adsabs/AstroCLIMB huggingface dataset:
Paper: Mitigating Worst-case Exozodiacal Dust Structure in High-contrast Images of Earth-like Exoplanets
Authors: Miles H. Currie, Christopher C. Stark, Jens Kammerer, Roser Juanola-Parramon, Victoria S. Meadows
Figure caption: Same as Figure 9, but for a 12 m mirror architecture. The smaller PSF of the larger mirror size helps to “resolve out” the exozodi, and thus the measured planetary S/N is improved in nearly all scenarios.
Paper: Discerning Parallax Amplitude in Astrometric Microlensing
Authors: Sedighe Sajadian, Arya Mahmoudzadeh, Setareh Moein
Figure caption: The NDs of ﹩{\mathrm{log}}_{10}[{\theta }_{{\rm{E}}}(\mathrm{mas})]﹩, u 0, and ﹩{\mathrm{log}}_{10}[{\pi }_{\mathrm{rel}}(\mathrm{mas})]﹩ from simulations (A), (B), and (C) are represented in green from top to bottom. Red lines represent the NDs of these parameters due to events in which π E can be measured (with a relative error of less than 4%) through either photometric or astrometric data. Blue and black lines are NDs due to events with measurable parallax amplitudes through photometric and astrometric data, respectively. Inside each panel, the average values of the parameters (θ E, u 0, π rel) from their distributions are indicated.
Paper: Discerning Parallax Amplitude in Astrometric Microlensing
Authors: Sedighe Sajadian, Arya Mahmoudzadeh, Setareh Moein
Figure caption: Scatter plots of δ θ rms (given by Equation (9)) for a sample of astrometric microlensing events due to ISMBHs toward the GB (top panels) and LMC (bottom panels) vs. D l(kpc), ﹩{\mathrm{log}}_{10}[{\pi }_{\mathrm{rel}}(\mathrm{mas})]﹩, and ﹩{\mathrm{log}}_{10}[{\theta }_{{\rm{E}}}(\mathrm{mas})]﹩ (left to right). In the bottom panels, self- and halo-lensing events are specified with blue triangles and green circles, respectively.
Paper: Discerning Parallax Amplitude in Astrometric Microlensing
Authors: Sedighe Sajadian, Arya Mahmoudzadeh, Setareh Moein
Figure caption: Two examples of simulated microlensing events that are detectable with the Roman telescope. For each event, the light curve and astrometric deflection are represented (left and right panels). The green and dark red data points are taken by the Roman telescope during its observing seasons and its large seasonal gap, respectively. Their parameters can be found at the top of the panels.
Paper: Discerning Parallax Amplitude in Astrometric Microlensing
Authors: Sedighe Sajadian, Arya Mahmoudzadeh, Setareh Moein
Figure caption: Examples of astrometric deflections in source trajectories in long-duration microlensing events toward the GB (top panels) and LMC (bottom panels) due to ISMBHs by ignoring (solid black curves) and including (dashed blue curves) the parallax effect. The dotted magenta curves are the first term in the astrometric deflection given by Equation (8), i.e., δ  θ  0. Their parameters are given at the top of the panels.
Paper: Discerning Parallax Amplitude in Astrometric Microlensing
Authors: Sedighe Sajadian, Arya Mahmoudzadeh, Setareh Moein
Figure caption: Same as Figure 3 but for observations toward the LMC with LSST. The simulated data points taken by LSST in the ugrizy filters are shown with purple, blue, dark green, yellowish green, orange, and red, respectively. The data taken with the ELT are depicted in dark red. The observing cadences for the LSST and ELT data are 3 and 10 days, respectively.
Paper: Discerning Parallax Amplitude in Astrometric Microlensing
Authors: Sedighe Sajadian, Arya Mahmoudzadeh, Setareh Moein
Figure caption: The NDs of relative errors in the parallax amplitudes, as measured through photometric (green) and astrometric (purple) observations based on simulations (A), (B), and (C), from top to bottom. The dashed black lines determine the threshold amount ﹩{\sigma }_{{\pi }_{{\rm{E}}}}/{\pi }_{{\rm{E}}}=4 \% ﹩. The fractions of events with relative parallax errors of less than 4% are given inside the panels.
