adsabs/AstroCLIMB huggingface dataset:
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: The median inclination relative to 90° vs. median eccentricity for the control sample. A degeneracy exists between inclination and eccentricity, excluding any systems with inclination near 90° and low eccentricity.
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: The posterior probability distribution of the mixture parameter λ for eight chains and the accepted samples of λ. Our mixture model fit prefers a roughly 50%/50% ratio of systems in an aligned Gaussian population to those in a random ﹩\sin (i)﹩ distribution.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Marginal posterior distribution and MAP estimates of orbital parameters for the HIP 89000 binary system as an SB2, and in the SB1 + p(ϖ), SB1 + p(m 1∣θ), and SB1 + p(ϖ) + p(m 1∣θ) scenarios.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Similar to Figure 9 but for the HIP 117186 binary system.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Marginal posterior distribution and MAP estimates of orbital parameters for the HIP 3504 binary system in the SB1, SB1 + p(ϖ), SB1 + p(m 1∣θ), and SB1 + p(ϖ) + p(m 1∣θ) cases.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Estimated orbit and RV curves for the HIP 89000 binary system. First column: MAP point estimate projection of the posterior distribution for the SB2, SB1 + p(ϖ), SB1 + p(m 1∣θ), and SB1 + p(ϖ) + p(m 1∣θ) cases. Second to fifth columns: projected posterior distribution for the SB2, SB1 + p(ϖ), SB1 + p(m 1∣θ), and SB1 + p(ϖ) + p(m 1∣θ) cases, respectively.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Similar to Figure 7 but for the HIP 111170 binary system.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Similar to Figure 4, but for the HIP 117186 binary system. In this case we appreciate a large discrepancy between the orbital and trigonometric parallaxes. The impact of this difference is further discussed in Section 3.2.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Similar to Figure 3, but for the HIP 117186 binary system.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Similar to Figure 8 but for the HIP 111170 binary system.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Similar to Figure 10 but for the HIP 117186 binary system.
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: An example of a star with a typical flicker that was monitored spectroscopically during TESS observations. A portion of the TESS light curve is shown (top-left panel), along with the Hα line from the spectroscopic observations (right panel). The colored triangles in the top-left panel indicate the spectroscopic epochs, with the corresponding line profiles in the right panel (following the same color code). Hα emission begins to appear near BJD—2457000 = 1720, indicating that material is being ejected into the circumstellar environment. The Hα equivalent width (EW) is plotted in the bottom-left panel, as measured between the vertical dashed lines in the right panel (with smaller values corresponding to more emission). Large symbol sizes in the bottom-left panel correspond to the thicker lines in the right panel to highlight spectra taken near the beginning of the flicker, near peak brightness, and late in the dissipation phase.
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: Correlations between various characteristics of the sample (blue (red) = positive (negative) correlation). The size of each dot is proportional to the strength of the (anti)correlation. From top to bottom, “early ST,” “mid ST,” “late ST,” and “unknown ST” refer to the spectral type bins. “Groups” include stars with one or more frequency groups, and “typical groups” refer to those with the typical group configuration. “Low freq,” “flickers,” “stochastic,” and “isolated freqs.” refer to the variability classifications introduced in Section 4. “High freqs.” and “very high freqs.” refer to systems with high (6 < f < 15 day−1) and very high (f > 15 day−1) frequencies. The remaining categories describe the relative strength of g1 and g2 in systems with the typical group configuration, where g1 is stronger (“A  g1 > A  g2”), where both groups are of similar strength (“A  g1 = A  g2”), and where g1 is weaker than g2 (“A  g1 < A  g2”).
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: Light curves (left) and frequency spectra (right) of a few example systems exhibiting low-frequency stochastic variability. In the frequency spectra plots, the lighter gray curve is computed from the raw data (shown in the light-curve plots), and the black curve is computed after removing signals with frequencies below 0.5 day−1.
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: Frequency spectra of systems with very high frequencies. Vertical dotted lines are at 6, 12, and 15 day−1 for reference. In the top panel, the x-axis extends to 100 day−1, while the remainder share the same axis, out to 40 day−1. The horizontal red line is 4× the mean amplitude for f > 15 day−1, shown only for reference. TIC IDs marked with an asterisk are rejected as classical Be stars (see Sections B.2 and B.3).
