adsabs/AstroCLIMB huggingface dataset:
Paper: Quiet Please: Detrending Radial Velocity Variations from Stellar Activity with a Physically Motivated Spot Model
Authors: Jared C. Siegel, Samuel Halverson, Jacob K. Luhn, Lily L. Zhao, Khaled Al Moulla, Paul Robertson, Chad F. Bender, Ryan C. Terrien, Arpita Roy, Suvrath Mahadevan, Fred Hearty, Joe P. Ninan, Jason T. Wright, Eric B. Ford, Christian Schwab, Guðmundur Stefánsson, Cullen H. Blake, Michael W. McElwain
Figure caption: The RC model greatly mitigates the stellar activity signal for the Sun and HD 26965. We present Lomb–Scargle periodograms of the spectrum-averaged RVs (gray), the RVs after linear detrending with the flux proxy (green), and the RVs post-RC detrending (purple). The NEID data sets also include FF′ detrending (dashed) for reference. Periodograms are shown for the NEID solar data, as well as the EXPRES and NEID HD 26965 data (the HARPS data is omitted due to the coarse sampling); the horizontal lines show the 1% false alarm probabilities. The presented results were all derived from the one-dimensional spectra (not the CCFs).
Paper: OGLE-IV Period–Luminosity Relation of the LMC: An Analysis Using Mean and Median Magnitudes
Authors: Jaime Muñoz, Alejandro García-Varela, Santiago Henao-Castellanos, Beatriz Sabogal, Luis Felipe Giraldo, Jorge Martínez
Figure caption: PL relation fitted in  I  0 by MM-regression. Panel (a): checking the model residuals implies statistically plotting the residuals vs. the fitted values (upper left panel) and the residuals vs. the logarithm of the period (upper-right panel). The first graph depicts a change in the residual model trend for magnitudes ranging from 13.3 to about 12. In addition, the second plot shows a break in the residuals when ﹩\mathrm{log}\ P\geqslant 1﹩, which is evident for residuals above the blue trend line. This behavior indicates a shift in tendency when Cepheids have periods longer or equal to 10 days. On the contrary, when comparing the upper plots and lower plots, the latter show the residuals after the new parameters have been introduced to the model, to adjust the zero-point and slope for Cepheids with periods longer than or equal to 10 days, solving the specification problem, since no break or change in tendency is shown by these plots. Observations 819, 1079, and 2029 have the highest residuals and correspond to Cepheid stars OGLE-LMC-CEP-1583, OGLE-LMC-CEP-2162, and OGLE-LMC-CEP-4023, respectively. Panel (b): the regression given by Equation (2) is shown with a blue line for Cepheids with ﹩\mathrm{log}\ P\lt 1﹩ and with a red line for Cepheids with ﹩\mathrm{log}\ P\geqslant 1﹩. The blue line has been projected farther with ﹩\mathrm{log}\ P\geqslant 1﹩ to enhance the visibility of the change when compared to the red line. The area between the green dashed lines shows the 95% confidence interval for the  I   0  expected values. This area increases when ﹩\mathrm{log}\ P\geqslant 1﹩, because Cepheids having these periods are more scattered around the regression line.