Paper: Discerning Parallax Amplitude in Astrometric Microlensing
Authors: Sedighe Sajadian, Arya Mahmoudzadeh, Setareh Moein
Figure caption: Same as Figure 3, but dark red points are hypothetically taken by the ELT in the K band with a 10 day observing cadence.
Paper: Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Authors: Elisa V. Quintana, Emily A. Gilbert, Thomas Barclay, Michele L. Silverstein, Joshua E. Schlieder, Ryan Cloutier, Samuel N. Quinn, Joseph E. Rodriguez, Andrew Vanderburg, Benjamin J. Hord, Dana R. Louie, Colby Ostberg, Stephen R. Kane, Kelsey Hoffman, Jason F. Rowe, Giada N. Arney, Prabal Saxena, Taran Richardson, Matthew S. Clement, Nicholas M. Kartvedt, Fred C. Adams, Marcus Alfred, Travis Berger, Allyson Bieryla, Paul Bonney, Patricia Boyd, Charles Cadieux, Douglas Caldwell, David R. Ciardi, David Charbonneau, Karen A. Collins, Knicole D. Colón, Dennis M. Conti, Mario Di Sora, Shawn Domagal-Goldman, Jessie Dotson, Thomas Fauchez, Erica J. Gonzales, Maximilian N. Günther, Christina Hedges, Giovanni Isopi, Erika Kohler, Ravi Kopparapu, Veselin B. Kostov, Jeffrey A. Larsen, Eric Lopez, Franco Mallia, Avi Mandell, Susan E. Mullally, Rishi R. Paudel, Brian P. Powell, George R. Ricker, Boris S. Safonov, Richard P. Schwarz, Ramotholo Sefako, Keivan G. Stassun, Robert Wilson, Joshua N. Winn, Roland K. Vanderspek
Figure caption: Transmission Spectroscopy Metric (TSM) for the TOI-2095 planets, compared to the TSM for confirmed planets (CP) in the NASA Exoplanet Archive. The color bar indicates other planets within the VZ. We label those planets near the outer edge of the VZ with equilibrium temperatures less than 400 K. Table 5 lists the properties of the eight planets labeled in this figure.
Paper: Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Authors: Elisa V. Quintana, Emily A. Gilbert, Thomas Barclay, Michele L. Silverstein, Joshua E. Schlieder, Ryan Cloutier, Samuel N. Quinn, Joseph E. Rodriguez, Andrew Vanderburg, Benjamin J. Hord, Dana R. Louie, Colby Ostberg, Stephen R. Kane, Kelsey Hoffman, Jason F. Rowe, Giada N. Arney, Prabal Saxena, Taran Richardson, Matthew S. Clement, Nicholas M. Kartvedt, Fred C. Adams, Marcus Alfred, Travis Berger, Allyson Bieryla, Paul Bonney, Patricia Boyd, Charles Cadieux, Douglas Caldwell, David R. Ciardi, David Charbonneau, Karen A. Collins, Knicole D. Colón, Dennis M. Conti, Mario Di Sora, Shawn Domagal-Goldman, Jessie Dotson, Thomas Fauchez, Erica J. Gonzales, Maximilian N. Günther, Christina Hedges, Giovanni Isopi, Erika Kohler, Ravi Kopparapu, Veselin B. Kostov, Jeffrey A. Larsen, Eric Lopez, Franco Mallia, Avi Mandell, Susan E. Mullally, Rishi R. Paudel, Brian P. Powell, George R. Ricker, Boris S. Safonov, Richard P. Schwarz, Ramotholo Sefako, Keivan G. Stassun, Robert Wilson, Joshua N. Winn, Roland K. Vanderspek
Figure caption: There are only two transits for TOI-2095.01 and only one for TOI-2095.02 in this sector, all with fairly low S/N, but there are no indications of false positives. Left: The difference image for TOI-2095 planet 1 for Sector 24, showing the position of the target (black star), the measured difference image photocenters from a point-spread-function and pixel-response-function (cyan triangle and red circle, respectively). Right: PDC SAP light curve of TOI-2059 for Sector 24 highlighting the two transits in the sector. Lower panels: Modshift results from DAVE, left for TOI-2095.01 and right for TOI-2095.02, respectively. The small panels show zoom-ins and corresponding fits to the primary transits, the odd and even transits, the most significant secondary transits, as well as to any additional negative (tertiary) or positive events.