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: Diagnostic plot for j Cen (=TIC 325170579). See Appendix D for an explanation of the various panels. The complete set of diagnostic plots is available on Zenodo: doi:10.5281/zenodo.6290288.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Correlation maps (normalized by standard deviation) for TRAPPIST-1 models with a water line list (Polyansky et al. 2018), in the 1.1–1.2 μm band. Top: Outgassed atmosphere model for TRAPPIST-1 b, with 10% spot coverage on the star. Noise added for 10 ELT visits. Middle: Archean model for TRAPPIST-1 e, with 10% spot coverage. Noise added for 30 ELT visits. Bottom: Same as middle panel, but with spectra at R = 200,000. RME/CLV correction was applied to all maps.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Comparison of K2-18–type model transits with pure stellar contamination and the existing HST/WFC3 and K2 data sets (black dots), in relative transit depths. The contamination models were taken with cold spots (T spot = 2600 K), with 10% (blue), and 20% (orange) spot coverage fractions.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Example of the RME correction process for the HD 189733 b model with the hot Jupiter atmosphere, but without stellar activity. Cross correlation is taken with a CO line list (Rothman et al. 2010) at 1200 K across the 2.29 μm CO band. The dashed lines indicate the true systemic and planetary RVs. Left panel: Correlation map (top) and CCF for individual spectra during transit (bottom) before applying any correction. Middle panel: Same, but for a bare rock planet. This includes only the correlation signal due to the occultation of the stellar surface. Right panel: Same again, after subtracting the RME correlation (middle panel) from the uncorrected correlation (left panel). The planet signal is now clearly visible, especially in the correlation map.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Top: correlation maps (normalized by standard deviation) for a transit model including the hot Jupiter atmosphere as well as 5% spot coverage on the host star. The true position of the planet signal is indicated by the black dot. Left: correlation with a water line list (Polyansky et al. 2018) at 1200 K across the 1.4 μm water band. No RME/CLV correction was applied. Correlation values are normalized by the standard deviation across the map, not including the peak. Photon noise was added as if the observations were taken during two transits from SPIRou/CFHT. Bottom: corresponding CCF for individual spectra during transit, with the dashed curve indicating the true planet RV. Right: correlation with a CO line list (Rothman et al. 2010) at 1200 K across the 2.29 μm CO band. The correction method (as shown in Figure 1) was applied. Photon noise was added as for three SPIRou/CFHT visits.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Comparison of the K2-18–type model atmosphere transits with and without stellar contamination. Uncertainty estimates are indicated as for 10 JWST transits, binned to R = 100. Top: the uncontaminated transit (blue) is plotted along with transits with 40% faculae (orange), 20% spots (green), and 20% spots with 40% faculae (red). Bottom: Relative transit depth for the same models (same colors).
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Comparison of the low-resolution (R = 100) atmospheric transit spectrum and pure stellar contamination transits for the K2-18 type model. Uncertainty estimates are indicated as for 10 JWST transits, binned to R = 100. Top: pictured are the pure atmospheric transit (blue), a 20% spot coverage transit (orange), a 30% spots transit (green), and a transit with 20% spots and 40% faculae (red). Bottom: relative transit depth of all the models (same colors).
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Comparison of optical low-resolution (R = 100) transit spectra for the HD 189733 b–type models. Shaded uncertainty regions are omitted here, since they are very small. The plot includes only stellar contamination transit spectra: 5% spots (blue), 10% spots (orange), and 20% faculae (green). The positions of some key atomic and molecular features are highlighted.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Comparison of near-infrared low-resolution (R = 100) transit spectra for the HD 189733 b–type models. Uncertainty estimates are indicated as for three JWST transits, binned to R = 100. Top: the atmosphere model transit (blue) is compared to a pure stellar contamination transit with 5% dark spots (red), an atmosphere transit with 5% spots (orange), and an atmosphere transit with 15% bright faculae (green). Bottom: Relative transit depth of three of the models (same colors).
