adsabs/AstroCLIMB huggingface dataset:
Paper: Disentangling Metallicity Effects in Hot Jupiter Occurrence across Galactic Birth Radius and Phase-space Density
Authors: Rayna Rampalli, Melissa K. Ness, Elisabeth R. Newton, Andrew Vanderburg, Tobias Buck, Jessica Mills
Figure caption: A. J. Winter et al. (2020) phase-space density analysis with injected hot Jupiters based on the hot Jupiter occurrence-metallicity power law from D.-C. Chen et al. (2023). Top: histograms of simulated hot Jupiters in phase-space underdensities (dotted lines and calculated P(dense) <0.16) and overdensities (solid lines and calculated P(dense) >0.84) shown for GALAH (green, left), APOGEE (purple, middle), and the NIHAO simulation (gray, right). We are able to replicate A. J. Winter et al. (2020)’s result, where >95% of hot Jupiter hosts are in overdensities compared to underdensities for GALAH (6078 vs. 262) and APOGEE (5832 vs. 224). The distribution of hot Jupiters in the NIHAO simulation is more evenly split (5814 vs. 5340) for reasons we discuss in Section 5.3. Middle: cumulative distribution functions (CDFs) in underdensities (dotted lines) and overdensities (solid lines) following Figure 3 of A. J. Winter et al. (2020) in [Fe/H]. Bottom: [Fe/H] distributions of stars with and without injected hot Jupiters for each underdense(top) and overdense (bottom) population per data set. The planet host CDFs for under/overdensities are very similar in [Fe/H]-space with average mean differences ≤0.02 dex compared to the planet and non-planet-host differences for each environment (0.04–0.12 dex) as shown in the two bottom panels here and in the left column of Figure 7.
Paper: Disentangling Metallicity Effects in Hot Jupiter Occurrence across Galactic Birth Radius and Phase-space Density
Authors: Rayna Rampalli, Melissa K. Ness, Elisabeth R. Newton, Andrew Vanderburg, Tobias Buck, Jessica Mills
Figure caption: Distributions of GALAH (in green), APOGEE (in purple), and NIHAO simulation (in gray) stars in overdense environments (shown as a solid line histogram and abbreviated as od) to those in underdense environments (shown as a dashed line histogram and abbreviated as ud) in [Fe/H]-, absolute VZ-, and [α/Fe]-space as classified by the analysis done in A. J. Winter et al. (2020). The means of each distribution of stars in overdensities and underdensities are denoted by solid and dashed vertical black lines, respectively. These distributions are for all stars, regardless of planet host status. For this parent population, stars in underdensities are on average more metal poor by 0.04–0.13 dex, kinematically hot by 10–22 km s−1, and α-enriched by 0.01–0.1 dex compared to stars in overdensities.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Selection of candidate single late-M dwarfs. The same color–magnitude diagram seen in Figure 2 is displayed as a two-dimensional histogram to show the density of stars with candidate single stars in blue and candidate binaries in gray. The black line shows the best fit to the main sequence (binned black data points). Plotted in red is the dividing line 0.38 mag above the empirical main sequence (Section 2.3), used to remove candidate equal-flux binary stars. The horizontal dashed line at MRP = 13.69 mag is an extension of this dividing line for G − GRP > 1.56 mag colors.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Empirical determination of the Gaia main sequence for G − GRP >  1.40 mag late-M dwarfs. This Gaia G − GRP vs. GRP color–magnitude diagram shows the 21,405 T ≤ 18 mag targets in the input sample. The 50% of the objects removed above and below the main sequence are in gray, with the remaining objects in blue. The mean and standard deviation for each 0.015 mag-wide bin are plotted in black.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Top: a histogram of the maximum number of available sectors of TESS data with either PDCSAP or eleanor reductions for the 399 likely single late-M dwarfs in this study. The histogram is divided into not periodic, possibly periodic, and periodic stars as defined in Section 3.3. Bottom: the fraction of stars in each bin that are not periodic, possibly periodic, and periodic. Overplotted in both panels is the binomial uncertainty of the nonperiodic fraction, and the red dashed line in the bottom panel is the line of best fit to these uncertainties. The implications of these plots are discussed in Section 4.3.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Gaia G – 2MASS J color vs. Gaia G − GRP color. The Gaia Catalogue of Nearby Stars (GCNS) is plotted as a density map in gray, with spectroscopically confirmed single field dwarfs from the UltraCoolSheet (W. Best et al. 2024) plotted in blue and binary field dwarfs in red. The red line marks the cutoff above which we select stars with reliable Gaia photometry, as computed in Section 2.1.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Target pixel files displaying three stars which are in crowded fields based on the three criteria, i (top left), ii (top right), and iii (bottom left), and one which is isolated (bottom right). The target (listed in the title of each plot) is plotted as a red star, while nearby stars with G < 20 mag in Gaia are plotted as orange circles. The red hatched boxes denote pixels within the SPOC PDCSAP aperture.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: A color–magnitude diagram of the Gaia Catalogue of Nearby Stars (GCNS), overlaid with late-M dwarf candidates. The colors indicate progressive selection for stars that are brighter than a TESS T magnitude of 18 (purple), are likely single (orange), are in uncrowded fields (red), and have PDCSAP photometry (blue; see Section 3.1).