Paper: Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Authors: Elisa V. Quintana, Emily A. Gilbert, Thomas Barclay, Michele L. Silverstein, Joshua E. Schlieder, Ryan Cloutier, Samuel N. Quinn, Joseph E. Rodriguez, Andrew Vanderburg, Benjamin J. Hord, Dana R. Louie, Colby Ostberg, Stephen R. Kane, Kelsey Hoffman, Jason F. Rowe, Giada N. Arney, Prabal Saxena, Taran Richardson, Matthew S. Clement, Nicholas M. Kartvedt, Fred C. Adams, Marcus Alfred, Travis Berger, Allyson Bieryla, Paul Bonney, Patricia Boyd, Charles Cadieux, Douglas Caldwell, David R. Ciardi, David Charbonneau, Karen A. Collins, Knicole D. Colón, Dennis M. Conti, Mario Di Sora, Shawn Domagal-Goldman, Jessie Dotson, Thomas Fauchez, Erica J. Gonzales, Maximilian N. Günther, Christina Hedges, Giovanni Isopi, Erika Kohler, Ravi Kopparapu, Veselin B. Kostov, Jeffrey A. Larsen, Eric Lopez, Franco Mallia, Avi Mandell, Susan E. Mullally, Rishi R. Paudel, Brian P. Powell, George R. Ricker, Boris S. Safonov, Richard P. Schwarz, Ramotholo Sefako, Keivan G. Stassun, Robert Wilson, Joshua N. Winn, Roland K. Vanderspek
Figure caption: Archival imaging of TOI-2095. From left to right, an image from the first Palomar Observatory Sky Survey (POSS-I) in a blue-sensitive emulsion, an image from the second Palomar Observatory Sky Survey (POSS-II) in a blue-sensitive emulsion, an image from the Panoramic Survey Telescope and Rapid Response System (PAN-STARRS) telescope in g-band, and the summed image from TESS during Sector 14. The present-day position of TOI-2095 is shown with a red cross, and in the Pan-STARRS and TESS images, the outline of the TESS photometric aperture from Sector 14 is shown as a solid red line. TOI 2095's high proper motion reveals no background sources at its present-day position that could give rise to the transits we see.
Paper: Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Authors: Elisa V. Quintana, Emily A. Gilbert, Thomas Barclay, Michele L. Silverstein, Joshua E. Schlieder, Ryan Cloutier, Samuel N. Quinn, Joseph E. Rodriguez, Andrew Vanderburg, Benjamin J. Hord, Dana R. Louie, Colby Ostberg, Stephen R. Kane, Kelsey Hoffman, Jason F. Rowe, Giada N. Arney, Prabal Saxena, Taran Richardson, Matthew S. Clement, Nicholas M. Kartvedt, Fred C. Adams, Marcus Alfred, Travis Berger, Allyson Bieryla, Paul Bonney, Patricia Boyd, Charles Cadieux, Douglas Caldwell, David R. Ciardi, David Charbonneau, Karen A. Collins, Knicole D. Colón, Dennis M. Conti, Mario Di Sora, Shawn Domagal-Goldman, Jessie Dotson, Thomas Fauchez, Erica J. Gonzales, Maximilian N. Günther, Christina Hedges, Giovanni Isopi, Erika Kohler, Ravi Kopparapu, Veselin B. Kostov, Jeffrey A. Larsen, Eric Lopez, Franco Mallia, Avi Mandell, Susan E. Mullally, Rishi R. Paudel, Brian P. Powell, George R. Ricker, Boris S. Safonov, Richard P. Schwarz, Ramotholo Sefako, Keivan G. Stassun, Robert Wilson, Joshua N. Winn, Roland K. Vanderspek
Figure caption: Observed minus calculated transit times for TOI-2095 b and c show no significant evidence for TTVs at this time. However, the number of transits is limited, and further observations may reveal a longer superperiod for transit times.