Paper: OGLE-IV Period–Luminosity Relation of the LMC: An Analysis Using Mean and Median Magnitudes
Authors: Jaime Muñoz, Alejandro García-Varela, Santiago Henao-Castellanos, Beatriz Sabogal, Luis Felipe Giraldo, Jorge Martínez
Figure caption: PL relation fitted in ﹩{{\boldsymbol{V}}}_{{\bf{0}}}^{{\boldsymbol{M}}}﹩ by MM-regression. Panel (a): checking the model residuals implies statistically plotting the residuals vs. the fitted values (upper left plot) and the residuals vs. the logarithm of the period (upper-right plot). The first graph depicts a change in the residual model trend for magnitudes ranging from 14 to about 13. In addition, the second plot shows a break in the residuals when ﹩\mathrm{log}\ P\geqslant 1﹩, which is evident for residuals above the blue trend line. This behavior indicates a shift in tendency when Cepheids have periods longer than or equal to 10 days. On the contrary, when comparing the upper plots and lower plots, the latter show the residuals after the new parameters are introduced into the model, to adjust the zero-point and slope for Cepheids with periods longer than or equal to 10 days, solving the specification problem, since no break or change in tendency is shown by these plots. Observations 820, 929, 1014, and 1262 have the highest residuals and correspond to Cepheids OGLE-LMC-CEP-1719, LMC-CEP-1940, OGLE-LMC-CEP-2162, and OGLE-LMC-CEP-2675, respectively. Panel (b): the regression given by Equation (3) is shown with a blue line for Cepheids with ﹩\mathrm{log}\ P\lt 1﹩ and with a red line for Cepheids with ﹩\mathrm{log}\ P\geqslant 1﹩. The blue line has been projected farther with ﹩\mathrm{log}\ P\geqslant 1﹩ to enhance the visibility of the change when compared to the red line. The area between the green dashed lines shows the 95% confidence interval for the ﹩{{\boldsymbol{V}}}_{{\bf{0}}}^{{\boldsymbol{M}}}﹩ expected values. This area increases when ﹩\mathrm{log}\ P\geqslant 1﹩, because Cepheids having these periods are more scattered around the regression line.
Paper: OGLE-IV Period–Luminosity Relation of the LMC: An Analysis Using Mean and Median Magnitudes
Authors: Jaime Muñoz, Alejandro García-Varela, Santiago Henao-Castellanos, Beatriz Sabogal, Luis Felipe Giraldo, Jorge Martínez
Figure caption: PL relation fitted in ﹩{{\boldsymbol{I}}}_{0}^{M}﹩ by MM-regression. Panel (a): checking the model residuals implies statistically plotting the residuals vs. the fitted values (upper left panel) and the residuals vs. the logarithm of the period (upper-right panel). The blue line helps to reveal the residual tendency changes. Observations 64, 819, and 2029 have the highest residuals and correspond to Cepheids OGLE-LMC-CEP-0130, OGLE-LMC-CEP-1583, and OGLE-LMC-CEP-4023, respectively. Panel (b): the regression given by Equation (1) is shown with a blue line for Cepheids with ﹩\mathrm{log}\ P\lt 1﹩ and with a red line for Cepheids with ﹩\mathrm{log}\ P\geqslant 1﹩. The blue line has been projected farther with ﹩\mathrm{log}\ P\geqslant 1﹩ to enhance the visibility of the change when compared to the red line. The area between the green dashed lines shows the 95% confidence interval for the ﹩{I}_{0}^{M}﹩ expected values. This area increases when ﹩\mathrm{log}\ P\geqslant 1﹩, because Cepheids having these periods are more scattered around the regression line.
Paper: OGLE-IV Period–Luminosity Relation of the LMC: An Analysis Using Mean and Median Magnitudes
Authors: Jaime Muñoz, Alejandro García-Varela, Santiago Henao-Castellanos, Beatriz Sabogal, Luis Felipe Giraldo, Jorge Martínez
Figure caption: Sky coordinates of the OGLE-IV fundamental mode classical Cepheids in the LMC, shown as gray dots. The Skowron et al. (2021) extinction map limits are shown with the dashed line, and the rejected stars are marked with crosses; the ones rejected because of the uncertainty of their color excesses are shown in red, and those that lie outside the extinction maps are shown in blue.
