence.
Paper: Search for the Blazhko Effect in Field RR Lyrae Stars Using LINEAR and ZTF Light Curves
Authors: Ema Donev, Željko Ivezić
Figure caption: The top two panels show a simulated periodogram for a sum of two sine functions with similar frequencies f1 and f2— the central peak corresponds to their mean (see Equations (3) and (4)). The bottom left panel shows a periodogram for an observed LINEAR light curve for ID = 1748058, and the bottom right panel shows its folded version (around the main frequency fo = 3.223 day−1). In the bottom left panel, the three vertical dashed lines show the three frequencies identified by the algorithm described in text, and the two dotted–dashed lines mark yearly aliases around the main frequency fo, at frequencies fo ± 0.0274 day−1. The two vertical lines in the bottom right panel have the same meaning, and the horizontal dashed line shows the noise level multiplied by 5.
Paper: Search for the Blazhko Effect in Field RR Lyrae Stars Using LINEAR and ZTF Light Curves
Authors: Ema Donev, Željko Ivezić
Figure caption: The phased light curves normalized to unit amplitude of the overall best-fit model are shown for single observing seasons and compared to the mean best-fit models (top six panels: LINEAR data; bottom six panels: ZTF data). Data shown are for star with LINEARid = 10030349 (period = 0.54073 day). Season-to-season phase and amplitude modulations are seen in both the LINEAR and the ZTF data.
Paper: Search for the Blazhko Effect in Field RR Lyrae Stars Using LINEAR and ZTF Light Curves
Authors: Ema Donev, Željko Ivezić
Figure caption: A comparison of cumulative distributions of period (left), amplitude (middle) and apparent magnitude for starting sample, selected Blazhko candidates, and visually verified Blazhko stars. The top row is based on LINEAR data and both ab-type and c-type stars. The middle and bottom rows are based on ZTF data, and show separately data for ab-type and c-type stars, respectively. The differences in period and amplitude distributions are further examined in Figure 11.
Paper: Search for the Blazhko Effect in Field RR Lyrae Stars Using LINEAR and ZTF Light Curves
Authors: Ema Donev, Željko Ivezić
Figure caption: Comparison of amplitude–period distributions (the Bailey diagram) for the starting sample of 1996 RR Lyrae stars (contours) and 228 selected candidate Blazhko stars (symbols). The clump in the lower left corresponds to c-type RR Lyrae and the other one to ab type. Note that the period distribution for ab-type Blazhko stars is shifted left (by about 0.03 day, or 5%).
Paper: Search for the Blazhko Effect in Field RR Lyrae Stars Using LINEAR and ZTF Light Curves
Authors: Ema Donev, Željko Ivezić
Figure caption: Analogous to Figure 7, except that star with LINEARid = 3196780 is shown. Amplitude modulation is clearly seen in LINEAR light curves (top two rows), while not discernible in ZTF light curves (bottom two rows). Additional stars with similar behavior include LINEARid = 2889542, 7723614, 8342007. This behavior strongly suggests that Blazhko effect can appear and disappear on timescales shorter than about a decade.
Paper: Search for the Blazhko Effect in Field RR Lyrae Stars Using LINEAR and ZTF Light Curves
Authors: Ema Donev, Željko Ivezić
Figure caption: Analogous to Figure 7, except that star with LINEARid = 16300450 is shown (period = 0.33562 day). Unlike example shown in Figure 7, only phase modulation is visible here, without any amplitude modulation, in both LINEAR and ZTF light curves.
Paper: Search for the Blazhko Effect in Field RR Lyrae Stars Using LINEAR and ZTF Light Curves
Authors: Ema Donev, Željko Ivezić
Figure caption: An illustration of visual analysis of phased light curves for the selected Blazhko candidates. The left panel shows LINEAR data and the right panel shows ZTF data (symbols with “error bars”) for star with LINEARid = 10030349. The dashed lines are best-fit models. The numbers listed on the right side were added to aid visual analysis. Note multiple coherent data point sequences offset from the best-fit mean model in the right panel.