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Examples of photometric variability curves for the active region coverage fractions in Table 4. Left: HD 189733. Center: K2-18. Right: TRAPPIST-1.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Comparison of multiple low-resolution (R = 100) transit spectra for different TRAPPIST-1 b models. Uncertainty estimates are indicated as for 10 JWST transits, binned to R = 100. Top: the plot includes the uncontaminated outgassed atmosphere model (red), the uncontaminated Venus-like model (green), a pure contamination transit with 10% spot coverage (blue), a pure contamination transit with 20% spots and 25% faculae (orange), the Venus-like model with 10% spots (purple), and the outgassed model with 30% faculae (brown). Bottom: Relative transit depth for four of these models (same colors).
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Correlation maps (normalized by standard deviation) for two different TRAPPIST-1 b model transits with a water line list (Polyansky et al. 2018) at 400 K. Top: Transit with 10% spot coverage only (no atmosphere). Middle: Transit with the outgassed atmosphere model and 10% spot coverage on the star. Bottom: Same as the middle panel but using models at R = 200,000. All correlation maps were corrected for the RME/CLV signal. In all cases, photon noise was added for 10 ELT visits.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Correlation maps (normalized by standard deviation) for a transit model with a sub-Neptune atmosphere and 10% spot coverage on the host star, correlated with a water line list (Polyansky et al. 2018) at 300 K. The true planetary RV (non-boosted) was used. The correction for the RME/CLV was applied. Top: R = 100,000, with photon noise added to the spectra as if they had been taken from 30 SPIRou/CFHT visits. Bottom: R = 200,000, with photon noise as for 30 SPIRou/CFHT visits.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Correlation maps (normalized by standard deviation) for two different TRAPPIST-1 e model transits with a water line list (Polyansky et al. 2018) at 300 K. Top: Transit with the Archean-Earth–like atmosphere only. Middle: Transit with the Archean atmosphere and 10% spot coverage on the star. Bottom: Same as middle but for models at R = 200,000. All maps were corrected for the RME/CLV signal and photon noise was added as for 30 ELT visits.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Comparison of multiple low-resolution (R = 100) transit spectra for different TRAPPIST-1 e models. Uncertainty estimates are indicated as for 10 JWST transits, binned to R = 100. Top: the plot includes the uncontaminated Archean-Earth–like atmosphere model (red), the uncontaminated aqua planet model (green), a pure contamination transit with 10% spot coverage (blue), a pure contamination transit with 20% spots and 25% faculae (orange), the aqua planet with 10% spots (purple), and the Archean-like model with 30% faculae (brown). Bottom: Relative transit depth for four of these models (same colors).
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Same as Figure 8, but in this case the orbital velocity of the planet was artificially boosted to K  p  = 141 km s−1 and 30 SPIRou/CFHT visits were used for the photon noise. The R = 100,000 model was used here.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Correlation map (normalized by standard deviation) for a TRAPPIST-1 e model transit with only 10% spot coverage on the host star (no planetary atmosphere) with a water line list (Polyansky et al. 2018) at 300 K. Corrected for RME/CLV. Photon noise was added as for 30 ELT visits.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Correlation map (normalized by standard deviation) for a transit model (R = 100,000) with only 10% spot coverage (no planetary atmosphere) on the K2-18–like host star, correlated with a water line list (Polyansky et al. 2018) at 300K. Top: Before correcting for the RME/CLV. Bottom: After the RME/CLV correction was applied. Photon noise was added for 30 SPIRou/CFHT visits in both cases.
Paper: On the Effect of Stellar Activity on Low-resolution Transit Spectroscopy and the use of High Resolution as Mitigation
Authors: Frédéric Genest, David Lafrenière, Anne Boucher, Antoine Darveau-Bernier, René Doyon, Étienne Artigau, Neil Cook
Figure caption: Correlation map (normalized by standard deviation) for the TRAPPIST-1 b outgassed atmosphere model and 10% spot coverage on the star with a water line list (Polyansky et al. 2018) at 400 K. No correction for RME/CLV was applied. Photon noise was added for 10 ELT visits.