Paper: OGLE-IV Period–Luminosity Relation of the LMC: An Analysis Using Mean and Median Magnitudes
Authors: Jaime Muñoz, Alejandro García-Varela, Santiago Henao-Castellanos, Beatriz Sabogal, Luis Felipe Giraldo, Jorge Martínez
Figure caption: PL relation fitted in  V   0  by MM-regression. Panel (a): checking the model residuals implies statistically plotting the residuals vs. the fitted values (upper left plot) and the residuals vs. the logarithm of the period (upper-right plot). The first graph depicts a change in the residual model trend for magnitudes ranging from 14 to about 13. In addition, the second plot shows a break in the residuals when ﹩\mathrm{log}\ P\geqslant 1﹩, which is evident for residuals above the blue trend line. This behavior indicates a shift in tendency when Cepheids have periods longer than or equal to 10 days. On the contrary, when comparing the upper plots and lower plots, the latter show the residuals after the new parameters are introduced into the model, to adjust the zero-point and slope for Cepheids with periods longer than or equal to 10 days, solving the specification problem, since no break or change in tendency is shown by these plots. Observations 820, 1014, and 1262 have the highest residuals and correspond to Cepheids OGLE-LMC-CEP-1719, OGLE-LMC-CEP-2162, and OGLE-LMC-CEP-2675, respectively. Plot (b): the regression given by Equation (4) is shown with a blue line for Cepheids with ﹩\mathrm{log}\ P\lt 1﹩ and with a red line for Cepheids with ﹩\mathrm{log}\ P\geqslant 1﹩. The blue line has been projected farther with ﹩\mathrm{log}\ P\geqslant 1﹩ to enhance the visibility of the change when compared to the red line. The area between the green dashed lines shows the 95% confidence interval for the  V   0  expected values. This area increases when ﹩\mathrm{log}\ P\geqslant 1﹩, because Cepheids having these periods are more scattered around the regression line.
Paper: The Discovery of Three Galactic Wolf–Rayet Stars
Authors: Laurella C. Marin, Philip Massey, Brian A. Skiff, Kennedy A. Farrell
Figure caption: Gaia spectra of our three newly found WRs. These sources were initially classified as Hα sources (The 1962, 1966; J. Hardorp et al. 1964) from objective prisms surveys. Our inspection of the Gaia spectra showed the broad, strong lines indicative of WR stars.
Paper: The Discovery of Three Galactic Wolf–Rayet Stars
Authors: Laurella C. Marin, Philip Massey, Brian A. Skiff, Kennedy A. Farrell
Figure caption: The spectra of the WR binary LS III +44 21. The bottom panel is zoomed in to the bluest part of the spectrum to show the absorption lines. The strongest interstellar (IS) lines have been identified, including the 4430 Å diffuse interstellar band (DIB). Compare to the lower resolution Gaia spectra shown in Figure 1.
Paper: The Discovery of Three Galactic Wolf–Rayet Stars
Authors: Laurella C. Marin, Philip Massey, Brian A. Skiff, Kennedy A. Farrell
Figure caption: The V-band light curve of LS III +44 21 based on ASAS-SN data. We have phased the data using a period of 4.4313725 days and a time of primary eclipse of Julian date 2457270.94 based on the values given in T. Jayasinghe et al. (2021). We note that their webpage for this star indicates that some of these data may be saturated.
Paper: The Discovery of Three Galactic Wolf–Rayet Stars
Authors: Laurella C. Marin, Philip Massey, Brian A. Skiff, Kennedy A. Farrell
Figure caption: The spectra of the two WC9 stars. The classification lines along with other strong lines are labeled. It may be instructive to compare these spectra to the lower resolution Gaia spectra shown in Figure 1.
Paper: Detecting Exoplanet Transits with the Next Generation of X-Ray Telescopes
Authors: Raven Cilley, George W. King, Lía Corrales
Figure caption: Stellar and planetary properties of our sample. The left plot shows log X-ray flux at Earth (0.2–2.4 keV) vs. log ﹩{\tfrac{{R}_{p}}{{R}_{* }}}^{2}﹩ (%). Each planetary system in the sample is plotted, with the host star’s spectral type determining the color and shape. Points with dark outlines have measured X-ray fluxes, and points surrounded by purple circles are in the list of the top 15 candidate targets for AXIS and NewAthena. The method for determining each X-ray flux is given in Section 2.1. For fluxes given in the literature in a band other than 0.2–2.4 keV, we used the XSPEC models described in Section 2.2 to convert the flux to 0.2–2.4 keV. The right plot shows the orbital period (days) and radii (Earth radii) of the planets in the NEA, with planets in our sample highlighted in blue squares. The top 15 candidate targets are shown with darker blue diamonds. The method for determining the top target candidates is described in Section 2.2.