Paper: Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Authors: Elisa V. Quintana, Emily A. Gilbert, Thomas Barclay, Michele L. Silverstein, Joshua E. Schlieder, Ryan Cloutier, Samuel N. Quinn, Joseph E. Rodriguez, Andrew Vanderburg, Benjamin J. Hord, Dana R. Louie, Colby Ostberg, Stephen R. Kane, Kelsey Hoffman, Jason F. Rowe, Giada N. Arney, Prabal Saxena, Taran Richardson, Matthew S. Clement, Nicholas M. Kartvedt, Fred C. Adams, Marcus Alfred, Travis Berger, Allyson Bieryla, Paul Bonney, Patricia Boyd, Charles Cadieux, Douglas Caldwell, David R. Ciardi, David Charbonneau, Karen A. Collins, Knicole D. Colón, Dennis M. Conti, Mario Di Sora, Shawn Domagal-Goldman, Jessie Dotson, Thomas Fauchez, Erica J. Gonzales, Maximilian N. Günther, Christina Hedges, Giovanni Isopi, Erika Kohler, Ravi Kopparapu, Veselin B. Kostov, Jeffrey A. Larsen, Eric Lopez, Franco Mallia, Avi Mandell, Susan E. Mullally, Rishi R. Paudel, Brian P. Powell, George R. Ricker, Boris S. Safonov, Richard P. Schwarz, Ramotholo Sefako, Keivan G. Stassun, Robert Wilson, Joshua N. Winn, Roland K. Vanderspek
Figure caption: Folded TOI-2095 b and c transits observed by TESS. The gray points are the observed data, folded on the best-fitting orbital period, the blue dots are binned data, and the orange curve is the best-fitting transit model.
Paper: Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Authors: Elisa V. Quintana, Emily A. Gilbert, Thomas Barclay, Michele L. Silverstein, Joshua E. Schlieder, Ryan Cloutier, Samuel N. Quinn, Joseph E. Rodriguez, Andrew Vanderburg, Benjamin J. Hord, Dana R. Louie, Colby Ostberg, Stephen R. Kane, Kelsey Hoffman, Jason F. Rowe, Giada N. Arney, Prabal Saxena, Taran Richardson, Matthew S. Clement, Nicholas M. Kartvedt, Fred C. Adams, Marcus Alfred, Travis Berger, Allyson Bieryla, Paul Bonney, Patricia Boyd, Charles Cadieux, Douglas Caldwell, David R. Ciardi, David Charbonneau, Karen A. Collins, Knicole D. Colón, Dennis M. Conti, Mario Di Sora, Shawn Domagal-Goldman, Jessie Dotson, Thomas Fauchez, Erica J. Gonzales, Maximilian N. Günther, Christina Hedges, Giovanni Isopi, Erika Kohler, Ravi Kopparapu, Veselin B. Kostov, Jeffrey A. Larsen, Eric Lopez, Franco Mallia, Avi Mandell, Susan E. Mullally, Rishi R. Paudel, Brian P. Powell, George R. Ricker, Boris S. Safonov, Richard P. Schwarz, Ramotholo Sefako, Keivan G. Stassun, Robert Wilson, Joshua N. Winn, Roland K. Vanderspek
Figure caption: An estimated transmission spectrum of TOI-2095 b with a 10 bar, cloudless Venus-like atmosphere (upper plot), and simulated JWST data of the same planet assuming 100 transit observations (lower plot). Note that the black line is the same spectrum in both the upper and lower plots, but the scale of the y-axis is larger in the lower plot to capture the uncertainty in the simulated JWST data.
