adsabs/AstroCLIMB huggingface dataset:
Paper: Characterization of an Instrument Model for Exoplanet Transit Spectrum Estimation through Wide-scale Analysis on HST Data
Authors: Noah Huber-Feely, Mark R. Swain, Gael Roudier, Raissa Estrela
Figure caption: The residual standard deviation in units of shot noise for the light curve of each fitted wavelength channel for the two targets displayed (left: HAT-P-26 b, right: GJ 3470 b, both in G141). Overlays the 3.25 RSDSN fit-quality threshold.
Paper: A Zwicky Transient Facility Look at Optical Variability of Young Stellar Objects in the North America and Pelican Nebulae Complex
Authors: Lynne A. Hillenbrand, Thaddaeus J. Kiker, Miles Gee, Owen Lester, Noah L. Braunfeld, Luisa M. Rebull, Michael A. Kuhn
Figure caption: Distribution of significant Lomb–Scargle periodogram peaks. Top panel shows shows all timescales from Table 2, regardless of light-curve classification. Bottom panel shows only stars labeled as “P” in Table 2, which are those that phase well to their periodogram peaks and likely have their origin in spot pattern modulation due to stellar rotation. As expected, the true stellar rotation periods are concentrated toward the shorter timescales, with values of a few days to a few weeks.
Paper: A Zwicky Transient Facility Look at Optical Variability of Young Stellar Objects in the North America and Pelican Nebulae Complex
Authors: Lynne A. Hillenbrand, Thaddaeus J. Kiker, Miles Gee, Owen Lester, Noah L. Braunfeld, Luisa M. Rebull, Michael A. Kuhn
Figure caption: Mean 1σ photometric uncertainty as a function of mean r magnitude, calculated from the ZTF DR4 data products. Objects in our final variable star sample are shown in darker blue, and those not meeting all photometric cuts in lighter blue. The outlier at r ≈ 18 and σ  r  ≈ 0.06 is FHK 96, a source that undergoes an abrupt dimming event of >4.5 mag approximately halfway through the observing window.
Paper: A Zwicky Transient Facility Look at Optical Variability of Young Stellar Objects in the North America and Pelican Nebulae Complex
Authors: Lynne A. Hillenbrand, Thaddaeus J. Kiker, Miles Gee, Owen Lester, Noah L. Braunfeld, Luisa M. Rebull, Michael A. Kuhn
Figure caption: Two exemplary dipper objects with r-band light curves shown in the top row, and the corresponding g vs. g − r CMDs presented in the bottom row. Both sources have CMD slope angles consistent with their photometric variability being caused by extinction changes, likely along a line of sight that passes through circumstellar material. The expected extinction vector is shown, for reference.
Paper: A Zwicky Transient Facility Look at Optical Variability of Young Stellar Objects in the North America and Pelican Nebulae Complex
Authors: Lynne A. Hillenbrand, Thaddaeus J. Kiker, Miles Gee, Owen Lester, Noah L. Braunfeld, Luisa M. Rebull, Michael A. Kuhn
Figure caption: Example ZTF data at low, intermediate, and high values of the asymmetry parameter M (upper panels) and the quasiperiodicity parameter Q (lower panels). Negative values of M indicate flaring or bursting type behavior, while positive values of M signify dipping or fading behavior. Low values of Q indicate more strictly periodic light curves, while high values of Q are characteristic of stochastic light curves.
Paper: A Zwicky Transient Facility Look at Optical Variability of Young Stellar Objects in the North America and Pelican Nebulae Complex
Authors: Lynne A. Hillenbrand, Thaddaeus J. Kiker, Miles Gee, Owen Lester, Noah L. Braunfeld, Luisa M. Rebull, Michael A. Kuhn
Figure caption: Flux asymmetry vs. quasiperiodicity for our sample of variables, color coded by light-curve morphological type as reported in Table 2. The size of each point is proportional to its linearly scaled peak-to-peak variability metric ν. Note that some objects, especially periodic sources with high values of Q, can fall outside of the defined boundaries between the morphological classes in the Q − M plane. However, the Q − M classification is fairly robust with only a minor number of sources deserving adjustment to their numerically assigned classes.
Paper: A Zwicky Transient Facility Look at Optical Variability of Young Stellar Objects in the North America and Pelican Nebulae Complex
Authors: Lynne A. Hillenbrand, Thaddaeus J. Kiker, Miles Gee, Owen Lester, Noah L. Braunfeld, Luisa M. Rebull, Michael A. Kuhn
Figure caption: Same as Figure 7, but for two burster objects. Both sources have CMD slope angles much shallower than the expectations from extinction changes. The extinction vector is shown, for reference.
