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Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: TESS transits of TOI-1759 b. The top panels present the TESS photometry of TOI-1759 in Sectors 16, 17, and 24 as a function of time (black points with error bars), along with the best-fit model, which consists of a transit model plus a Gaussian process (blue curve). Note there is only a single transit observed in each sector. The bottom panels shows a close-up to each of those transits, which have been phased around the time of midtransit (gray points with error bars); the Gaussian process component has been removed from this photometry. The black line in these panels show the best-fit transit model; blue bands represent the 68% and 95% credibility bands of the model.
Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: Ground-based follow-up transit photometry of TOI-1759 b. Transit of TOI-1759 b on 2020 May 21 captured by three different observatories: the OAA telescope of the Observatori Astronòmic Albanyà, the RCO telescope of the Grand-Pra Observatory, and the OMC telescope of the Montcabrer Observatori. The duration and depth of the event are consistent between instruments.
Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: Synthetic JWST transmission atmospheric spectra of TOI-1759 b. Top: fiducial models with solar abundance. Bottom: enhanced metallicity by a factor of 100, considering haze opacity (solid blue lines) and no haze opacity (solid red lines). Estimated uncertainties are shown for the observation of one transit with JWST NIRISS-SOSS, NIRSpec-G395M, and MIRI-LRS configurations.
Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: GLS periodograms of the TJO photometry, SNO photometry, and the CARMENES spectral activity indicators. Analogous to the periodograms of the RVs, the period of the transiting planet, P = 18.85 days, and the additional present long-term periodicity with P ≈ 270 days are marked by the solid red and yellow lines, respectively. The stellar rotation period, P ≈ 80 days, and its first harmonic are indicated by the blue solid and dashed lines. The horizontal dashed gray lines show the analytical false-alarm probabilities (FAP) of 10%, 1%, and 0.1%.
Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: Near-infrared high spatial resolution imaging of TOI-1759. NIRC2 imaging observations obtained for TOI-1759 on Keck II reveals no close companion down to 0.1″, dimmer than about Δm = 4−5 mag than the target.
Paper: A Transiting, Temperate Mini-Neptune Orbiting the M Dwarf TOI-1759 Unveiled by TESS
Authors: Néstor Espinoza, Enric Pallé, Jonas Kemmer, Rafael Luque, José  A. Caballero, Carlos Cifuentes, Enrique Herrero, Víctor J. Sánchez Béjar, Stephan Stock, Karan Molaverdikhani, Giuseppe Morello, Diana Kossakowski, Martin Schlecker, Pedro J. Amado, Paz Bluhm, Miriam Cortés-Contreras, Thomas Henning, Laura Kreidberg, Martin Kürster, Marina Lafarga, Nicolas Lodieu, Juan Carlos Morales, Mahmoudreza Oshagh, Vera M. Passegger, Alexey Pavlov, Andreas Quirrenbach, Sabine Reffert, Ansgar Reiners, Ignasi Ribas, Eloy Rodríguez, Cristina Rodríguez López, Andreas Schweitzer, Trifon Trifonov, Priyanka Chaturvedi, Stefan Dreizler, Sandra V. Jeffers, Adrian Kaminski, María José López-González, Jorge Lillo-Box, David Montes, Grzegorz Nowak, Santos Pedraz, Siegfried Vanaverbeke, Maria R. Zapatero Osorio, Mathias Zechmeister, Karen A. Collins, Eric Girardin, Pere Guerra, Ramon Naves, Ian J. M. Crossfield, Elisabeth C. Matthews, Steve B. Howell, David R. Ciardi, Erica Gonzales, Rachel A. Matson, Charles A. Beichman, Joshua E. Schlieder, Thomas Barclay, Michael Vezie, Jesus Noel Villaseñor, Tansu Daylan, Ismael Mireies, Diana Dragomir, Joseph D. Twicken, Jon Jenkins, Joshua N. Winn, David Latham, George Ricker, Sara Seager
Figure caption: High spatial resolution imaging of TOI-1759. Two-band speckle imaging observations obtained with the ’Alopeke speckle imaging camera on the 8 m Gemini North telescope for TOI-1759 reveal no close companion down to 0.1″, dimmer than about Δm = 4−5 mag than the target.