Paper: Search for the Blazhko Effect in Field RR Lyrae Stars Using LINEAR and ZTF Light Curves
Authors: Ema Donev, Željko Ivezić
Figure caption: An illustration of visual analysis of full light curves for the selected Blazhko candidates with emphasis on their repeatability between observing seasons, marked with vertical lines (left: LINEAR data; right: ZTF data). Data shown are for star with LINEARid = 10030349. Note strong amplitude modulation between observing seasons.
Paper: Search for the Blazhko Effect in Field RR Lyrae Stars Using LINEAR and ZTF Light Curves
Authors: Ema Donev, Željko Ivezić
Figure caption: Analogous to Figure 2, except that here only 228 visually verified Blazhko stars are shown.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: AU Mic’s Lyα emission line observed on 1998 September (left: no transit; orbits are 56–63 hr after AU Mic b: midtransit), 2020 July (second-from-left: undetected AU Mic b transit; orbits are 6 hr prior to 2 hr after transit midtime with one final orbit 17 hr after transit), 2021 October (third-from-left: detected AU Mic b transit; orbits are 4 hr prior to 4 hr after midtransit) and 2023 May (right: during AU Mic c transit; orbits are 3 hr prior to 4 hr after AU Mic c: midtransit). The gray shaded regions on the left and right of each panel correspond to the integrated blue- and red-wing regions, respectively. The region in between the wings is where geocoronal contamination and ISM absorption occurs. The legends specify each orbit in the four visits. The individual HST/STIS observations for all four observations are available as the data behind the figure. These files are also used in Figures 4 and A1.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: AU Mic light curves observed by HST/STIS on 1998 September (left: no transit but plotted in reference to AU Mic b ephemeris), 2020 July (second-from-left: undetected AU Mic b transit), 2021 October (third-from-left: detected AU Mic b transit) and 2023 May (right: during AU Mic c transit). The Lyα blue and red wings, O I and C II are shown to search for planetary absorption. Si IV and C IV are also shown as the FUV emission lines most sensitive to stellar activity in this work. The gray regions indicate the white-light transit durations of AU Mic b and c. Flares are highlighted in gold. All other FUV emission lines from Table 3 can be found in Figure A2.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: AU Mic spectra observed by HST/STIS on September 1998 (left: no transit), 2020 July (second-from-left: undetected AU Mic b transit that also displayed a large flare), and 2021 October (third-from-left: detected AU Mic b transit), and 2023 May (right: during AU Mic c transit). O I and C II are shown to search for planetary absorption. Si IV and C IV are also shown as the FUV emission lines most sensitive to stellar activity in this work. The gray regions show the wavelength ranges integrated over to obtain the light curves in Figure 6. Each line color corresponds to same orbit from Figure 3. All other FUV emission lines from Table 3 can be found in Figure A1.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: All potential TTV model periods of AU Mic d (y-axis labels) and their associated impact on the midtransit ephemeris of AU Mic c (horizontal lines of different colors) from J. M. Wittrock et al. (2023) around our data acquisition. The error bars represent the uncertainty in the ephemeris predicted by that model. The most favorable model, 12.7 days, is within the red rectangle. The gray regions indicate the HST exposures presented in this work. The black vertical line is the AU Mic c ephemeris used for this work, which was calculated using the planet’s epoch and period reported in J. M. Wittrock et al. (2023), which was recently confirmed by Á. Boldog et al. (2025). The light hatched region is the 4.236 hr white-light transit duration assuming the black vertical line as midtransit.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: AU Mic C IV, Si IV, and Lyα (divided by 10 plus 3) emission over time during the 2020 July (top; AU Mic b transit), 2021 October (middle; AU Mic b transit), and 2023 May (bottom; AU Mic c transit) visits. Flares are highlighted in gold. The best-fit flare models for the 2023 May flares are shown in bold. Figure A3 contains similar FUV continuum light curves.