Paper: A Zwicky Transient Facility Look at Optical Variability of Young Stellar Objects in the North America and Pelican Nebulae Complex
Authors: Lynne A. Hillenbrand, Thaddaeus J. Kiker, Miles Gee, Owen Lester, Noah L. Braunfeld, Luisa M. Rebull, Michael A. Kuhn
Figure caption: Full sample of selected likely members of the North America (left) and Pelican (center) nebulae star-forming complex plotted over a DSS2-R red photographic image of the region. Our final sample of 323 variable sources from the ZTF is in darker blue, with the remaining likely member sources that do not meet all of the applied ZTF photometric cuts represented in lighter blue.
Paper: A Zwicky Transient Facility Look at Optical Variability of Young Stellar Objects in the North America and Pelican Nebulae Complex
Authors: Lynne A. Hillenbrand, Thaddaeus J. Kiker, Miles Gee, Owen Lester, Noah L. Braunfeld, Luisa M. Rebull, Michael A. Kuhn
Figure caption: Normalized peak-to-peak variability metric ν as a function of mean r magnitude for our sample of 392 NAP stars that meet the cuts on magnitude and minimum number of observations. Objects in darker blue above the dashed 15th percentile line are the 323 sources included in our variable star sample, while those not included are in lighter blue.
Paper: New CCD Astrometric Observations of Himalia Using Gaia DR2 in 2015–2021
Authors: Y. J. Shang, Q. Y. Peng, Z. J. Zheng, A. Vienne, B. F. Guo, F. R. Lin, Y. Chen
Figure caption: Typical CCD frames of Himalia and its nearby star, as obtained with 1 m telescope of the Yunnan Observatory on 2015 February 14. Upper-left (right) panel: CCD frame before (and after) the ePSF-subtracted technique. Lower-left (right) panel: a slice of the Himalia image that links through the centers of Himalia and nearby star and the same slice after the ePSF-subtracted technique.
Paper: TOI-1670 b and c: An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have Originated from High-eccentricity Migration
Authors: Quang H. Tran, Brendan P. Bowler, Michael Endl, William D. Cochran, Phillip J. MacQueen, Davide Gandolfi, Carina M. Persson, Malcolm Fridlund, Enric Palle, Grzegorz Nowak, Hans J. Deeg, Rafael Luque, John H. Livingston, Petr Kabáth, Marek Skarka, Ján Šubjak, Steve B. Howell, Simon H. Albrecht, Karen A. Collins, Massimiliano Esposito, Vincent Van Eylen, Sascha Grziwa, Elisa Goffo, Chelsea X. Huang, Jon M. Jenkins, Marie Karjalainen, Raine Karjalainen, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, David W. Latham, Alan M. Levine, H. L. M. Osborne, Samuel N. Quinn, Seth Redfield, George R. Ricker, S. Seager, Luisa Maria Serrano, Alexis M. S. Smith, Joseph D. Twicken, Joshua N. Winn
Figure caption: Lomb–Scargle periodograms of the undetrended TESS photometry after removing transit signals (first panel), combined Tull Coudé and HARPS-N RVs after subtracting the systemic velocities (second panel), combined Mt. Wilson S-index from Tull Coudé and HARPS-N spectra (third panel), and spectral window function (fourth panel). The 1% and 0.1% FAP (blue dashed and dotted, respectively) lines are calculated using bootstrap resampling. The purple and pink vertical lines are the ∼10.9 and ∼40.7 day planetary signals determined by the TESS SPOC, respectively. The highest peak of each periodogram is shown as a dashed black vertical line. There are no counterpart peaks in the periodogram of the S-index that correspond to the ∼40.7 day signal seen in the periodogram of the RV, and no peaks rise above the 1% FAP threshold. No peaks are visible in the spectral window function periodogram. The only significant period (<0.1% FAP) in the RVs is at 41.1 days, consistent with the WJ (TOI-1670 c).