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Top panels: normalized (black) and median detrended (blue) light curves for Sector 24 of TESS data on the M7 target Gaia DR3 1325528616668262784 with 30 minutes cadence. PDCSAP is on the left, and eleanor photometry is on the right. Middle panels: LS periodograms for the respective light curves. Large pink and orange X’s mark the highest peak, while small pink and orange x’s mark lower-power peaks still above the FAP but not above the window function. Bottom panels: light curves folded on the period with the highest peak in the periodogram, for both before (black) and after (blue) 2 day median detrending. The solid colored points are the data binned to one-hundredth the phase, included only to visualize periodicity. The red curve is fit to the unbinned data. All four reduction methods produce the same 0.269 day period that is passed to the Gaussian process (Section 3.3) for further refinement.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: GP results for Sector 21 of the M8 target Gaia DR3 856550486098139648 shown in Figure 11. The candidate period determined from the LS analysis and passed onto the GP is 3.19 days, and the final period is 3.246﹩{}_{-0.049}^{+0.022}﹩ days from the Sector 21 PDCSAP nondetrended data. Left panels: binned pdfs displaying the distribution of periods from the nested sampling process for each of the four data reduction methods (see titles of right-hand panels). The most likely periods are marked with vertical red dashed lines. The cdfs are plotted in teal, from which the 68% confidence intervals (black dashed lines) are calculated. Right panels: corresponding light curves folded on the best periods from the nested sampling process.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: The same as Figure 10, but for the M6 dwarf Gaia DR3 856550486098139648 with an astrophysical ≈3.2 days period, recovered by three of the four reduction methods. The 1.6 day period seen in the eleanor detrended data (bottom right) is a half-harmonic of the true period. Note that the 3.2 days period falls in a trough of the window function, so it is not caused by a spacecraft systematic.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Normalized light curves of two targets in the sample. The left plot shows a target where the eleanor data (offset by +0.25 for clarity), after outlier rejection, are cleaner than the PDCSAP flux, and the right plot shows the opposite. Colored points indicate data clipped before analysis (blue = eleanor, red = PDCSAP).
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: A comparison of Gaia G − GRP color and spectral type of stars with spectral types from the literature taken from the SIMBAD astronomical database (M. Wenger et al. 2000) compared to standard values selected by M. J. Pecaut & E. E. Mamajek (2013). Gray dashed lines indicate the halfway point between the M. J. Pecaut & E. E. Mamajek (2013) values, marking a cutoff between approximated spectral types.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: The same as Figure 14, but for PDCSAP nondetrended reductions for all sectors of available data. The candidate period determined from the LS analysis is confirmed in Sectors 21 and 48. Note: the 3.96 and 4.28 days periods determined in Sectors 14 and 15 are spurious, as the pdf peaks at or very near the edge of a bin.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: A histogram of the spectral types of stars in the 399 likely single late-M dwarfs in this study. The histogram is divided into not periodic, possibly periodic, and periodic stars as defined in Section 3.3. The majority of stars have spectral types M6 or later. Spectral types were taken from the SIMBAD astronomical database (M. Wenger et al. 2000), and where unavailable were calculated from G − GRP.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Normalized light curves of Gaia DR3 2514882469124238464 (G − GRP = 1.41 mag, ∼M6) from Sectors 4, 31, 42, and 43, folded on the best period from the LS of 0.553 days. Individual sectors are offset from each other to display the changing amplitude of periodicity.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Decision tree to determine whether a candidate period from Step 2 (LS) should be passed for validation to Step 3 (Gaussian process). See Section 3.2 for details.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Examples of different scenarios in TL. Top two rows: amplitude heat maps (top row) and the corresponding TPFs (second row) for TL FALSE results. The left panels show a case where a distant bright star located just off the TPF is the true periodic source, contaminating our star. The right panels show a case where the passed period is a TESS systematic, mapping the stars in the amplitude heat map. Bottom two rows: the same as the top, for cases where TL returned TRUE. The left panels show a good result, in which the periodicity is confirmed to be colocated with the target star. The middle panels show a case where the p-value is low due to the high proper motion of the star. However, our visual inspection of this result retains it as a confirmed period. The right panels show an example where TL returns TRUE, but the period is not confirmed. This is a case of the same systematic as in the right panels of the top two rows, but here our target is the brightest star in the field.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Comparison of periods determined in this study to previously published ones, where they exist in the literature (listed in Table 4). Where multiple published periods exist for a star, we have adopted the most significant one. The gray dashed lines indicate the 1:1, 1:2, and 2:1 lines. Open circles indicate possible periods in this work, whereas closed circles are those which we consider real. Uncertainties in this work and in the literature (when available) are typically smaller than the data point. References in the legend with “+” indicate periods from multiple sources which were compiled by the named paper.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Top panels: rotation period vs. Gaia G − GRP color (and corresponding spectral type from M. J. Pecaut & E. E. Mamajek 2013; left) and rotation period vs. TESS magnitude (right) of the targets in the sample. Middle panels: histograms showing the distribution of periodic objects in the sample. Bottom panels: the fraction of stars in each bin that are not periodic, possibly periodic, or periodic. The left panel shows no correlation between period detections and G − GRP color, whereas there is a clear correlation between TESS magnitude and period detection in the right panel.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Amplitude vs. TESS magnitude of the sinusoidal variation of the folded light curve for the periodic (filled blue circles) and possibly periodic (empty blue circles) targets in this sample. Also plotted with crosses are the 2 minutes, 10 minutes, and 30 minutes cadence amplitude sensitivity limits to <1 day periodic variations of TESS as determined by P. A. Miles-Páez et al. (2023).