Paper: GRASS: Distinguishing Planet-induced Doppler Signatures from Granulation with a Synthetic Spectra Generator
Authors: Michael L. Palumbo III, Eric B. Ford, Jason T. Wright, Suvrath Mahadevan, Alexander W. Wise, Johannes Löhner-Böttcher
Figure caption: Distributions of mean velocities measured from many realizations of synthetic observing programs. The number of exposures, each lasting 300 s, is varied between panels, as annotated in the top right of each panel. For each given realization of a synthetic observation program, the velocities measured within the same night are averaged. Each distribution is built up from these averaged velocity measurements. The black histograms correspond to simulated observing plans with short, 30 s lags between simulated exposures. The blue histograms correspond to long, 60 min lags between simulated exposures. The relative values of the measured velocities are themselves arbitrary, and correspond to the difference in rest-frame and CCF-template wavelengths. As expected, the distributions visibly narrow as the number of exposures is increased. However, there is no significant difference in the width of the short-wait and long-wait distributions in all panels (see Table 2), in apparent disagreement with past studies, which have shown that long waits between observations produce lower scatter in measured RVs (e.g., Dumusque et al. 2011; Meunier et al. 2015; Collier Cameron et al. 2019). In the future, input data spanning longer than 20 minutes would allow a more robust comparison of observing strategies, since our short baseline input data do not preserve longer-timescale variability (e.g., as in supergranulation).
Paper: GRASS: Distinguishing Planet-induced Doppler Signatures from Granulation with a Synthetic Spectra Generator
Authors: Michael L. Palumbo III, Eric B. Ford, Jason T. Wright, Suvrath Mahadevan, Alexander W. Wise, Johannes Löhner-Böttcher
Figure caption: Validation of GRASS line synthesis against the IAG solar atlas. Left: Observed (blue) and synthetic (black) Fe I 5434.5 Å absorption lines in disk-integrated light are overplotted. We additionally plot the IAG spectrum cleaned of shallow line blends in green, which nearly completely covers the black synthetic curve. Residuals between the IAG spectrum and the synthetic spectrum are shown in the bottom panel. Our synthetic spectrum deviates from the observed IAG spectrum at most by ∼5% (blue squares), but only by ∼0.5% from the cleaned IAG spectrum (green circles). Right: The observed IAG (blue) and synthetic (black) Fe I 5434.5 Å bisectors, which have been arbitrarily shifted horizontally (i.e., in velocity) to achieve maximal alignment, generally agree in shape up to 60% of the continuum level. The cleaned IAG (green) and synthetic bisectors are in much greater agreement. The residuals shown in the right panel further show that the blend cleaning greatly improves the agreement between model and observation, especially in the upper portion of the bisector.
Paper: GRASS: Distinguishing Planet-induced Doppler Signatures from Granulation with a Synthetic Spectra Generator
Authors: Michael L. Palumbo III, Eric B. Ford, Jason T. Wright, Suvrath Mahadevan, Alexander W. Wise, Johannes Löhner-Böttcher
Figure caption: Effect of simulation spatial grid size on the generated synthetic spectra. Points indicate the mean rms calculated from many RV time series, and error bars the standard error of the mean. Two measurements of the RV variability from solar granulation are shown as the orange forward-hatched (Elsworth et al. 1994) and green back-hatched (Pallé et al. 1999) regions. We find that our ideal grid size of N 2 = 1322 (vertical dashed line), chosen to produce grid cells with angular area matching the weighted-average spatial resolution of the input observations, intersects the power-law relation within the Pallé et al. (1999) region. At spatial resolutions greater than N ∼  400, the angular size of the grid cells becomes much smaller than that of the smallest-footprint input observations and consequently loses physical validity.
Paper: GRASS: Distinguishing Planet-induced Doppler Signatures from Granulation with a Synthetic Spectra Generator
Authors: Michael L. Palumbo III, Eric B. Ford, Jason T. Wright, Suvrath Mahadevan, Alexander W. Wise, Johannes Löhner-Böttcher
Figure caption: Temporal and spatial variability in input bisectors encode turbulent granulation velocities. Left: To capture the line-of-sight variation observed in solar bisectors, observations were carried out at many discrete disk positions along each of the four solar limbs plus disk center. Figure adapted from Figure 1 of L18. Right: Line bisectors differ in shape with both time and apparent position on the solar disk. From disk center (μ = 1) to the limb (μ = 0), bisectors transition from a distorted “C”-shape to something more resembling a “\”-shape. This behavior results from the different viewing angles of convective granules along different lines of sight (Figure 17.13 of Gray 2008). The solid, dashed, and dotted lines trace the time-averaged bisector for each limb position. The shaded regions correspond to the±1σ temporal variability of the bisectors at each limb position. Error bars in velocity are not shown; with an absolute wavelength calibration accuracy on order ∼0.02 mÅ (∼1  m s−1), the observed temporal variations are much larger than the typical uncertainty.
Paper: GRASS: Distinguishing Planet-induced Doppler Signatures from Granulation with a Synthetic Spectra Generator
Authors: Michael L. Palumbo III, Eric B. Ford, Jason T. Wright, Suvrath Mahadevan, Alexander W. Wise, Johannes Löhner-Böttcher
Figure caption: Example preprocessed input data showing granular variability at disk center (μ = 1). Each curve shows the input data at one snapshot in time. The color gradient has been added to aid the eye in separating out these realizations. Left: Line bisectors show variation due to pulsations and granulation. Changes in bisector shape encode granulation, and changes in position result from the combined effects of pulsations and granulation. Above continuum-normalized flux of 0.8 (gray hatched region), we model the bisector as the extrapolation from lower flux values. Right: Line widths measured as a function of depth show only slight variation with time. These width measurements display significantly less temporal variability compared to the line bisectors. Together, line bisectors and width as a function of depth uniquely specify the shape of a line at a given instance in time.