Paper: TOI-1670 b and c: An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have Originated from High-eccentricity Migration
Authors: Quang H. Tran, Brendan P. Bowler, Michael Endl, William D. Cochran, Phillip J. MacQueen, Davide Gandolfi, Carina M. Persson, Malcolm Fridlund, Enric Palle, Grzegorz Nowak, Hans J. Deeg, Rafael Luque, John H. Livingston, Petr Kabáth, Marek Skarka, Ján Šubjak, Steve B. Howell, Simon H. Albrecht, Karen A. Collins, Massimiliano Esposito, Vincent Van Eylen, Sascha Grziwa, Elisa Goffo, Chelsea X. Huang, Jon M. Jenkins, Marie Karjalainen, Raine Karjalainen, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, David W. Latham, Alan M. Levine, H. L. M. Osborne, Samuel N. Quinn, Seth Redfield, George R. Ricker, S. Seager, Luisa Maria Serrano, Alexis M. S. Smith, Joseph D. Twicken, Joshua N. Winn
Figure caption: Detrended TESS light curve of TOI-1670. The full light curve is shown in black. Purple and pink points are relative photometry within four transit durations before and after transits of TOI-1670 b and c, respectively, and are used in the global RV and light-curve model fit. Times of transit are also marked by triangles plotted along the time axis. Gaps in the light curve correspond to periods where TESS uploaded data, result from data quality cuts, or are during Sector 17, when TOI-1670 was not observed. TESS sectors are shown in blue above the light curve.
Paper: TOI-1670 b and c: An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have Originated from High-eccentricity Migration
Authors: Quang H. Tran, Brendan P. Bowler, Michael Endl, William D. Cochran, Phillip J. MacQueen, Davide Gandolfi, Carina M. Persson, Malcolm Fridlund, Enric Palle, Grzegorz Nowak, Hans J. Deeg, Rafael Luque, John H. Livingston, Petr Kabáth, Marek Skarka, Ján Šubjak, Steve B. Howell, Simon H. Albrecht, Karen A. Collins, Massimiliano Esposito, Vincent Van Eylen, Sascha Grziwa, Elisa Goffo, Chelsea X. Huang, Jon M. Jenkins, Marie Karjalainen, Raine Karjalainen, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, David W. Latham, Alan M. Levine, H. L. M. Osborne, Samuel N. Quinn, Seth Redfield, George R. Ricker, S. Seager, Luisa Maria Serrano, Alexis M. S. Smith, Joseph D. Twicken, Joshua N. Winn
Figure caption: The SED of TOI-1670. Broadband photometry (Table 3) is shown with orange circles, with horizontal errors representing the bandpass width. The best-fitting model SED is shown in black, and the blue diamonds are the model flux integrated over each bandpass. The residuals normalized by the photometric errors are shown in the bottom panel.
Paper: TOI-1670 b and c: An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have Originated from High-eccentricity Migration
Authors: Quang H. Tran, Brendan P. Bowler, Michael Endl, William D. Cochran, Phillip J. MacQueen, Davide Gandolfi, Carina M. Persson, Malcolm Fridlund, Enric Palle, Grzegorz Nowak, Hans J. Deeg, Rafael Luque, John H. Livingston, Petr Kabáth, Marek Skarka, Ján Šubjak, Steve B. Howell, Simon H. Albrecht, Karen A. Collins, Massimiliano Esposito, Vincent Van Eylen, Sascha Grziwa, Elisa Goffo, Chelsea X. Huang, Jon M. Jenkins, Marie Karjalainen, Raine Karjalainen, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, David W. Latham, Alan M. Levine, H. L. M. Osborne, Samuel N. Quinn, Seth Redfield, George R. Ricker, S. Seager, Luisa Maria Serrano, Alexis M. S. Smith, Joseph D. Twicken, Joshua N. Winn
Figure caption: The RV curve of TOI-1670, phase-folded to the orbital period of the WJ, TOI-1670 c, with the contributions of the inner companion removed. The different colored points denote the different spectrographs, and the best-fitting RV model is shown by the solid black line. The fit residuals are shown in the lower panel. The colored error bars are nominal RV errors, and the gray error bars include the systematic jitter term.
Paper: TOI-1670 b and c: An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have Originated from High-eccentricity Migration
Authors: Quang H. Tran, Brendan P. Bowler, Michael Endl, William D. Cochran, Phillip J. MacQueen, Davide Gandolfi, Carina M. Persson, Malcolm Fridlund, Enric Palle, Grzegorz Nowak, Hans J. Deeg, Rafael Luque, John H. Livingston, Petr Kabáth, Marek Skarka, Ján Šubjak, Steve B. Howell, Simon H. Albrecht, Karen A. Collins, Massimiliano Esposito, Vincent Van Eylen, Sascha Grziwa, Elisa Goffo, Chelsea X. Huang, Jon M. Jenkins, Marie Karjalainen, Raine Karjalainen, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, David W. Latham, Alan M. Levine, H. L. M. Osborne, Samuel N. Quinn, Seth Redfield, George R. Ricker, S. Seager, Luisa Maria Serrano, Alexis M. S. Smith, Joseph D. Twicken, Joshua N. Winn
Figure caption: Transit light curve folded to the orbital period of TOI-1670 b. The TESS photometry is shown in purple, and the solid black line is the best-fitting transit model. The black circles are the photometric data binned over 20 minute intervals. The middle panel zooms in on the best-fit transit model and binned data points. The fit residuals are shown in the lower panel.