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Color–magnitude diagrams showing all the rotation periods in the literature discussed in this work (left) and the rotation periods of the three studies specifically targeting late-M dwarfs in TESS (S21, P24, and F24; right). Note that reddening and extinction are disregarded, as L22 is the only study with stars further than 150 pc. References in the legend with “+” indicate periods from multiple sources which were compiled by the named paper.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: A comparison of the p-values for TL results in which the target is the source of periodicity (TRUE) and where it is not (FALSE). The vertical line indicates a value of 0.1, below which all TRUE results are visually examined.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: A histogram of rotation periods in our sample. An inset is included to show the distribution of periods under 1 day, which comprises the majority of the rotation periods identified.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Decision tree detailing variability validation with TL.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Decision tree to determine whether a target is periodic, based on the GP in Step 3 of the analysis.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Top: a comparison of Gaia G − GRP color (and correlated spectral type from M. J. Pecaut & E. E. Mamajek 2013) to the rotation period of M dwarfs and brown dwarfs. Bottom: period vs. spectral type for periodic targets in this work and in the literature. Where spectral types were unavailable, they were calculated from G − GRP color down to G − GRP = 1.6 mag and J − H for fainter objects (M. J. Pecaut & E. E. Mamajek 2013). While the lower boundary on period appears to be astrophysical, the upper boundary for >M6 dwarfs stems from the difficulty of observing longer periods of faint objects. L22 is represented by a two-dimensional histogram due to the large number of stars. References in the legend with “+” indicate periods from multiple sources which were compiled by the named paper.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Periodic late-M dwarf members of young stellar associations (YSAs; colored) compared against our sample of 399 candidate single uncontaminated TESS late-M dwarfs with PDCSAP data (gray) on a plot of rotation period versus Gaia G − GRP color. The color of the point indicates the age of the YSA.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: A histogram of late-M dwarf periods from this work and the literature, for objects with 1.4 mag <G − GRP <  1.6 mag and periods less than 1 day. After accounting for previously known periods, our study expands the number of known <1 day periods by 76%.
Paper: Rotation Periods of Candidate Single Late-M Dwarfs in TESS
Authors: Samantha Lambier, Stanimir Metchev, Paulo Miles-Páez, Leslie Moranta, Dakota Wolfe, Joelene Hales, Jeffrey Martinovic
Figure caption: Distribution of periodic, possibly periodic, and not periodic stars in each young stellar association, from youngest to oldest.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Comparison between MG,NN and MG,geo. This is based on stars with precise Gaia parallax measurements (ω/σω > 10) of the test sample. Four subsamples are shown according to different ranges in S/N of their spectra, with the S/N range shown by the text in corresponding panels. The residuals of ΔMG = MG,NN–MG,geo are also shown at the four lower bottom panels. The red solid line marks MG,NN = MG,geo, and the dashed line is offset by 0.75 mag from the red solid line. There are two-band structures: single stars are distributed along the solid line, while the dashed line may correspond to binary systems (further detailed in Section 5).
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Example of PCA reconstruction, focusing on a DESI B-arm spectrum with a S/N of 3 for a randomly selected star. Here, S(λ) in the top panel denotes the log flux of stellar spectra after subtracting the mean and after logarithmic transformation (Equation (1) and Section 2.4). The middle panel shows the reconstructed spectrum based on the first 100 principal components. The bottom panel shows the residuals.