Paper: Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Authors: Elisa V. Quintana, Emily A. Gilbert, Thomas Barclay, Michele L. Silverstein, Joshua E. Schlieder, Ryan Cloutier, Samuel N. Quinn, Joseph E. Rodriguez, Andrew Vanderburg, Benjamin J. Hord, Dana R. Louie, Colby Ostberg, Stephen R. Kane, Kelsey Hoffman, Jason F. Rowe, Giada N. Arney, Prabal Saxena, Taran Richardson, Matthew S. Clement, Nicholas M. Kartvedt, Fred C. Adams, Marcus Alfred, Travis Berger, Allyson Bieryla, Paul Bonney, Patricia Boyd, Charles Cadieux, Douglas Caldwell, David R. Ciardi, David Charbonneau, Karen A. Collins, Knicole D. Colón, Dennis M. Conti, Mario Di Sora, Shawn Domagal-Goldman, Jessie Dotson, Thomas Fauchez, Erica J. Gonzales, Maximilian N. Günther, Christina Hedges, Giovanni Isopi, Erika Kohler, Ravi Kopparapu, Veselin B. Kostov, Jeffrey A. Larsen, Eric Lopez, Franco Mallia, Avi Mandell, Susan E. Mullally, Rishi R. Paudel, Brian P. Powell, George R. Ricker, Boris S. Safonov, Richard P. Schwarz, Ramotholo Sefako, Keivan G. Stassun, Robert Wilson, Joshua N. Winn, Roland K. Vanderspek
Figure caption: Speckle SAI image of TOI-2095 (inset) and contrast curve.
Paper: Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Authors: Elisa V. Quintana, Emily A. Gilbert, Thomas Barclay, Michele L. Silverstein, Joshua E. Schlieder, Ryan Cloutier, Samuel N. Quinn, Joseph E. Rodriguez, Andrew Vanderburg, Benjamin J. Hord, Dana R. Louie, Colby Ostberg, Stephen R. Kane, Kelsey Hoffman, Jason F. Rowe, Giada N. Arney, Prabal Saxena, Taran Richardson, Matthew S. Clement, Nicholas M. Kartvedt, Fred C. Adams, Marcus Alfred, Travis Berger, Allyson Bieryla, Paul Bonney, Patricia Boyd, Charles Cadieux, Douglas Caldwell, David R. Ciardi, David Charbonneau, Karen A. Collins, Knicole D. Colón, Dennis M. Conti, Mario Di Sora, Shawn Domagal-Goldman, Jessie Dotson, Thomas Fauchez, Erica J. Gonzales, Maximilian N. Günther, Christina Hedges, Giovanni Isopi, Erika Kohler, Ravi Kopparapu, Veselin B. Kostov, Jeffrey A. Larsen, Eric Lopez, Franco Mallia, Avi Mandell, Susan E. Mullally, Rishi R. Paudel, Brian P. Powell, George R. Ricker, Boris S. Safonov, Richard P. Schwarz, Ramotholo Sefako, Keivan G. Stassun, Robert Wilson, Joshua N. Winn, Roland K. Vanderspek
Figure caption: Two transits of TOI-2095 observed by LCOGT. The upper panel shows the partial transit of planet b and the lower panel shows the full transit of planet c.
Paper: Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Authors: Elisa V. Quintana, Emily A. Gilbert, Thomas Barclay, Michele L. Silverstein, Joshua E. Schlieder, Ryan Cloutier, Samuel N. Quinn, Joseph E. Rodriguez, Andrew Vanderburg, Benjamin J. Hord, Dana R. Louie, Colby Ostberg, Stephen R. Kane, Kelsey Hoffman, Jason F. Rowe, Giada N. Arney, Prabal Saxena, Taran Richardson, Matthew S. Clement, Nicholas M. Kartvedt, Fred C. Adams, Marcus Alfred, Travis Berger, Allyson Bieryla, Paul Bonney, Patricia Boyd, Charles Cadieux, Douglas Caldwell, David R. Ciardi, David Charbonneau, Karen A. Collins, Knicole D. Colón, Dennis M. Conti, Mario Di Sora, Shawn Domagal-Goldman, Jessie Dotson, Thomas Fauchez, Erica J. Gonzales, Maximilian N. Günther, Christina Hedges, Giovanni Isopi, Erika Kohler, Ravi Kopparapu, Veselin B. Kostov, Jeffrey A. Larsen, Eric Lopez, Franco Mallia, Avi Mandell, Susan E. Mullally, Rishi R. Paudel, Brian P. Powell, George R. Ricker, Boris S. Safonov, Richard P. Schwarz, Ramotholo Sefako, Keivan G. Stassun, Robert Wilson, Joshua N. Winn, Roland K. Vanderspek
Figure caption: Keck II NIRC2 K-band adaptive optics image of TOI-2095 (inset) and contrast curve. No faint companions were detected down to 6 mag of contrast at separations of 0.″2 and 7.″5 mag at separations >0.″5