Paper: Detecting Exoplanet Transits with the Next Generation of X-Ray Telescopes
Authors: Raven Cilley, George W. King, Lía Corrales
Figure caption: HD 189733 b example simulated transit light curve and null hypothesis analysis. Left: HD 189733 b transit model (solid blue curve) and simulated data for 10 averaged AXIS observations (gray). Right: the ﹩{({L}_{t}/{L}_{0})}_{n}﹩ distribution generated for 104 sets of data with no transit and a distribution of ﹩{({L}_{t}/{L}_{0})}_{d}﹩ values for 104 sets of simulated AXIS HD 189733 b transit data. The median p-value is ≤10−5, indicating that HD 189733 b could be detected at ≥4.4σ significance with AXIS. Our method for analyzing transit light curves is described in Section 2.3.
Paper: Detecting Exoplanet Transits with the Next Generation of X-Ray Telescopes
Authors: Raven Cilley, George W. King, Lía Corrales
Figure caption: Simulated transit light-curve data sets for one transit (blue circles) and 10 averaged transit observations (blue diamonds) of WASP-93 b. The 10 averaged data set has less statistical scatter and is much closer to the transit model (black line) than that of the single set of simulated data. The two points to the right of the light curve show the standard deviation of each data set.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption: Cumulative distribution of J–K colors for inner, middle, and outer MBAs. The steepest slope belongs to the inner belt, showing that the inner belt is less dominated by very red objects than the other two regions. Left: the colors of S-, C-, and D-type asteroids are marked, along with a 50% line for reference. There are several possible causes for the middle and outer belts presenting redder colors than the inner belt, as described in Section 5. Right: same cumulative distributions as the left panel, but zoomed in. Here, instead of showing mean colors for S, C, and D types, we show the mean calculated color for inner, middle, and outer MBAs from the smallest size range (5–20 km) in DeMeo & Carry (2014). In the inner main belt, our results are bluer than DeMeo predicts. In the outer and middle main belts, our results are less red than the DeMeo result, while our middle and outer belt samples are more red. This result is discussed in detail in Section 5.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption:  VJK color–color diagram of asteroids recovered. Each symbol represents the typical position in VJK color space of the specified type of asteroid. The canonical asteroid colors are derived from spectra from DeMeo & Carry (2014), as described in the text. The blue points show the 601 asteroids in this survey with J–K colors. Our sample consists primarily of C- and S-type asteroids. K, L, Q, R, T, and X types fall near the S and C types and are difficult to distinguish in this color–color space.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption: Comparison of recovery rate before and after introducing a maximum of 1.″0 between predicted location and source. Left: the red line (left y-axis) shows detected asteroids with no match threshold, and the orange line (right y-axis) shows detections with a 1.″0 threshold. The peaks are set to the same height to demonstrate the recovery rate in each bin. Right: fraction of matches retained after imposing the 1.″0 limitation, as a function of semimajor axis. The recovery rate is a function of the semimajor axis, with inner MBAs affected more strongly. A possible explanation is that the faster speeds in the inner belt create more mismatches.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption: Dependence of J–K color on absolute magnitude by region. Recovered inner main-belt objects are, on average, both smaller and less red than their counterparts in the middle and outer main belts.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Compilation of all literature photometry and spectroscopy on HD 19467 B, including JWST NIRCam coronagraph data published in Greenbaum et al. and re-reduced using SpaceKLIP and historical NIR ground-based data. The NIR spectra from Mesa et al. (2020) and Crepp et al. (2015) exhibit broad deep absorption features that are characteristics of T dwarfs but they lack the sensitivity and spectral resolution to pick up the less abundant molecules identified with JWST. The best-fit model from the NEWERA-PHOENIX grid is overplotted in light gray behind all of the available data. The model provides an excellent fit for most photometric data, but in the bluer wavelengths, it overestimates the flux slightly. This could be caused by a variety of reasons, including the speckle subtraction in that area of the spectrum and not including clouds in our NEWERA-PHOENIX grid.