Paper: GRASS: Distinguishing Planet-induced Doppler Signatures from Granulation with a Synthetic Spectra Generator
Authors: Michael L. Palumbo III, Eric B. Ford, Jason T. Wright, Suvrath Mahadevan, Alexander W. Wise, Johannes Löhner-Böttcher
Figure caption: Doppler velocity variability weakly scales with synthetic line depth for lines deeper than 20% of continuum level. As in Figure 4, points indicate the mean rms calculated from many RV time series, and error bars the standard error of the mean. The shaded blue region encloses 68% of all rms values across all runs. From line depths of 0.5% to 20%, the rms of an RV time series obtained from GRASS output spectra appears to decrease. From 20% to 95% depth, the rms then appears to steadily increase. However, the shallowest lines (gray hatched region) are synthesized exclusively from extrapolated input data (see Figure 2 and associated text). The trend in this region may therefore be unreliable.
Paper: GRASS: Distinguishing Planet-induced Doppler Signatures from Granulation with a Synthetic Spectra Generator
Authors: Michael L. Palumbo III, Eric B. Ford, Jason T. Wright, Suvrath Mahadevan, Alexander W. Wise, Johannes Löhner-Böttcher
Figure caption: RV time-series variability and stellar inclination. As in Figure 4, points indicate the mean rms calculated from many RV time series, and error bars the standard error of the mean. As in Figure 5, the shaded blue region encloses 68% of all rms values across all runs. Equator-on stars do not appear to show any significant difference in granulation-driven RV variability compared to pole-on stars. Additionally, neither the width of the RV rms distributions (blue shaded region) nor the error on the mean (error bars) appear to scale with inclination, suggesting that the impact of additional uncertainty introduced by a broader CCF profile for the Sun when viewed equator-on is small in comparison to the variability introduced by granulation signals.
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: Fitted CMD slope angle in degrees vs. Pythagorean vector length in magnitudes, differentiated by flux asymmetry (M) class. The vast majority of sources have slope angles much shallower than the expectations from reddening (shaded band), indicating that the observed color variability is dominated by accretion effects rather than by (or in addition to) extinction effects.
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: Effect of light-curve cadence on the Q metric, illustrated for two different values of the light-curve precision. Abscissa shows Q values calculated at the native cadence of K2, while ordinate shows Q values for the same K2 data but down sampled to the true cadence of our ZTF observations over the same limited time interval, with the indicated errors included. Lines indicate the relationships shown in the legend. Cadence has a large effect on Q, with more scatter toward higher Q. The effects of error are apparent, with overestimated errors leading to a drop in Q. The values go negative for some stars, particularly in the higher-error (right) panel, causing them to fall outside the bounds of the plot.
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: Effect of light-curve precision on the Q metric. Abscissa shows Q values calculated in the absence of error, while ordinate shows Q values for the same data but including realistic ground-based errors appropriate to our ZTF observations (0.036 mag). Lines indicate the relationships shown in the legend. Photometric error reduces Q by an amount that likely depends on light-curve amplitude relative to the photometric error, and light-curve morphology. While the shift is systematic, many stars are unaffected and the slope remains close to unity.
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: Light curves, periodograms, and phased light curves at the two strongest peaks for FHK 176 and FHK 286. Each of these sources has a complex periodogram structure that includes a double-peak around ∼1 day and another double-peak around ∼40 day. The latter periodic signal can be seen directly in the unphased light curves. However, in both cases, the short period just below one day appears to be the real period. See text for how the signal can be deciphered.
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:  De-reddened infrared color–color diagrams with objects having different Q − M classifications distinguished. Except for the bluest 5%–10% of the sample, the sources have colors consistent with those of Class II YSOs. The objects classified as periodic tend to have small infrared colors, while those with other behavior tend to have larger infrared colors, indicative of excesses consistent with the presence of circumstellar dust.
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:  De-reddened infrared color vs. ν metric, measuring normalized amplitude of the optical variability. Colors redder than 0.2 mag in these bandpasses indicate young stars with infrared excess. Essentially all sources with ν > 0.02 appear to have excess infrared color, indicating young stars surrounded by circumstellar dust.
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: Comparison of periods for objects that overlap between our work and previous literature. Lines indicate the 1:1 relationship between the periods P, and the P/2 and 2P harmonics (dashed), and the (∣1/P ± 1)∣−1 beats with the ∼1 day sampling (dotted). Circles are sources we find to exhibit true periodic behavior, whereas squares are sources that we designate as having timescales rather than strict periods, based on their high Q values.