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Sodium amplitude from the transmission spectra of WASP-6b (red diamonds; Nikolov et al. 2015; Carter et al. 2020), WASP-96b (blue stars; Nikolov et al. 2018; McGruder et al. 2022), and WASP-110b (green circles; Nikolov et al. 2021) vs. their host-star metallicities. In McGruder et al. (2023), “Na I Amplitude” was the depth of the bin centered around the Na feature minus the average depth of all bins in the surrounding continuum. Here we take that value and divide it by the theoretical difference of the peak depth from Na and the continuum, in order to incorporate slight differences in the planets’ scale heights and temperature. scipy.odr was used to obtain a weighted linear fit with these three planetary signals and is shown as a dashed blue line. Its regression score, R 2, is 0.75. The 1σ interval of the fit is shaded around the dashed line and was calculated including the uncertainties in both metallicity and Na signal. Using the same method for WASP-6b and WASP-110b (i.e., average R  p /R  s  centered at 5892.9 Å minus average R  p /R  s  within 5340–5820 Å and 5960–6440 Å), we calculated the Na signals of WASP-25b (purple squares) and WASP-124b (purple triangles). A weighted linear fit with all five planet signals is shown as a purple dashed–dotted line, with an R 2 of 0.71. Although our new measurements have larger uncertainties they are consistent with the trend identified in McGruder et al. (2023). The metallicity range of WASP-55b and HATS-29b are plotted as yellow shaded regions.
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Light curves (LCs) in each step of the detrending process when utilizing the CMC+Poly method (see Section 3.2), for each bin of transit UT180329. Left: LC produced from the quotient of the WASP-25 and comparison LCs. For all other transits there are multiple comparisons; in that situation the sum of comparison light curves is used instead. The wavelength range [nm] used is printed in the bottom left regions. Middle: quotient of the LCs on the left and common-mode correction term. Overplotted in violet is the best-fit polynomial correction term. If there were any frames clipped for a given bin, it is marked with a black x and the total number of clipped values is in the lower left regions. The precision, assuming only photon noise, is printed as  σ  w . Right: final detrended LC with the best-fit transit model overplotted in violet. The standard deviations of the residuals (σ  r ) and σ  r /σ  w  (β) are printed. The error bars shown are determined by multiplying the photon noise precision of each frame by the β for that bin.
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Left: LCs in each step of the detrending process when utilizing the PCA+GP method (see Sections 3), for each bin of transit UT180915. Each column shows on the left the raw LCs produced directly from the extracted spectrum in Figure 1, in the middle the binned transit LCs of WASP-124b corrected with PCA (the best GP systematic fits are overplotted in violet), and on the right the final detrended LC with the best-fit transit model overplotted in violet. The best-fit GP jitter term was used to approximate the error bars shown in the middle and right columns. The wavelength ranges used, clipped frames, photon noise precisions, standard deviations of residuals, and β are printed on the figures just as in Figure 6. Right: same as Figure 6 but for transit UT190826.
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Final transmission spectra of WASP-25b (top) and WASP-124b (bottom). The final weighted-average spectra are shown in violet for WASP-25 and blue for WASP-124, with their individual transmission spectra used for the combined spectra plotted in transparent colors. The best-fit PLATON retrieval models are plotted as a black line with the 1σ confidence interval highlighted in light blue. For both targets the best-fit models are the ones that just include activity, but in the case of WASP-124b, this model is not significantly preferred over any other model.
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Same as Figure 6 but for transit UT211002 (left) and transit UT220605 (right).
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Left: same as Figure 6 but for transit UT210809. Right: same left side of Figure 9 but for transit UT210905.
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Same as Figure 6 but for transits UT210306 (left) and UT220325 (right).