Paper: TOI-1670 b and c: An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have Originated from High-eccentricity Migration
Authors: Quang H. Tran, Brendan P. Bowler, Michael Endl, William D. Cochran, Phillip J. MacQueen, Davide Gandolfi, Carina M. Persson, Malcolm Fridlund, Enric Palle, Grzegorz Nowak, Hans J. Deeg, Rafael Luque, John H. Livingston, Petr Kabáth, Marek Skarka, Ján Šubjak, Steve B. Howell, Simon H. Albrecht, Karen A. Collins, Massimiliano Esposito, Vincent Van Eylen, Sascha Grziwa, Elisa Goffo, Chelsea X. Huang, Jon M. Jenkins, Marie Karjalainen, Raine Karjalainen, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, David W. Latham, Alan M. Levine, H. L. M. Osborne, Samuel N. Quinn, Seth Redfield, George R. Ricker, S. Seager, Luisa Maria Serrano, Alexis M. S. Smith, Joseph D. Twicken, Joshua N. Winn
Figure caption: Reconstructed speckle images of TOI-1670 from NESSI (top) and ‘Alopeke (bottom) in the 562 and 832 nm bands and their corresponding 5σ contrast curves. North is up, and east is to the left.
Paper: TOI-1670 b and c: An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have Originated from High-eccentricity Migration
Authors: Quang H. Tran, Brendan P. Bowler, Michael Endl, William D. Cochran, Phillip J. MacQueen, Davide Gandolfi, Carina M. Persson, Malcolm Fridlund, Enric Palle, Grzegorz Nowak, Hans J. Deeg, Rafael Luque, John H. Livingston, Petr Kabáth, Marek Skarka, Ján Šubjak, Steve B. Howell, Simon H. Albrecht, Karen A. Collins, Massimiliano Esposito, Vincent Van Eylen, Sascha Grziwa, Elisa Goffo, Chelsea X. Huang, Jon M. Jenkins, Marie Karjalainen, Raine Karjalainen, Emil Knudstrup, Judith Korth, Kristine W. F. Lam, David W. Latham, Alan M. Levine, H. L. M. Osborne, Samuel N. Quinn, Seth Redfield, George R. Ricker, S. Seager, Luisa Maria Serrano, Alexis M. S. Smith, Joseph D. Twicken, Joshua N. Winn
Figure caption: Transit light curve folded to the orbital period of TOI-1670 c. The TESS photometry is shown in pink, and the solid black line is the best-fitting transit model. Black points are the photometric data binned over 20 minute intervals.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Temperature variation of offsets in u 1 and u 2 when, theoretically, LDCs are calculated using tables provided by Claret (2017) using the q-method and r-method. The dashed–dotted lines show the best-fit model to the residuals.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Same as Figure 20 but using SPAM LDCs.
Paper: Empirical Limb-darkening Coefficients and Transit Parameters of Known Exoplanets from TESS
Authors: Jayshil A. Patel, Néstor Espinoza
Figure caption: Same as Figure 19 but using SPAM LDCs.
Paper: Exploring the Effects of Active Magnetic Drag in a General Circulation Model of the Ultrahot Jupiter WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Michael T. Roman, Abigail Guilliat
Figure caption: Magnetic Reynolds number for the 3 G model of WASP-76b (left) and magnetic drag timescales (right) based on the atmospheric structure at the end our simulation. Our kinematic MHD framework is appropriate for R  m  < 1, which is the case for most of the atmosphere. The hottest regions at the dayside upper atmosphere, where R  m  is the largest, is where atmospheric circulation can induce a magnetic field component comparable to the global field strength. On the right, we show the range in values for our active drag timescale. Across a single pressure level, the magnetic drag timescale can vary by many orders of magnitude. Since our magnetic drag varies with latitude, a single temperature and pressure will have a range of timescales, which explains the nonmonotonic behavior in portions of the plot.