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Results of T eff = ﹩{1103}_{-103}^{+97}﹩ K, log g = ﹩{4.5}_{-0.36}^{+0.5}﹩, and log10(K  zz ) = ﹩{5.03}_{-0.030}^{+0.414}﹩ model fits with varying abundances for H2O, CO, CO2, and CH4 to our continuum-subtracted NIRSpec spectrum. The abundances are given in units relative to the ratio in the Sun, such that a value of zero implies the solar value. The scalings of most molecules prefer solar. CO could be slightly subsolar, but with the distributions being broad they are consistent with no scaling at all. For CO2 and CH4, the mixing ratios were ﹩{1.000}_{-0.369}^{+0.585}﹩. For CO and H2O the mixing ratios were ﹩{0.631}_{-0.233}^{+0.369}﹩. These ratios are all consistent with a solar C/O ratio, which is to be expected in a T5.5 brown dwarf.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Left: orbit fit of HD 19467 B using the orbit-fitting code orvara (Brandt et al. 2021). The thick black line represents the highest likelihood orbit; the thin colored lines represent 500 orbits drawn randomly from the posterior distribution. Dark purple corresponds to a low companion mass and light yellow corresponds to a high companion mass. The dotted black line shows the periastron passage, and the arrow at the periastron passage shows the direction of the orbit. The dashed line indicates the line of nodes. Predicted past and future relative astrometric points are shown by black circles with their respective years, while the observed relative astrometric points are shown by the blue-filled data points, where the measurement error is smaller than the plotted symbol. Right: RV changes induced by HD 19467 B. Shown are the RV data from HIRES (blue points) and HARPS (yellow points). Again the thick line shows the highest likelihood fit; the thin colored lines show 500 orbits drawn randomly from the posterior distribution. The residuals of the radial velocities are shown in the bottom panel.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Our continuum-subtracted NIRSpec spectrum of HD 19467 B in black plotted against the best-fit models; BT-Settl08 in magenta in the top panel, Sonora Bobcat in blue in the second panel, DRIFT-PHOENIX in orange in the third panel, and NEWERA-PHOENIX, in green in the fourth panel. The residuals are plotted in the final panel in the corresponding colors to their models with the NIRSpec high-pass-filtered errors plotted in gray. A black line was drawn at zero, and the smallest residuals were from the NEWERA-PHOENIX model grid.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Corner plot from our MCMC fits using the BT-Settl08 grid for our continuum NIRSpec spectra. The diagonal shows the marginalized posteriors. The covariances between all the parameters are in the corresponding 2D histograms. The blue lines represent the 50th percentile, and the dotted lines represent the 16th and 84th percentiles. The ﹩{C}_{{F}_{\lambda }}﹩ corresponds to the dilution factor that scales the model by (radius)2(distance)−2 and C noise is a scaled noise parameter.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Acceleration induced by the companion on the host star as measured from absolute astrometry from HIPPARCOS and Gaia for μ  α  (left) and μ  δ  (right). The thick black line represents the highest likelihood orbit; the thin colored lines are 500 orbits drawn randomly from the posterior distribution. Darker purple represents a lower companion mass and light yellow represents a higher companion mass. The residuals of the proper motions are shown in the bottom panels.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Relative separation (left) and position angle (right) of HD 19467 B across multi epochs of relative astrometry as listed in Table 5. The residuals are shown in the bottom two panels.